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1. Achievement of the Planetary Defense Investigations of the Double Asteroid Redirection Test (DART) Mission

Author: Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Chabot, Nancy, Rivkin, Andy, Cheng, Andy F., Barnouin, Olivier, Fahnestock, Eugene G., Richardson, Derek C., Stickle, Angela M., Thomas, Cristina, Ernst, Carolyn, Daly, R. Terik, Dotto, Elisabetta, Rizos, Juan L., Rossi, Alessandro, Roth, Nathan X., Rożek, Agata, Rozitis, Benjamin, Ryan, Eileen, Ryan, William, Sánchez, Paul, Santana-Ros, Toni, Scheeres, Daniel J., Zinzi, Angelo, Scheirich, Peter, Senel, Cem Berk, Snodgrass, Colin, Soldini, Stefania, Souami, Damya, Statler, Thomas S., Street, Rachel, Stubbs, Timothy J., Sunshine, Jessica M., Tan, Nicole J., Chesley, Steven, Tancredi, Gonzalo, Tinsman, Calley L., Tortora, Paolo, Tusberti, Filippo, Walker, James D., Waller, C. Dany, Wünnemann, Kai, Zannoni, Marco, Zhang, Yun, Moskovitz, Nicholas A., Barbee, Brent, Abell, Paul, Agrusa, Harrison F., Bannister, Michele T., Beccarelli, Joel, Bekker, Dmitriy L., Bruck Syal, Megan, Buratti, Bonnie J., Busch, Michael W., Campo Bagatin, Adriano, Chatelain, Joseph, Chocron, Sidney, Collins, Gareth S., Conversi, Luca, Davison, Thomas M., DeCoster, Mallory E., Deshapriya, J. D. Prasanna, Eggl, Siegfried, Espiritu, Raymond C., Farnham, Tony, Ferrais, Marin, Ferrari, Fabio, Föhring, Dora, Fuentes-Muñoz, Oscar, Gai, Igor, Giordano, Carmine, Glenar, David A., Gomez, Edward, Graninger, Dawn M., Green, Simon F., Greenstreet, Sarah, Hasselmann, Pedro H., Herreros, Isabel, Hirabayashi, Masatoshi, Husárik, Marek, Ieva, Simone, Ivanovski, Stavro, Jackson, Samuel L., Jehin, Emmanuel, Jutzi, Martin, Karatekin, Ozgür, Knight, Matthew M., Kolokolova, Ludmilla, Kumamoto, Kathryn M., Küppers, Michael, La Forgia, Fiorangela, Lazzarin, Monica, Li, Jian-Yang, Lister, Tim, Lolachi, Ramin, Lucas, Michael P., Lucchetti, Alice, Luther, Robert, Makadia, Rahil, Mazzotta Epifani, Elena, McMahon, Jay, Merisio, Gianmario, Merrill, Colby C., Meyer, Alex J., Michel, Patrick, Micheli, Marco, Migliorini, Alessandra, Minker, Kate, Modenini, Dario, Moreno, Fernando, Murdoch, Naomi, Murphy, Brian, Naidu, Shantanu P., Nair, Hari, Nakano, Ryota, Opitom, Cyrielle, Ormö, Jens, Owen, J. Michael, Pajola, Maurizio, Palmer, Eric E., Palumbo, Pasquale, Panicucci, Paolo, Parro, Laura M., Pearl, Jason M., Penttila, Antti, Perna, Davide, Petrescu, Elisabeta, Pravec, Petr, Raducan, Sabina D., Ramesh, K. T., Ridden-Harper, Ryan, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Chabot, Nancy, Rivkin, Andy, Cheng, Andy F., Barnouin, Olivier, Fahnestock, Eugene G., Richardson, Derek C., Stickle, Angela M., Thomas, Cristina, Ernst, Carolyn, Daly, R. Terik, Dotto, Elisabetta, Rizos, Juan L., Rossi, Alessandro, Roth, Nathan X., Rożek, Agata, Rozitis, Benjamin, Ryan, Eileen, Ryan, William, Sánchez, Paul, Santana-Ros, Toni, Scheeres, Daniel J., Zinzi, Angelo, Scheirich, Peter, Senel, Cem Berk, Snodgrass, Colin, Soldini, Stefania, Souami, Damya, Statler, Thomas S., Street, Rachel, Stubbs, Timothy J., Sunshine, Jessica M., Tan, Nicole J., Chesley, Steven, Tancredi, Gonzalo, Tinsman, Calley L., Tortora, Paolo, Tusberti, Filippo, Walker, James D., Waller, C. Dany, Wünnemann, Kai, Zannoni, Marco, Zhang, Yun, Moskovitz, Nicholas A., Barbee, Brent, Abell, Paul, Agrusa, Harrison F., Bannister, Michele T., Beccarelli, Joel, Bekker, Dmitriy L., Bruck Syal, Megan, Buratti, Bonnie J., Busch, Michael W., Campo Bagatin, Adriano, Chatelain, Joseph, Chocron, Sidney, Collins, Gareth S., Conversi, Luca, Davison, Thomas M., DeCoster, Mallory E., Deshapriya, J. D. Prasanna, Eggl, Siegfried, Espiritu, Raymond C., Farnham, Tony, Ferrais, Marin, Ferrari, Fabio, Föhring, Dora, Fuentes-Muñoz, Oscar, Gai, Igor, Giordano, Carmine, Glenar, David A., Gomez, Edward, Graninger, Dawn M., Green, Simon F., Greenstreet, Sarah, Hasselmann, Pedro H., Herreros, Isabel, Hirabayashi, Masatoshi, Husárik, Marek, Ieva, Simone, Ivanovski, Stavro, Jackson, Samuel L., Jehin, Emmanuel, Jutzi, Martin, Karatekin, Ozgür, Knight, Matthew M., Kolokolova, Ludmilla, Kumamoto, Kathryn M., Küppers, Michael, La Forgia, Fiorangela, Lazzarin, Monica, Li, Jian-Yang, Lister, Tim, Lolachi, Ramin, Lucas, Michael P., Lucchetti, Alice, Luther, Robert, Makadia, Rahil, Mazzotta Epifani, Elena, McMahon, Jay, Merisio, Gianmario, Merrill, Colby C., Meyer, Alex J., Michel, Patrick, Micheli, Marco, Migliorini, Alessandra, Minker, Kate, Modenini, Dario, Moreno, Fernando, Murdoch, Naomi, Murphy, Brian, Naidu, Shantanu P., Nair, Hari, Nakano, Ryota, Opitom, Cyrielle, Ormö, Jens, Owen, J. Michael, Pajola, Maurizio, Palmer, Eric E., Palumbo, Pasquale, Panicucci, Paolo, Parro, Laura M., Pearl, Jason M., Penttila, Antti, Perna, Davide, Petrescu, Elisabeta, Pravec, Petr, Raducan, Sabina D., Ramesh, K. T., and Ridden-Harper, Ryan
Published: 2024

2. Characterization of the Surfaces and Near-Surface Atmospheres of Ganymede, Europa and Callisto by JUICE

Author: Tosi, Federico, Roatsch, Thomas, Galli, Andre, Hauber, Ernst, Lucchetti, Alice, Molyneux, Philippa, Stephan, Katrin, Achilleos, Nicholas, Bovolo, Francesca, Carter, John, Cavalie, Thibault, Cimo, Giuseppe, D'Aversa, Emiliano, Gwinner, Klaus, Hartogh, Paul, Huybrighs, Hans, Langevin, Yves, Lellouch, Emmanuel, Migliorini, Alessandra, Palumbo, Pasquale, Piccioni, Giuseppe, Plaut, Jeffrey J., Postberg, Frank, Poulet, Francois, Retherford, Kurt, Rezac, Ladislav, Roth, Lorenz, Solomonidou, Anezina, Tobie, Gabriel, Tortora, Paolo, Tubiana, Cecilia, Wagner, Roland, Wirström, Eva, Wurz, Peter, Zambon, Francesca, Zannoni, Marco, Barabash, Stas, Bruzzone, Lorenzo, Dougherty, Michele, Gladstone, Randy, Gurvits, Leonid I., Hussmann, Hauke, Iess, Luciano, Wahlund, Jan-Erik, Witasse, Olivier, Vallat, Claire, Lorente, Rosario, Tosi, Federico, Roatsch, Thomas, Galli, Andre, Hauber, Ernst, Lucchetti, Alice, Molyneux, Philippa, Stephan, Katrin, Achilleos, Nicholas, Bovolo, Francesca, Carter, John, Cavalie, Thibault, Cimo, Giuseppe, D'Aversa, Emiliano, Gwinner, Klaus, Hartogh, Paul, Huybrighs, Hans, Langevin, Yves, Lellouch, Emmanuel, Migliorini, Alessandra, Palumbo, Pasquale, Piccioni, Giuseppe, Plaut, Jeffrey J., Postberg, Frank, Poulet, Francois, Retherford, Kurt, Rezac, Ladislav, Roth, Lorenz, Solomonidou, Anezina, Tobie, Gabriel, Tortora, Paolo, Tubiana, Cecilia, Wagner, Roland, Wirström, Eva, Wurz, Peter, Zambon, Francesca, Zannoni, Marco, Barabash, Stas, Bruzzone, Lorenzo, Dougherty, Michele, Gladstone, Randy, Gurvits, Leonid I., Hussmann, Hauke, Iess, Luciano, Wahlund, Jan-Erik, Witasse, Olivier, Vallat, Claire, and Lorente, Rosario
Abstract: We present the state of the art on the study of surfaces and tenuous atmospheres of the icy Galilean satellites Ganymede, Europa and Callisto, from past and ongoing space exploration conducted with several spacecraft to recent telescopic observations, and we show how the ESA JUICE mission plans to explore these surfaces and atmospheres in detail with its scientific payload. The surface geology of the moons is the main evidence of their evolution and reflects the internal heating provided by tidal interactions. Surface composition is the result of endogenous and exogenous processes, with the former providing valuable information about the potential composition of shallow subsurface liquid pockets, possibly connected to deeper oceans. Finally, the icy Galilean moons have tenuous atmospheres that arise from charged particle sputtering affecting their surfaces. In the case of Europa, plumes of water vapour have also been reported, whose phenomenology at present is poorly understood and requires future close exploration. In the three main sections of the article, we discuss these topics, highlighting the key scientific objectives and investigations to be achieved by JUICE. Based on a recent predicted trajectory, we also show potential coverage maps and other examples of reference measurements. The scientific discussion and observation planning presented here are the outcome of the JUICE Working Group 2 (WG2): "Surfaces and Near-surface Exospheres of the Satellites, dust and rings".
Published: 2024
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3. Geophysical Characterization of the Interiors of Ganymede, Callisto and Europa by ESA's JUpiter ICy moons Explorer

Author: Van Hoolst, Tim, Tobie, Gabriel, Vallat, Claire, Altobelli, Nicolas, Bruzzone, Lorenzo, Cao, Hao, Dirkx, Dominic, Genova, Antonio, Hussmann, Hauke, Iess, Luciano, Kimura, Jun, Khurana, Krishan, Lucchetti, Alice, Mitri, Giuseppe, Moore, William, Saur, Joachim, Stark, Alexander, Vorburger, Audrey, Wieczorek, Mark, Aboudan, Alessio, Bergman, Jan, Bovolo, Francesca, Breuer, Doris, Cappuccio, Paolo, Carrer, Leonardo, Cecconi, Baptiste, Choblet, Gaël, De Marchi, Fabrizio, Fayolle, Marie, Fienga, Agnès, Futaana, Yoshifumi, Hauber, Ernst, Kofman, Wlodek, Kumamoto, Atsushi, Lainey, Valery, Molyneux, Philippa, Mousis, Olivier, Plaut, Jeff, Puccio, Walter, Retherford, Kurt, Roth, Lorenz, Seignovert, Benoit, Steinbrügge, Gregor, Thakur, Sanchari, Tortora, Paolo, Tosi, Federico, Zannoni, Marco, Barabash, Stas, Dougherty, Michele, Gladstone, Randy, Gurvits, Leonid I., Hartogh, Paul, Palumbo, Pasquale, Poulet, Francois, Wahlund, Jan-Erik, Grasset, Olivier, Witasse, Olivier, Van Hoolst, Tim, Tobie, Gabriel, Vallat, Claire, Altobelli, Nicolas, Bruzzone, Lorenzo, Cao, Hao, Dirkx, Dominic, Genova, Antonio, Hussmann, Hauke, Iess, Luciano, Kimura, Jun, Khurana, Krishan, Lucchetti, Alice, Mitri, Giuseppe, Moore, William, Saur, Joachim, Stark, Alexander, Vorburger, Audrey, Wieczorek, Mark, Aboudan, Alessio, Bergman, Jan, Bovolo, Francesca, Breuer, Doris, Cappuccio, Paolo, Carrer, Leonardo, Cecconi, Baptiste, Choblet, Gaël, De Marchi, Fabrizio, Fayolle, Marie, Fienga, Agnès, Futaana, Yoshifumi, Hauber, Ernst, Kofman, Wlodek, Kumamoto, Atsushi, Lainey, Valery, Molyneux, Philippa, Mousis, Olivier, Plaut, Jeff, Puccio, Walter, Retherford, Kurt, Roth, Lorenz, Seignovert, Benoit, Steinbrügge, Gregor, Thakur, Sanchari, Tortora, Paolo, Tosi, Federico, Zannoni, Marco, Barabash, Stas, Dougherty, Michele, Gladstone, Randy, Gurvits, Leonid I., Hartogh, Paul, Palumbo, Pasquale, Poulet, Francois, Wahlund, Jan-Erik, Grasset, Olivier, and Witasse, Olivier
Abstract: The JUpiter ICy moons Explorer (JUICE) of ESA was launched on 14 April 2023 and will arrive at Jupiter and its moons in July 2031. In this review article, we describe how JUICE will investigate the interior of the three icy Galilean moons, Ganymede, Callisto and Europa, during its Jupiter orbital tour and the final orbital phase around Ganymede. Detailed geophysical observations about the interior of the moons can only be performed from close distances to the moons, and best estimates of signatures of the interior, such as an induced magnetic field, tides and rotation variations, and radar reflections, will be obtained during flybys of the moons with altitudes of about 1000 km or less and during the Ganymede orbital phase at an average altitude of 490 km. The 9-month long orbital phase around Ganymede, the first of its kind around another moon than our Moon, will allow an unprecedented and detailed insight into the moon's interior, from the central regions where a magnetic field is generated to the internal ocean and outer ice shell. Multiple flybys of Callisto will clarify the differences in evolution compared to Ganymede and will provide key constraints on the origin and evolution of the Jupiter system. JUICE will visit Europa only during two close flybys and the geophysical investigations will focus on selected areas of the ice shell. A prime goal of JUICE is the characterisation of the ice shell and ocean of the Galilean moons, and we here specifically emphasise the synergistic aspects of the different geophysical investigations, showing how different instruments will work together to probe the hydrosphere. We also describe how synergies between JUICE instruments will contribute to the assessment of the deep interior of the moons, their internal differentiation, dynamics and evolution. In situ measurements and remote sensing observations will support the geophysical instruments to achieve these goals, but will also, together with subsurface radar sounding, provi
Published: 2024
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4. The Dimorphos ejecta plume properties revealed by LICIACube

Author: Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Dotto, Elisabetta, Deshapriya, J. D. Prasanna, Gai, Igor, Hasselmann, Pedro H., Mazzotta Epifani, Elena, Poggiali, Giovanni, Rossi, Alessandro, Zanotti, Giovanni, Zinzi, Angelo, Bertini, Ivano, Brucato, John Robert, Dall’Ora, Massimo, Della Corte, Vincenzo, Ivanovski, Stavro, Lucchetti, Alice, Pajola, Maurizio, Amoroso, Marilena, Barnouin, Olivier, Campo Bagatin, Adriano, Capannolo, Andrea, Caporali, S., Ceresoli, M., Chabot, Nancy, Cheng, Andy F., Cremonese, Gabriele, Fahnestock, Eugene G., Farnham, Tony, Ferrari, Fabio, Gomez Casajus, L., Gramigna, Edoardo, Hirabayashi, Masatoshi, Ieva, Simone, Impresario, Gabriele, Jutzi, Martin, Lasagni Manghi, Riccardo, Lavagna, Michèle, Li, Jian-Yang, Lombardo, M., Modenini, Dario, Palumbo, Pasquale, Perna, Davide, Pirrotta, Simone, Raducan, Sabina D., Richardson, Derek C., Rivkin, Andy, Stickle, Angela M., Sunshine, Jessica M., Tortora, Paolo, Tusberti, Filippo, Zannoni, Marco, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Dotto, Elisabetta, Deshapriya, J. D. Prasanna, Gai, Igor, Hasselmann, Pedro H., Mazzotta Epifani, Elena, Poggiali, Giovanni, Rossi, Alessandro, Zanotti, Giovanni, Zinzi, Angelo, Bertini, Ivano, Brucato, John Robert, Dall’Ora, Massimo, Della Corte, Vincenzo, Ivanovski, Stavro, Lucchetti, Alice, Pajola, Maurizio, Amoroso, Marilena, Barnouin, Olivier, Campo Bagatin, Adriano, Capannolo, Andrea, Caporali, S., Ceresoli, M., Chabot, Nancy, Cheng, Andy F., Cremonese, Gabriele, Fahnestock, Eugene G., Farnham, Tony, Ferrari, Fabio, Gomez Casajus, L., Gramigna, Edoardo, Hirabayashi, Masatoshi, Ieva, Simone, Impresario, Gabriele, Jutzi, Martin, Lasagni Manghi, Riccardo, Lavagna, Michèle, Li, Jian-Yang, Lombardo, M., Modenini, Dario, Palumbo, Pasquale, Perna, Davide, Pirrotta, Simone, Raducan, Sabina D., Richardson, Derek C., Rivkin, Andy, Stickle, Angela M., Sunshine, Jessica M., Tortora, Paolo, Tusberti, Filippo, and Zannoni, Marco
Abstract: The Double Asteroid Redirection Test (DART) had an impact with Dimorphos (a satellite of the asteroid Didymos) on 26 September 20221. Ground-based observations showed that the Didymos system brightened by a factor of 8.3 after the impact because of ejecta, returning to the pre-impact brightness 23.7 days afterwards2. Hubble Space Telescope observations made from 15 minutes after impact to 18.5 days after, with a spatial resolution of 2.1 kilometres per pixel, showed a complex evolution of the ejecta3, consistent with other asteroid impact events. The momentum enhancement factor, determined using the measured binary period change4, ranges between 2.2 and 4.9, depending on the assumptions about the mass and density of Dimorphos5. Here we report observations from the LUKE and LEIA instruments on the LICIACube cube satellite, which was deployed 15 days in advance of the impact of DART. Data were taken from 71 seconds before the impact until 320 seconds afterwards. The ejecta plume was a cone with an aperture angle of 140 ± 4 degrees. The inner region of the plume was blue, becoming redder with increasing distance from Dimorphos. The ejecta plume exhibited a complex and inhomogeneous structure, characterized by filaments, dust grains and single or clustered boulders. The ejecta velocities ranged from a few tens of metres per second to about 500 metres per second.
Published: 2024

5. The bearing capacity of asteroid (65803) Didymos estimated from boulder tracks

Author: Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Bigot, Jeanne, Lombardo, Pauline, Murdoch, Naomi, Scheeres, Daniel J., Vivet, Damien, Zhang, Yun, Sunshine, Jessica M., Vincent, Jean-Baptiste, Barnouin, Olivier, Ernst, Carolyn, Daly, R. Terik, Sunday, Cecily, Michel, Patrick, Campo Bagatin, Adriano, Lucchetti, Alice, Pajola, Maurizio, Rivkin, Andy, Chabot, Nancy, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Bigot, Jeanne, Lombardo, Pauline, Murdoch, Naomi, Scheeres, Daniel J., Vivet, Damien, Zhang, Yun, Sunshine, Jessica M., Vincent, Jean-Baptiste, Barnouin, Olivier, Ernst, Carolyn, Daly, R. Terik, Sunday, Cecily, Michel, Patrick, Campo Bagatin, Adriano, Lucchetti, Alice, Pajola, Maurizio, Rivkin, Andy, and Chabot, Nancy
Abstract: The bearing capacity - the ability of a surface to support applied loads - is an important parameter for understanding and predicting the response of a surface. Previous work has inferred the bearing capacity and trafficability of specific regions of the Moon using orbital imagery and measurements of the boulder tracks visible on its surface. Here, we estimate the bearing capacity of the surface of an asteroid for the first time using DART/DRACO images of suspected boulder tracks on the surface of asteroid (65803) Didymos. Given the extremely low surface gravity environment, special attention is paid to the underlying assumptions of the geotechnical approach. The detailed analysis of the boulder tracks indicates that the boulders move from high to low gravitational potential, and provides constraints on whether the boulders may have ended their surface motion by entering a ballistic phase. From the 9 tracks identified with sufficient resolution to estimate their dimensions, we find an average boulder track width and length of 8.9 1.5 m and 51.6 13.3 m, respectively. From the track widths, the mean bearing capacity of Didymos is estimated to be 70 N/m2, implying that every 1 m2 of Didymos’ surface at the track location can support only ~70 N of force before experiencing general shear failure. This value is at least 3 orders of magnitude less than the bearing capacity of dry sand on Earth, or lunar regolith.
Published: 2024

