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209 results on '"Asteroiden und Kometen"'

1. Convex Shape and Rotation Model of Lucy Target (11351) Leucus from Lightcurves and Occultations

Author

Simone Marchi, Harold F. Levison, Stefano Mottola, Marc W. Buie, Amanda M. Zangari, S. Hellmich, and Michael E. Brown

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, Rotation period, Asteroiden und Kometen, Ecliptic coordinate system, Planetengeodäsie, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Phase curve, Light curves, Light curve, Stellar occultation, Occultation, Jupiter trojans, Geophysics, Space and Planetary Science, Sidereal time, Geometric albedo, Orientation (geometry), Earth and Planetary Sciences (miscellaneous), Astrophysics::Earth and Planetary Astrophysics, CCD photometry, Astrophysics - Earth and Planetary Astrophysics
Abstract

We report new photometric lightcurve observations of the Lucy Mission target (11351) Leucus acquired during the 2017, 2018, and 2019 apparitions. We use these data in combination with stellar occultations captured during five epochs to determine the sidereal rotation period, the spin axis orientation, a convex shape model, the absolute scale of the object, its geometric albedo, and a model of the photometric properties of the target. We find that Leucus is a prograde rotator with a spin axis located within a sky-projected radius of 3° (1σ) from J2000 Ecliptic coordinates (λ = 208°, β = +77°) or J2000 Equatorial Coordinates (R.A. = 248°, decl. = +58°). The sidereal period is refined to P sid = 445.683 ± 0.007 h. The convex shape model is irregular, with maximum dimensions of 60.8, 39.1, and 27.8 km. The convex model accounts for global features of the occultation silhouettes, although minor deviations suggest that local and global concavities are present. We determine a geometric albedo of p V = 0.043 ± 0.002. The derived phase curve supports a D-type classification for Leucus.

Published
2020
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2. Lineaments on the Surface of the Consolidated Material of the Comet 67P/Churyumov−Gerasimenko Nucleus

Author

Horst Uwe Keller, S. S. Krasilnikov, Stubbe F. Hviid, Urs Mall, Yuri V. Skorov, and Alexander T. Basilevsky

Subjects
Asteroiden und Kometen, 010504 meteorology & atmospheric sciences, Lineament, Population, Mineralogy, 01 natural sciences, Power law, 0103 physical sciences, medicine, education, 010303 astronomy & astrophysics, Image resolution, 0105 earth and related environmental sciences, education.field_of_study, Pixel, nucleus, Astronomy and Astrophysics, Rosetta 67P Comets Lineaments, medicine.anatomical_structure, fracture, Space and Planetary Science, spacing, consolidated material, Layering, Nucleus, Geology
Abstract

orphologic analysis of the fragments (500 × 500 pixels) of images of comet 67P/Churyumov−Gerasimenko obtained with the OSIRIS camera for 18 regions, where the consolidated material is exposed on the surface, has been carried out. In terms of resolution, the images form a series from 0.04 to 1.29 m/pixel; consequently, the areas covered by these fragments vary from 400 to ~400 000 m2. In all of the regions, lineaments resembling tension fractures—several dozens of structures per region—are seen; and their number scarcely changes when passing from high-resolution images to lower-resolution ones. It is clear that relatively small lineaments cease to be reliably distinguished when the image resolution worsens, but the largest and well-defined ones remain observable, while the number of larger lineaments grows proportionally to the survey area increasing. Undoubtedly, this is an observational effect, which was demonstrated by examples with an artificially worsened resolution. However, on the other hand, this means that the tension fractures of the consolidated nucleus material represent a hierarchic population of smaller (meters long) to larger (decameters and longer) features. The lineaments seen in the analyzed fragments of images were counted, their lengths were measured, and the spacings (the mean distances between lineaments) and, from them, the depths of penetration of fractures into the nucleus material were estimated. It has been shown that the mean length of lineaments within each studied region depend s on its area (which here correlates with the image resolution) and the depths of fracture penetration into the nucleus body depends on the mean length of lineaments. Both dependences are close to a power law. In the images of four regions covering the areas from 100 000 to 400 000 m2 with a resolution of 0.66−1.29 m/pixel, the structures that look like layering or sheet jointing are seen in addition to fracture lineaments. The tension fractures are apparently formed due to seasonal and diurnal variations of the temperature, while the nature of the formation of the layer-like structures is not yet fully understood.

