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1. Photometry of the Didymos System across the DART Impact Apparition

Author

Nicholas Moskovitz, Cristina Thomas, Petr Pravec, Tim Lister, Tom Polakis, David Osip, Theodore Kareta, Agata Rożek, Steven R. Chesley, Shantanu P. Naidu, Peter Scheirich, William Ryan, Eileen Ryan, Brian Skiff, Colin Snodgrass, Matthew M. Knight, Andrew S. Rivkin, Nancy L. Chabot, Vova Ayvazian, Irina Belskaya, Zouhair Benkhaldoun, Daniel N. Berteşteanu, Mariangela Bonavita, Terrence H. Bressi, Melissa J. Brucker, Martin J. Burgdorf, Otabek Burkhonov, Brian Burt, Carlos Contreras, Joseph Chatelain, Young-Jun Choi, Matthew Daily, Julia de León, Kamoliddin Ergashev, Tony Farnham, Petr Fatka, Marin Ferrais, Stefan Geier, Edward Gomez, Sarah Greenstreet, Hannes Gröller, Carl Hergenrother, Carrie Holt, Kamil Hornoch, Marek Husárik, Raguli Inasaridze, Emmanuel Jehin, Elahe Khalouei, Jean-Baptiste Kikwaya Eluo, Myung-Jin Kim, Yurij Krugly, Hana Kučáková, Peter Kušnirák, Jeffrey A. Larsen, Hee-Jae Lee, Cassandra Lejoly, Javier Licandro, Penélope Longa-Peña, Ronald A. Mastaler, Curtis McCully, Hong-Kyu Moon, Nidia Morrell, Arushi Nath, Dagmara Oszkiewicz, Daniel Parrott, Liz Phillips, Marcel M. Popescu, Donald Pray, George Pantelimon Prodan, Markus Rabus, Michael T. Read, Inna Reva, Vernon Roark, Toni Santana-Ros, James V. Scotti, Taiyo Tatara, Audrey Thirouin, David Tholen, Volodymyr Troianskyi, Andrew F. Tubbiolo, and Katelyn Villa

Subjects
Near-Earth objects, Asteroids, Small Solar System bodies, Astronomy, QB1-991
Abstract

On 2022 September 26, the Double Asteroid Redirection Test (DART) spacecraft impacted Dimorphos, the satellite of binary near-Earth asteroid (65803) Didymos. This demonstrated the efficacy of a kinetic impactor for planetary defense by changing the orbital period of Dimorphos by 33 minutes. Measuring the period change relied heavily on a coordinated campaign of lightcurve photometry designed to detect mutual events (occultations and eclipses) as a direct probe of the satellite’s orbital period. A total of 28 telescopes contributed 224 individual lightcurves during the impact apparition from 2022 July to 2023 February. We focus here on decomposable lightcurves, i.e., those from which mutual events could be extracted. We describe our process of lightcurve decomposition and use that to release the full data set for future analysis. We leverage these data to place constraints on the postimpact evolution of ejecta. The measured depths of mutual events relative to models showed that the ejecta became optically thin within the first ∼1 day after impact and then faded with a decay time of about 25 days. The bulk magnitude of the system showed that ejecta no longer contributed measurable brightness enhancement after about 20 days postimpact. This bulk photometric behavior was not well represented by an HG photometric model. An HG _1 G _2 model did fit the data well across a wide range of phase angles. Lastly, we note the presence of an ejecta tail through at least 2023 March. Its persistence implied ongoing escape of ejecta from the system many months after DART impact.

Published
2024
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2. Concept of Operations for OSIRIS-REx Optical Navigation Image Planning

Author

Coralie D. Adam, Peter G. Antreasian, Brian T. Carcich, Jason M. Leonard, Erik J. Lessac-Chenen, Leilah K. McCarthy, Derek S. Nelson, John Y. Pelgrift, Eric M. Sahr, Daniel R. Wibben, Sara Knutson, Heather L. Enos, Karl Harshman, Carl Hergenrother, John N. Kidd Jr, Diane Lambert, Anjani T. Polit, Bashar Rizk, Dante S. Lauretta, Olivia Billett, Mykal Lefevre, Michael C. Moreau, Brent J. Bos, Andrew Calloway, Nayi Castro, Joseph Cavaluzzi, Kenneth M. Getzandanner, Ronald Mink, and Devin Poland

Subjects
Spacecraft Instrumentation And Astrionics, Lunar And Planetary Science And Exploration
Abstract

Optical navigation (OpNav) is a critical subsystem of the OSIRIS-REx asteroid sample return mission, which operated in the vicinity of near-Earth asteroid (101955) Bennu from August 2018 through April 2021. A substantial amount of mission resources across multiple subsystems and institutions is required to ensure that the OpNav data are successfully acquired. The KinetX OpNav team, part of the Flight Dynamics System (FDS), is responsible for performing required analysis to develop the OpNav operations plans; requesting, reviewing and verifying the plans; and ultimately using the image data for critical navigation operations. The FDS team, responsible for the mission navigation, is operated by KinetX Aerospace with management and operations support from NASA’s Goddard Space Flight Center. The Science Processing and Operations Center (SPOC), located at the University of Arizona’s Lunar and Planetary Laboratory, is responsible for generating the planning products for all science and most OpNav data. These plans are integrated into the spacecraft sequences, tested, and commanded by the Mission Support Area (MSA) at Lockheed Martin Space. To ensure mission-critical navigation image data are successfully acquired, the plan is developed through a waterfall of planning cycles over the course of 3 months prior to onboard plan execution. During the initial strategic planning for a mission phase, detailed analysis is performed by the OpNav team to conceptualize the concept of operations (ConOps) for image data collection. This phase OpNav Narrative is included along with other strategic planning documents for the key ground segment stakeholders to review and provide feedback. The detailed OpNav plans get defined in the tactical planning cycle, which spans 8 to 3 weeks before the week-long integrated sequence is executed on-board the spacecraft. During the tactical cycle, the initial OpNav Request is submitted along with the science requests, kicking off development of the science and OpNav plans. Once the initial plan is drafted, interfaces are exercised so that the plan can be reviewed and iterated, if necessary. A rigorous schedule is followed by the planning teams during the implementation cycle, spanning the last 18 days before uplink, to ensure all the necessary integration, testing, and reviewing can occur on time. The development of the OpNav planning ConOps, including responsibilities, interfaces, timelines, and procedures, took extensive collaboration across mission elements and institutions. The process was robust throughout the 137 weeks of continuous Optical Navigation Operations at Bennu, which concluded on April 9th, 2021.