6. Fast boulder fracturing by thermal fatigue detected on stony asteroids

Author: Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Lucchetti, Alice, Cambioni, Saverio, Nakano, Ryota, Barnouin, Olivier, Pajola, Maurizio, Penasa, L., Tusberti, Filippo, Ramesh, K. T., Dotto, Elisabetta, Ernst, Carolyn, Daly, R. Terik, Mazzotta Epifani, Elena, Hirabayashi, Masatoshi, Parro, Laura M., Poggiali, Giovanni, Campo Bagatin, Adriano, Ballouz, Ronald-Louis, Chabot, Nancy, Michel, Patrick, Murdoch, Naomi, Vincent, Jean-Baptiste, Karatekin, Ozgür, Rivkin, Andy, Sunshine, Jessica M., Kohout, Tomas, Deshapriya, J. D. Prasanna, Hasselmann, Pedro H., Ieva, Simone, Beccarelli, Joel, Ivanovski, Stavro, Rossi, Alessandro, Ferrari, Fabio, Rossi, C., Raducan, Sabina D., Steckloff, Jordan, Schwartz, Stephen R., Brucato, John Robert, Dall’Ora, Massimo, Zinzi, Angelo, Cheng, Andy F., Amoroso, Marilena, Bertini, Ivano, Capannolo, Andrea, Caporali, S., Ceresoli, M., Cremonese, Gabriele, Della Corte, Vincenzo, Gai, Igor, Gomez Casajus, L., Gramigna, Edoardo, Impresario, Gabriele, Lasagni Manghi, Riccardo, Lavagna, Michèle, Lombardo, M., Modenini, Dario, Palumbo, Pasquale, Perna, Davide, Pirrotta, Simone, Tortora, Paolo, Zannoni, Marco, Zanotti, Giovanni, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Lucchetti, Alice, Cambioni, Saverio, Nakano, Ryota, Barnouin, Olivier, Pajola, Maurizio, Penasa, L., Tusberti, Filippo, Ramesh, K. T., Dotto, Elisabetta, Ernst, Carolyn, Daly, R. Terik, Mazzotta Epifani, Elena, Hirabayashi, Masatoshi, Parro, Laura M., Poggiali, Giovanni, Campo Bagatin, Adriano, Ballouz, Ronald-Louis, Chabot, Nancy, Michel, Patrick, Murdoch, Naomi, Vincent, Jean-Baptiste, Karatekin, Ozgür, Rivkin, Andy, Sunshine, Jessica M., Kohout, Tomas, Deshapriya, J. D. Prasanna, Hasselmann, Pedro H., Ieva, Simone, Beccarelli, Joel, Ivanovski, Stavro, Rossi, Alessandro, Ferrari, Fabio, Rossi, C., Raducan, Sabina D., Steckloff, Jordan, Schwartz, Stephen R., Brucato, John Robert, Dall’Ora, Massimo, Zinzi, Angelo, Cheng, Andy F., Amoroso, Marilena, Bertini, Ivano, Capannolo, Andrea, Caporali, S., Ceresoli, M., Cremonese, Gabriele, Della Corte, Vincenzo, Gai, Igor, Gomez Casajus, L., Gramigna, Edoardo, Impresario, Gabriele, Lasagni Manghi, Riccardo, Lavagna, Michèle, Lombardo, M., Modenini, Dario, Palumbo, Pasquale, Perna, Davide, Pirrotta, Simone, Tortora, Paolo, Zannoni, Marco, and Zanotti, Giovanni
Abstract: Spacecraft observations revealed that rocks on carbonaceous asteroids, which constitute the most numerous class by composition, can develop millimeter-to-meter-scale fractures due to thermal stresses. However, signatures of this process on the second-most populous group of asteroids, the S-complex, have been poorly constrained. Here, we report observations of boulders’ fractures on Dimorphos, which is the moonlet of the S-complex asteroid (65803) Didymos, the target of NASA’s Double Asteroid Redirection Test (DART) planetary defense mission. We show that the size-frequency distribution and orientation of the mapped fractures are consistent with formation through thermal fatigue. The fractures’ preferential orientation supports that these have originated in situ on Dimorphos boulders and not on Didymos boulders later transferred to Dimorphos. Based on our model of the fracture propagation, we propose that thermal fatigue on rocks exposed on the surface of S-type asteroids can form shallow, horizontally propagating fractures in much shorter timescales (100 kyr) than in the direction normal to the boulder surface (order of Myrs). The presence of boulder fields affected by thermal fracturing on near-Earth asteroid surfaces may contribute to an enhancement in the ejected mass and momentum from kinetic impactors when deflecting asteroids.
Published: 2024

7. Evidence for multi-fragmentation and mass shedding of boulders on rubble-pile binary asteroid system (65803) Didymos

Author: Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Pajola, Maurizio, Tusberti, Filippo, Lucchetti, Alice, Barnouin, Olivier, Cambioni, Saverio, Ernst, Carolyn, Dotto, Elisabetta, Daly, R. Terik, Poggiali, Giovanni, Hirabayashi, Masatoshi, Nakano, Ryota, Mazzotta Epifani, Elena, Chabot, Nancy, Della Corte, Vincenzo, Rivkin, Andy, Agrusa, Harrison F., Zhang, Yun, Penasa, L., Ballouz, Ronald-Louis, Ivanovski, Stavro, Murdoch, Naomi, Rossi, Alessandro, Robin, Colas Q., Ieva, Simone, Vincent, Jean-Baptiste, Ferrari, Fabio, Raducan, Sabina D., Campo Bagatin, Adriano, Parro, Laura M., Benavídez, Paula Gabriela, Tancredi, Gonzalo, Karatekin, Ozgür, Trigo-Rodríguez, Josep M., Sunshine, Jessica M., Farnham, Tony, Asphaug, Erik, Deshapriya, J. D. Prasanna, Hasselmann, Pedro H., Beccarelli, Joel, Schwartz, Stephen R., Abell, Paul, Michel, Patrick, Cheng, Andy F., Brucato, John Robert, Zinzi, Angelo, Amoroso, Marilena, Pirrotta, Simone, Impresario, Gabriele, Bertini, Ivano, Capannolo, Andrea, Caporali, S., Ceresoli, M., Cremonese, Gabriele, Dall’Ora, Massimo, Gai, Igor, Gomez Casajus, L., Gramigna, Edoardo, Lasagni Manghi, Riccardo, Lavagna, Michèle, Lombardo, M., Modenini, Dario, Palumbo, Pasquale, Perna, Davide, Tortora, Paolo, Zannoni, Marco, Zanotti, Giovanni, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Pajola, Maurizio, Tusberti, Filippo, Lucchetti, Alice, Barnouin, Olivier, Cambioni, Saverio, Ernst, Carolyn, Dotto, Elisabetta, Daly, R. Terik, Poggiali, Giovanni, Hirabayashi, Masatoshi, Nakano, Ryota, Mazzotta Epifani, Elena, Chabot, Nancy, Della Corte, Vincenzo, Rivkin, Andy, Agrusa, Harrison F., Zhang, Yun, Penasa, L., Ballouz, Ronald-Louis, Ivanovski, Stavro, Murdoch, Naomi, Rossi, Alessandro, Robin, Colas Q., Ieva, Simone, Vincent, Jean-Baptiste, Ferrari, Fabio, Raducan, Sabina D., Campo Bagatin, Adriano, Parro, Laura M., Benavídez, Paula Gabriela, Tancredi, Gonzalo, Karatekin, Ozgür, Trigo-Rodríguez, Josep M., Sunshine, Jessica M., Farnham, Tony, Asphaug, Erik, Deshapriya, J. D. Prasanna, Hasselmann, Pedro H., Beccarelli, Joel, Schwartz, Stephen R., Abell, Paul, Michel, Patrick, Cheng, Andy F., Brucato, John Robert, Zinzi, Angelo, Amoroso, Marilena, Pirrotta, Simone, Impresario, Gabriele, Bertini, Ivano, Capannolo, Andrea, Caporali, S., Ceresoli, M., Cremonese, Gabriele, Dall’Ora, Massimo, Gai, Igor, Gomez Casajus, L., Gramigna, Edoardo, Lasagni Manghi, Riccardo, Lavagna, Michèle, Lombardo, M., Modenini, Dario, Palumbo, Pasquale, Perna, Davide, Tortora, Paolo, Zannoni, Marco, and Zanotti, Giovanni
Abstract: Asteroids smaller than 10 km are thought to be rubble piles formed from the reaccumulation of fragments produced in the catastrophic disruption of parent bodies. Ground-based observations reveal that some of these asteroids are today binary systems, in which a smaller secondary orbits a larger primary asteroid. However, how these asteroids became binary systems remains unclear. Here, we report the analysis of boulders on the surface of the stony asteroid (65803) Didymos and its moonlet, Dimorphos, from data collected by the NASA DART mission. The size-frequency distribution of boulders larger than 5 m on Dimorphos and larger than 22.8 m on Didymos confirms that both asteroids are piles of fragments produced in the catastrophic disruption of their progenitors. Dimorphos boulders smaller than 5 m have size best-fit by a Weibull distribution, which we attribute to a multi-phase fragmentation process either occurring during coalescence or during surface evolution. The density per km2 of Dimorphos boulders ≥1 m is 2.3x with respect to the one obtained for (101955) Bennu, while it is 3.0x with respect to (162173) Ryugu. Such values increase once Dimorphos boulders ≥5 m are compared with Bennu (3.5x), Ryugu (3.9x) and (25143) Itokawa (5.1x). This is of interest in the context of asteroid studies because it means that contrarily to the single bodies visited so far, binary systems might be affected by subsequential fragmentation processes that largely increase their block density per km2. Direct comparison between the surface distribution and shapes of the boulders on Didymos and Dimorphos suggest that the latter inherited its material from the former. This finding supports the hypothesis that some asteroid binary systems form through the spin up and mass shedding of a fraction of the primary asteroid.
Published: 2024

8. The geology and evolution of the Near-Earth binary asteroid system (65803) Didymos

Author: Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Barnouin, Olivier, Ballouz, Ronald-Louis, Marchi, Simone, Vincent, Jean-Baptiste, Agrusa, Harrison F., Zhang, Yun, Ernst, Carolyn, Pajola, Maurizio, Tusberti, Filippo, Lucchetti, Alice, Daly, R. Terik, Palmer, Eric E., Walsh, Kevin J., Michel, Patrick, Sunshine, Jessica M., Rizos, Juan L., Farnham, Tony, Richardson, Derek C., Parro, Laura M., Murdoch, Naomi, Robin, Colas Q., Hirabayashi, Masatoshi, Kahout, Tomas, Asphaug, Erik, Raducan, Sabina D., Jutzi, Martin, Ferrari, Fabio, Hasselmann, Pedro H., Campo Bagatin, Adriano, Chabot, Nancy, Li, Jian-Yang, Cheng, Andy F., Nolan, Michael C., Stickle, Angela M., Karatekin, Ozgür, Dotto, Elisabetta, Della Corte, Vincenzo, Mazzotta Epifani, Elena, Rossi, Alessandro, Gai, Igor, Deshapriya, J. D. Prasanna, Bertini, Ivano, Zinzi, Angelo, Trigo-Rodríguez, Josep M., Beccarelli, Joel, Ivanovski, Stavro, Brucato, John Robert, Poggiali, Giovanni, Zanotti, Giovanni, Amoroso, Marilena, Capannolo, Andrea, Cremonese, Gabriele, Dall’Ora, Massimo, Ieva, Simone, Impresario, Gabriele, Lavagna, Michèle, Modenini, Dario, Palumbo, Pasquale, Perna, Davide, Pirrotta, Simone, Tortora, Paolo, Zannoni, Marco, Rivkin, Andy, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Barnouin, Olivier, Ballouz, Ronald-Louis, Marchi, Simone, Vincent, Jean-Baptiste, Agrusa, Harrison F., Zhang, Yun, Ernst, Carolyn, Pajola, Maurizio, Tusberti, Filippo, Lucchetti, Alice, Daly, R. Terik, Palmer, Eric E., Walsh, Kevin J., Michel, Patrick, Sunshine, Jessica M., Rizos, Juan L., Farnham, Tony, Richardson, Derek C., Parro, Laura M., Murdoch, Naomi, Robin, Colas Q., Hirabayashi, Masatoshi, Kahout, Tomas, Asphaug, Erik, Raducan, Sabina D., Jutzi, Martin, Ferrari, Fabio, Hasselmann, Pedro H., Campo Bagatin, Adriano, Chabot, Nancy, Li, Jian-Yang, Cheng, Andy F., Nolan, Michael C., Stickle, Angela M., Karatekin, Ozgür, Dotto, Elisabetta, Della Corte, Vincenzo, Mazzotta Epifani, Elena, Rossi, Alessandro, Gai, Igor, Deshapriya, J. D. Prasanna, Bertini, Ivano, Zinzi, Angelo, Trigo-Rodríguez, Josep M., Beccarelli, Joel, Ivanovski, Stavro, Brucato, John Robert, Poggiali, Giovanni, Zanotti, Giovanni, Amoroso, Marilena, Capannolo, Andrea, Cremonese, Gabriele, Dall’Ora, Massimo, Ieva, Simone, Impresario, Gabriele, Lavagna, Michèle, Modenini, Dario, Palumbo, Pasquale, Perna, Davide, Pirrotta, Simone, Tortora, Paolo, Zannoni, Marco, and Rivkin, Andy
Abstract: Images collected during NASA’s Double Asteroid Redirection Test (DART) mission provide the first resolved views of the Didymos binary asteroid system. These images reveal that the primary asteroid, Didymos, is flattened and has plausible undulations along its equatorial perimeter. At high elevations, its surface is rough and contains large boulders and craters; at low elevations its surface is smooth and possesses fewer large boulders and craters. Didymos’ moon, Dimorphos, possesses an intimate mixture of boulders, several asteroid-wide lineaments, and a handful of craters. The surfaces of both asteroids include boulders that are large relative to their host body, suggesting that both asteroids are rubble piles. Based on these observations, our models indicate that Didymos has a surface cohesion ≤ 1 Pa and an interior cohesion of ∼10 Pa, while Dimorphos has a surface cohesion of <0.9 Pa. Crater size-frequency analyzes indicate the surface age of Didymos is 40–130 times older than Dimorphos, with likely absolute ages of ∼ 12.5 Myr and <0.3 Myr, respectively. Solar radiation could have increased Didymos’ spin rate leading to internal deformation and surface mass shedding, which likely created Dimorphos.
Published: 2024

9. Mechanical properties of rubble pile asteroids (Dimorphos, Itokawa, Ryugu, and Bennu) through surface boulder morphological analysis

Author: Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Robin, Colas Q., Duchene, Alexia, Murdoch, Naomi, Vincent, Jean-Baptiste, Lucchetti, Alice, Pajola, Maurizio, Ernst, Carolyn, Daly, R. Terik, Barnouin, Olivier, Raducan, Sabina D., Michel, Patrick, Hirabayashi, Masatoshi, Stott, Alexander, Cuervo, Gabriela, Jawin, Erica R., Trigo-Rodríguez, Josep M., Parro, Laura M., Sunday, Cecily, Vivet, Damien, Mimoun, David, Rivkin, Andy, Chabot, Nancy, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Robin, Colas Q., Duchene, Alexia, Murdoch, Naomi, Vincent, Jean-Baptiste, Lucchetti, Alice, Pajola, Maurizio, Ernst, Carolyn, Daly, R. Terik, Barnouin, Olivier, Raducan, Sabina D., Michel, Patrick, Hirabayashi, Masatoshi, Stott, Alexander, Cuervo, Gabriela, Jawin, Erica R., Trigo-Rodríguez, Josep M., Parro, Laura M., Sunday, Cecily, Vivet, Damien, Mimoun, David, Rivkin, Andy, and Chabot, Nancy
Abstract: Planetary defense efforts rely on estimates of the mechanical properties of asteroids, which are difficult to constrain accurately from Earth. The mechanical properties of asteroid material are also important in the interpretation of the Double Asteroid Redirection Test (DART) impact. Here we perform a detailed morphological analysis of the surface boulders on Dimorphos using images, the primary data set available from the DART mission. We estimate the bulk angle of internal friction of the boulders to be 32.7 ± 2. 5° from our measurements of the roundness of the 34 best-resolved boulders ranging in size from 1.67–6.64 m. The elongated nature of the boulders around the DART impact site implies that they were likely formed through impact processing. Finally, we find striking similarities in the morphology of the boulders on Dimorphos with those on other rubble pile asteroids (Itokawa, Ryugu and Bennu). This leads to very similar internal friction angles across the four bodies and suggests that a common formation mechanism has shaped the boulders. Our results provide key inputs for understanding the DART impact and for improving our knowledge about the physical properties, the formation and the evolution of both near-Earth rubble-pile and binary asteroids.
Published: 2024

10. VADER: Probing the Dark Side of Dimorphos with LICIACube LUKE

Author: Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Zinzi, Angelo, Hasselmann, Pedro H., Della Corte, Vincenzo, Deshapriya, J. D. Prasanna, Gai, Igor, Lucchetti, Alice, Pajola, Maurizio, Rossi, Alessandro, Dotto, Elisabetta, Mazzotta Epifani, Elena, Daly, R. Terik, Hirabayashi, Masatoshi, Farnham, Tony, Ernst, Carolyn, Ivanovski, Stavro, Li, Jian-Yang, Parro, Laura M., Amoroso, Marilena, Beccarelli, Joel, Bertini, Ivano, Brucato, John Robert, Capannolo, Andrea, Caporali, S., Ceresoli, M., Cremonese, Gabriele, Dall’Ora, Massimo, Gomez Casajus, L., Gramigna, Edoardo, Ieva, Simone, Impresario, Gabriele, Lasagni Manghi, Riccardo, Lavagna, Michèle, Lombardo, M., Modenini, Dario, Negri, B., Palumbo, Pasquale, Perna, Davide, Pirrotta, Simone, Poggiali, Giovanni, Tortora, Paolo, Tusberti, Filippo, Zannoni, Marco, Zanotti, Giovanni, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Zinzi, Angelo, Hasselmann, Pedro H., Della Corte, Vincenzo, Deshapriya, J. D. Prasanna, Gai, Igor, Lucchetti, Alice, Pajola, Maurizio, Rossi, Alessandro, Dotto, Elisabetta, Mazzotta Epifani, Elena, Daly, R. Terik, Hirabayashi, Masatoshi, Farnham, Tony, Ernst, Carolyn, Ivanovski, Stavro, Li, Jian-Yang, Parro, Laura M., Amoroso, Marilena, Beccarelli, Joel, Bertini, Ivano, Brucato, John Robert, Capannolo, Andrea, Caporali, S., Ceresoli, M., Cremonese, Gabriele, Dall’Ora, Massimo, Gomez Casajus, L., Gramigna, Edoardo, Ieva, Simone, Impresario, Gabriele, Lasagni Manghi, Riccardo, Lavagna, Michèle, Lombardo, M., Modenini, Dario, Negri, B., Palumbo, Pasquale, Perna, Davide, Pirrotta, Simone, Poggiali, Giovanni, Tortora, Paolo, Tusberti, Filippo, Zannoni, Marco, and Zanotti, Giovanni
Abstract: The ASI cubesat LICIACube has been part of the first planetary defense mission DART, having among its scopes to complement the DRACO images to better constrain the Dimorphos shape. LICIACube had two different cameras, LEIA and LUKE, and to accomplish its goal, it exploited the unique possibility of acquiring images of the Dimorphos hemisphere not seen by DART from a vantage point of view, in both time and space. This work is indeed aimed at constraining the tridimensional shape of Dimorphos, starting from both LUKE images of the nonimpacted hemisphere of Dimorphos and the results obtained by DART looking at the impacted hemisphere. To this aim, we developed a semiautomatic Computer Vision algorithm, named VADER, able to identify objects of interest on the basis of physical characteristics, subsequently used as input to retrieve the shape of the ellipse projected in the LUKE images analyzed. Thanks to this shape, we then extracted information about the Dimorphos ellipsoid by applying a series of quantitative geometric considerations. Although the solution space coming from this analysis includes the triaxial ellipsoid found by using DART images, we cannot discard the possibility that Dimorphos has a more elongated shape, more similar to what is expected from previous theories and observations. The result of our work seems therefore to emphasize the unique value of the LICIACube mission and its images, making even clearer the need of having different points of view to accurately define the shape of an asteroid.
Published: 2024

11. Recent collisional history of (65803) Didymos

Author: Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Campo Bagatin, Adriano, Dell'Oro, Aldo, Parro, Laura M., Benavídez, Paula Gabriela, Jacobson, Seth A., Lucchetti, Alice, Marzari, Francesco, Michel, Patrick, Pajola, Maurizio, Vincent, Jean-Baptiste, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Campo Bagatin, Adriano, Dell'Oro, Aldo, Parro, Laura M., Benavídez, Paula Gabriela, Jacobson, Seth A., Lucchetti, Alice, Marzari, Francesco, Michel, Patrick, Pajola, Maurizio, and Vincent, Jean-Baptiste
Abstract: The Double Asteroid Redirection Test (DART, NASA) spacecraft revealed that the primary of the (65803) Didymos near-Earth asteroid (NEA) binary system is not exactly the expected spinning top shape observed for other km-size asteroids. Ground based radar observations predicted that such shape was compatible with the uncertainty along the direction of the asteroid spin axis. Indeed, Didymos shows crater and landslide features, and evidence for boulder motion at low equatorial latitudes. Altogether, the primary seems to have undergone sudden structural failure in its recent history, which may even result in the formation of the secondary. The high eccentricity of Didymos sets its aphelion distance inside the inner main belt, where it spends more than 1/3 of its orbital period and it may undergo many more collisions than in the NEA region. In this work, we investigate the collisional environment of this asteroid and estimate the probability of collision with multi-size potential impactors. We analyze the possibility that such impacts produced the surface features observed on Didymos by comparing collisional intervals with estimated times for surface destabilization by the Yarkovsky-O’Keefe-Radzievskii-Paddack (YORP) effect. We find that collisional effects dominate over potential local or global deformation due to YORP spin up.
Published: 2024