Published
2018
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3. Compressive strength and elastic modulus at Agilkia on comet 67P/Churyumov-Gerasimenko derived from the SESAME/CASSE touchdown signals

Author

Alberto Flandes, K. Thiel, D. Möhlmann, Hans-Herbert Fischer, Frank Scholten, Martin Knapmeyer, Harald Krüger, Claudia Faber, R. Roll, Walter Arnold, and Klaus J. Seidensticker

Subjects
Asteroiden und Kometen, Materials science, 010504 meteorology & atmospheric sciences, Planetengeodäsie, Leitungsbereich PF, Touchdown, Astronomy and Astrophysics, Fracture mechanics, Mechanics, 01 natural sciences, Elasticity, Nutzerzentrum für Weltraumexperimente (MUSC), Depth sounding, Comet surface material, Compressive strength, Planetenphysik, Space and Planetary Science, Compression strength, 0103 physical sciences, Contact zone, Elasticity (economics), Porosity, 010303 astronomy & astrophysics, Elastic modulus, 0105 earth and related environmental sciences
Abstract

We report an analysis of the Comet Acoustic Surface Sounding Experiment (CASSE) acceleration signals at Philae's first touchdown site Agilkia on comet 67P/Churyumov-Gerasimenko. The signals yield the forces in the contact zone foot-sole and comet surface, and from these forces a compression strength of approximately 10 kPa can be derived. The sole's contact-resonances provide an elastic modulus of the order of 10 MPa. Our results are partially based on calibration experiments, which are described in the appendix of the current paper. Relations known in material science, linking porosity to elasticity and fracture energy, allow one to check the interdependence between compression strength and elasticity.

Published
2018
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4. Evidence of sub-surface energy storage in comet 67P from the outburst of 2016 July 03

Author

M. A. Barucci, Eberhard Grün, Giampiero Naletto, Ivano Bertini, M. De Cecco, Pedro Hasselmann, S. Mottola, Wing-Huen Ip, Laurent Jorda, Bernhard Geiger, Xian Shi, Maurizio Pajola, Jouni Rynö, Gabriele Cremonese, Oliver Stenzel, J. J. Lopez Moreno, J. L. Bertaux, J. Kissel, S. Höfner, M. F. A'Hearn, Olivier Groussin, Martin Hilchenbach, B. Zaprudin, Steve Boudreault, V. Da Deppo, Alessandra Rotundi, Ludmilla Kolokolova, Dennis Bodewits, Philippe Lamy, Jessica Agarwal, Marc Hofmann, Paul D. Feldman, Horst Uwe Keller, Stefano Debei, Sihane Merouane, J. Wm. Parker, Monica Lazzarin, Stubbe F. Hviid, Michael Küppers, Stavro Ivanovski, Cesare Barbieri, Jean-Baptiste Vincent, Francesco Marzari, Detlef Koschny, Yves Langevin, Sonia Fornasier, N. Oklay, L. M. Lara, Jakob Deller, Zhong-Yi Lin, A. Koch, Andrew J. Steffl, R. Rodrigo, Björn Davidsson, J.-R. Kramm, Carsten Güttler, E. Kührt, Cecilia Tubiana, Klaus Hornung, P. J. Gutierrez, Stephen C. Lowry, Jörg Knollenberg, Holger Sierks, Henning Fischer, Marco Fulle, V. Della Corte, A. Gicquel, Harold A. Weaver, Nicolas Thomas, Lori M. Feaga, Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Dipartimento di Scienze e Tecnologie [Napoli] (DIST), Università degli Studi di Napoli 'Parthenope' = University of Naples (PARTHENOPE), Department of Physics and Astronomy [Baltimore], Johns Hopkins University (JHU), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Università degli Studi di Padova = University of Padua (Unipd), Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, 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 Kernphysik (MPIK), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Istituto Nazionale di Astrofisica (INAF), NASA Ames Research Center (ARC), Department of Space Studies [Boulder], Southwest Research Institute [Boulder] (SwRI), Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), Dipartimento di Fisica e Astronomia 'Galileo Galilei', PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), CNR Institute for Photonics and Nanotechnologies (IFN), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Industrial Engineering [Padova], INAF - Osservatorio Astronomico di Trieste (OAT), 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), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Universität der Bundeswehr München [Neubiberg], DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Institute of Astronomy [Taiwan] (IANCU), National Central University [Taiwan] (NCU), Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], von Hoerner und Sulger GmbH, European Space Research and Technology Centre (ESTEC), Research and Scientific Support Department, ESTEC (RSSD), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Centre for Astrophysics and Planetary Science [Canterbury] (CAPS), University of Kent [Canterbury], CNR Istituto di Fotonica e Nanotecnologie [Padova] (IFN), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), International Space Science Institute [Bern] (ISSI), Finnish Meteorological Institute (FMI), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Tuorla Observatory, University of Turku, Lowry, S.C., ITA, FRA, DEU, ESP, Centre National de la Recherche Scientifique (France), German Centre for Air and Space Travel, Agenzia Spaziale Italiana, Swedish National Space Board, Ministerio de Economía y Competitividad (España), European Space Agency, Max-Planck-Institut für Sonnensystemforschung (MPS), Universita degli studi di Napoli 'Parthenope' [Napoli], European Space Agency (ESA), Universita degli Studi di Padova, Universität Bern [Bern], Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Consiglio Nazionale delle Ricerche [Roma] (CNR), California Institute of Technology (CALTECH)-NASA, European Space Agency (ESA)-European Space Agency (ESA), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Asteroiden und Kometen, Solid state: refractory, Acceleration of particles, 010504 meteorology & atmospheric sciences, 01 natural sciences, law.invention, Astrobiology, Scattering, individual: 67P/Churyumov-Gerasimenko [Comets], law, Rosetta, 0103 physical sciences, Surface change, Astrophysics::Solar and Stellar Astrophysics, Sunrise, OSIRIS, Solid state: volatile, Crystallization, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Comets: individual: 67P/Churyumov-Gerasimenko, [PHYS]Physics [physics], Physics, ta115, 520 Astronomy, volatile [Solid state], general [Comets], Astronomy and Astrophysics, Solar illumination, 620 Engineering, Surface energy, Amorphous solid, Comets: general, On board, 13. Climate action, Space and Planetary Science, acceleration of particles, scattering, solid state: refractory, solid state: volatile, comets: general, comets: individual: 67P/Churyumov-Gerasimenko, Physics::Space Physics, Sublimation (phase transition), QB651, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], refractory [Solid state]
Abstract