Published
2021
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3. Volatile-rich Asteroids in the Inner Solar System

Author

Joseph A. Nuth, III, Neyda Abreu, Frank T Ferguson, Daniel P Glavin, Carl Hergenrother, Hugh G. M. Hill, Natasha M. Johnson, Maurizio Pajola, and Kevin Walsh

Subjects
Space Sciences (General), Exobiology
Abstract

Bennu (101195), target of the Origins, Spectral Interpretation, Resource Identification, Security, Regolith Explorer (OSIRIS-REx) mission, is a type-B asteroid with abundant spectral evidence for hydrated silicates, low thermal inertia “boulders” and frequent bursts of particle emission. We suggest that Bennu’s parent body formed in the outer solar system before it was perturbed into the asteroid belt and then evolved into a near-Earth object. We show that this is consistent with models of planetesimal evolution. Bennu has many characteristics expected for a dormant comet, and could potentially contain a minimum of 1 wt.% adsorbed water if its gross mineralogy is consistent with the Orgueil meteorite. This is in addition to any ice or water contained within the hydrous minerals themselves. Based on this hypothesis, we predict the properties of the samples that will be returned to Earth by the OSIRIS-REx mission, including abundant phyllosilicate minerals, amorphous hydrated silicates and low-density, very high-porosity aggregates, already observed by the OSIRIS-REx instrument suite. We predict enrichments in D/H and 15N/14N, high C/Mg ratios (>∼7 wt%), and a greater range of organic compositions than found in meteorites, including an organic component poor in aromatics, and a more labile organic fraction. Ammonium salts, ranging from NH4Cl to ammonium–organic acid salts could carry much of the nitrogen in comets, yet only NH4CH3COO and heavier salts are sufficiently stable to be found in these returned samples. Water adsorbed onto highly porous grains should also be detected provided that the sample return capsule remains below 300 K during Earth return, and this water should be isotopically heavy.

Published
2020
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6. Variations in color and reflectance on the surface of asteroid (101955) Bennu

Author

Kevin J. Walsh, N. Shultz, Jian-Yang Li, L. F. Lim, K. N. Burke, Michael Daly, S. Sugita, Erica Jawin, Juliette I. Brodbeck, Dante S. Lauretta, Daniella DellaGiustina, Kris J. Becker, Tammy L. Becker, Ben Rozitis, Alexis Parkinson, Beth E. Clark, Jennifer Nolau, Carina Bennett, Amanda R. Hendrix, L. Le Corre, P. Michel, Bashar Rizk, C. W. V. Wolner, Pedro Hasselmann, Ronald-Louis Ballouz, Carl Hergenrother, David Trang, Marco Delbo, Sonia Fornasier, N. A. Porter, Eri Tatsumi, Daniel M. Applin, M. A. Barucci, C. Drouet d'Aubigny, Michael C. Nolan, Antara Sen, Maurizio Pajola, C. Avdellidou, Edward A. Cloutis, Koki Yumoto, Ellen S. Howell, J. D. Prasanna Deshapriya, Marcel Popescu, V. E. Hamilton, J. L. Rizos, Hannah Kaplan, Dathon Golish, K. L. Edmundson, Amy Simon, R. B. Van Auken, William F. Bottke, Andrew Ryan, Harold C. Connolly, M. Al Asad, Jamie Molaro, J. D. De Leon, E. B. Bierhaus, P. H. Smith, Humberto Campins, Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Southwest Research Institute [Boulder] (SwRI), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Surface (mathematics), Multidisciplinary, 010504 meteorology & atmospheric sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Multispectral image, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics, 01 natural sciences, Reflectivity, Texture (geology), Space weathering, Wavelength, Impact crater, 13. Climate action, Asteroid, [SDU]Sciences of the Universe [physics], 0103 physical sciences, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

The complex history of Bennu's surface The near-Earth asteroid (101955) Bennu is a carbon-rich body with a rubble pile structure, formed from debris ejected by an impact on a larger parent asteroid. The Origins, Spectral Interpretation, Resource Identification, Security, Regolith Explorer (OSIRIS-REx) spacecraft is designed to collect a sample of Bennu's surface and return it to Earth. After arriving at Bennu, OSIRIS-REx performed a detailed survey of the asteroid and reconnaissance of potential sites for sample collection. Three papers present results from those mission phases. DellaGiustina et al. mapped the optical color and albedo of Bennu's surface and established how they relate to boulders and impact craters, finding complex evolution caused by space weathering processes. Simon et al. analyzed near-infrared spectra, finding evidence for organic and carbonate materials that are widely distributed across the surface but are most concentrated on individual boulders. Kaplan et al. examined more detailed data collected on the primary sample site, called Nightingale. They identified bright veins with a distinct infrared spectrum in some boulders, which they interpreted as being carbonates formed by aqueous alteration on the parent asteroid. Together, these results constrain Bennu's evolution and provide context for the sample collected in October 2020. Science , this issue p. eabc3660 , p. eabc3522 , p. eabc3557

Published
2020
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7. Autonomous Detection of Particles and Tracks in Optical Images

Author

J. Y. Pelgrift, Derek S. Nelson, Carl Hergenrother, Michael C. Moreau, Jason M. Leonard, Jason C. Swenson, Steven R. Chesley, Andrew J. Liounis, Joshua R. Lyzhoft, J. Small, K. Getzandanner, Coralie D. Adam, Benjamin W. Ashman, Brent J. Bos, and Dante S. Lauretta

Subjects
010504 meteorology & atmospheric sciences, Computer science, lcsh:Astronomy, particle detection, FOS: Physical sciences, Image processing, Environmental Science (miscellaneous), 010502 geochemistry & geophysics, Tracking (particle physics), 01 natural sciences, particle tracking, lcsh:QB1-991, Sample return mission, active asteroid, Computer vision, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Monocular, Spacecraft, business.industry, lcsh:QE1-996.5, image processing, Optical navigation, lcsh:Geology, Identification (information), Asteroid, General Earth and Planetary Sciences, Artificial intelligence, Astrophysics - Instrumentation and Methods for Astrophysics, business
Abstract