12. Geophysical Characterization of the Interiors of Ganymede, Callisto and Europa by ESA's JUpiter ICy moons Explorer

Author: Van Hoolst, Tim, Tobie, Gabriel, Vallat, Claire, Altobelli, Nicolas, Bruzzone, Lorenzo, Cao, Hao, Dirkx, Dominic, Genova, Antonio, Hussmann, Hauke, Iess, Luciano, Kimura, Jun, Khurana, Krishan, Lucchetti, Alice, Mitri, Giuseppe, Moore, William, Saur, Joachim, Stark, Alexander, Vorburger, Audrey, Wieczorek, Mark, Aboudan, Alessio, Bergman, Jan, Bovolo, Francesca, Breuer, Doris, Cappuccio, Paolo, Carrer, Leonardo, Cecconi, Baptiste, Choblet, Gaël, De Marchi, Fabrizio, Fayolle, Marie, Fienga, Agnès, Futaana, Yoshifumi, Hauber, Ernst, Kofman, Wlodek, Kumamoto, Atsushi, Lainey, Valery, Molyneux, Philippa, Mousis, Olivier, Plaut, Jeff, Puccio, Walter, Retherford, Kurt, Roth, Lorenz, Seignovert, Benoit, Steinbrügge, Gregor, Thakur, Sanchari, Tortora, Paolo, Tosi, Federico, Zannoni, Marco, Barabash, Stas, Dougherty, Michele, Gladstone, Randy, Gurvits, Leonid I., Hartogh, Paul, Palumbo, Pasquale, Poulet, Francois, Wahlund, Jan-Erik, Grasset, Olivier, Witasse, Olivier, Van Hoolst, Tim, Tobie, Gabriel, Vallat, Claire, Altobelli, Nicolas, Bruzzone, Lorenzo, Cao, Hao, Dirkx, Dominic, Genova, Antonio, Hussmann, Hauke, Iess, Luciano, Kimura, Jun, Khurana, Krishan, Lucchetti, Alice, Mitri, Giuseppe, Moore, William, Saur, Joachim, Stark, Alexander, Vorburger, Audrey, Wieczorek, Mark, Aboudan, Alessio, Bergman, Jan, Bovolo, Francesca, Breuer, Doris, Cappuccio, Paolo, Carrer, Leonardo, Cecconi, Baptiste, Choblet, Gaël, De Marchi, Fabrizio, Fayolle, Marie, Fienga, Agnès, Futaana, Yoshifumi, Hauber, Ernst, Kofman, Wlodek, Kumamoto, Atsushi, Lainey, Valery, Molyneux, Philippa, Mousis, Olivier, Plaut, Jeff, Puccio, Walter, Retherford, Kurt, Roth, Lorenz, Seignovert, Benoit, Steinbrügge, Gregor, Thakur, Sanchari, Tortora, Paolo, Tosi, Federico, Zannoni, Marco, Barabash, Stas, Dougherty, Michele, Gladstone, Randy, Gurvits, Leonid I., Hartogh, Paul, Palumbo, Pasquale, Poulet, Francois, Wahlund, Jan-Erik, Grasset, Olivier, and Witasse, Olivier
Abstract: The JUpiter ICy moons Explorer (JUICE) of ESA was launched on 14 April 2023 and will arrive at Jupiter and its moons in July 2031. In this review article, we describe how JUICE will investigate the interior of the three icy Galilean moons, Ganymede, Callisto and Europa, during its Jupiter orbital tour and the final orbital phase around Ganymede. Detailed geophysical observations about the interior of the moons can only be performed from close distances to the moons, and best estimates of signatures of the interior, such as an induced magnetic field, tides and rotation variations, and radar reflections, will be obtained during flybys of the moons with altitudes of about 1000 km or less and during the Ganymede orbital phase at an average altitude of 490 km. The 9-month long orbital phase around Ganymede, the first of its kind around another moon than our Moon, will allow an unprecedented and detailed insight into the moon's interior, from the central regions where a magnetic field is generated to the internal ocean and outer ice shell. Multiple flybys of Callisto will clarify the differences in evolution compared to Ganymede and will provide key constraints on the origin and evolution of the Jupiter system. JUICE will visit Europa only during two close flybys and the geophysical investigations will focus on selected areas of the ice shell. A prime goal of JUICE is the characterisation of the ice shell and ocean of the Galilean moons, and we here specifically emphasise the synergistic aspects of the different geophysical investigations, showing how different instruments will work together to probe the hydrosphere. We also describe how synergies between JUICE instruments will contribute to the assessment of the deep interior of the moons, their internal differentiation, dynamics and evolution. In situ measurements and remote sensing observations will support the geophysical instruments to achieve these goals, but will also, together with subsurface radar sounding, provi
Published: 2024
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13. Characterization of the Surfaces and Near-Surface Atmospheres of Ganymede, Europa and Callisto by JUICE

Author: Tosi, Federico, Roatsch, Thomas, Galli, Andre, Hauber, Ernst, Lucchetti, Alice, Molyneux, Philippa, Stephan, Katrin, Achilleos, Nicholas, Bovolo, Francesca, Carter, John, Cavalie, Thibault, Cimo, Giuseppe, D'Aversa, Emiliano, Gwinner, Klaus, Hartogh, Paul, Huybrighs, Hans, Langevin, Yves, Lellouch, Emmanuel, Migliorini, Alessandra, Palumbo, Pasquale, Piccioni, Giuseppe, Plaut, Jeffrey J., Postberg, Frank, Poulet, Francois, Retherford, Kurt, Rezac, Ladislav, Roth, Lorenz, Solomonidou, Anezina, Tobie, Gabriel, Tortora, Paolo, Tubiana, Cecilia, Wagner, Roland, Wirström, Eva, Wurz, Peter, Zambon, Francesca, Zannoni, Marco, Barabash, Stas, Bruzzone, Lorenzo, Dougherty, Michele, Gladstone, Randy, Gurvits, Leonid I., Hussmann, Hauke, Iess, Luciano, Wahlund, Jan-Erik, Witasse, Olivier, Vallat, Claire, Lorente, Rosario, Tosi, Federico, Roatsch, Thomas, Galli, Andre, Hauber, Ernst, Lucchetti, Alice, Molyneux, Philippa, Stephan, Katrin, Achilleos, Nicholas, Bovolo, Francesca, Carter, John, Cavalie, Thibault, Cimo, Giuseppe, D'Aversa, Emiliano, Gwinner, Klaus, Hartogh, Paul, Huybrighs, Hans, Langevin, Yves, Lellouch, Emmanuel, Migliorini, Alessandra, Palumbo, Pasquale, Piccioni, Giuseppe, Plaut, Jeffrey J., Postberg, Frank, Poulet, Francois, Retherford, Kurt, Rezac, Ladislav, Roth, Lorenz, Solomonidou, Anezina, Tobie, Gabriel, Tortora, Paolo, Tubiana, Cecilia, Wagner, Roland, Wirström, Eva, Wurz, Peter, Zambon, Francesca, Zannoni, Marco, Barabash, Stas, Bruzzone, Lorenzo, Dougherty, Michele, Gladstone, Randy, Gurvits, Leonid I., Hussmann, Hauke, Iess, Luciano, Wahlund, Jan-Erik, Witasse, Olivier, Vallat, Claire, and Lorente, Rosario
Abstract: We present the state of the art on the study of surfaces and tenuous atmospheres of the icy Galilean satellites Ganymede, Europa and Callisto, from past and ongoing space exploration conducted with several spacecraft to recent telescopic observations, and we show how the ESA JUICE mission plans to explore these surfaces and atmospheres in detail with its scientific payload. The surface geology of the moons is the main evidence of their evolution and reflects the internal heating provided by tidal interactions. Surface composition is the result of endogenous and exogenous processes, with the former providing valuable information about the potential composition of shallow subsurface liquid pockets, possibly connected to deeper oceans. Finally, the icy Galilean moons have tenuous atmospheres that arise from charged particle sputtering affecting their surfaces. In the case of Europa, plumes of water vapour have also been reported, whose phenomenology at present is poorly understood and requires future close exploration. In the three main sections of the article, we discuss these topics, highlighting the key scientific objectives and investigations to be achieved by JUICE. Based on a recent predicted trajectory, we also show potential coverage maps and other examples of reference measurements. The scientific discussion and observation planning presented here are the outcome of the JUICE Working Group 2 (WG2): "Surfaces and Near-surface Exospheres of the Satellites, dust and rings".
Published: 2024
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14. Geophysical Characterization of the Interiors of Ganymede, Callisto and Europa by ESA's JUpiter ICy moons Explorer

Author: Van Hoolst, Tim, Tobie, Gabriel, Vallat, Claire, Altobelli, Nicolas, Bruzzone, Lorenzo, Cao, Hao, Dirkx, Dominic, Genova, Antonio, Hussmann, Hauke, Iess, Luciano, Kimura, Jun, Khurana, Krishan, Lucchetti, Alice, Mitri, Giuseppe, Moore, William, Saur, Joachim, Stark, Alexander, Vorburger, Audrey, Wieczorek, Mark, Aboudan, Alessio, Bergman, Jan, Bovolo, Francesca, Breuer, Doris, Cappuccio, Paolo, Carrer, Leonardo, Cecconi, Baptiste, Choblet, Gaël, De Marchi, Fabrizio, Fayolle, Marie, Fienga, Agnès, Futaana, Yoshifumi, Hauber, Ernst, Kofman, Wlodek, Kumamoto, Atsushi, Lainey, Valery, Molyneux, Philippa, Mousis, Olivier, Plaut, Jeff, Puccio, Walter, Retherford, Kurt, Roth, Lorenz, Seignovert, Benoit, Steinbrügge, Gregor, Thakur, Sanchari, Tortora, Paolo, Tosi, Federico, Zannoni, Marco, Barabash, Stas, Dougherty, Michele, Gladstone, Randy, Gurvits, Leonid I., Hartogh, Paul, Palumbo, Pasquale, Poulet, Francois, Wahlund, Jan-Erik, Grasset, Olivier, Witasse, Olivier, Van Hoolst, Tim, Tobie, Gabriel, Vallat, Claire, Altobelli, Nicolas, Bruzzone, Lorenzo, Cao, Hao, Dirkx, Dominic, Genova, Antonio, Hussmann, Hauke, Iess, Luciano, Kimura, Jun, Khurana, Krishan, Lucchetti, Alice, Mitri, Giuseppe, Moore, William, Saur, Joachim, Stark, Alexander, Vorburger, Audrey, Wieczorek, Mark, Aboudan, Alessio, Bergman, Jan, Bovolo, Francesca, Breuer, Doris, Cappuccio, Paolo, Carrer, Leonardo, Cecconi, Baptiste, Choblet, Gaël, De Marchi, Fabrizio, Fayolle, Marie, Fienga, Agnès, Futaana, Yoshifumi, Hauber, Ernst, Kofman, Wlodek, Kumamoto, Atsushi, Lainey, Valery, Molyneux, Philippa, Mousis, Olivier, Plaut, Jeff, Puccio, Walter, Retherford, Kurt, Roth, Lorenz, Seignovert, Benoit, Steinbrügge, Gregor, Thakur, Sanchari, Tortora, Paolo, Tosi, Federico, Zannoni, Marco, Barabash, Stas, Dougherty, Michele, Gladstone, Randy, Gurvits, Leonid I., Hartogh, Paul, Palumbo, Pasquale, Poulet, Francois, Wahlund, Jan-Erik, Grasset, Olivier, and Witasse, Olivier
Abstract: The JUpiter ICy moons Explorer (JUICE) of ESA was launched on 14 April 2023 and will arrive at Jupiter and its moons in July 2031. In this review article, we describe how JUICE will investigate the interior of the three icy Galilean moons, Ganymede, Callisto and Europa, during its Jupiter orbital tour and the final orbital phase around Ganymede. Detailed geophysical observations about the interior of the moons can only be performed from close distances to the moons, and best estimates of signatures of the interior, such as an induced magnetic field, tides and rotation variations, and radar reflections, will be obtained during flybys of the moons with altitudes of about 1000 km or less and during the Ganymede orbital phase at an average altitude of 490 km. The 9-month long orbital phase around Ganymede, the first of its kind around another moon than our Moon, will allow an unprecedented and detailed insight into the moon's interior, from the central regions where a magnetic field is generated to the internal ocean and outer ice shell. Multiple flybys of Callisto will clarify the differences in evolution compared to Ganymede and will provide key constraints on the origin and evolution of the Jupiter system. JUICE will visit Europa only during two close flybys and the geophysical investigations will focus on selected areas of the ice shell. A prime goal of JUICE is the characterisation of the ice shell and ocean of the Galilean moons, and we here specifically emphasise the synergistic aspects of the different geophysical investigations, showing how different instruments will work together to probe the hydrosphere. We also describe how synergies between JUICE instruments will contribute to the assessment of the deep interior of the moons, their internal differentiation, dynamics and evolution. In situ measurements and remote sensing observations will support the geophysical instruments to achieve these goals, but will also, together with subsurface radar sounding, provi
Published: 2024
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15. Geophysical Characterization of the Interiors of Ganymede, Callisto and Europa by ESA's JUpiter ICy moons Explorer

Author: Van Hoolst, Tim, Tobie, Gabriel, Vallat, Claire, Altobelli, Nicolas, Bruzzone, Lorenzo, Cao, Hao, Dirkx, Dominic, Genova, Antonio, Hussmann, Hauke, Iess, Luciano, Kimura, Jun, Khurana, Krishan, Lucchetti, Alice, Mitri, Giuseppe, Moore, William, Saur, Joachim, Stark, Alexander, Vorburger, Audrey, Wieczorek, Mark, Aboudan, Alessio, Bergman, Jan, Bovolo, Francesca, Breuer, Doris, Cappuccio, Paolo, Carrer, Leonardo, Cecconi, Baptiste, Choblet, Gaël, De Marchi, Fabrizio, Fayolle, Marie, Fienga, Agnès, Futaana, Yoshifumi, Hauber, Ernst, Kofman, Wlodek, Kumamoto, Atsushi, Lainey, Valery, Molyneux, Philippa, Mousis, Olivier, Plaut, Jeff, Puccio, Walter, Retherford, Kurt, Roth, Lorenz, Seignovert, Benoit, Steinbrügge, Gregor, Thakur, Sanchari, Tortora, Paolo, Tosi, Federico, Zannoni, Marco, Barabash, Stas, Dougherty, Michele, Gladstone, Randy, Gurvits, Leonid I., Hartogh, Paul, Palumbo, Pasquale, Poulet, Francois, Wahlund, Jan-Erik, Grasset, Olivier, Witasse, Olivier, Van Hoolst, Tim, Tobie, Gabriel, Vallat, Claire, Altobelli, Nicolas, Bruzzone, Lorenzo, Cao, Hao, Dirkx, Dominic, Genova, Antonio, Hussmann, Hauke, Iess, Luciano, Kimura, Jun, Khurana, Krishan, Lucchetti, Alice, Mitri, Giuseppe, Moore, William, Saur, Joachim, Stark, Alexander, Vorburger, Audrey, Wieczorek, Mark, Aboudan, Alessio, Bergman, Jan, Bovolo, Francesca, Breuer, Doris, Cappuccio, Paolo, Carrer, Leonardo, Cecconi, Baptiste, Choblet, Gaël, De Marchi, Fabrizio, Fayolle, Marie, Fienga, Agnès, Futaana, Yoshifumi, Hauber, Ernst, Kofman, Wlodek, Kumamoto, Atsushi, Lainey, Valery, Molyneux, Philippa, Mousis, Olivier, Plaut, Jeff, Puccio, Walter, Retherford, Kurt, Roth, Lorenz, Seignovert, Benoit, Steinbrügge, Gregor, Thakur, Sanchari, Tortora, Paolo, Tosi, Federico, Zannoni, Marco, Barabash, Stas, Dougherty, Michele, Gladstone, Randy, Gurvits, Leonid I., Hartogh, Paul, Palumbo, Pasquale, Poulet, Francois, Wahlund, Jan-Erik, Grasset, Olivier, and Witasse, Olivier
Abstract: The JUpiter ICy moons Explorer (JUICE) of ESA was launched on 14 April 2023 and will arrive at Jupiter and its moons in July 2031. In this review article, we describe how JUICE will investigate the interior of the three icy Galilean moons, Ganymede, Callisto and Europa, during its Jupiter orbital tour and the final orbital phase around Ganymede. Detailed geophysical observations about the interior of the moons can only be performed from close distances to the moons, and best estimates of signatures of the interior, such as an induced magnetic field, tides and rotation variations, and radar reflections, will be obtained during flybys of the moons with altitudes of about 1000 km or less and during the Ganymede orbital phase at an average altitude of 490 km. The 9-month long orbital phase around Ganymede, the first of its kind around another moon than our Moon, will allow an unprecedented and detailed insight into the moon's interior, from the central regions where a magnetic field is generated to the internal ocean and outer ice shell. Multiple flybys of Callisto will clarify the differences in evolution compared to Ganymede and will provide key constraints on the origin and evolution of the Jupiter system. JUICE will visit Europa only during two close flybys and the geophysical investigations will focus on selected areas of the ice shell. A prime goal of JUICE is the characterisation of the ice shell and ocean of the Galilean moons, and we here specifically emphasise the synergistic aspects of the different geophysical investigations, showing how different instruments will work together to probe the hydrosphere. We also describe how synergies between JUICE instruments will contribute to the assessment of the deep interior of the moons, their internal differentiation, dynamics and evolution. In situ measurements and remote sensing observations will support the geophysical instruments to achieve these goals, but will also, together with subsurface radar sounding, provi
Published: 2024
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16. Characterization of the Surfaces and Near-Surface Atmospheres of Ganymede, Europa and Callisto by JUICE

Author: Tosi, Federico, Roatsch, Thomas, Galli, Andre, Hauber, Ernst, Lucchetti, Alice, Molyneux, Philippa, Stephan, Katrin, Achilleos, Nicholas, Bovolo, Francesca, Carter, John, Cavalie, Thibault, Cimo, Giuseppe, D'Aversa, Emiliano, Gwinner, Klaus, Hartogh, Paul, Huybrighs, Hans, Langevin, Yves, Lellouch, Emmanuel, Migliorini, Alessandra, Palumbo, Pasquale, Piccioni, Giuseppe, Plaut, Jeffrey J., Postberg, Frank, Poulet, Francois, Retherford, Kurt, Rezac, Ladislav, Roth, Lorenz, Solomonidou, Anezina, Tobie, Gabriel, Tortora, Paolo, Tubiana, Cecilia, Wagner, Roland, Wirström, Eva, Wurz, Peter, Zambon, Francesca, Zannoni, Marco, Barabash, Stas, Bruzzone, Lorenzo, Dougherty, Michele, Gladstone, Randy, Gurvits, Leonid I., Hussmann, Hauke, Iess, Luciano, Wahlund, Jan-Erik, Witasse, Olivier, Vallat, Claire, Lorente, Rosario, Tosi, Federico, Roatsch, Thomas, Galli, Andre, Hauber, Ernst, Lucchetti, Alice, Molyneux, Philippa, Stephan, Katrin, Achilleos, Nicholas, Bovolo, Francesca, Carter, John, Cavalie, Thibault, Cimo, Giuseppe, D'Aversa, Emiliano, Gwinner, Klaus, Hartogh, Paul, Huybrighs, Hans, Langevin, Yves, Lellouch, Emmanuel, Migliorini, Alessandra, Palumbo, Pasquale, Piccioni, Giuseppe, Plaut, Jeffrey J., Postberg, Frank, Poulet, Francois, Retherford, Kurt, Rezac, Ladislav, Roth, Lorenz, Solomonidou, Anezina, Tobie, Gabriel, Tortora, Paolo, Tubiana, Cecilia, Wagner, Roland, Wirström, Eva, Wurz, Peter, Zambon, Francesca, Zannoni, Marco, Barabash, Stas, Bruzzone, Lorenzo, Dougherty, Michele, Gladstone, Randy, Gurvits, Leonid I., Hussmann, Hauke, Iess, Luciano, Wahlund, Jan-Erik, Witasse, Olivier, Vallat, Claire, and Lorente, Rosario
Abstract: We present the state of the art on the study of surfaces and tenuous atmospheres of the icy Galilean satellites Ganymede, Europa and Callisto, from past and ongoing space exploration conducted with several spacecraft to recent telescopic observations, and we show how the ESA JUICE mission plans to explore these surfaces and atmospheres in detail with its scientific payload. The surface geology of the moons is the main evidence of their evolution and reflects the internal heating provided by tidal interactions. Surface composition is the result of endogenous and exogenous processes, with the former providing valuable information about the potential composition of shallow subsurface liquid pockets, possibly connected to deeper oceans. Finally, the icy Galilean moons have tenuous atmospheres that arise from charged particle sputtering affecting their surfaces. In the case of Europa, plumes of water vapour have also been reported, whose phenomenology at present is poorly understood and requires future close exploration. In the three main sections of the article, we discuss these topics, highlighting the key scientific objectives and investigations to be achieved by JUICE. Based on a recent predicted trajectory, we also show potential coverage maps and other examples of reference measurements. The scientific discussion and observation planning presented here are the outcome of the JUICE Working Group 2 (WG2): "Surfaces and Near-surface Exospheres of the Satellites, dust and rings".
Published: 2024
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17. Characterization of the Surfaces and Near-Surface Atmospheres of Ganymede, Europa and Callisto by JUICE

Author: Tosi, Federico, Roatsch, Thomas, Galli, Andre, Hauber, Ernst, Lucchetti, Alice, Molyneux, Philippa, Stephan, Katrin, Achilleos, Nicholas, Bovolo, Francesca, Carter, John, Cavalie, Thibault, Cimo, Giuseppe, D'Aversa, Emiliano, Gwinner, Klaus, Hartogh, Paul, Huybrighs, Hans, Langevin, Yves, Lellouch, Emmanuel, Migliorini, Alessandra, Palumbo, Pasquale, Piccioni, Giuseppe, Plaut, Jeffrey J., Postberg, Frank, Poulet, Francois, Retherford, Kurt, Rezac, Ladislav, Roth, Lorenz, Solomonidou, Anezina, Tobie, Gabriel, Tortora, Paolo, Tubiana, Cecilia, Wagner, Roland, Wirström, Eva, Wurz, Peter, Zambon, Francesca, Zannoni, Marco, Barabash, Stas, Bruzzone, Lorenzo, Dougherty, Michele, Gladstone, Randy, Gurvits, Leonid I., Hussmann, Hauke, Iess, Luciano, Wahlund, Jan-Erik, Witasse, Olivier, Vallat, Claire, Lorente, Rosario, Tosi, Federico, Roatsch, Thomas, Galli, Andre, Hauber, Ernst, Lucchetti, Alice, Molyneux, Philippa, Stephan, Katrin, Achilleos, Nicholas, Bovolo, Francesca, Carter, John, Cavalie, Thibault, Cimo, Giuseppe, D'Aversa, Emiliano, Gwinner, Klaus, Hartogh, Paul, Huybrighs, Hans, Langevin, Yves, Lellouch, Emmanuel, Migliorini, Alessandra, Palumbo, Pasquale, Piccioni, Giuseppe, Plaut, Jeffrey J., Postberg, Frank, Poulet, Francois, Retherford, Kurt, Rezac, Ladislav, Roth, Lorenz, Solomonidou, Anezina, Tobie, Gabriel, Tortora, Paolo, Tubiana, Cecilia, Wagner, Roland, Wirström, Eva, Wurz, Peter, Zambon, Francesca, Zannoni, Marco, Barabash, Stas, Bruzzone, Lorenzo, Dougherty, Michele, Gladstone, Randy, Gurvits, Leonid I., Hussmann, Hauke, Iess, Luciano, Wahlund, Jan-Erik, Witasse, Olivier, Vallat, Claire, and Lorente, Rosario
Abstract: We present the state of the art on the study of surfaces and tenuous atmospheres of the icy Galilean satellites Ganymede, Europa and Callisto, from past and ongoing space exploration conducted with several spacecraft to recent telescopic observations, and we show how the ESA JUICE mission plans to explore these surfaces and atmospheres in detail with its scientific payload. The surface geology of the moons is the main evidence of their evolution and reflects the internal heating provided by tidal interactions. Surface composition is the result of endogenous and exogenous processes, with the former providing valuable information about the potential composition of shallow subsurface liquid pockets, possibly connected to deeper oceans. Finally, the icy Galilean moons have tenuous atmospheres that arise from charged particle sputtering affecting their surfaces. In the case of Europa, plumes of water vapour have also been reported, whose phenomenology at present is poorly understood and requires future close exploration. In the three main sections of the article, we discuss these topics, highlighting the key scientific objectives and investigations to be achieved by JUICE. Based on a recent predicted trajectory, we also show potential coverage maps and other examples of reference measurements. The scientific discussion and observation planning presented here are the outcome of the JUICE Working Group 2 (WG2): "Surfaces and Near-surface Exospheres of the Satellites, dust and rings".
Published: 2024
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18. Geophysical Characterization of the Interiors of Ganymede, Callisto and Europa by ESA's JUpiter ICy moons Explorer

Author: Van Hoolst, Tim, Tobie, Gabriel, Vallat, Claire, Altobelli, Nicolas, Bruzzone, Lorenzo, Cao, Hao, Dirkx, Dominic, Genova, Antonio, Hussmann, Hauke, Iess, Luciano, Kimura, Jun, Khurana, Krishan, Lucchetti, Alice, Mitri, Giuseppe, Moore, William, Saur, Joachim, Stark, Alexander, Vorburger, Audrey, Wieczorek, Mark, Aboudan, Alessio, Bergman, Jan, Bovolo, Francesca, Breuer, Doris, Cappuccio, Paolo, Carrer, Leonardo, Cecconi, Baptiste, Choblet, Gaël, De Marchi, Fabrizio, Fayolle, Marie, Fienga, Agnès, Futaana, Yoshifumi, Hauber, Ernst, Kofman, Wlodek, Kumamoto, Atsushi, Lainey, Valery, Molyneux, Philippa, Mousis, Olivier, Plaut, Jeff, Puccio, Walter, Retherford, Kurt, Roth, Lorenz, Seignovert, Benoit, Steinbrügge, Gregor, Thakur, Sanchari, Tortora, Paolo, Tosi, Federico, Zannoni, Marco, Barabash, Stas, Dougherty, Michele, Gladstone, Randy, Gurvits, Leonid I., Hartogh, Paul, Palumbo, Pasquale, Poulet, Francois, Wahlund, Jan-Erik, Grasset, Olivier, Witasse, Olivier, Van Hoolst, Tim, Tobie, Gabriel, Vallat, Claire, Altobelli, Nicolas, Bruzzone, Lorenzo, Cao, Hao, Dirkx, Dominic, Genova, Antonio, Hussmann, Hauke, Iess, Luciano, Kimura, Jun, Khurana, Krishan, Lucchetti, Alice, Mitri, Giuseppe, Moore, William, Saur, Joachim, Stark, Alexander, Vorburger, Audrey, Wieczorek, Mark, Aboudan, Alessio, Bergman, Jan, Bovolo, Francesca, Breuer, Doris, Cappuccio, Paolo, Carrer, Leonardo, Cecconi, Baptiste, Choblet, Gaël, De Marchi, Fabrizio, Fayolle, Marie, Fienga, Agnès, Futaana, Yoshifumi, Hauber, Ernst, Kofman, Wlodek, Kumamoto, Atsushi, Lainey, Valery, Molyneux, Philippa, Mousis, Olivier, Plaut, Jeff, Puccio, Walter, Retherford, Kurt, Roth, Lorenz, Seignovert, Benoit, Steinbrügge, Gregor, Thakur, Sanchari, Tortora, Paolo, Tosi, Federico, Zannoni, Marco, Barabash, Stas, Dougherty, Michele, Gladstone, Randy, Gurvits, Leonid I., Hartogh, Paul, Palumbo, Pasquale, Poulet, Francois, Wahlund, Jan-Erik, Grasset, Olivier, and Witasse, Olivier
Abstract: The JUpiter ICy moons Explorer (JUICE) of ESA was launched on 14 April 2023 and will arrive at Jupiter and its moons in July 2031. In this review article, we describe how JUICE will investigate the interior of the three icy Galilean moons, Ganymede, Callisto and Europa, during its Jupiter orbital tour and the final orbital phase around Ganymede. Detailed geophysical observations about the interior of the moons can only be performed from close distances to the moons, and best estimates of signatures of the interior, such as an induced magnetic field, tides and rotation variations, and radar reflections, will be obtained during flybys of the moons with altitudes of about 1000 km or less and during the Ganymede orbital phase at an average altitude of 490 km. The 9-month long orbital phase around Ganymede, the first of its kind around another moon than our Moon, will allow an unprecedented and detailed insight into the moon's interior, from the central regions where a magnetic field is generated to the internal ocean and outer ice shell. Multiple flybys of Callisto will clarify the differences in evolution compared to Ganymede and will provide key constraints on the origin and evolution of the Jupiter system. JUICE will visit Europa only during two close flybys and the geophysical investigations will focus on selected areas of the ice shell. A prime goal of JUICE is the characterisation of the ice shell and ocean of the Galilean moons, and we here specifically emphasise the synergistic aspects of the different geophysical investigations, showing how different instruments will work together to probe the hydrosphere. We also describe how synergies between JUICE instruments will contribute to the assessment of the deep interior of the moons, their internal differentiation, dynamics and evolution. In situ measurements and remote sensing observations will support the geophysical instruments to achieve these goals, but will also, together with subsurface radar sounding, provi
Published: 2024
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19. Direct $N$-body simulations of satellite formation around small asteroids: insights from DART's encounter with the Didymos system

Author: Agrusa, Harrison F., Zhang, Yun, Richardson, Derek C., Pravec, Petr, Ćuk, Matija, Michel, Patrick, Ballouz, Ronald-Louis, Jacobson, Seth A., Scheeres, Daniel J., Walsh, Kevin, Barnouin, Olivier, Daly, R. Terik, Palmer, Eric, Pajola, Maurizio, Lucchetti, Alice, Tusberti, Filippo, DeMartini, Joseph V., Ferrari, Fabio, Meyer, Alex J., Raducan, Sabina D., Sánchez, Paul, Agrusa, Harrison F., Zhang, Yun, Richardson, Derek C., Pravec, Petr, Ćuk, Matija, Michel, Patrick, Ballouz, Ronald-Louis, Jacobson, Seth A., Scheeres, Daniel J., Walsh, Kevin, Barnouin, Olivier, Daly, R. Terik, Palmer, Eric, Pajola, Maurizio, Lucchetti, Alice, Tusberti, Filippo, DeMartini, Joseph V., Ferrari, Fabio, Meyer, Alex J., Raducan, Sabina D., and Sánchez, Paul
Abstract: We explore binary asteroid formation by spin-up and rotational disruption considering the NASA DART mission's encounter with the Didymos-Dimorphos binary, which was the first small binary visited by a spacecraft. Using a suite of $N$-body simulations, we follow the gravitational accumulation of a satellite from meter-sized particles following a mass-shedding event from a rapidly rotating primary. The satellite's formation is chaotic, as it undergoes a series of collisions, mergers, and close gravitational encounters with other moonlets, leading to a wide range of outcomes in terms of the satellite's mass, shape, orbit, and rotation state. We find that a Dimorphos-like satellite can form rapidly, in a matter of days, following a realistic mass-shedding event in which only ${\sim}2-3\%$ of the primary's mass is shed. Satellites can form in synchronous rotation due to their formation near the Roche limit. There is a strong preference for forming prolate (elongated) satellites, although some simulations result in oblate spheroids like Dimorphos. The distribution of simulated secondary shapes is broadly consistent with other binary systems, measured through radar or lightcurves. Unless Dimorphos's shape is an outlier, and considering the observational bias against lightcurve-based determination of secondary elongations for oblate bodies, we suggest there could be a significant population of oblate secondaries. If these satellites initially form with elongated shapes, a yet-unidentified pathway is needed to explain how they become oblate. Finally, we show that this chaotic formation pathway occasionally forms asteroid pairs and stable triples, including co-orbital satellites and satellites in mean motion resonances., Comment: 41 pages, 23 figures, accepted to PSJ, movies available at https://zenodo.org/doi/10.5281/zenodo.8387043
Published: 2024
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20. Ejecta from the DART-produced active asteroid Dimorphos

Author: Li, Jian-Yang, Hirabayashi, Masatoshi, Farnham, Tony L., Sunshine, Jessica M., Knight, Matthew M., Tancredi, Gonzalo, Moreno, Fernando, Murphy, Brian, Opitom, Cyrielle, Chesley, Steve, Scheeres, Daniel J., Thomas, Cristina A., Fahnestock, Eugene G., Cheng, Andrew F., Dressel, Linda, Ernst, Carolyn M., Ferrari, Fabio, Fitzsimmons, Alan, Ieva, Simone, Ivanovski, Stavro L., Kareta, Theodore, Kolokolova, Ludmilla, Lister, Tim, Raducan, Sabina D., Rivkin, Andrew S., Rossi, Alessandro, Soldini, Stefania, Stickle, Angela M., Vick, Alison, Vincent, Jean-Baptiste, Weaver, Harold A., Bagnulo, Stefano, Bannister, Michele T., Cambioni, Saverio, Campo Bagatin, Adriano, Chabot, Nancy L., Cremonese, Gabriele, Daly, R. Terik, Dotto, Elisabetta, Glenar, David A., Granvik, Mikael, Hasselmann, Pedro H., Herreros, Isabel, Jacobson, Seth, Jutzi, Martin, Kohout, Tomas, La Forgia, Fiorangela, Lazzarin, Monica, Lin, Zhong-Yi, Lolachi, Ramin, Lucchetti, Alice, Makadia, Rahil, Mazzotta Epifani, Elena, Michel, Patrick, Migliorini, Alessandra, Moskovitz, Nicholas A., Ormö, Jens, Pajola, Maurizio, Sánchez, Paul, Schwartz, Stephen R., Snodgrass, Colin, Steckloff, Jordan, Stubbs, Timothy J., Trigo-Rodríguez, Josep M., Li, Jian-Yang, Hirabayashi, Masatoshi, Farnham, Tony L., Sunshine, Jessica M., Knight, Matthew M., Tancredi, Gonzalo, Moreno, Fernando, Murphy, Brian, Opitom, Cyrielle, Chesley, Steve, Scheeres, Daniel J., Thomas, Cristina A., Fahnestock, Eugene G., Cheng, Andrew F., Dressel, Linda, Ernst, Carolyn M., Ferrari, Fabio, Fitzsimmons, Alan, Ieva, Simone, Ivanovski, Stavro L., Kareta, Theodore, Kolokolova, Ludmilla, Lister, Tim, Raducan, Sabina D., Rivkin, Andrew S., Rossi, Alessandro, Soldini, Stefania, Stickle, Angela M., Vick, Alison, Vincent, Jean-Baptiste, Weaver, Harold A., Bagnulo, Stefano, Bannister, Michele T., Cambioni, Saverio, Campo Bagatin, Adriano, Chabot, Nancy L., Cremonese, Gabriele, Daly, R. Terik, Dotto, Elisabetta, Glenar, David A., Granvik, Mikael, Hasselmann, Pedro H., Herreros, Isabel, Jacobson, Seth, Jutzi, Martin, Kohout, Tomas, La Forgia, Fiorangela, Lazzarin, Monica, Lin, Zhong-Yi, Lolachi, Ramin, Lucchetti, Alice, Makadia, Rahil, Mazzotta Epifani, Elena, Michel, Patrick, Migliorini, Alessandra, Moskovitz, Nicholas A., Ormö, Jens, Pajola, Maurizio, Sánchez, Paul, Schwartz, Stephen R., Snodgrass, Colin, Steckloff, Jordan, Stubbs, Timothy J., and Trigo-Rodríguez, Josep M.
Abstract: Some active asteroids have been proposed to be formed as a result of impact events1. Because active asteroids are generally discovered by chance only after their tails have fully formed, the process of how impact ejecta evolve into a tail has, to our knowledge, not been directly observed. The Double Asteroid Redirection Test (DART) mission of NASA2, in addition to having successfully changed the orbital period of Dimorphos3, demonstrated the activation process of an asteroid resulting from an impact under precisely known conditions. Here we report the observations of the DART impact ejecta with the Hubble Space Telescope from impact time T + 15 min to T + 18.5 days at spatial resolutions of around 2.1 km per pixel. Our observations reveal the complex evolution of the ejecta, which are first dominated by the gravitational interaction between the Didymos binary system and the ejected dust and subsequently by solar radiation pressure. The lowest-speed ejecta dispersed through a sustained tail that had a consistent morphology with previously observed asteroid tails thought to be produced by an impact4,5. The evolution of the ejecta after the controlled impact experiment of DART thus provides a framework for understanding the fundamental mechanisms that act on asteroids disrupted by a natural impact1,6., Validerad;2023;Nivå 2;2023-12-12 (hanlid);For funding information see: https://doi.org/10.1038/s41586-023-05811-4;Full text license: CC BY
Published: 2023
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21. Ejecta from the DART-produced active asteroid Dimorphos

Author: Li, Jian-Yang, Hirabayashi, Masatoshi, Farnham, Tony L., Sunshine, Jessica M., Knight, Matthew M., Tancredi, Gonzalo, Moreno, Fernando, Murphy, Brian, Opitom, Cyrielle, Chesley, Steve, Scheeres, Daniel J., Thomas, Cristina A., Fahnestock, Eugene G., Cheng, Andrew F., Dressel, Linda, Ernst, Carolyn M., Ferrari, Fabio, Fitzsimmons, Alan, Ieva, Simone, Ivanovski, Stavro L., Kareta, Theodore, Kolokolova, Ludmilla, Lister, Tim, Raducan, Sabina D., Rivkin, Andrew S., Rossi, Alessandro, Soldini, Stefania, Stickle, Angela M., Vick, Alison, Vincent, Jean-Baptiste, Weaver, Harold A., Bagnulo, Stefano, Bannister, Michele T., Cambioni, Saverio, Campo Bagatin, Adriano, Chabot, Nancy L., Cremonese, Gabriele, Daly, R. Terik, Dotto, Elisabetta, Glenar, David A., Granvik, Mikael, Hasselmann, Pedro H., Herreros, Isabel, Jacobson, Seth, Jutzi, Martin, Kohout, Tomas, La Forgia, Fiorangela, Lazzarin, Monica, Lin, Zhong-Yi, Lolachi, Ramin, Lucchetti, Alice, Makadia, Rahil, Mazzotta Epifani, Elena, Michel, Patrick, Migliorini, Alessandra, Moskovitz, Nicholas A., Ormö, Jens, Pajola, Maurizio, Sánchez, Paul, Schwartz, Stephen R., Snodgrass, Colin, Steckloff, Jordan, Stubbs, Timothy J., Trigo-Rodríguez, Josep M., Li, Jian-Yang, Hirabayashi, Masatoshi, Farnham, Tony L., Sunshine, Jessica M., Knight, Matthew M., Tancredi, Gonzalo, Moreno, Fernando, Murphy, Brian, Opitom, Cyrielle, Chesley, Steve, Scheeres, Daniel J., Thomas, Cristina A., Fahnestock, Eugene G., Cheng, Andrew F., Dressel, Linda, Ernst, Carolyn M., Ferrari, Fabio, Fitzsimmons, Alan, Ieva, Simone, Ivanovski, Stavro L., Kareta, Theodore, Kolokolova, Ludmilla, Lister, Tim, Raducan, Sabina D., Rivkin, Andrew S., Rossi, Alessandro, Soldini, Stefania, Stickle, Angela M., Vick, Alison, Vincent, Jean-Baptiste, Weaver, Harold A., Bagnulo, Stefano, Bannister, Michele T., Cambioni, Saverio, Campo Bagatin, Adriano, Chabot, Nancy L., Cremonese, Gabriele, Daly, R. Terik, Dotto, Elisabetta, Glenar, David A., Granvik, Mikael, Hasselmann, Pedro H., Herreros, Isabel, Jacobson, Seth, Jutzi, Martin, Kohout, Tomas, La Forgia, Fiorangela, Lazzarin, Monica, Lin, Zhong-Yi, Lolachi, Ramin, Lucchetti, Alice, Makadia, Rahil, Mazzotta Epifani, Elena, Michel, Patrick, Migliorini, Alessandra, Moskovitz, Nicholas A., Ormö, Jens, Pajola, Maurizio, Sánchez, Paul, Schwartz, Stephen R., Snodgrass, Colin, Steckloff, Jordan, Stubbs, Timothy J., and Trigo-Rodríguez, Josep M.
Abstract: Some active asteroids have been proposed to be formed as a result of impact events1. Because active asteroids are generally discovered by chance only after their tails have fully formed, the process of how impact ejecta evolve into a tail has, to our knowledge, not been directly observed. The Double Asteroid Redirection Test (DART) mission of NASA2, in addition to having successfully changed the orbital period of Dimorphos3, demonstrated the activation process of an asteroid resulting from an impact under precisely known conditions. Here we report the observations of the DART impact ejecta with the Hubble Space Telescope from impact time T + 15 min to T + 18.5 days at spatial resolutions of around 2.1 km per pixel. Our observations reveal the complex evolution of the ejecta, which are first dominated by the gravitational interaction between the Didymos binary system and the ejected dust and subsequently by solar radiation pressure. The lowest-speed ejecta dispersed through a sustained tail that had a consistent morphology with previously observed asteroid tails thought to be produced by an impact4,5. The evolution of the ejecta after the controlled impact experiment of DART thus provides a framework for understanding the fundamental mechanisms that act on asteroids disrupted by a natural impact1,6., Validerad;2023;Nivå 2;2023-12-12 (hanlid);For funding information see: https://doi.org/10.1038/s41586-023-05811-4;Full text license: CC BY
Published: 2023
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22. Near to Mid-Infrared Spectroscopy of (65803) Didymos as observed by JWST: Characterization Observations Supporting the Double Asteroid Redirection Test