During its initial orbital phase in early 2019, the Origins, Spectral Interpretation, Resource Identification, and Security-Regolith Explorer (OSIRIS-REx) asteroid sample return mission detected small particles apparently emanating from the surface of the near-Earth asteroid (101955) Bennu in optical navigation images. Identification and characterization of the physical and dynamical properties of these objects became a mission priority in terms of both spacecraft safety and scientific investigation. Traditional techniques for particle identification and tracking typically rely on manual inspection and are often time-consuming. The large number of particles associated with the Bennu events and the mission criticality rendered manual inspection techniques infeasible for long-term operational support. In this work, we present techniques for autonomously detecting potential particles in monocular images and providing initial correspondences between observations in sequential images, as implemented for the OSIRIS-REx mission., Comment: 23 pages, 10 figures

Published
2020

8. Meteoroid Impacts as a Source of Bennu's Particle Ejection Events

Author

David Vokrouhlický, Stephen R. Schwartz, Michael C. Nolan, Jamie Molaro, William F. Bottke, A. Moorhead, Dante S. Lauretta, Carl Hergenrother, Harold C. Connolly, Kevin J. Walsh, Patrick Michel, Southwest Research Institute [Boulder] (SwRI), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Lunar and Planetary Laboratory [Tucson] (LPL), and University of Arizona

Subjects
010504 meteorology & atmospheric sciences, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Noon, ejecta, 01 natural sciences, Astrobiology, Planetary Sciences: Solar System Objects, Impact crater, Geochemistry and Petrology, Impact Phenomena, Cratering, Comets, OSIRIS‐REx, Earth and Planetary Sciences (miscellaneous), impacts, meteoroids, Ejecta, Planetary Sciences: Solid Surface Planets, Research Articles, 0105 earth and related environmental sciences, Meteoroid, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Impact Phenomena, Dust, Debris, Asteroids, Surfaces, Exploration of the Activity of Asteroid (101955) Bennu, Tectonophysics, Geophysics, Atmosphere of the Moon, 13. Climate action, Space and Planetary Science, Asteroid, [SDU]Sciences of the Universe [physics], Local time, Comets: Dust Tails and Trails, Bennu, Planetary Sciences: Comets and Small Bodies, Other, Natural Hazards, Geology, Research Article
Abstract

Asteroid (101955) Bennu, a near‐Earth object with a primitive carbonaceous chondrite‐like composition, was observed by the Origins, Spectral Interpretation, Resource Identification, and Security‐Regolith Explorer (OSIRIS‐REx) spacecraft to undergo multiple particle ejection events near perihelion between December 2018 and February 2019. The three largest events observed during this period, which all occurred 3.5 to 6 hr after local noon, placed numerous particles, Key Points Meteoroids derived from comets strike Bennu near perihelion once every 2 weeks on average with an impact kinetic energy >7,000 JThey can explain the particle sizes (

Published
2020
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9. Dynamical Evolution of Simulated Particles Ejected from Asteroid Bennu

Author

Y. Takahashi, Davide Farnocchia, Carl Hergenrother, Daniel J. Scheeres, Joshua P. Emery, Pasquale Tricarico, B. Bierhaus, Benjamin Rozitis, Jay W. McMahon, Steven R. Chesley, D. N. Brack, Erwan Mazarico, Andrew French, and Dante S. Lauretta

Subjects
Physics, Spacecraft, business.industry, Astrophysics, Radius, Geophysics, Radiation pressure, Impact crater, Space and Planetary Science, Geochemistry and Petrology, Asteroid, Equatorial bulge, Thermal radiation, Physics::Space Physics, Earth and Planetary Sciences (miscellaneous), Orbit (dynamics), Astrophysics::Earth and Planetary Astrophysics, business
Abstract

In early 2019, the OSIRIS‐REx spacecraft discovered small particles being ejected from the surface of the near‐Earth asteroid Bennu. Although they were seen to be ejected at slow speeds, on the order of tens of cm/s, a number of particles were surprisingly seen to orbit for multiple revolutions and days, which requires a dynamical mechanism to quickly and substantially modify the orbit to prevent re‐impact upon their first periapse passage. This paper demonstrates that, based on simulations constrained by the conditions of the observed events, the combined effects of gravity, solar radiation pressure, and thermal radiation pressure from Bennu can produce many sustained orbits for ejected particles. Furthermore, the simulated populations exhibit two interesting phenomena that could play an important role in the geophysical evolution of bodies such as Bennu. First, small particles (

Published
2020

10. Implications for Ice Stability and Particle Ejection From High-Resolution Temperature Modeling of Asteroid (101955) Bennu

Author

Carl Hergenrother, Hannah C.M. Susorney, Ben Rozitis, Josh Emery, Jamie Molaro, Dante S. Lauretta, and Matthew A. Siegler

Subjects
010504 meteorology & atmospheric sciences, Diurnal temperature variation, Geophysics, 01 natural sciences, Latitude, Amplitude, Space and Planetary Science, Geochemistry and Petrology, Asteroid, Thermal, Earth and Planetary Sciences (miscellaneous), Polar, Sublimation (phase transition), Surface water, Geology, 0105 earth and related environmental sciences
Abstract

The finding by the OSIRIS-REx (Origins, Spectral Interpretation, Resource Identification, and Security–Regolith Explorer) mission that its target (101955) Bennu is an active asteroid has raised questions as to whether the observed particle ejection events are driven by temperature. To investigate sublimation of water ice and rock thermal fracture as possible temperature-driven causes, we modeled the global temperatures of Bennu and searched for correlations with the identified ejection points on the asteroid surface. We computed temperatures with the Advanced Thermophysical Model and the 75-cm-resolution global shape model of Bennu derived by the OSIRIS-REx mission. We find that ~1856 m^2 of Bennu's polar regions have orbit-averaged temperatures that are sufficiently cold to enable water ice, if buried within the top few meters of the surface, to remain stable over geological timescales. Millimeter-thick layers of surface water ice are also stable over ~10^3-year timescales within polar centimeter-scale cold traps. However, we do not find evidence of conditions enabling ice stability in the warmer equatorial regions, where ejection events have been observed, implying that sublimation of water ice is not the cause of particle ejection. Conversely, rock thermal fracture remains a possible mechanism of particle ejection. We find high amplitudes of diurnal temperature variation, a proxy for the efficacy of thermal fracturing, at all latitudes on Bennu due to its extreme ruggedness. Therefore, if rock thermal fracture is the mechanism, particles could be ejected from any latitude, which is consistent with the continued observations of particle ejection by OSIRIS-REx.