Author: Rivkin, Andrew S., Thomas, Cristina A., Wong, Ian, Rozitis, Benjamin, de León, Julia, Holler, Bryan, Milam, Stefanie N., Howell, Ellen S., Hammel, Heidi B., Arredondo, Anicia, Brucato, John R., Epifani, Elena M., Ieva, Simone, La Forgia, Fiorangela, Lucas, Michael P., Lucchetti, Alice, Pajola, Maurizio, Poggiali, Giovanni, Sunshine, Jessica N., Trigo-Rodríguez, Josep M., Rivkin, Andrew S., Thomas, Cristina A., Wong, Ian, Rozitis, Benjamin, de León, Julia, Holler, Bryan, Milam, Stefanie N., Howell, Ellen S., Hammel, Heidi B., Arredondo, Anicia, Brucato, John R., Epifani, Elena M., Ieva, Simone, La Forgia, Fiorangela, Lucas, Michael P., Lucchetti, Alice, Pajola, Maurizio, Poggiali, Giovanni, Sunshine, Jessica N., and Trigo-Rodríguez, Josep M.
Abstract: The Didymos binary asteroid was the target of the Double Asteroid Redirection Test (DART) mission, which intentionally impacted Dimorphos, the smaller member of the binary system. We used the Near-Infrared Spectrograph (NIRSpec) and Mid-Infrared Instrument (MIRI) instruments on JWST to measure the 0.6-5 $\mu$m and 5-20 $\mu$m spectra of Didymos approximately two months after the DART impact. These observations confirm that Didymos belongs to the S asteroid class and is most consistent with LL chondrite composition as was previously determined from its 0.6-2.5-$\mu$m reflectance spectrum. Measurements at wavelengths $>$ 2.5 $\mu$m show Didymos to have thermal properties typical for an S-complex asteroid of its size and to be lacking absorptions deeper than $\sim$2\% due to OH or H2O. Didymos' mid-infrared emissivity spectrum is within the range of what has been observed on S-complex asteroids observed with Spitzer Space Telescope and is most consistent with emission from small ($<$ 25 $\mu$m) surface particles. We conclude that the observed reflectance and physical properties make the Didymos system a good proxy for the type of ordinary chondrite asteroids that cross near-Earth space, and a good representative of likely future impactors., Comment: Accepted by the Planetary Science Journal, 16 October 2023 Paper has 29 pages, 13 figures, 1 table
Published: 2023

23. Ejecta from the DART-produced active asteroid Dimorphos

Author: Li, Jian-Yang, Hirabayashi, Masatoshi, Farnham, Tony L., Sunshine, Jessica M., Knight, Matthew M., Tancredi, Gonzalo, Moreno, Fernando, Murphy, Brian, Opitom, Cyrielle, Chesley, Steve, Scheeres, Daniel J., Thomas, Cristina A., Fahnestock, Eugene G., Cheng, Andrew F., Dressel, Linda, Ernst, Carolyn M., Ferrari, Fabio, Fitzsimmons, Alan, Ieva, Simone, Ivanovski, Stavro L., Kareta, Teddy, Kolokolova, Ludmilla, Lister, Tim, Raducan, Sabina D., Rivkin, Andrew S., Rossi, Alessandro, Soldini, Stefania, Stickle, Angela M., Vick, Alison, Vincent, Jean-Baptiste, Weaver, Harold A., Bagnulo, Stefano, Bannister, Michele T., Cambioni, Saverio, Bagatin, Adriano Campo, Chabot, Nancy L., Cremonese, Gabriele, Daly, R. Terik, Dotto, Elisabetta, Glenar, David A., Granvik, Mikael, Hasselmann, Pedro H., Herreros, Isabel, Jacobson, Seth, Jutzi, Martin, Kohout, Tomas, La Forgia, Fiorangela, Lazzarin, Monica, Lin, Zhong-Yi, Lolachi, Ramin, Lucchetti, Alice, Makadia, Rahil, Epifani, Elena Mazzotta, Michel, Patrick, Migliorini, Alessandra, Moskovitz, Nicholas A., Orm., Jens, Pajola, Maurizio, nchez, Paul S., Schwartz, Stephen R., Snodgrass, Colin, Steckloff, Jordan, Stubbs, Timothy J., Trigo-Rodriguez, Josep M., Li, Jian-Yang, Hirabayashi, Masatoshi, Farnham, Tony L., Sunshine, Jessica M., Knight, Matthew M., Tancredi, Gonzalo, Moreno, Fernando, Murphy, Brian, Opitom, Cyrielle, Chesley, Steve, Scheeres, Daniel J., Thomas, Cristina A., Fahnestock, Eugene G., Cheng, Andrew F., Dressel, Linda, Ernst, Carolyn M., Ferrari, Fabio, Fitzsimmons, Alan, Ieva, Simone, Ivanovski, Stavro L., Kareta, Teddy, Kolokolova, Ludmilla, Lister, Tim, Raducan, Sabina D., Rivkin, Andrew S., Rossi, Alessandro, Soldini, Stefania, Stickle, Angela M., Vick, Alison, Vincent, Jean-Baptiste, Weaver, Harold A., Bagnulo, Stefano, Bannister, Michele T., Cambioni, Saverio, Bagatin, Adriano Campo, Chabot, Nancy L., Cremonese, Gabriele, Daly, R. Terik, Dotto, Elisabetta, Glenar, David A., Granvik, Mikael, Hasselmann, Pedro H., Herreros, Isabel, Jacobson, Seth, Jutzi, Martin, Kohout, Tomas, La Forgia, Fiorangela, Lazzarin, Monica, Lin, Zhong-Yi, Lolachi, Ramin, Lucchetti, Alice, Makadia, Rahil, Epifani, Elena Mazzotta, Michel, Patrick, Migliorini, Alessandra, Moskovitz, Nicholas A., Orm., Jens, Pajola, Maurizio, nchez, Paul S., Schwartz, Stephen R., Snodgrass, Colin, Steckloff, Jordan, Stubbs, Timothy J., and Trigo-Rodriguez, Josep M.
Abstract: Some active asteroids have been proposed to be the result of impact events. Because active asteroids are generally discovered serendipitously only after their tail formation, the process of the impact ejecta evolving into a tail has never been directly observed. NASA's Double Asteroid Redirection Test (DART) mission, apart from having successfully changed the orbital period of Dimorphos, demonstrated the activation process of an asteroid from an impact under precisely known impact conditions. Here we report the observations of the DART impact ejecta with the Hubble Space Telescope (HST) from impact time T+15 minutes to T+18.5 days at spatial resolutions of ~2.1 km per pixel. Our observations reveal a complex evolution of ejecta, which is first dominated by the gravitational interaction between the Didymos binary system and the ejected dust and later by solar radiation pressure. The lowest-speed ejecta dispersed via a sustained tail that displayed a consistent morphology with previously observed asteroid tails thought to be produced by impact. The ejecta evolution following DART's controlled impact experiment thus provides a framework for understanding the fundamental mechanisms acting on asteroids disrupted by natural impact., Comment: accepted by Nature
Published: 2023
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24. Momentum Transfer from the DART Mission Kinetic Impact on Asteroid Dimorphos

Author: Cheng, Andrew F., Agrusa, Harrison F., Barbee, Brent W., Meyer, Alex J., Farnham, Tony L., Raducan, Sabina D., Richardson, Derek C., Dotto, Elisabetta, Zinzi, Angelo, Della Corte, Vincenzo, Statler, Thomas S., Chesley, Steven, Naidu, Shantanu P., Hirabayashi, Masatoshi, Li, Jian-Yang, Eggl, Siegfried, Barnouin, Olivier S., Chabot, Nancy L., Chocron, Sidney, Collins, Gareth S., Daly, R. Terik, Davison, Thomas M., DeCoster, Mallory E., Ernst, Carolyn M., Ferrari, Fabio, Graninger, Dawn M., Jacobson, Seth A., Jutzi, Martin, Kumamoto, Kathryn M., Luther, Robert, Lyzhoft, Joshua R., Michel, Patrick, Murdoch, Naomi, Nakano, Ryota, Palmer, Eric, Rivkin, Andrew S., Scheeres, Daniel J., Stickle, Angela M., Sunshine, Jessica M., Trigo-Rodriguez, Josep M., Vincent, Jean-Baptiste, Walker, James D., Wünnemann, Kai, Zhang, Yun, Amoroso, Marilena, Bertini, Ivano, Brucato, John R., Capannolo, Andrea, Cremonese, Gabriele, Dall'Ora, Massimo, Deshapriya, Prasanna J. D., Gai, Igor, Hasselmann, Pedro H., Ieva, Simone, Impresario, Gabriele, Ivanovski, Stavro L., Lavagna, Michèle, Lucchetti, Alice, Epifani, Elena M., Modenini, Dario, Pajola, Maurizio, Palumbo, Pasquale, Perna, Davide, Pirrotta, Simone, Poggiali, Giovanni, Rossi, Alessandro, Tortora, Paolo, Zannoni, Marco, Zanotti, Giovanni, Cheng, Andrew F., Agrusa, Harrison F., Barbee, Brent W., Meyer, Alex J., Farnham, Tony L., Raducan, Sabina D., Richardson, Derek C., Dotto, Elisabetta, Zinzi, Angelo, Della Corte, Vincenzo, Statler, Thomas S., Chesley, Steven, Naidu, Shantanu P., Hirabayashi, Masatoshi, Li, Jian-Yang, Eggl, Siegfried, Barnouin, Olivier S., Chabot, Nancy L., Chocron, Sidney, Collins, Gareth S., Daly, R. Terik, Davison, Thomas M., DeCoster, Mallory E., Ernst, Carolyn M., Ferrari, Fabio, Graninger, Dawn M., Jacobson, Seth A., Jutzi, Martin, Kumamoto, Kathryn M., Luther, Robert, Lyzhoft, Joshua R., Michel, Patrick, Murdoch, Naomi, Nakano, Ryota, Palmer, Eric, Rivkin, Andrew S., Scheeres, Daniel J., Stickle, Angela M., Sunshine, Jessica M., Trigo-Rodriguez, Josep M., Vincent, Jean-Baptiste, Walker, James D., Wünnemann, Kai, Zhang, Yun, Amoroso, Marilena, Bertini, Ivano, Brucato, John R., Capannolo, Andrea, Cremonese, Gabriele, Dall'Ora, Massimo, Deshapriya, Prasanna J. D., Gai, Igor, Hasselmann, Pedro H., Ieva, Simone, Impresario, Gabriele, Ivanovski, Stavro L., Lavagna, Michèle, Lucchetti, Alice, Epifani, Elena M., Modenini, Dario, Pajola, Maurizio, Palumbo, Pasquale, Perna, Davide, Pirrotta, Simone, Poggiali, Giovanni, Rossi, Alessandro, Tortora, Paolo, Zannoni, Marco, and Zanotti, Giovanni
Abstract: The NASA Double Asteroid Redirection Test (DART) mission performed a kinetic impact on asteroid Dimorphos, the satellite of the binary asteroid (65803) Didymos, at 23:14 UTC on September 26, 2022 as a planetary defense test. DART was the first hypervelocity impact experiment on an asteroid at size and velocity scales relevant to planetary defense, intended to validate kinetic impact as a means of asteroid deflection. Here we report the first determination of the momentum transferred to an asteroid by kinetic impact. Based on the change in the binary orbit period, we find an instantaneous reduction in Dimorphos's along-track orbital velocity component of 2.70 +/- 0.10 mm/s, indicating enhanced momentum transfer due to recoil from ejecta streams produced by the impact. For a Dimorphos bulk density range of 1,500 to 3,300 kg/m$^3$, we find that the expected value of the momentum enhancement factor, $\beta$, ranges between 2.2 and 4.9, depending on the mass of Dimorphos. If Dimorphos and Didymos are assumed to have equal densities of 2,400 kg/m$^3$, $\beta$= 3.61 +0.19/-0.25 (1 $\sigma$). These $\beta$ values indicate that significantly more momentum was transferred to Dimorphos from the escaping impact ejecta than was incident with DART. Therefore, the DART kinetic impact was highly effective in deflecting the asteroid Dimorphos., Comment: accepted by Nature
Published: 2023
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25. Successful Kinetic Impact into an Asteroid for Planetary Defense

Author: Daly, R. Terik, Ernst, Carolyn M., Barnouin, Olivier S., Chabot, Nancy L., Rivkin, Andrew S., Cheng, Andrew F., Adams, Elena Y., Agrusa, Harrison F., Abel, Elisabeth D., Alford, Amy L., Asphaug, Erik I., Atchison, Justin A., Badger, Andrew R., Baki, Paul, Ballouz, Ronald-L., Bekker, Dmitriy L., Bellerose, Julie, Bhaskaran, Shyam, Buratti, Bonnie J., Cambioni, Saverio, Chen, Michelle H., Chesley, Steven R., Chiu, George, Collins, Gareth S., Cox, Matthew W., DeCoster, Mallory E., Ericksen, Peter S., Espiritu, Raymond C., Faber, Alan S., Farnham, Tony L., Ferrari, Fabio, Fletcher, Zachary J., Gaskell, Robert W., Graninger, Dawn M., Haque, Musad A., Harrington-Duff, Patricia A., Hefter, Sarah, Herreros, Isabel, Hirabayashi, Masatoshi, Huang, Philip M., Hsieh, Syau-Yun W., Jacobson, Seth A., Jenkins, Stephen N., Jensenius, Mark A., John, Jeremy W., Jutzi, Martin, Kohout, Tomas, Krueger, Timothy O., Laipert, Frank E., Lopez, Norberto R., Luther, Robert, Lucchetti, Alice, Mages, Declan M., Marchi, Simone, Martin, Anna C., McQuaide, Maria E., Michel, Patrick, Moskovitz, Nicholas A., Murphy, Ian W., Murdoch, Naomi, Naidu, Shantanu P., Nair, Hari, Nolan, Michael C., Ormö, Jens, Pajola, Maurizio, Palmer, Eric E., Peachey, James M., Pravec, Petr, Raducan, Sabina D., Ramesh, K. T., Ramirez, Joshua R., Reynolds, Edward L., Richman, Joshua E., Robin, Colas Q., Rodriguez, Luis M., Roufberg, Lew M., Rush, Brian P., Sawyer, Carolyn A., Scheeres, Daniel J., Scheirich, Petr, Schwartz, Stephen R., Shannon, Matthew P., Shapiro, Brett N., Shearer, Caitlin E., Smith, Evan J., Steele, R. Joshua, Steckloff, Jordan K, Stickle, Angela M., Sunshine, Jessica M., Superfin, Emil A., Tarzi, Zahi B., Thomas, Cristina A., Thomas, Justin R., Trigo-Rodríguez, Josep M., Tropf, B. Teresa, Vaughan, Andrew T., Velez, Dianna, Waller, C. Dany, Wilson, Daniel S., Wortman, Kristin A., Zhang, Yun, Daly, R. Terik, Ernst, Carolyn M., Barnouin, Olivier S., Chabot, Nancy L., Rivkin, Andrew S., Cheng, Andrew F., Adams, Elena Y., Agrusa, Harrison F., Abel, Elisabeth D., Alford, Amy L., Asphaug, Erik I., Atchison, Justin A., Badger, Andrew R., Baki, Paul, Ballouz, Ronald-L., Bekker, Dmitriy L., Bellerose, Julie, Bhaskaran, Shyam, Buratti, Bonnie J., Cambioni, Saverio, Chen, Michelle H., Chesley, Steven R., Chiu, George, Collins, Gareth S., Cox, Matthew W., DeCoster, Mallory E., Ericksen, Peter S., Espiritu, Raymond C., Faber, Alan S., Farnham, Tony L., Ferrari, Fabio, Fletcher, Zachary J., Gaskell, Robert W., Graninger, Dawn M., Haque, Musad A., Harrington-Duff, Patricia A., Hefter, Sarah, Herreros, Isabel, Hirabayashi, Masatoshi, Huang, Philip M., Hsieh, Syau-Yun W., Jacobson, Seth A., Jenkins, Stephen N., Jensenius, Mark A., John, Jeremy W., Jutzi, Martin, Kohout, Tomas, Krueger, Timothy O., Laipert, Frank E., Lopez, Norberto R., Luther, Robert, Lucchetti, Alice, Mages, Declan M., Marchi, Simone, Martin, Anna C., McQuaide, Maria E., Michel, Patrick, Moskovitz, Nicholas A., Murphy, Ian W., Murdoch, Naomi, Naidu, Shantanu P., Nair, Hari, Nolan, Michael C., Ormö, Jens, Pajola, Maurizio, Palmer, Eric E., Peachey, James M., Pravec, Petr, Raducan, Sabina D., Ramesh, K. T., Ramirez, Joshua R., Reynolds, Edward L., Richman, Joshua E., Robin, Colas Q., Rodriguez, Luis M., Roufberg, Lew M., Rush, Brian P., Sawyer, Carolyn A., Scheeres, Daniel J., Scheirich, Petr, Schwartz, Stephen R., Shannon, Matthew P., Shapiro, Brett N., Shearer, Caitlin E., Smith, Evan J., Steele, R. Joshua, Steckloff, Jordan K, Stickle, Angela M., Sunshine, Jessica M., Superfin, Emil A., Tarzi, Zahi B., Thomas, Cristina A., Thomas, Justin R., Trigo-Rodríguez, Josep M., Tropf, B. Teresa, Vaughan, Andrew T., Velez, Dianna, Waller, C. Dany, Wilson, Daniel S., Wortman, Kristin A., and Zhang, Yun
Abstract: While no known asteroid poses a threat to Earth for at least the next century, the catalog of near-Earth asteroids is incomplete for objects whose impacts would produce regional devastation. Several approaches have been proposed to potentially prevent an asteroid impact with Earth by deflecting or disrupting an asteroid. A test of kinetic impact technology was identified as the highest priority space mission related to asteroid mitigation. NASA's Double Asteroid Redirection Test (DART) mission is the first full-scale test of kinetic impact technology. The mission's target asteroid was Dimorphos, the secondary member of the S-type binary near-Earth asteroid (65803) Didymos. This binary asteroid system was chosen to enable ground-based telescopes to quantify the asteroid deflection caused by DART's impact. While past missions have utilized impactors to investigate the properties of small bodies those earlier missions were not intended to deflect their targets and did not achieve measurable deflections. Here we report the DART spacecraft's autonomous kinetic impact into Dimorphos and reconstruct the impact event, including the timeline leading to impact, the location and nature of the DART impact site, and the size and shape of Dimorphos. The successful impact of the DART spacecraft with Dimorphos and the resulting change in Dimorphos's orbit demonstrates that kinetic impactor technology is a viable technique to potentially defend Earth if necessary., Comment: Accepted by Nature
Published: 2023
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26. Ejecta from the DART-produced active asteroid Dimorphos

Author: Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Li, Jian-Yang, Hirabayashi, Masatoshi, Farnham, Tony, Sunshine, Jessica M., Knight, Matthew M., Tancredi, Gonzalo, Moreno, Fernando, Murphy, Brian, Opitom, Cyrielle, Chesley, Steven, Scheeres, Daniel J., Thomas, Cristina, Fahnestock, Eugene G., Cheng, Andy F., Dressel, Linda, Ernst, Carolyn, Ferrari, Fabio, Fitzsimmons, Alan, Ieva, Simone, Ivanovski, Stavro, Kareta, Teddy, Kolokolova, Ludmilla, Lister, Tim, Raducan, Sabina D., Rivkin, Andy, Rossi, Alessandro, Soldini, Stefania, Stickle, Angela M., Vick, Alison, Vincent, Jean-Baptiste, Weaver, Harold A., Bagnulo, Stefano, Bannister, Michele T., Cambioni, Saverio, Campo Bagatin, Adriano, Chabot, Nancy, Cremonese, Gabriele, Daly, R. Terik, Dotto, Elisabetta, Glenar, David A., Granvik, Mikael, Hasselmann, Pedro H., Herreros, Isabel, Jacobson, Seth A., Jutzi, Martin, Kohout, Tomas, La Forgia, Fiorangela, Lazzarin, Monica, Lin, Zhong-Yi, Lolachi, Ramin, Lucchetti, Alice, Makadia, Rahil, Mazzotta Epifani, Elena, Michel, Patrick, Migliorini, Alessandra, Moskovitz, Nicholas A., Ormö, Jens, Pajola, Maurizio, Sánchez, Paul, Schwartz, Stephen R., Snodgrass, Colin, Steckloff, Jordan, Stubbs, Timothy J., Trigo-Rodríguez, Josep M., Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Li, Jian-Yang, Hirabayashi, Masatoshi, Farnham, Tony, Sunshine, Jessica M., Knight, Matthew M., Tancredi, Gonzalo, Moreno, Fernando, Murphy, Brian, Opitom, Cyrielle, Chesley, Steven, Scheeres, Daniel J., Thomas, Cristina, Fahnestock, Eugene G., Cheng, Andy F., Dressel, Linda, Ernst, Carolyn, Ferrari, Fabio, Fitzsimmons, Alan, Ieva, Simone, Ivanovski, Stavro, Kareta, Teddy, Kolokolova, Ludmilla, Lister, Tim, Raducan, Sabina D., Rivkin, Andy, Rossi, Alessandro, Soldini, Stefania, Stickle, Angela M., Vick, Alison, Vincent, Jean-Baptiste, Weaver, Harold A., Bagnulo, Stefano, Bannister, Michele T., Cambioni, Saverio, Campo Bagatin, Adriano, Chabot, Nancy, Cremonese, Gabriele, Daly, R. Terik, Dotto, Elisabetta, Glenar, David A., Granvik, Mikael, Hasselmann, Pedro H., Herreros, Isabel, Jacobson, Seth A., Jutzi, Martin, Kohout, Tomas, La Forgia, Fiorangela, Lazzarin, Monica, Lin, Zhong-Yi, Lolachi, Ramin, Lucchetti, Alice, Makadia, Rahil, Mazzotta Epifani, Elena, Michel, Patrick, Migliorini, Alessandra, Moskovitz, Nicholas A., Ormö, Jens, Pajola, Maurizio, Sánchez, Paul, Schwartz, Stephen R., Snodgrass, Colin, Steckloff, Jordan, Stubbs, Timothy J., and Trigo-Rodríguez, Josep M.
Abstract: Some active asteroids have been proposed to be the result of impact events1. Because active asteroids are generally discovered serendipitously only after their tail formation, the process of the impact ejecta evolving into a tail has never been directly observed. NASA's Double Asteroid Redirection Test (DART) mission2, apart from having successfully changed the orbital period of Dimorphos3, demonstrated the activation process of an asteroid from an impact under precisely known impact conditions. Here we report the observations of the DART impact ejecta with the Hubble Space Telescope (HST) from impact time T+15 minutes to T+18.5 days at spatial resolutions of ~2.1 km per pixel. Our observations reveal a complex evolution of ejecta, which is first dominated by the gravitational interaction between the Didymos binary system and the ejected dust and later by solar radiation pressure. The lowest-speed ejecta dispersed via a sustained tail that displayed a consistent morphology with previously observed asteroid tails thought to be produced by impact4,5. The ejecta evolution following DART’s controlled impact experiment thus provides a framework for understanding the fundamental mechanisms acting on asteroids disrupted by natural impact1,6.
Published: 2023

27. Anticipated geological assessment of the (65803) Didymos–Dimorphos system, target of the DART–LICIACube mission

Author: Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, University of Arizona, National Aeronautics and Space Administration (US), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Agencia Estatal de Investigación (España), European Space Agency, Centre National de la Recherche Scientifique (France), Pajola, Maurizio, Barnouin, Olivier S., Lucchetti, Alice, Ernst, Carolyn M., Trigo-Rodríguez, Josep María, Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, University of Arizona, National Aeronautics and Space Administration (US), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Agencia Estatal de Investigación (España), European Space Agency, Centre National de la Recherche Scientifique (France), Pajola, Maurizio, Barnouin, Olivier S., Lucchetti, Alice, Ernst, Carolyn M., and Trigo-Rodríguez, Josep María
Abstract: On 2022 September 26, the DART spacecraft will impact the surface of Dimorphos, the ∼160 m size satellite of the binary near-Earth asteroid (NEA) (65803) Didymos. What will be observed on the surfaces of both asteroids and at the DART impact site is largely unknown, beyond the details of Didymos revealed by previous Arecibo and Goldstone radar observations. We present here the expected DART and LICIACube observations of the Didymos system and discuss the planned mapping strategies. By searching similar geological features and processes identified on other NEAs, we constrain the impact conditions that DART might encounter at Dimorphos, assessing both the asteroid's surface and interior structure.
Published: 2022

28. Shape modeling of dimorphos for the Double Asteroid Redirection Test (DART)

Author: Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, National Aeronautics and Space Administration (US), Agencia Estatal de Investigación (España), European Commission, European Research Council, Ministerio de Ciencia, Innovación y Universidades (España), Daly, R. Terik, Ernst, Carolyn M., Barnouin, Olivier S., Gaskell, Robert W., Palmer, Eric E., Nair, Hari, Espiritu, Ray C., Hasnain, Sarah, Waller, Dany, Stickle, Angela M., Nolan, Michael C., Trigo-Rodríguez, Josep María, Dotto, Elisabetta, Lucchetti, Alice, Pajola, Maurizio, Ieva, Simone, Michel, Patrick, Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, National Aeronautics and Space Administration (US), Agencia Estatal de Investigación (España), European Commission, European Research Council, Ministerio de Ciencia, Innovación y Universidades (España), Daly, R. Terik, Ernst, Carolyn M., Barnouin, Olivier S., Gaskell, Robert W., Palmer, Eric E., Nair, Hari, Espiritu, Ray C., Hasnain, Sarah, Waller, Dany, Stickle, Angela M., Nolan, Michael C., Trigo-Rodríguez, Josep María, Dotto, Elisabetta, Lucchetti, Alice, Pajola, Maurizio, Ieva, Simone, and Michel, Patrick
Abstract: The Double Asteroid Redirection Test (DART) is the first planetary defense test mission. It will demonstrate the kinetic impactor technique by intentionally colliding the DART spacecraft with the near-Earth asteroid Dimorphos. The main DART spacecraft is accompanied by the Italian Space Agency Light Italian CubeSat for Imaging of Asteroids (LICIACube). Shape modeling efforts will estimate the volume of Dimorphos and constrain the nature of the impact site. The DART mission uses stereophotoclinometry (SPC) as its primary shape modeling technique. DART is essentially a worst-case scenario for any image-based shape modeling approach because images taken by the camera on board the DART spacecraft, called the Didymos Reconnaissance and Asteroid Camera for Optical navigation (DRACO), possess little stereo and no lighting variation; they simply zoom in on the asteroid. LICIACube images add some stereo, but the images are substantially lower in resolution than the DRACO images. Despite the far-from-optimal imaging conditions, our tests indicate that we can identify the impact site to an accuracy and precision better than 10% the size of the spacecraft core, estimate the volume of Dimorphos to better than 25%, and measure tilts at the impact site over the scale of the spacecraft with an accuracy better than 7°. In short, we will know with excellent accuracy where the DART spacecraft hit, with reasonable knowledge of local tilt, and determine the volume well enough that uncertainties in the density of Dimorphos will be comparable to or dominate the uncertainty in the estimated mass. The tests reported here demonstrate that SPC is a robust technique for shape modeling, even with suboptimal images.
Published: 2022

29. Effects of impact and target parameters on the results of a kinetic impactor: predictions for the Double Asteroid Redirection Test (DART) mission

Author: Stickle, Angela M., DeCoster, Mallory E., Burger, Christoph, Caldwell, Wendy K., Graninger, Dawn, Kumamoto, Kathryn M., Luther, Robert, Ormö, Jens, Raducan, Sabina, Rainey, Emma, Schäfer, Christoph M., Walker, James D., Zhang, Yun, Michel, Patrick, Owen, J. Michael, Barnouin, Olivier, Cheng, Andy F., Cochron, Sidney, Collins, Gareth S., Davison, Thomas M., Dotto, Elisabetta, Ferrari, Fabio, Herreros, M. Isabel, Ivanovski, Stavro L., Jutzi, Martin, Lucchetti, Alice, Martellato, Elena, Pajola, Maurizio, Plesko, Cathy S., Syal, Megan Bruck, Schwartz, Stephen R., Sunshine, Jessica M., Wünnemann, Kai, Stickle, Angela M., DeCoster, Mallory E., Burger, Christoph, Caldwell, Wendy K., Graninger, Dawn, Kumamoto, Kathryn M., Luther, Robert, Ormö, Jens, Raducan, Sabina, Rainey, Emma, Schäfer, Christoph M., Walker, James D., Zhang, Yun, Michel, Patrick, Owen, J. Michael, Barnouin, Olivier, Cheng, Andy F., Cochron, Sidney, Collins, Gareth S., Davison, Thomas M., Dotto, Elisabetta, Ferrari, Fabio, Herreros, M. Isabel, Ivanovski, Stavro L., Jutzi, Martin, Lucchetti, Alice, Martellato, Elena, Pajola, Maurizio, Plesko, Cathy S., Syal, Megan Bruck, Schwartz, Stephen R., Sunshine, Jessica M., and Wünnemann, Kai
Abstract: The Double Asteroid Redirection Test (DART) spacecraft will impact into the asteroid Dimorphos on September 26, 2022 as a test of the kinetic impactor technique for planetary defense. The efficiency of the deflection following a kinetic impactor can be represented using the momentum enhancement factor, Beta, which is dependent on factors such as impact geometry and the specific target material properties. Currently, very little is known about Dimorphos and its material properties that introduces uncertainty in the results of the deflection efficiency observables, including crater formation, ejecta distribution, and Beta. The DART Impact Modeling Working Group (IWG) is responsible for using impact simulations to better understand the results of the DART impact. Pre-impact simulation studies also provide considerable insight into how different properties and impact scenarios affect momentum enhancement following a kinetic impact. This insight provides a basis for predicting the effects of the DART impact and the first understanding of how to interpret results following the encounter. Following the DART impact, the knowledge gained from these studies will inform the initial simulations that will recreate the impact conditions, including providing estimates for potential material properties of Dimorphos and Beta resulting from DARTs impact. This paper summarizes, at a high level, what has been learned from the IWG simulations and experiments in preparation for the DART impact. While unknown, estimates for reasonable potential material properties of Dimorphos provide predictions for Beta of 1-5, depending on end-member cases in the strength regime., Comment: Accepted to PSJ Didymos-DART Focus Issue
Published: 2022

30. After DART: Using the first full-scale test of a kinetic impactor to inform a future planetary defense mission

Author: Statler, Thomas S., Raducan, Sabina D., Barnouin, Olivier S., DeCoster, Mallory E., Chesley, Steven R., Barbee, Brent, Agrusa, Harrison F., Cambioni, Saverio, Cheng, Andrew F., Dotto, Elisabetta, Eggl, Siegfried, Fahnestock, Eugene G., Ferrari, Fabio, Graninger, Dawn, Herique, Alain, Herreros, Isabel, Hirabayashi, Masatoshi, Ivanovski, Stavro, Jutzi, Martin, Karatekin, Özgür, Lucchetti, Alice, Luther, Robert, Makadia, Rahil, Marzari, Francesco, Michel, Patrick, Murdoch, Naomi, Nakano, Ryota, Ormö, Jens, Pajola, Maurizio, Rivkin, Andrew S., Rossi, Alessandro, Sánchez, Paul, Schwartz, Stephen R., Soldini, Stefania, Souami, Damya, Stickle, Angela, Tortora, Paolo, Trigo-Rodríguez, Josep M., Venditti, Flaviane, Vincent, Jean-Baptiste, Wünnemann, Kai, Statler, Thomas S., Raducan, Sabina D., Barnouin, Olivier S., DeCoster, Mallory E., Chesley, Steven R., Barbee, Brent, Agrusa, Harrison F., Cambioni, Saverio, Cheng, Andrew F., Dotto, Elisabetta, Eggl, Siegfried, Fahnestock, Eugene G., Ferrari, Fabio, Graninger, Dawn, Herique, Alain, Herreros, Isabel, Hirabayashi, Masatoshi, Ivanovski, Stavro, Jutzi, Martin, Karatekin, Özgür, Lucchetti, Alice, Luther, Robert, Makadia, Rahil, Marzari, Francesco, Michel, Patrick, Murdoch, Naomi, Nakano, Ryota, Ormö, Jens, Pajola, Maurizio, Rivkin, Andrew S., Rossi, Alessandro, Sánchez, Paul, Schwartz, Stephen R., Soldini, Stefania, Souami, Damya, Stickle, Angela, Tortora, Paolo, Trigo-Rodríguez, Josep M., Venditti, Flaviane, Vincent, Jean-Baptiste, and Wünnemann, Kai
Abstract: NASA's Double Asteroid Redirection Test (DART) is the first full-scale test of an asteroid deflection technology. Results from the hypervelocity kinetic impact and Earth-based observations, coupled with LICIACube and the later Hera mission, will result in measurement of the momentum transfer efficiency accurate to ~10% and characterization of the Didymos binary system. But DART is a single experiment; how could these results be used in a future planetary defense necessity involving a different asteroid? We examine what aspects of Dimorphos's response to kinetic impact will be constrained by DART results; how these constraints will help refine knowledge of the physical properties of asteroidal materials and predictive power of impact simulations; what information about a potential Earth impactor could be acquired before a deflection effort; and how design of a deflection mission should be informed by this understanding. We generalize the momentum enhancement factor $\beta$, showing that a particular direction-specific $\beta$ will be directly determined by the DART results, and that a related direction-specific $\beta$ is a figure of merit for a kinetic impact mission. The DART $\beta$ determination constrains the ejecta momentum vector, which, with hydrodynamic simulations, constrains the physical properties of Dimorphos's near-surface. In a hypothetical planetary defense exigency, extrapolating these constraints to a newly discovered asteroid will require Earth-based observations and benefit from in-situ reconnaissance. We show representative predictions for momentum transfer based on different levels of reconnaissance and discuss strategic targeting to optimize the deflection and reduce the risk of a counterproductive deflection in the wrong direction., Comment: 30 pages, 7 figures. Planetary Science Journal, in press, accepted 2022 September 22
Published: 2022

31. Captured Small Solar System Bodies in the Ice Giant Region

Author: Holt, Timothy R., Buratti, Bonnie, Castillo-Rogez, Julie, Davidsson, Bjorn J. R., Denk, Tilmann, Horner, Jonti, Holler, Bryan J, Jha, Devanshu, Lucchetti, Alice, Nesvorny, David, Pajola, Maurizio, Porter, Simon, Rhoden, Alyssa, Rappolee, Steven, Schindhelm, Rebecca, Spilker, Linda, Verbiscer, Anne, Holt, Timothy R., Buratti, Bonnie, Castillo-Rogez, Julie, Davidsson, Bjorn J. R., Denk, Tilmann, Horner, Jonti, Holler, Bryan J, Jha, Devanshu, Lucchetti, Alice, Nesvorny, David, Pajola, Maurizio, Porter, Simon, Rhoden, Alyssa, Rappolee, Steven, Schindhelm, Rebecca, Spilker, Linda, and Verbiscer, Anne
Abstract: This white paper advocates for the inclusion of small, captured Outer Solar system objects, found in the Ice Giant region in the next Decadal Survey. These objects include the Trojans and Irregular satellite populations of Uranus and Neptune. The captured small bodies provide vital clues as to the formation of our Solar system. They have unique dynamical situations, which any model of Solar system formation needs to explain. The major issue is that so few of these objects have been discovered, with very little information known about them. The purpose of this document is to prioritize further discovery and characterization of these objects. This will require the use of NASA and NSF facilities over the 2023 2032 decade, including additional support for analysis. This is in preparation for potential future insitu missions in the following decades., Comment: Community Science White Paper for the Planetary and Astrobiology Decadal Survey, 2023-2032
Published: 2020

32. High Quality Software for Planetary Science from Space

Author: Lazzarotto, Francesco, Cremonese, Gabriele, Lucchetti, Alice, Re, Cristina, Simioni, Emanuele, Pajola, Maurizio, Cambianica, Pamela, Munaretto, Giovanni, Lazzarotto, Francesco, Cremonese, Gabriele, Lucchetti, Alice, Re, Cristina, Simioni, Emanuele, Pajola, Maurizio, Cambianica, Pamela, and Munaretto, Giovanni
Abstract: Planetary science space missions need high quality software ed efficient algorithms in order to extract innovative scientific results from flight data. Reliable and efficient software technologies are increasingly vital to improve and prolong the exploiting of the results of a mission, to allow the application of established algorithms and technologies also to future space missions and for the scientific analysis of archived data. Here after will be given an in-depth analysis study accompanied by implementation examples on ESA and ASI missions and some remarkable results fruit of decades of important experience reached by space agencies and research institutes in the field. Space applications software quality analysis is not different from other application contexts, among the hi-tech and hi-reliability fields. We describe here a Software Quality study in general, then we will focus on the quality of space mission software (s/w) with details on some notable cases., Comment: presentation at XVI Congresso Nazionale di Scienze Planetarie (National Conference on Planetary Sciences) held at Centro Culturale San Gaetano, via Altinate, 71, Padova, Italy on 3-7 February, 2020 Affiliation: University of Padova, 6 pages, 4 figures
Published: 2020
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33. High Quality Software for Planetary Science from Space

Author: Lazzarotto, Francesco, Cremonese, Gabriele, Lucchetti, Alice, Re, Cristina, Simioni, Emanuele, Pajola, Maurizio, Cambianica, Pamela, Munaretto, Giovanni, Lazzarotto, Francesco, Cremonese, Gabriele, Lucchetti, Alice, Re, Cristina, Simioni, Emanuele, Pajola, Maurizio, Cambianica, Pamela, and Munaretto, Giovanni
Abstract: Planetary science space missions need high quality software ed efficient algorithms in order to extract innovative scientific results from flight data. Reliable and efficient software technologies are increasingly vital to improve and prolong the exploiting of the results of a mission, to allow the application of established algorithms and technologies also to future space missions and for the scientific analysis of archived data. Here after will be given an in-depth analysis study accompanied by implementation examples on ESA and ASI missions and some remarkable results fruit of decades of important experience reached by space agencies and research institutes in the field. Space applications software quality analysis is not different from other application contexts, among the hi-tech and hi-reliability fields. We describe here a Software Quality study in general, then we will focus on the quality of space mission software (s/w) with details on some notable cases., Comment: presentation at XVI Congresso Nazionale di Scienze Planetarie (National Conference on Planetary Sciences) held at Centro Culturale San Gaetano, via Altinate, 71, Padova, Italy on 3-7 February, 2020 Affiliation: University of Padova, 6 pages, 4 figures
Published: 2020
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34. Abundance and size-frequency distributions of boulders in Linne crater's ejecta (Moon)

Author: Pajola, Maurizio, Pozzobon, Riccardo, Lucchetti, Alice, Rossato, Sandro, Baratti, Emanuele, Galluzzi, Valentina, Cremonese, Gabriele, Pajola, Maurizio, Pozzobon, Riccardo, Lucchetti, Alice, Rossato, Sandro, Baratti, Emanuele, Galluzzi, Valentina, and Cremonese, Gabriele
Abstract: This paper presents the abundances and the size-frequency distributions (SFD) of the ejected boulders surrounding the Linne crater, located on the Moon's Mare Serenitatis basin. By means of Lunar Reconnaissance Orbiter Camera high-resolution images we prepare a context geological map of the Linne crater as well as we identify 12000 boulders > 4.4 m, with a maximum measured size of 30.8 m. The cumulative number of boulders per km2 is fitted with a power-law curve with index -4.03 +0.09/-0.10. By studying the radial ejecta abundances, we find that the largest ones are located within the first 2 km from the crater's centre, while few tens of boulders with sizes < 8 m are detectable above 5 km from the crater's rim. We find that the Linne proximal ejecta blanket is slightly asymmetrical, as indicated in the geological map too, showing a density increase in the NE-SW direction. This may be the result of an oblique impact emplacement of the original impactor, or it may be explained with a perpendicular impact in the Mare Serenitatis location, but on a surface with lunar basalts with different local mechanical properties. By exploiting our boulders size density as a function of the distance from the crater's centre, we derive a possible regolith thickness at the Linne impact of 4.75 m, supporting similar values based on Earth-based radar and optical data in the Mare Serenitatis basin., Comment: Paper accepted by Planetary and Space Science Journal on 27 Nov 2018
Published: 2018

35. Towards a Global Unified Model of Europa's Tenuous Atmosphere

Author: Plainaki, Christina, Cassidy, Tim A., Shematovich, Valery I., Milillo, Anna, Wurz, Peter, Vorburger, Audrey, Roth, Lorenz, Galli, Andre, Rubin, Martin, Bloecker, Aljona, Brandt, Pontus C., Crary, Frank, Dandouras, Iannis, Jia, Xianzhe, Grassi, Davide, Hartogh, Paul, Lucchetti, Alice, McGrath, Melissa, Mangano, Valeria, Mura, Alessandro, Orsini, Stefano, Paranicas, Chris, Radioti, Aikaterini, Retherford, Kurt D., Saur, Joachim, Teolis, Ben, Plainaki, Christina, Cassidy, Tim A., Shematovich, Valery I., Milillo, Anna, Wurz, Peter, Vorburger, Audrey, Roth, Lorenz, Galli, Andre, Rubin, Martin, Bloecker, Aljona, Brandt, Pontus C., Crary, Frank, Dandouras, Iannis, Jia, Xianzhe, Grassi, Davide, Hartogh, Paul, Lucchetti, Alice, McGrath, Melissa, Mangano, Valeria, Mura, Alessandro, Orsini, Stefano, Paranicas, Chris, Radioti, Aikaterini, Retherford, Kurt D., Saur, Joachim, and Teolis, Ben
Abstract: Despite the numerous modeling efforts of the past, our knowledge on the radiation-induced physical and chemical processes in Europa's tenuous atmosphere and on the exchange of material between the moon's surface and Jupiter's magnetosphere remains limited. In lack of an adequate number of in situ observations, the existence of a wide variety of models based on different scenarios and considerations has resulted in a fragmentary understanding of the interactions of the magnetospheric ion population with both the moon's icy surface and neutral gas envelope. Models show large discrepancy in the source and loss rates of the different constituents as well as in the determination of the spatial distribution of the atmosphere and its variation with time. The existence of several models based on very different approaches highlights the need of a detailed comparison among them with the final goal of developing a unified model of Europa's tenuous atmosphere. The availability to the science community of such a model could be of particular interest in view of the planning of the future mission observations ( e.g., ESA's JUpiter ICy moons Explorer ( JUICE) mission, and NASA's Europa Clipper mission). We review the existing models of Europa's tenuous atmosphere and discuss each of their derived characteristics of the neutral environment. We also discuss discrepancies among different models and the assumptions of the plasma environment in the vicinity of Europa. A summary of the existing observations of both the neutral and the plasma environments at Europa is also presented. The characteristics of a global unified model of the tenuous atmosphere are, then, discussed. Finally, we identify needed future experimental work in laboratories and propose some suitable observation strategies for upcoming missions.
Published: 2018