Published
2020
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11. Episodes of particle ejection from the surface of the active asteroid (101955) Bennu

Author

Christine Hartzell, Guy Libourel, Bashar Rizk, Jian-Yang Li, Daniel J. Scheeres, David Vokrouhlický, C. Drouet d'Aubigny, Derek S. Nelson, Y. Takahashi, Robert A. Jacobson, Michael C. Moreau, Harold C. Connolly, Eric M. Sahr, William F. Bottke, J. A. Seabrook, J. Y. Pelgrift, Leilah K. McCarthy, J. M. Leonard, Ben Rozitis, Kris J. Becker, S. Selznick, J. de León, Josh Emery, Humberto Campins, Javier Licandro, Carl Hergenrother, Erica Jawin, Marina Brozovic, M. Al Asad, A. B. Davis, Florian Thuillet, Jamie Molaro, Pasquale Tricarico, E. J. Lessac-Chenen, Peter G. Antreasian, Jason P. Dworkin, C. K. Maleszewski, Davide Farnocchia, Carina Bennett, Jay W. McMahon, C. Manzoni, C. W. V. Wolner, Steven R. Chesley, P. Michel, Peter Jenniskens, Andrew J. Liounis, J. N. Kidd, Ronald-Louis Ballouz, Dathon Golish, Michael Daly, Daniella DellaGiustina, Daniel P. Glavin, H. L. Roper, William M. Owen, Coralie D. Adam, Brent J. Bos, B. May, Dante S. Lauretta, Laboratoire Kastler Brossel (LKB (Lhomond)), Université Pierre et Marie Curie - Paris 6 (UPMC)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Dept. of Physics, University of Central Florida [Orlando] (UCF), IHU-LIRYC, Université Bordeaux Segalen - Bordeaux 2-CHU Bordeaux [Bordeaux], Universidad Autonoma de Nuevo Leon [Mexique] (UANL), NASA Goddard Space Flight Center (GSFC), Laboratoire de physique de l'état condensé (LPEC), Centre National de la Recherche Scientifique (CNRS)-Le Mans Université (UM), Dipartimento di Matematica, University of Pisa - Università di Pisa, Université de Washington Seattle, University of Michigan Medical School [Ann Arbor], University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofisica de Canarias (IAC), Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, The Open University [Milton Keynes] (OU), Institute of Astronomy, Charles University [Prague] (CU), ANR-15-IDEX-0001,UCA JEDI,Idex UCA JEDI(2015), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), University of Central Florida [Orlando], CHU Bordeaux [Bordeaux]-Université Bordeaux Segalen - Bordeaux 2, Le Mans Université (UM)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherches Pétrographiques et Géochimiques (CRPG), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Politecnico di Milano [Milan] (POLIMI), Service d'hépato-gastro-entérologie [Hôpital Saint-Louis], Groupe Hospitalier Saint Louis - Lariboisière - Fernand Widal [Paris], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Laboratoire Avancé de Spectroscopie pour les Intéractions la Réactivité et l'Environnement - UMR 8516 (LASIRe), Ecole Nationale Supérieure de Chimie de Lille (ENSCL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Charles University [Prague], and ANR: 15-IDEX-0001,UCA JEDI,Idex UCA JEDI(2015)

Subjects
Solar System, 010504 meteorology & atmospheric sciences, Origin of water on Earth, Population, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics, 01 natural sciences, 0103 physical sciences, education, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, education.field_of_study, Multidisciplinary, Meteoroid, Spacecraft, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], business.industry, 13. Climate action, Asteroid, [SDU]Sciences of the Universe [physics], Solar time, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, business, Orbit determination, Geology
Abstract

INTRODUCTION Active asteroids are small bodies in the Solar System that show ongoing mass loss, such as the ejection of dust, which may be caused by large impacts, volatile release, or rotational acceleration. Studying them informs our understanding of the evolution and destruction of asteroids and the origin of volatile materials such as water on Earth. The OSIRIS-REx (Origins, Spectral Interpretation, Resource Identification, and Security–Regolith Explorer) spacecraft has rendezvoused with the near-Earth asteroid (101955) Bennu. The selection of Bennu as the OSIRIS-REx target was partially based on its spectral similarity to some active asteroids. Observations designed to detect mass loss at Bennu were conducted from Earth and during the spacecraft’s approach, but no signs of asteroid activity were found. However, when the spacecraft entered orbit in January 2019, we serendipitously observed particles in the vicinity of Bennu that had apparently been ejected from its surface. RATIONALE We analyzed the properties and behavior of particles ejected from Bennu to determine the possible mechanisms of ejection and provide understanding of the broader population of active asteroids. Images obtained by the spacecraft indicate multiple discrete ejection events with a range of energies and resultant particle trajectories. We characterized three large ejection events that respectively occurred on 6 January, 19 January, and 11 February 2019. Tracking of individual particles across multiple images by means of optical navigation techniques provided the initial conditions for orbit determination modeling. By combining these approaches, we estimated the locations and times of ejection events and determined initial velocity vectors of particles. We estimated the particle sizes and the minimum energies of the ejection events using a particle albedo and density consistent with observations of Bennu. RESULTS Particles with diameters from 3 m s–1. Estimated energies ranged from 270 mJ for the 6 January event to 8 mJ for the 11 February event. The three events arose from widely separated sites, which do not show any obvious geological distinction from the rest of Bennu’s surface. However, these events all occurred in the late afternoon, between about 15:00 and 18:00 local solar time. In addition to discrete ejection events, we detected a persistent background of particles in the Bennu environment. Some of these background particles have been observed to persist on temporary orbits that last several days—in one case, with a semimajor axis >1 km. The orbital characteristics of these gravitationally bound objects make it possible to determine the ratio of their cross-sectional area to their mass. Combined with their photometric phase functions, this information constrains the parameter space of the particles’ diameters, densities, and albedos. CONCLUSION Plausible mechanisms for the large ejection events include thermal fracturing, volatile release through dehydration of phyllosilicates, and meteoroid impacts. The late-afternoon timing of the events is consistent with any of these mechanisms. Bennu’s boulder geology indicates that thermal fracturing, perhaps enhanced by volatile release, could occur on the asteroid surface. Smaller events, especially those that occur on the night side of Bennu, could be attributable to reimpacting particles. Our observations classify Bennu as an active asteroid. Active asteroids are commonly identified by major mass loss events observable with telescopes, on scales much greater than we observed at Bennu. Our findings indicate that there is a continuum of mass loss event magnitudes among active asteroids.