36. Towards a Global Unified Model of Europa's Tenuous Atmosphere

Author: Plainaki, Christina, Cassidy, Tim A., Shematovich, Valery I., Milillo, Anna, Wurz, Peter, Vorburger, Audrey, Roth, Lorenz, Galli, Andre, Rubin, Martin, Bloecker, Aljona, Brandt, Pontus C., Crary, Frank, Dandouras, Iannis, Jia, Xianzhe, Grassi, Davide, Hartogh, Paul, Lucchetti, Alice, McGrath, Melissa, Mangano, Valeria, Mura, Alessandro, Orsini, Stefano, Paranicas, Chris, Radioti, Aikaterini, Retherford, Kurt D., Saur, Joachim, Teolis, Ben, Plainaki, Christina, Cassidy, Tim A., Shematovich, Valery I., Milillo, Anna, Wurz, Peter, Vorburger, Audrey, Roth, Lorenz, Galli, Andre, Rubin, Martin, Bloecker, Aljona, Brandt, Pontus C., Crary, Frank, Dandouras, Iannis, Jia, Xianzhe, Grassi, Davide, Hartogh, Paul, Lucchetti, Alice, McGrath, Melissa, Mangano, Valeria, Mura, Alessandro, Orsini, Stefano, Paranicas, Chris, Radioti, Aikaterini, Retherford, Kurt D., Saur, Joachim, and Teolis, Ben
Abstract: Despite the numerous modeling efforts of the past, our knowledge on the radiation-induced physical and chemical processes in Europa's tenuous atmosphere and on the exchange of material between the moon's surface and Jupiter's magnetosphere remains limited. In lack of an adequate number of in situ observations, the existence of a wide variety of models based on different scenarios and considerations has resulted in a fragmentary understanding of the interactions of the magnetospheric ion population with both the moon's icy surface and neutral gas envelope. Models show large discrepancy in the source and loss rates of the different constituents as well as in the determination of the spatial distribution of the atmosphere and its variation with time. The existence of several models based on very different approaches highlights the need of a detailed comparison among them with the final goal of developing a unified model of Europa's tenuous atmosphere. The availability to the science community of such a model could be of particular interest in view of the planning of the future mission observations ( e.g., ESA's JUpiter ICy moons Explorer ( JUICE) mission, and NASA's Europa Clipper mission). We review the existing models of Europa's tenuous atmosphere and discuss each of their derived characteristics of the neutral environment. We also discuss discrepancies among different models and the assumptions of the plasma environment in the vicinity of Europa. A summary of the existing observations of both the neutral and the plasma environments at Europa is also presented. The characteristics of a global unified model of the tenuous atmosphere are, then, discussed. Finally, we identify needed future experimental work in laboratories and propose some suitable observation strategies for upcoming missions.
Published: 2018

37. Abundance and size-frequency distributions of boulders in Linne crater's ejecta (Moon)

Author: Pajola, Maurizio, Pozzobon, Riccardo, Lucchetti, Alice, Rossato, Sandro, Baratti, Emanuele, Galluzzi, Valentina, Cremonese, Gabriele, Pajola, Maurizio, Pozzobon, Riccardo, Lucchetti, Alice, Rossato, Sandro, Baratti, Emanuele, Galluzzi, Valentina, and Cremonese, Gabriele
Abstract: This paper presents the abundances and the size-frequency distributions (SFD) of the ejected boulders surrounding the Linne crater, located on the Moon's Mare Serenitatis basin. By means of Lunar Reconnaissance Orbiter Camera high-resolution images we prepare a context geological map of the Linne crater as well as we identify 12000 boulders > 4.4 m, with a maximum measured size of 30.8 m. The cumulative number of boulders per km2 is fitted with a power-law curve with index -4.03 +0.09/-0.10. By studying the radial ejecta abundances, we find that the largest ones are located within the first 2 km from the crater's centre, while few tens of boulders with sizes < 8 m are detectable above 5 km from the crater's rim. We find that the Linne proximal ejecta blanket is slightly asymmetrical, as indicated in the geological map too, showing a density increase in the NE-SW direction. This may be the result of an oblique impact emplacement of the original impactor, or it may be explained with a perpendicular impact in the Mare Serenitatis location, but on a surface with lunar basalts with different local mechanical properties. By exploiting our boulders size density as a function of the distance from the crater's centre, we derive a possible regolith thickness at the Linne impact of 4.75 m, supporting similar values based on Earth-based radar and optical data in the Mare Serenitatis basin., Comment: Paper accepted by Planetary and Space Science Journal on 27 Nov 2018
Published: 2018

38. The southern hemisphere of 67P/Churyumov-Gerasimenko : Analysis of the preperihelion size-frequency distribution of boulders >= 7m

Author: Pajola, Maurizio, Lucchetti, Alice, Vincent, Jean-Baptiste, Oklay, Nilda, El-Maarry, Mohamed R., Bertini, Ivano, Naletto, Giampiero, Lazzarin, Monica, Massironi, Matteo, Sierks, Holger, Barbieri, Cesare, Lamy, Philippe, Rodrigo, Rafael, Koschny, Detlef, Rickman, Hans, Keller, Horst U., Agarwal, Jessica, A'Hearn, Michael F., Barucci, Maria A., Bertaux, Jean-Loup, Boudreault, Steve, Cremonese, Gabriele, Da Deppo, Vania, Davidsson, Bjorn, Debei, Stefano, De Cecco, Mariolino, Deller, Jakob, Fornasier, Sonia, Fulle, Marco, Gicquel, Adeline, Groussin, Olivier, Gutierrez, Pedro J., Guetler, Carsten, Hofmann, Marc, Hoefner, Sebastian, Hviid, Stubbe F., Ip, Wing-Huen, Jorda, Laurent, Knollenberg, Joerg, Kramm, J. -Rainer, Kuehrt, Ekkehard, Kuppers, Michael, La Forgia, Fiorangela, Lara, Luisa M., Lee, Jui-Chi, Lin, Zhong-Yi, Lopez Moreno, Jose J., Marzari, Francesco, Michalik, Harald, Mottola, Stefano, Preusker, Frank, Scholten, Frank, Thomas, Nicholas, Toth, Imre, Tubiana, Cecilia, Pajola, Maurizio, Lucchetti, Alice, Vincent, Jean-Baptiste, Oklay, Nilda, El-Maarry, Mohamed R., Bertini, Ivano, Naletto, Giampiero, Lazzarin, Monica, Massironi, Matteo, Sierks, Holger, Barbieri, Cesare, Lamy, Philippe, Rodrigo, Rafael, Koschny, Detlef, Rickman, Hans, Keller, Horst U., Agarwal, Jessica, A'Hearn, Michael F., Barucci, Maria A., Bertaux, Jean-Loup, Boudreault, Steve, Cremonese, Gabriele, Da Deppo, Vania, Davidsson, Bjorn, Debei, Stefano, De Cecco, Mariolino, Deller, Jakob, Fornasier, Sonia, Fulle, Marco, Gicquel, Adeline, Groussin, Olivier, Gutierrez, Pedro J., Guetler, Carsten, Hofmann, Marc, Hoefner, Sebastian, Hviid, Stubbe F., Ip, Wing-Huen, Jorda, Laurent, Knollenberg, Joerg, Kramm, J. -Rainer, Kuehrt, Ekkehard, Kuppers, Michael, La Forgia, Fiorangela, Lara, Luisa M., Lee, Jui-Chi, Lin, Zhong-Yi, Lopez Moreno, Jose J., Marzari, Francesco, Michalik, Harald, Mottola, Stefano, Preusker, Frank, Scholten, Frank, Thomas, Nicholas, Toth, Imre, and Tubiana, Cecilia
Abstract: Aims. We calculate the size-frequency distribution of the boulders on the southern hemisphere of comet 67P Churyumov-Gerasimenko (67P), which was in shadow before the end of April 2015. We compare the new results with those derived from the northern hemisphere and equatorial regions of 67P, highlighting the possible physical processes that lead to these boulder size distributions. Methods. We used images acquired by the OSIRIS Narrow Angle Camera (NAC) on 2 May 2015 at a distance of 125 km from the nucleus. The scale of this dataset is 2.3 m/px; the high resolution of the images, coupled with the favorable observation phase angle of 62 degrees, provided the possibility to unambiguously identify boulders >= 7 m on the surface of 67P and to manually extract them with the software ArcGIS. We derived the size-frequency distribution of the illuminated southern hemisphere. Results. We found a power-law index of -3.6 +/- 0.2 for the boulders on the southern hemisphere with a diameter range of 7-35 m. The power-law index is equal to the one previously found on northern and equatorial regions of 67P, suggesting that similar boulder formation processes occur in both hemispheres. The power-law index is related to gravitational events triggered by sublimation and/or thermal fracturing causing regressive erosion. In addition, the presence of a larger number of boulders per km(2) in the southern hemisphere, which is a factor of 3 higher with respect to the northern hemisphere, suggests that the southernmost terrains of 67P are affected by a stronger thermal fracturing and sublimating activity, hence possibly causing larger regressive erosion and gravitational events.
Published: 2016
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39. Simulation of Europa's water plume and structures related to energetic activities on solar system bodies from satellite images

Author: Lucchetti, Alice and Lucchetti, Alice
Abstract: This PhD thesis focuses on the analysis of different high energetic processes that affect the surface of planets, satellites and minor bodies as well as modify their surrounding environment. Specifically, this work concerns three main topics: (i) the simulation and analysis of one of the most geological energetic process, i.e. impact cratering; (ii) the investigation of the fragmentation processes that could have generated boulders on comet Churyumov-Gerasimenko 67P; (iii) the analysis of a possible transient plume originating from cryovolcanic events on Europa, the Jovian icy satellite, combined with an accurate characterisation of its exospheric background. The first topic addresses the investigation of the impact formation process through numerical modelling. Shocks code represent the most feasible method for studying impact craters, as they can simulate a large span of conditions beyond the reach of experiments (e.g., velocity, size). The iSALE hydrocode was used to simulate two different impact structures located on Mercury and Mars. On Mercury, the simulation allows to determine the genesis of a particular landform, i.e. a steep-sided cone with associated pyroclastic deposits, which was revealed by images acquired by MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft. On Mars, the simulation of the Firsoff crater in Arabia Terra permits a better understanding the subsequent geologic processes that led to crater post modification, defining which rheological structure is more likely in that region. In both cases, we conclude that the numerical modelling of impact process is a powerful tool to improve the comprehension of the Solar System. The second topic of the thesis has been developed after the Rosetta mission got inserted around the comet Churyumov-Gerasimenko 67P. We investigated the surface of comet Churyumov-Gerasimenko 67P focusing on the possible energetic events that lead to the formation of boulders; i.e. blocks that
Published: 2016

40. Size-frequency distribution of boulders >= 7 m on comet 67P/Churyumov-Gerasimenko

Author: Pajola, Maurizio, Vincent, Jean-Baptiste, Guettler, Carsten, Lee, Jui-Chi, Bertini, Ivano, Massironi, Matteo, Simioni, Emanuele, Marzari, Francesco, Giacomini, Lorenza, Lucchetti, Alice, Barbieri, Cesare, Cremonese, Gabriele, Naletto, Giampiero, Pommerol, Antoine, El-Maarry, Mohamed R., Besse, Sebastien, Kueppers, Michael, La Forgia, Fiorangela, Lazzarin, Monica, Thomas, Nicholas, Auger, Anne-Therese, Sierks, Holger, Lamy, Philippe, Rodrigo, Rafael, Koschny, Detlef, Rickman, Hans, Keller, Horst U., Agarwal, Jessica, A'Hearn, Michael F., Barucci, Maria A., Bertaux, Jean-Loup, Da Deppo, Vania, Davidsson, Björn, De Cecco, Mariolino, Debei, Stefano, Ferri, Francesca, Fornasier, Sonia, Fulle, Marco, Groussin, Olivier, Gutierrez, Pedro J., Hviid, Stubbe F., Ip, Wing-Huen, Jorda, Laurent, Knollenberg, Joerg, Kramm, J. -Rainer, Kuert, Ekkehard, Lara, Luisa M., Lin, Zhong-Yi, Lopez Moreno, Jose J., Magrin, Sara, Marchi, Simone, Michalik, Harald, Moissl, Richard, Mottola, Stefano, Oklay, Nilda, Preusker, Frank, Scholten, Frank, Tubiana, Cecilia, Pajola, Maurizio, Vincent, Jean-Baptiste, Guettler, Carsten, Lee, Jui-Chi, Bertini, Ivano, Massironi, Matteo, Simioni, Emanuele, Marzari, Francesco, Giacomini, Lorenza, Lucchetti, Alice, Barbieri, Cesare, Cremonese, Gabriele, Naletto, Giampiero, Pommerol, Antoine, El-Maarry, Mohamed R., Besse, Sebastien, Kueppers, Michael, La Forgia, Fiorangela, Lazzarin, Monica, Thomas, Nicholas, Auger, Anne-Therese, Sierks, Holger, Lamy, Philippe, Rodrigo, Rafael, Koschny, Detlef, Rickman, Hans, Keller, Horst U., Agarwal, Jessica, A'Hearn, Michael F., Barucci, Maria A., Bertaux, Jean-Loup, Da Deppo, Vania, Davidsson, Björn, De Cecco, Mariolino, Debei, Stefano, Ferri, Francesca, Fornasier, Sonia, Fulle, Marco, Groussin, Olivier, Gutierrez, Pedro J., Hviid, Stubbe F., Ip, Wing-Huen, Jorda, Laurent, Knollenberg, Joerg, Kramm, J. -Rainer, Kuert, Ekkehard, Lara, Luisa M., Lin, Zhong-Yi, Lopez Moreno, Jose J., Magrin, Sara, Marchi, Simone, Michalik, Harald, Moissl, Richard, Mottola, Stefano, Oklay, Nilda, Preusker, Frank, Scholten, Frank, and Tubiana, Cecilia
Abstract: Aims. We derive for the first time the size-frequency distribution of boulders on a comet, 67P/Churyumov-Gerasimenko (67P), computed from the images taken by the Rosetta/OSIRIS imaging system. We highlight the possible physical processes that lead to these boulder size distributions. Methods. We used images acquired by the OSIRIS Narrow Angle Camera, NAC. on 5 and 6 August 2014. The scale of these images (2.44-2.03 m/px) is such that boulders >= 7 m can be identified and manually extracted from the datasets with the software ArcGIS. We derived both global and localized size-frequency distributions. The three-pixel sampling detection, coupled with the favorable shadowine of the surface (observation phase angle ranging from 48 to 53), enables unequivocally detecting boulders scattered all over the illuminated side of 67P. Results. We identify 3546 boulders larger than 7 m on the imaged surface (36.4 km(2)), with a global number density of nearly 100/km(2) and a cumulative size-frequency distribution represented by a power-law with index of -3.6 +0.2/-0.3. The two lobes of 67P appear to have slightly different distributions, with an index of -3.5 +0.2/-0.3 for the main lobe (body) and -4.0 +0.31-0.2 for the small lobe (head). The steeper distribution of the small lobe might be due to a more pervasive fracturing. The difference of the distribution for the connecting region (neck) is much more significant, with an index value of -2.2 +0.2/-0.2. We propose that the boulder field located in the neck area is the result of blocks falling from the contiguous Hathor cliff. The lower slope of the size-frequency distribution we see today in the neck area might be due to the concurrent processes acting on the smallest boulders, such as i) disintegration or fragmentation and vanishing through sublimation; ii) uplifting by gas drag and consequent redistribution; and iii) burial beneath a debris blanket. We also derived the cumulative size-frequency distribution per km(2) of loca
Published: 2015
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41. Achievement of the Planetary Defense Investigations of the Double Asteroid Redirection Test (DART) Mission

Author: Chabot, Nancy L., Rivkin, Andrew S., Cheng, Andrew F., Barnouin, Olivier S., Fahnestock, Eugene G., Richardson, Derek C., Stickle, Angela M., Thomas, Cristina A., Ernst, Carolyn M., Terik Daly, R., Dotto, Elisabetta, Zinzi, Angelo, Chesley, Steven R., Moskovitz, Nicholas A., Barbee, Brent W., Abell, Paul, Agrusa, Harrison F., Bannister, Michele T., Beccarelli, Joel, Bekker, Dmitriy L., Bruck Syal, Megan, Buratti, Bonnie J., Busch, Michael W., Campo Bagatin, Adriano, Chatelain, Joseph P., Chocron, Sidney, Collins, Gareth S., Conversi, Luca, Davison, Thomas M., DeCoster, Mallory E., Prasanna Deshapriya, J. D., Eggl, Siegfried, Espiritu, Raymond C., Farnham, Tony L., Ferrais, Marin, Ferrari, Fabio, Föhring, Dora, Fuentes-Muñoz, Oscar, Gai, Igor, Giordano, Carmine, Glenar, David A., Gomez, Edward, Graninger, Dawn M., Green, Simon F., Greenstreet, Sarah, Hasselmann, Pedro H., Herreros, Isabel, Hirabayashi, Masatoshi, Husárik, Marek, Ieva, Simone, Ivanovski, Stavro L., Jackson, Samuel L., Jehin, Emmanuel, Jutzi, Martin, Karatekin, Ozgur, Knight, Matthew M., Kolokolova, Ludmilla, Kumamoto, Kathryn M., Küppers, Michael, La Forgia, Fiorangela, Lazzarin, Monica, Li, Jian-Yang, Lister, Tim A., Lolachi, Ramin, Lucas, Michael P., Lucchetti, Alice, Luther, Robert, Makadia, Rahil, Mazzotta Epifani, Elena, McMahon, Jay, Merisio, Gianmario, Merrill, Colby C., Meyer, Alex J., Michel, Patrick, Micheli, Marco, Migliorini, Alessandra, Minker, Kate, Modenini, Dario, Moreno, Fernando, Murdoch, Naomi, Murphy, Brian, Naidu, Shantanu P., Nair, Hari, Nakano, Ryota, Opitom, Cyrielle, Ormö, Jens, Michael Owen, J., Pajola, Maurizio, Palmer, Eric E., Palumbo, Pasquale, Panicucci, Paolo, Parro, Laura M., Pearl, Jason M., Penttilä, Antti, Perna, Davide, Petrescu, Elisabeta, Pravec, Petr, Raducan, Sabina D., Ramesh, K. T., Ridden-Harper, Ryan, Rizos, Juan L., Rossi, Alessandro, Roth, Nathan X., Rożek, Agata, Rozitis, Benjamin, Ryan, Eileen V., Ryan, William H., Sánchez, Paul, Santana-Ros, Toni, Scheeres, Daniel J., Scheirich, Peter, Berk Senel, Cem, Snodgrass, Colin, Soldini, Stefania, Souami, Damya, Statler, Thomas S., Street, Rachel, Stubbs, Timothy J., Sunshine, Jessica M., Tan, Nicole J., Tancredi, Gonzalo, Tinsman, Calley L., Tortora, Paolo, Tusberti, Filippo, Walker, James D., Waller, C. Dany, Wünnemann, Kai, Zannoni, Marco, Zhang, Yun, Chabot, Nancy L., Rivkin, Andrew S., Cheng, Andrew F., Barnouin, Olivier S., Fahnestock, Eugene G., Richardson, Derek C., Stickle, Angela M., Thomas, Cristina A., Ernst, Carolyn M., Terik Daly, R., Dotto, Elisabetta, Zinzi, Angelo, Chesley, Steven R., Moskovitz, Nicholas A., Barbee, Brent W., Abell, Paul, Agrusa, Harrison F., Bannister, Michele T., Beccarelli, Joel, Bekker, Dmitriy L., Bruck Syal, Megan, Buratti, Bonnie J., Busch, Michael W., Campo Bagatin, Adriano, Chatelain, Joseph P., Chocron, Sidney, Collins, Gareth S., Conversi, Luca, Davison, Thomas M., DeCoster, Mallory E., Prasanna Deshapriya, J. D., Eggl, Siegfried, Espiritu, Raymond C., Farnham, Tony L., Ferrais, Marin, Ferrari, Fabio, Föhring, Dora, Fuentes-Muñoz, Oscar, Gai, Igor, Giordano, Carmine, Glenar, David A., Gomez, Edward, Graninger, Dawn M., Green, Simon F., Greenstreet, Sarah, Hasselmann, Pedro H., Herreros, Isabel, Hirabayashi, Masatoshi, Husárik, Marek, Ieva, Simone, Ivanovski, Stavro L., Jackson, Samuel L., Jehin, Emmanuel, Jutzi, Martin, Karatekin, Ozgur, Knight, Matthew M., Kolokolova, Ludmilla, Kumamoto, Kathryn M., Küppers, Michael, La Forgia, Fiorangela, Lazzarin, Monica, Li, Jian-Yang, Lister, Tim A., Lolachi, Ramin, Lucas, Michael P., Lucchetti, Alice, Luther, Robert, Makadia, Rahil, Mazzotta Epifani, Elena, McMahon, Jay, Merisio, Gianmario, Merrill, Colby C., Meyer, Alex J., Michel, Patrick, Micheli, Marco, Migliorini, Alessandra, Minker, Kate, Modenini, Dario, Moreno, Fernando, Murdoch, Naomi, Murphy, Brian, Naidu, Shantanu P., Nair, Hari, Nakano, Ryota, Opitom, Cyrielle, Ormö, Jens, Michael Owen, J., Pajola, Maurizio, Palmer, Eric E., Palumbo, Pasquale, Panicucci, Paolo, Parro, Laura M., Pearl, Jason M., Penttilä, Antti, Perna, Davide, Petrescu, Elisabeta, Pravec, Petr, Raducan, Sabina D., Ramesh, K. T., Ridden-Harper, Ryan, Rizos, Juan L., Rossi, Alessandro, Roth, Nathan X., Rożek, Agata, Rozitis, Benjamin, Ryan, Eileen V., Ryan, William H., Sánchez, Paul, Santana-Ros, Toni, Scheeres, Daniel J., Scheirich, Peter, Berk Senel, Cem, Snodgrass, Colin, Soldini, Stefania, Souami, Damya, Statler, Thomas S., Street, Rachel, Stubbs, Timothy J., Sunshine, Jessica M., Tan, Nicole J., Tancredi, Gonzalo, Tinsman, Calley L., Tortora, Paolo, Tusberti, Filippo, Walker, James D., Waller, C. Dany, Wünnemann, Kai, Zannoni, Marco, and Zhang, Yun

42. Near to Mid-infrared Spectroscopy of (65803) Didymos as Observed by JWST: Characterization Observations Supporting the Double Asteroid Redirection Test

Author: Rivkin, Andrew S., Thomas, Cristina A., Wong, Ian, Rozitis, Benjamin, de León, Julia, Holler, Bryan, Milam, Stefanie N., Howell, Ellen S., Hammel, Heidi B., Arredondo, Anicia, Brucato, John R., Epifani, Elena M., Ieva, Simone, La Forgia, Fiorangela, Lucas, Michael P., Lucchetti, Alice, Pajola, Maurizio, Poggiali, Giovanni, Sunshine, Jessica N., Trigo-Rodríguez, Josep M., Rivkin, Andrew S., Thomas, Cristina A., Wong, Ian, Rozitis, Benjamin, de León, Julia, Holler, Bryan, Milam, Stefanie N., Howell, Ellen S., Hammel, Heidi B., Arredondo, Anicia, Brucato, John R., Epifani, Elena M., Ieva, Simone, La Forgia, Fiorangela, Lucas, Michael P., Lucchetti, Alice, Pajola, Maurizio, Poggiali, Giovanni, Sunshine, Jessica N., and Trigo-Rodríguez, Josep M.