Published
2019
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12. Detection of Rotational Acceleration of Bennu using HST Lightcurve Observations

Author

Jay W. McMahon, Josh Emery, Michael C. Nolan, Daniel J. Scheeres, Ellen S. Howell, Carl Hergenrother, Dante S. Lauretta, S. R. Chesley, Keith S. Noll, and Oleksiy Golubov

Subjects
Physics, Earth and Planetary Astrophysics (astro-ph.EP), Angular acceleration, Angular momentum, FOS: Physical sciences, Acceleration (differential geometry), Astrophysics, Moment of inertia, Rotation, Light curve, Geophysics (physics.geo-ph), Physics - Geophysics, Geophysics, Asteroid, General Earth and Planetary Sciences, Astrophysics::Earth and Planetary Astrophysics, Spin-up, Astrophysics - Earth and Planetary Astrophysics
Abstract

We observed the near‐Earth asteroid (101955) Bennu from the ground in 1999 and 2005, and with the Hubble Space Telescope (HST) in 2012, to constrain its rotation rate. The data reveal an acceleration of 2.64±1.05 × 10−6deg/day2, which could be due to a change in the moment of inertia of Bennu or to spin up from the Yarkovsky‐O'Keefe‐Radzievskii‐Paddack effect or other source of angular momentum. The best solution is within 1 σ of the period determined by Nolan et al. (2013, https://doi.org/10.1016/j.icarus.2013.05.028). The Origins, Spectral Interpretation, Resource Identification, and Security–Regolith Explorer (OSIRIS‐REx) mission will determine the rotation state independently in 2019.Those measurements should show whether the change in rotation rate is a steady increase (due, e.g., to the Yarkovsky‐O'Keefe‐Radzievskii‐Paddack effect) or some other phenomenon. The precise shape and surface properties measured by the OSIRIS‐REx science team will allow for a better understanding of variations in rotation rate of small asteroids.

Published
2019

13. Results from the Worldwide Coma Morphology Campaign for Comet ISON (C/2012 S1)

Author

Jayant Murthy, Brian D. Ottum, Firoza Sutaria, T. A. Lister, Stephanie Carlino, Susan Hoban, Valerie Rapson, Jean-Baptist Kikwaya Eluo, Nikolai Kiselev, E. Guido, John Caruso, Carl Hergenrother, Mike Holloway, Margarita Safonova, Joseph H. Jones, Betty P.S. Lau, Zhong-Yi Lin, Edward Gomez, Beatrice E. A. Mueller, Roy Prouty, Colin Snodgrass, David G. Schleicher, Quanzhi Ye, Nick Howes, Xing Gao, David C. Vogel, José Luis Martin, Noah Brosch, Onur Yorukoglu, Nalin H. Samarasinha, Thomas G. Kaye, Man-To Hui, Dennis Whitmer, Jim Wyrosdick, Samuel R. Thomas, Joel Schmid, Leo Kellett, Frank Dimino, Matthew M. Knight, John Briol, Tyler B. Penland, Cihan T. Tezcan, M. Nicolini, Aleksandra V. Ivanova, Brandon Doyle, Chris Pruzenski, Tony L. Farnham, David Trowbridge, and A. S. Moskvitin

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, Space and Planetary Science, Continuum (design consultancy), Comet, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Coma (optics), Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the results of a global coma morphology campaign for comet C/2012 S1 (ISON), which was organized to involve both professional and amateur observers. In response to the campaign, many hundreds of images, from nearly two dozen groups were collected. Images were taken primarily in the continuum, which help to characterize the behavior of dust in the coma of comet ISON. The campaign received images from January 12 through November 22, 2013 (an interval over which the heliocentric distance decreased from 5.1 AU to 0.35 AU), allowing monitoring of the long-term evolution of coma morphology during the pre-perihelion leg of comet ISON. Data were contributed by observers spread around the world, resulting in particularly good temporal coverage during November when comet ISON was brightest but its visibility was limited from any one location due to the small solar elongation. We analyze the northwestern sunward continuum coma feature observed in comet ISON during the first half of 2013, finding that it was likely present from at least February through May and did not show variations on diurnal time scales. From these images we constrain the grain velocities to ~10 m/s, and we find that the grains spent 2-4 weeks in the sunward side prior to merging with the dust tail. We present a rationale for the lack of continuum coma features from September until mid-November 2013, determining that if the feature from the first half of 2013 was present, it was likely too small to be clearly detected. We also analyze the continuum coma morphology observed subsequent to the November 12 outburst, and constrain the first appearance of new features in the continuum to later than November 13.99 UT., 23 pages, 7 figures

Published
2015

14. Lightcurve, Color and Phase Function Photometry of the OSIRIS-REx Target Asteroid (101955) Bennu

Author

Daniel J. Scheeres, Michael C. Nolan, Richard P. Binzel, M. A. Barucci, Daniela Lazzaro, Javier Licandro, Christian Drouet d'Aubigny, Carl Hergenrother, Dante S. Lauretta, E. C. Beshore, Edward A. Cloutis, Beth E. Clark, Humberto Campins, Bashar Rizk, Noemi Pinilla-Alonso, Patrick Michel, Economics, University of Hull, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Geography [Winnipeg], University of Winnipeg, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), De la Préhistoire à l'Actuel : Culture, Environnement et Anthropologie (PACEA), Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Flight Dynamics and Control (University of Michigan), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Instituto de Astrofisica de Canarias (IAC), and Université de Bordeaux (UB)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, ICARUS, Rotation period, [PHYS]Physics [physics], Near-Earth object, 010504 meteorology & atmospheric sciences, biology, Synodic day, Astronomy, Astronomy and Astrophysics, biology.organism_classification, 01 natural sciences, Photometry (optics), Space and Planetary Science, Asteroid, 0103 physical sciences, Phase function, Osiris, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

The NASA OSIRIS-REx mission will retrieve a sample of the carbonaceous near-Earth Asteroid (101955) Bennu and return it to Earth in 2023. Photometry in the Eight Color Asteroid Survey (ECAS) filter system and Johnson–Cousins V and R filters were conducted during the two most recent apparitions in 2005/2006 and 2011/2012. Lightcurve observations over the nights of September 14–17, 2005 yielded a synodic rotation period of 4.2905 ± 0.0065 h, which is consistent with the results of Nolan et al. (2013). ECAS color measurements made during the same nights confirm the B-type classification of Clark et al. (Clark, B.E., Binzel, R.P., Howell, E.S., Cloutis, E.A., Ockert-Bell, M., Christensen, P., Barucci, M.A., DeMeo, F., Lauretta, D.S., Connolly, H., Soderberg, A., Hergenrother, C., Lim, L., Emery, J., Mueller, M. [2011]. Icarus 216, 462–475). A search for the 0.7 μm hydration feature using the method of Vilas (Vilas, F. [1994]. Icarus 111, 456–467) did not reveal its presence. Photometry was obtained over a range of phase angles from 15° to 96° between 2005 and 2012. The resulting phase function slope of 0.040 magnitudes per degree is consistent with the phase slopes of other low albedo near-Earth asteroids (Belskaya, I.N., Shevchenko, V.G. [2000]. Icarus 147, 94–105).