43. Enceladus as a potential oasis for life: Science goals and investigations for future explorations

Author: Choblet, Gael, Tobie, Gabriel, Buch, Arnaud, Cadek, Ondrej, Barge, Laura M., Behounkova, Marie, Camprubi, Eloi, Freissinet, Caroline, Hedman, Matt, Jones, Geraint, Lainey, Valery, Le Gall, Alice, Lucchetti, Alice, MacKenzie, Shannon, Mitri, Giuseppe, Neveu, Marc, Nimmo, Francis, Olsson-Francis, Karen, Panning, Mark, Postberg, Frank, Saur, Joachim, Schmidt, Juergen, Sekine, Yasuhito, Shibuya, Takazo, Sotin, Christophe, Soucek, Ondrej, Szopa, Cyril, Usui, Tomohiro, Vance, Steven, Van Hoolst, Tim, Choblet, Gael, Tobie, Gabriel, Buch, Arnaud, Cadek, Ondrej, Barge, Laura M., Behounkova, Marie, Camprubi, Eloi, Freissinet, Caroline, Hedman, Matt, Jones, Geraint, Lainey, Valery, Le Gall, Alice, Lucchetti, Alice, MacKenzie, Shannon, Mitri, Giuseppe, Neveu, Marc, Nimmo, Francis, Olsson-Francis, Karen, Panning, Mark, Postberg, Frank, Saur, Joachim, Schmidt, Juergen, Sekine, Yasuhito, Shibuya, Takazo, Sotin, Christophe, Soucek, Ondrej, Szopa, Cyril, Usui, Tomohiro, Vance, Steven, and Van Hoolst, Tim
Abstract: Enceladus is the first planetary object for which direct sampling of a subsurface water reservoir, likely habitable, has been performed. Over a decade of flybys and seven flythroughs of its watery plume, the Cassini spacecraft determined that Enceladus possesses all the ingredients for life. The existence of active eruptions blasting fresh water into space, makes Enceladus the easiest target in the search for life elsewhere in the Solar System. Flying again through the plume with more advanced instruments, landing at the surface near active sources and collecting a sample for return to Earth are the natural next steps for assessing whether life emerges in this active world. Characterizing this habitable world also requires detailed mapping and monitoring of its tidally-induced activity, from the orbit as well as from the surface using complementary platforms. Such ambitious goals may be achieved in the future in the framework of ESA large or medium-class missions in partnership with other international agencies, in the same spirit of the successful Cassini-Huygens mission. For all these reasons, exploring habitable ocean worlds, with Enceladus as a primary target, should be a priority topic of the ESA Voyage 2050 programme.

44. Rationale for BepiColombo Studies of Mercury’s Surface and Composition

Author: Rothery, David A., Massironi, Matteo, Alemanno, Giulia, Barraud, Océane, Besse, Sebastien, Bott, Nicolas, Brunetto, Rosario, Bunce, Emma, Byrne, Paul, Capaccioni, Fabrizio, Capria, Maria Teresa, Carli, Cristian, Charlier, Bernard, Cornet, Thomas, Cremonese, Gabriele, D’Amore, Mario, De Sanctis, M. Cristina, Doressoundiram, Alain, Ferranti, Luigi, Filacchione, Gianrico, Galluzzi, Valentina, Giacomini, Lorenza, Grande, Manuel, Guzzetta, Laura G., Helbert, Jörn, Heyner, Daniel, Hiesinger, Harald, Hussmann, Hauke, Hyodo, Ryuku, Kohout, Tomas, Kozyrev, Alexander, Litvak, Maxim, Lucchetti, Alice, Malakhov, Alexey, Malliband, Christopher, Mancinelli, Paolo, Martikainen, Julia, Martindale, Adrian, Maturilli, Alessandro, Milillo, Anna, Mitrofanov, Igor, Mokrousov, Maxim, Morlok, Andreas, Muinonen, Karri, Namur, Olivier, Owens, Alan, Nittler, Larry R., Oliveira, Joana S., Palumbo, Pasquale, Pajola, Maurizio, Pegg, David L., Penttilä, Antti, Politi, Romolo, Quarati, Francesco, Re, Cristina, Sanin, Anton, Schulz, Rita, Stangarone, Claudia, Stojic, Aleksandra, Tretiyakov, Vladislav, Väisänen, Timo, Varatharajan, Indhu, Weber, Iris, Wright, Jack, Wurz, Peter, Zambon, Francesca, Rothery, David A., Massironi, Matteo, Alemanno, Giulia, Barraud, Océane, Besse, Sebastien, Bott, Nicolas, Brunetto, Rosario, Bunce, Emma, Byrne, Paul, Capaccioni, Fabrizio, Capria, Maria Teresa, Carli, Cristian, Charlier, Bernard, Cornet, Thomas, Cremonese, Gabriele, D’Amore, Mario, De Sanctis, M. Cristina, Doressoundiram, Alain, Ferranti, Luigi, Filacchione, Gianrico, Galluzzi, Valentina, Giacomini, Lorenza, Grande, Manuel, Guzzetta, Laura G., Helbert, Jörn, Heyner, Daniel, Hiesinger, Harald, Hussmann, Hauke, Hyodo, Ryuku, Kohout, Tomas, Kozyrev, Alexander, Litvak, Maxim, Lucchetti, Alice, Malakhov, Alexey, Malliband, Christopher, Mancinelli, Paolo, Martikainen, Julia, Martindale, Adrian, Maturilli, Alessandro, Milillo, Anna, Mitrofanov, Igor, Mokrousov, Maxim, Morlok, Andreas, Muinonen, Karri, Namur, Olivier, Owens, Alan, Nittler, Larry R., Oliveira, Joana S., Palumbo, Pasquale, Pajola, Maurizio, Pegg, David L., Penttilä, Antti, Politi, Romolo, Quarati, Francesco, Re, Cristina, Sanin, Anton, Schulz, Rita, Stangarone, Claudia, Stojic, Aleksandra, Tretiyakov, Vladislav, Väisänen, Timo, Varatharajan, Indhu, Weber, Iris, Wright, Jack, Wurz, Peter, and Zambon, Francesca
Abstract: BepiColombo has a larger and in many ways more capable suite of instruments relevant for determination of the topographic, physical, chemical and mineralogical properties of Mercury’s surface than the suite carried by NASA’s MESSENGER spacecraft. Moreover, BepiColombo’s data rate is substantially higher. This equips it to confirm, elaborate upon, and go beyond many of MESSENGER’s remarkable achievements. Furthermore, the geometry of BepiColombo’s orbital science campaign, beginning in 2026, will enable it to make uniformly resolved observations of both northern and southern hemispheres. This will offer more detailed and complete imaging and topographic mapping, element mapping with better sensitivity and improved spatial resolution, and totally new mineralogical mapping. We discuss MESSENGER data in the context of preparing for BepiColombo, and describe the contributions that we expect BepiColombo to make towards increased knowledge and understanding of Mercury’s surface and its composition. Much current work, including analysis of analogue materials, is directed towards better preparing ourselves to understand what BepiColombo might reveal. Some of MESSENGER’s more remarkable observations were obtained under unique or extreme conditions. BepiColombo should be able to confirm the validity of these observations and reveal the extent to which they are representative of the planet as a whole. It will also make new observations to clarify geological processes governing and reflecting crustal origin and evolution. We anticipate that the insights gained into Mercury’s geological history and its current space weathering environment will enable us to better understand the relationships of surface chemistry, morphologies and structures with the composition of crustal types, including the nature and mobility of volatile species. This will enable estimation of the composition of the mantle from which the crust was derived, and lead to tighter constraints on models for Mercury’

45. A cone on Mercury: analysis of a residual central peak encircled by an explosive volcanic vent

Author: Thomas, Rebecca J., Lucchetti, Alice, Cremonese, Gabriele, Rothery, David A., Massironi, Matteo, Re, Cristina, Conway, Susan J., Anand, Mahesh, Thomas, Rebecca J., Lucchetti, Alice, Cremonese, Gabriele, Rothery, David A., Massironi, Matteo, Re, Cristina, Conway, Susan J., and Anand, Mahesh
Abstract: We analyse a seemingly-unique landform on Mercury: a conical structure, encircled by a trough, and surrounded by a 23,000 km2 relatively bright and red anomaly of a type interpreted elsewhere on the planet as a pyroclastic deposit. At first glance, this could be interpreted as a volcanically-constructed cone, but if so, it would be the only example of such a landform on Mercury. We make and test the alternative hypothesis that the cone is the intrinsic central peak of an impact crater, the rim crest of which is visible beyond the cone-encircling trough, and that the trough is a vent formed through explosive volcanism that also produced the surrounding bright, red spectral anomaly. We test this hypothesis by comparing the morphology of the cone and the associated landform assemblage with morphologically-fresh impact craters of the same diameter as the putative host crater, and additionally, by modelling the original morphology of such a crater using a hydrocode model. We show that the present topography can be explained by formation of a vent completely encircling the crater’s central peak and also make the observation that explosive volcanic vents frequently occur circumferential to the central peaks of impact craters on Mercury. This indicates that, although this cone initially appears unique, it is in fact an unusually well-developed example of a common process by which impact-related faults localize magma ascent near the centre of impact craters on Mercury, and represents an extreme end-member of the resulting landforms.

46. Enceladus as a potential oasis for life: Science goals and investigations for future explorations

Author: Choblet, Gael, Tobie, Gabriel, Buch, Arnaud, Cadek, Ondrej, Barge, Laura M., Behounkova, Marie, Camprubi, Eloi, Freissinet, Caroline, Hedman, Matt, Jones, Geraint, Lainey, Valery, Le Gall, Alice, Lucchetti, Alice, MacKenzie, Shannon, Mitri, Giuseppe, Neveu, Marc, Nimmo, Francis, Olsson-Francis, Karen, Panning, Mark, Postberg, Frank, Saur, Joachim, Schmidt, Juergen, Sekine, Yasuhito, Shibuya, Takazo, Sotin, Christophe, Soucek, Ondrej, Szopa, Cyril, Usui, Tomohiro, Vance, Steven, Van Hoolst, Tim, Choblet, Gael, Tobie, Gabriel, Buch, Arnaud, Cadek, Ondrej, Barge, Laura M., Behounkova, Marie, Camprubi, Eloi, Freissinet, Caroline, Hedman, Matt, Jones, Geraint, Lainey, Valery, Le Gall, Alice, Lucchetti, Alice, MacKenzie, Shannon, Mitri, Giuseppe, Neveu, Marc, Nimmo, Francis, Olsson-Francis, Karen, Panning, Mark, Postberg, Frank, Saur, Joachim, Schmidt, Juergen, Sekine, Yasuhito, Shibuya, Takazo, Sotin, Christophe, Soucek, Ondrej, Szopa, Cyril, Usui, Tomohiro, Vance, Steven, and Van Hoolst, Tim
Abstract: Enceladus is the first planetary object for which direct sampling of a subsurface water reservoir, likely habitable, has been performed. Over a decade of flybys and seven flythroughs of its watery plume, the Cassini spacecraft determined that Enceladus possesses all the ingredients for life. The existence of active eruptions blasting fresh water into space, makes Enceladus the easiest target in the search for life elsewhere in the Solar System. Flying again through the plume with more advanced instruments, landing at the surface near active sources and collecting a sample for return to Earth are the natural next steps for assessing whether life emerges in this active world. Characterizing this habitable world also requires detailed mapping and monitoring of its tidally-induced activity, from the orbit as well as from the surface using complementary platforms. Such ambitious goals may be achieved in the future in the framework of ESA large or medium-class missions in partnership with other international agencies, in the same spirit of the successful Cassini-Huygens mission. For all these reasons, exploring habitable ocean worlds, with Enceladus as a primary target, should be a priority topic of the ESA Voyage 2050 programme.

47. A cone on Mercury: analysis of a residual central peak encircled by an explosive volcanic vent

Author: Thomas, Rebecca J., Lucchetti, Alice, Cremonese, Gabriele, Rothery, David A., Massironi, Matteo, Re, Cristina, Conway, Susan J., Anand, Mahesh, Thomas, Rebecca J., Lucchetti, Alice, Cremonese, Gabriele, Rothery, David A., Massironi, Matteo, Re, Cristina, Conway, Susan J., and Anand, Mahesh
Abstract: We analyse a seemingly-unique landform on Mercury: a conical structure, encircled by a trough, and surrounded by a 23,000 km2 relatively bright and red anomaly of a type interpreted elsewhere on the planet as a pyroclastic deposit. At first glance, this could be interpreted as a volcanically-constructed cone, but if so, it would be the only example of such a landform on Mercury. We make and test the alternative hypothesis that the cone is the intrinsic central peak of an impact crater, the rim crest of which is visible beyond the cone-encircling trough, and that the trough is a vent formed through explosive volcanism that also produced the surrounding bright, red spectral anomaly. We test this hypothesis by comparing the morphology of the cone and the associated landform assemblage with morphologically-fresh impact craters of the same diameter as the putative host crater, and additionally, by modelling the original morphology of such a crater using a hydrocode model. We show that the present topography can be explained by formation of a vent completely encircling the crater’s central peak and also make the observation that explosive volcanic vents frequently occur circumferential to the central peaks of impact craters on Mercury. This indicates that, although this cone initially appears unique, it is in fact an unusually well-developed example of a common process by which impact-related faults localize magma ascent near the centre of impact craters on Mercury, and represents an extreme end-member of the resulting landforms.

48. Enceladus as a potential oasis for life: Science goals and investigations for future explorations

Author: Choblet, Gaël, Tobie, Gabriel, Buch, Arnaud, Čadek, Ondrej, Barge, Laura M., Bēhounková, Marie, Camprubi, Eloi, Freissinet, Caroline, Hedman, Matt, Jones, Geraint, Lainey, Valery, Le Gall, Alice, Lucchetti, Alice, MacKenzie, Shannon, Mitri, Giuseppe, Neveu, Marc, Nimmo, Francis, Olsson-Francis, Karen, Panning, Mark, Postberg, Frank, Saur, Joachim, Schmidt, Jürgen, Sekine, Yasuhito, Shibuya, Takazo, Sotin, Christophe, Soucek, Ondrej, Szopa, Cyril, Usui, Tomohiro, Vance, Steven, Van Hoolst, Tim, Choblet, Gaël, Tobie, Gabriel, Buch, Arnaud, Čadek, Ondrej, Barge, Laura M., Bēhounková, Marie, Camprubi, Eloi, Freissinet, Caroline, Hedman, Matt, Jones, Geraint, Lainey, Valery, Le Gall, Alice, Lucchetti, Alice, MacKenzie, Shannon, Mitri, Giuseppe, Neveu, Marc, Nimmo, Francis, Olsson-Francis, Karen, Panning, Mark, Postberg, Frank, Saur, Joachim, Schmidt, Jürgen, Sekine, Yasuhito, Shibuya, Takazo, Sotin, Christophe, Soucek, Ondrej, Szopa, Cyril, Usui, Tomohiro, Vance, Steven, and Van Hoolst, Tim
Abstract: Enceladus is the first planetary object for which direct sampling of a subsurface water reservoir, likely habitable, has been performed. Over a decade of flybys and seven flythroughs of its watery plume, the Cassini spacecraft determined that Enceladus possesses all the ingredients for life. The existence of active eruptions blasting fresh water into space, makes Enceladus the easiest target in the search for life elsewhere in the Solar System. Flying again through the plume with more advanced instruments, landing at the surface near active sources and collecting a sample for return to Earth are the natural next steps for assessing whether life emerges in this active world. Characterizing this habitable world also requires detailed mapping and monitoring of its tidally-induced activity, from the orbit as well as from the surface using complementary platforms. Such ambitious goals may be achieved in the future in the framework of ESA large or medium-class missions in partnership with other international agencies, in the same spirit of the successful Cassini-Huygens mission. For all these reasons, exploring habitable ocean worlds, with Enceladus as a primary target, should be a priority topic of the ESA Voyage 2050 programme.

49. Rationale for BepiColombo Studies of Mercury’s Surface and Composition

Author: Rothery, David A., Massironi, Matteo, Alemanno, Giulia, Barraud, Océane, Besse, Sebastien, Bott, Nicolas, Brunetto, Rosario, Bunce, Emma, Byrne, Paul, Capaccioni, Fabrizio, Capria, Maria Teresa, Carli, Cristian, Charlier, Bernard, Cornet, Thomas, Cremonese, Gabriele, D’Amore, Mario, De Sanctis, M. Cristina, Doressoundiram, Alain, Ferranti, Luigi, Filacchione, Gianrico, Galluzzi, Valentina, Giacomini, Lorenza, Grande, Manuel, Guzzetta, Laura G., Helbert, Jörn, Heyner, Daniel, Hiesinger, Harald, Hussmann, Hauke, Hyodo, Ryuku, Kohout, Tomas, Kozyrev, Alexander, Litvak, Maxim, Lucchetti, Alice, Malakhov, Alexey, Malliband, Christopher, Mancinelli, Paolo, Martikainen, Julia, Martindale, Adrian, Maturilli, Alessandro, Milillo, Anna, Mitrofanov, Igor, Mokrousov, Maxim, Morlok, Andreas, Muinonen, Karri, Namur, Olivier, Owens, Alan, Nittler, Larry R., Oliveira, Joana S., Palumbo, Pasquale, Pajola, Maurizio, Pegg, David L., Penttilä, Antti, Politi, Romolo, Quarati, Francesco, Re, Cristina, Sanin, Anton, Schulz, Rita, Stangarone, Claudia, Stojic, Aleksandra, Tretiyakov, Vladislav, Väisänen, Timo, Varatharajan, Indhu, Weber, Iris, Wright, Jack, Wurz, Peter, Zambon, Francesca, Rothery, David A., Massironi, Matteo, Alemanno, Giulia, Barraud, Océane, Besse, Sebastien, Bott, Nicolas, Brunetto, Rosario, Bunce, Emma, Byrne, Paul, Capaccioni, Fabrizio, Capria, Maria Teresa, Carli, Cristian, Charlier, Bernard, Cornet, Thomas, Cremonese, Gabriele, D’Amore, Mario, De Sanctis, M. Cristina, Doressoundiram, Alain, Ferranti, Luigi, Filacchione, Gianrico, Galluzzi, Valentina, Giacomini, Lorenza, Grande, Manuel, Guzzetta, Laura G., Helbert, Jörn, Heyner, Daniel, Hiesinger, Harald, Hussmann, Hauke, Hyodo, Ryuku, Kohout, Tomas, Kozyrev, Alexander, Litvak, Maxim, Lucchetti, Alice, Malakhov, Alexey, Malliband, Christopher, Mancinelli, Paolo, Martikainen, Julia, Martindale, Adrian, Maturilli, Alessandro, Milillo, Anna, Mitrofanov, Igor, Mokrousov, Maxim, Morlok, Andreas, Muinonen, Karri, Namur, Olivier, Owens, Alan, Nittler, Larry R., Oliveira, Joana S., Palumbo, Pasquale, Pajola, Maurizio, Pegg, David L., Penttilä, Antti, Politi, Romolo, Quarati, Francesco, Re, Cristina, Sanin, Anton, Schulz, Rita, Stangarone, Claudia, Stojic, Aleksandra, Tretiyakov, Vladislav, Väisänen, Timo, Varatharajan, Indhu, Weber, Iris, Wright, Jack, Wurz, Peter, and Zambon, Francesca
Abstract: BepiColombo has a larger and in many ways more capable suite of instruments relevant for determination of the topographic, physical, chemical and mineralogical properties of Mercury’s surface than the suite carried by NASA’s MESSENGER spacecraft. Moreover, BepiColombo’s data rate is substantially higher. This equips it to confirm, elaborate upon, and go beyond many of MESSENGER’s remarkable achievements. Furthermore, the geometry of BepiColombo’s orbital science campaign, beginning in 2026, will enable it to make uniformly resolved observations of both northern and southern hemispheres. This will offer more detailed and complete imaging and topographic mapping, element mapping with better sensitivity and improved spatial resolution, and totally new mineralogical mapping. We discuss MESSENGER data in the context of preparing for BepiColombo, and describe the contributions that we expect BepiColombo to make towards increased knowledge and understanding of Mercury’s surface and its composition. Much current work, including analysis of analogue materials, is directed towards better preparing ourselves to understand what BepiColombo might reveal. Some of MESSENGER’s more remarkable observations were obtained under unique or extreme conditions. BepiColombo should be able to confirm the validity of these observations and reveal the extent to which they are representative of the planet as a whole. It will also make new observations to clarify geological processes governing and reflecting crustal origin and evolution. We anticipate that the insights gained into Mercury’s geological history and its current space weathering environment will enable us to better understand the relationships of surface chemistry, morphologies and structures with the composition of crustal types, including the nature and mobility of volatile species. This will enable estimation of the composition of the mantle from which the crust was derived, and lead to tighter constraints on models for Mercury’

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