Published
2013
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15. Physical and dynamical characterisation of low Delta-V NEA (190491) 2000 FJ10

Author

S. Duddy, T. Kwiatkowski, Carl Hergenrother, Amanda A. S. Gulbis, Alan Fitzsimmons, Apostolos A. Christou, and M. Butkiewicz

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Absolute magnitude, Rotation period, Near-Earth object, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Asteroid family, Photometry (optics), Space and Planetary Science, Asteroid, William Herschel Telescope, Southern African Large Telescope, Geology, Astrophysics - Earth and Planetary Astrophysics
Abstract

We investigated the physical properties and dynamical evolution of Near Earth Asteroid (NEA) (190491) 2000 FJ10 in order to assess the suitability of this accessible NEA as a space mission target. Photometry and colour determination were carried out with the 1.54 m Kuiper Telescope and the 10 m Southern African Large Telescope during the object's recent favourable apparition in 2011-12. During the earlier 2008 apparition, a spectrum of the object in the 6000-9000 Angstrom region was obtained with the 4.2 m William Herschel Telescope. Interpretation of the observational results was aided by numerical simulations of 1000 dynamical clones of 2000 FJ10 up to 10^6 yr in the past and in the future. The asteroid's spectrum and colours determined by our observations suggest a taxonomic classification within the S-complex although other classifications (V, D, E, M, P) cannot be ruled out. On this evidence, it is unlikely to be a primitive, relatively unaltered remnant from the early history of the solar system and thus a low priority target for robotic sample return. Our photometry placed a lower bound of 2 hrs to the asteroid's rotation period. Its absolute magnitude was estimated to be 21.54+-0.1 which, for a typical S-complex albedo, translates into a diameter of 130+-20 m. Our dynamical simulations show that it has likely been an Amor for the past 10^5 yr. Although currently not Earth-crossing, it will likely become so during the period 50 - 100 kyr in the future. It may have arrived from the inner or central Main Belt > 1 Myr ago as a former member of a low-inclination S-class asteroid family. Its relatively slow rotation and large size make it a suitable destination for a human mission. We show that ballistic Earth-190491-Earth transfer trajectories with Delta-V < 2 km s^-1 at the asteroid exist between 2052 and 2061., 2 Tables, 11 Figures, accepted for publication in Astronomy & Astrophysics

Published
2012

16. Asteroid (101955) 1999 RQ36: Spectroscopy from 0.4 to 2.4 mum and meteorite analogs

Author

Edward A. Cloutis, Alicia M. Soderberg, Maria Antonietta Barucci, Dante S. Lauretta, Ellen S. Howell, Philip R. Christensen, Beth E. Clark, F. DeMeo, Richard P. Binzel, M. Ockert-Bell, Harold C. Connolly, Carl Hergenrother, Josh Emery, Michael Mueller, Lucy F. Lim, Department of Physics, Ithaca College, Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Arecibo Observatory, Department of Geography, University of Winnipeg, Arizona State University, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Guest observer at NASA Infrared Telescope Facility, Lunar and Planetary Laboratory [University of Arizona] (LPL), University of Arizona, Earth and Planetary Sciences, City University of New York, Department of Astronomy, Harvard University, Deutsches Geodätisches Forschungsinstitut (DGFI), Department of Earth and Planetary Science, University of Tennessee, Observatoire de la Côte d'Azur (OCA), and Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Meteorite, Space and Planetary Science, Infrared, Asteroid, Chondrite, Carbonaceous chondrite, Astronomy, Astronomy and Astrophysics, Spectroscopy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Spectrograph, Spectral line
Abstract

International audience; We present reflectance spectra from 0.4 to 2.4 mum of Asteroid (101955) 1999 RQ36, the target of the OSIRIS-REx spacecraft mission. The visible spectral data were obtained at the McDonald Observatory 2.1-m telescope with the ES2 spectrograph. The infrared spectral data were obtained at the NASA Infrared Telescope Facility using the SpeX instrument. The average visible spectrum is combined with the average near-infrared wavelength spectrum to form a composite spectrum. We use three methods to constrain the compositional information in the composite spectrum of Asteroid (101955) 1999 RQ36 (hereafter RQ36). First, we perform a least-squares search for meteorite spectral analogs using 15,000 spectra from the RELAB database. Three most likely meteorite analogs are proposed based on the least-squares search. Next, six spectral parameters are measured for RQ36 and their values are compared with the ranges in parameter values of the carbonaceous chondrite meteorite classes. A most likely meteorite analog group is proposed based on the depth of overlap in parameter values. The results of the least-squares search and the parametric comparisons point to CIs and/or CMs as the most likely meteorite analogs for RQ36, and COs and CHs as the least likely. RQ36 has a spectrally "blue" continuum slope that is also observed in carbonaceous chondrites containing magnetite. We speculate that RQ36 is composed of a "CM1"-like material. Finally, we compare RQ36 to other B-type asteroids measured by Clark et al. (Clark, B.E. et al. [2010]. J. Geophys. Res. 115, E06005). The results of this comparison are inconclusive. RQ36 is comparable to Themis spectral properties in terms of its albedo, visible spectrum, and near-infrared spectrum from 1.1 to 1.45 mum. However, RQ36 is more similar to Pallas in terms of its near-infrared spectrum from 1.6 to 2.3 mum. Thus it is possible that B-type asteroids form a spectral continuum and that RQ36 is a transitional object, spectrally intermediate between the two end-members. This is particularly interesting because Asteroid 24 Themis was recently discovered to have H 2O ice on the surface (Rivkin, A., Emery, J. [2010]. Nature 464, 1322-1323; Campins, H. et al. [2010a]. Nature 464, 1320-1321).

Published
2011
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17. Comet 162P/Siding Spring: A Surprisingly Large Nucleus

Author

Richard P. Binzel, Javier Licandro, M. Kassis, Humberto Campins, Joseph L. Hora, Yanga R. Fernandez, Joseph D. Adams, and Carl Hergenrother

Subjects
Physics, Effective radius, Astrophysics (astro-ph), Comet, FOS: Physical sciences, Astronomy and Astrophysics, Coma (optics), Astrophysics, Spectral line, Astron, medicine.anatomical_structure, Space and Planetary Science, Geometric albedo, medicine, Spectral energy distribution, Nucleus
Abstract

We present an analysis of thermal emission from comet 162P/Siding Spring (P/2004 TU12) measured during its discovery apparition in 2004 December. The comet showed no dust coma at this time, so we have sampled emission from the comet's nucleus. Observations using the Mid-Infrared Spectrometer and Imager (MIRSI) were performed at NASA's Infrared Telescope Facility, where the peak of the comet's spectral energy distribution was observed between 8 and 25 microns. In combination with the three near-IR spectra presented by Campins et al. (2006, Astron. J. 132, 1346) that show the Wien-law tail of the thermal emission, the data provide powerful constraints on surface properties of the nucleus. We find that the nucleus's effective radius is 6.0+/-0.8 km. This is one of the largest radii known among Jupiter-family comets, which is unusual considering that the comet was discovered only recently. Its geometric albedo is 0.059+/-0.023 in the H band, 0.037+/-0.014 in the R band, and 0.034+/-0.013 in the V band. We also find that the nucleus of 162P has little IR beaming, and this implies that the nucleus has low thermal inertia. Including all near-IR spectra yields a beaming parameter of 1.01+/-0.20. This result is in agreement with others showing that cometary nuclei have low thermal inertia and little IR beaming. If confirmed for many nuclei, the interpretation of radiometry may not be as problematic as feared., 17 pages, 4 figures, appearing in The Astronomical Journal, September 2006 issue

Published
2006

18. The Transit Light Curve (TLC) Project. I. Four Consecutive Transits of the Exoplanet XO-1b

Author

David W. Latham, Carl Hergenrother, Mark E. Everett, Matthew J. Holman, Gáspár Á. Bakos, David Charbonneau, Francis T. O'Donovan, Gilbert A. Esquerdo, Joshua N. Winn, and András Pál

Subjects
Physics, Stellar mass, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Radius, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Light curve, Exoplanet, Jupiter, Photometry (optics), Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, High Energy Physics::Experiment, Transit (astronomy), Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present RIz photometry of four consecutive transits of the newly discovered exoplanet XO-1b. We improve upon the estimates of the transit parameters, finding the planetary radius to be R_P = 1.184 +0.028/-0.018 R_Jupiter and the stellar radius to be R_S = 0.928 +0.018/-0.013 R_Sun, assuming a stellar mass of M_S = 1.00 +/- 0.03 M_Sun. The uncertainties in the planetary and stellar radii are dominated by the uncertainty in the stellar mass. These uncertainties increase by a factor of 2-3 if a more conservative uncertainty of 0.10 M_Sun is assumed for the stellar mass. Our estimate of the planetary radius is smaller than that reported by McCullough et al. (2006) and yields a mean density that is comparable to that of TrES-1 and HD 189733b. The timings of the transits have an accuracy ranging from 0.2 to 2.5 minutes, and are marginally consistent with a uniform period., 22 pages, 5 figures, 2 tables. Accepted for publication in ApJ

Published
2006

19. Refined parameters of the planet orbiting HD 189733

Author

Michel Mayor, Frederic Pont, C. Moutou, François Bouchy, Avi Shporer, David Charbonneau, David W. Latham, Tsevi Mazeh, Carl Hergenrother, Didier Queloz, Heather A. Knutson, András Pál, Stéphane Udry, R. W. Noyes, Gáspár Á. Bakos, Mark E. Everett, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Université de Genève (UNIGE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Beaussier, Catherine

Subjects
Physics, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radius, Ephemeris, Orbital period, Exoplanet, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Current sample, Photometry (astronomy), Space and Planetary Science, Planet, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Transit (astronomy)
Abstract

We report on the BVRI multi-band follow-up photometry of the transiting extrasolar planet HD 189733b. We revise the transit parameters and find planetary radius RP = 1.154+/- 0.032RJ and inclination i_P = 85.79+/-0.24deg. The new density (~ 1g cm-3) is significantly higher than the former estimate (~ 0.75g cm-3); this shows that from the current sample of 9 transiting planets, only HD 209458 (and possibly OGLE-10b) have anomalously large radii and low densities. We note that due to the proximity of the parent star, HD 189733b currently has one of the most precise radius determinations among extrasolar planets. We calculate new ephemerides: P = 2.218573+/-0.000020 days, T0 = 2453629.39420+/-0.00024 (HJD), and estimate the timing offsets of the 11 distinct transits with respect to the predictions of a constant orbital period, which can be used to reveal the presence of additional planets in the system., Comment: 10 pages, 4 figures, submitted to ApJ

Published
2006

20. Deep Impact: Observations from a Worldwide Earth-Based Campaign

Author

Jean Manfroid, Miroslav Filipovic, Christiaan Sterken, Maria Teresa Capria, M. J. S. Belton, N. Ageorges, U.W. Kamath, L. M. Woodney, Randy D. Campbell, Tomohiko Sekiguchi, Diane H. Wooden, Tetsuharu Fuse, Nicholas B. Suntzeff, S.K. Pandea, Michael J. Mumma, Jacques Crovisier, Emmanuel Jehin, Itsuki Sakon, R. Fugate, H. U. Kaufl, D. Fong, L. Barrera, Anita L. Cochran, Ivo Saviane, Jeremy Bailey, K. von Braun, R. Barrena, G. Ruch, G. R. Stecklein, Sunao Hasegawa, Miquel Serra-Ricart, J. Watanabe, T. Carroll, Damien Hutsemekers, Brian M. Patten, Ronald L. Snell, R. G. Sharp, Takuya Fujiyoshi, S. Fisher, Geraint H. Jones, R. Cleis, Scott J. Wolk, Geoffrey A. Blake, Toshihiko Kadono, Susan M. Lederer, Michael F. A'Hearn, David J. Wilner, William F. Welsh, Daisuke Kinoshita, S.D. Rodgers, L. Dundon, J.-H. Wu, Marc W. Buie, Jianguo Li, Luisa Lara, Yanga R. Fernandez, Paul A. Jones, Wiphu Rujopakarn, Geronimo L. Villanueva, Michael G. Burton, Ramprasad Rao, Florian Kerber, Takaki Miyata, S. M. Larson, Stephen C. Lowry, Remi A. Cabanac, J. Debuizer, Richard J. Wainscoat, Paul R. Weissman, D. K. Sahu, Heike Rauer, Ellen S. Howell, T. Yamashita, Boncho P. Bonev, Stefano Bagnulo, G. P. Tozzi, Hideyo Kawakita, Tushar P. Prabhu, P. Colom, H. Tran, J. Aycock, Andrew J. Coates, Jack D. Drummond, Chick E Woodward, N. Biver, Harold A. Weaver, James E. Lyke, Bin Yang, Patrick Seitzer, Alan Fitzsimmons, Richard Dekany, Michael S. P. Kelley, Zhong-Yi Lin, Shigehisa Takakuwa, M. Sumner, Mark Gurwell, Rita Schulz, Harold J. Reitsema, Karen J. Meech, Bidushi Bhattacharya, Choogon Lee, Gerald Moriarty-Schieven, Samuel Gulkis, O. Marco, D. Harrington, Matthew M. Knight, David E. Harker, Roberto Vázquez, Olivier Hainaut, R. Swaters, M. Schirmer, Z.J. Jiang, X. Zhao, Fernando Selman, Humberto Campins, Tom Stallard, Maria Womack, Daisuke Iono, Noemi Pinilla-Alonso, Pierre Martin, E. Thompson, William M. Jackson, Alan T. Tokunaga, Bryan E. Penprase, Al Conrad, Amy J. Lovell, Mitsuhiko Honda, Rosemary Barber, A. C. Zook, David K. Lynch, A. Delsanti, Hermann Boehnhardt, B. E. A. Mueller, Wing-Huen Ip, G. LoCurto, Xin Zhou, Faith Vilas, Kevin J. Walsh, Peter H. Schultz, Y.-B. Yang, Chunhua Qi, R. Furusho, A. Zauderer, Erika L. Gibb, J. Pittichova, M. Weiler, Steven B. Charnley, Dominique Bockelée-Morvan, Gary J. Melnick, R. Vasundhara, Shigeyuki Sako, Anny Chantal Levasseur-Regourd, David J. Osip, Naruhisa Takato, Claude Arpigny, Iain Coulson, Mitchell Troy, R. Ruane, M. Kidger, Alison B. Peck, Javier Licandro, N. Moskovitz, Carl Hergenrother, Eric Pantin, David A. Neufeld, Colin Snodgrass, N. Dello Russo, Harold M. Butner, Takafumi Ootsubo, P.B. Etzel, Seiji Sugita, J. E. Thomas-Osip, Karen Magee-Sauer, Klaus-Werner Hodapp, W. Weaver, J. de León, James M. Bauer, Olivier Groussin, G. Maheswar, Tony L. Farnham, P. Rodriguez, A. Ates, F. Bensch, G. Petitas, Paul Hirst, Michael A. DiSanti, Rachel Paterno-Mahler, F. Chaffee, Patrick M. Vora, J. van Cleve, J.-M. Zucconi, Tanyu Bonev, Steve Miller, J. Ma, Martin Harwit, Z.-Y. Wu, J. A. Stüwe, Carey M. Lisse, Toshihiro Kasuga, S. Muneer, John Sarkissian, Chadwick A. Trujillo, Emanuela Pompei, Nalin H. Samarasinha, Paul D. Feldman, Qiang Li, Edith Hadamcik, Haruhiko Fujiwara, S. Yokogawa, Institute for Astronomy [Honolulu], University of Hawaii at Manoa ( UHM ), European Southern Observatory [Santiago] ( ESO ), European Southern Observatory ( ESO ), Department of Astronomy [College Park], University of Maryland [College Park], Université de Liège, Pomona College, Australian Centre for Astrobiology, University of New South Wales [Sydney] ( UNSW ), University College of London [London] ( UCL ), Universidad Metropolitana de Ciencias de la Educación ( UMCE ), Instituto de Astrofisica de Canarias ( IAC ), Jet Propulsion Laboratory ( JPL ), California Institute of Technology ( CALTECH ) -NASA, RadioAstronomisches Institut [Bonn] ( RAIUB ), Bonn Universität [Bonn], California Institute of Technology ( CALTECH ), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Istituto Nazionale di Astrofisica ( INAF ), Mullard Space Science Laboratory ( MSSL ), Service d'aéronomie ( SA ), Centre National de la Recherche Scientifique ( CNRS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ), Atmospheric Physics Laboratory [UCL London], Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), Department of Physics and Astronomy [UCL London], Laboratoire d'astrophysique de l'observatoire de Besançon ( LAOB ), Université de Franche-Comté ( UFC ), University of Hawai‘i [Mānoa] (UHM), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), University of Maryland System-University of Maryland System, University of New South Wales [Sydney] (UNSW), University College of London [London] (UCL), Universidad Metropolitana de Ciencias de la Educación (UMCE), Instituto de Astrofisica de Canarias (IAC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Belton Space Initiatives, RadioAstronomisches Institut [Bonn] (RAIUB), Rheinische Friedrich-Wilhelms-Universität Bonn, California Institute of Technology (CALTECH), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, University of Toledo, Institute of Astronomy of the Bulgarian Academy of Sciences, Bulgarian Academy of Sciences (BAS), Lowell Observatory [Flagstaff], Joint Astronomy Center (JAC), Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), W.M. Keck Observatory, University of Central Florida [Orlando] (UCF), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Istituto Nazionale di Astrofisica (INAF), NASA Ames Research Center (ARC), Air Force Research Laboratory (AFRL), United States Air Force (USAF), Mullard Space Science Laboratory (MSSL), University of Texas at Austin [Austin], Gemini Observatory [Southern Operations Center], Association of Universities for Research in Astronomy (AURA), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), NASA Goddard Space Flight Center (GSFC), San Diego State University (SDSU), University of Maryland System, Johns Hopkins University (JHU), Western Sydney University, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Isaac Newton Group of Telescopes (ING), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) (LAOB), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH)-NASA, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), University of Central Florida [Orlando], Western Sydney University (UWS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), and Laboratoire d'astrophysique de l'observatoire de Besançon (LAOB)

Subjects
Cosmic Dust, Multidisciplinary, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Comet, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Meteoroids, Mass ratio, 01 natural sciences, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrobiology, Photometry, Deep Impact, [ PHYS.ASTR.EP ] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Jupiter, 0103 physical sciences, Organic Chemicals, Ejecta, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

著者人数: 209名, Accepted: 2005-09-01, 資料番号: SA1004082000

Published
2005
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