On 2016 July 03, several instruments onboard ESA's Rosetta spacecraft detected signs of an outburst event on comet 67P, at a heliocentric distance of 3.32 au from the Sun, outbound from perihelion. We here report on the inferred properties of the ejected dust and the surface change at the site of the outburst. The activity coincided with the local sunrise and continued over a time interval of 14-68 min. It left a 10-m-sized icy patch on the surface. The ejected material comprised refractory grains of several hundred microns in size, and sub-micron-sized water ice grains. The high dust mass production rate is incompatible with the free sublimation of crystalline water ice under solar illumination as the only acceleration process. Additional energy stored near the surface must have increased the gas density. We suggest a pressurized sub-surface gas reservoir, or the crystallization of amorphous water ice as possible causes.© 2015 The Authors., The support of the national funding agencies of Germany (DLR, grant 50 QP 1302), France (CNES), Austria, Finland and the ESA Technical Directorate is gratefully acknowledged.

Published
2017
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5. Long-term survival of surface water ice on comet 67P

Author

Alice Lucchetti, M. De Cecco, R. Rodrigo, Michael Küppers, Laurent Jorda, Ivano Bertini, Nilda Oklay, W-H. Ip, Detlef Koschny, Marc Hofmann, J. L. Bertaux, Frank Scholten, Nicolas Thomas, J.-R. Kramm, V. Da Deppo, Clement Feller, P. J. Gutierrez, Dennis Bodewits, Sonia Fornasier, Carsten Güttler, I. Hall, Maurizio Pajola, Nafiseh Masoumzadeh, Francesco Marzari, Marco Fulle, A. Gicquel, M. A. Barucci, Jörg Knollenberg, Holger Sierks, Cesare Barbieri, Monica Lazzarin, Jakob Deller, Zhong-Yi Lin, David Kappel, Olivier Groussin, J. J. Lopez Moreno, Jean-Baptiste Vincent, Horst Uwe Keller, Michael F. A'Hearn, Luisa Lara, Giampiero Naletto, Pedro Hasselmann, Björn Davidsson, Cecilia Tubiana, Philippe Lamy, Antoine Pommerol, Stubbe F. Hviid, Hans Rickman, Frank Preusker, Xian Shi, Stefano Mottola, Gábor L. Kovács, Gabriele Cremonese, Ekkehard Kührt, J. D. P. Deshapriya, Stefano Debei, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), NASA Ames Research Center (ARC), 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), Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Dipartimento di Fisica e Astronomia 'Galileo Galilei', Università degli Studi di Padova = University of Padua (Unipd), 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), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), International Space Science Institute [Bern] (ISSI), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), Department of Physics and Astronomy [Uppsala], Uppsala University, Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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)-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), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), CNR Institute for Photonics and Nanotechnologies (IFN), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Industrial Engineering [Padova], University of Trento [Trento], INAF - Osservatorio Astronomico di Trieste (OAT), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institute of Space Science [Taiwan], National Central University [Taiwan] (NCU), Operations Department (ESAC), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Department of Information Engineering [Padova] (DEI), Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), Max-Planck-Institut für Sonnensystemforschung (MPS), Universita degli Studi di Padova, 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), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), European Space Agency (ESA), Consiglio Nazionale delle Ricerche [Roma] (CNR), European Space Agency (ESA)-European Space Agency (ESA), Universität Bern [Bern], and California Institute of Technology (CALTECH)-NASA

Subjects
Asteroiden und Kometen, 010504 meteorology & atmospheric sciences, Infrared, Comet, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Techniques: image processing, Narrow angle, Astrophysics, 01 natural sciences, Methods: data analysis, 0103 physical sciences, Long term survival, Techniques: imaging spectroscopy, Variation (astronomy), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Comets: individual: 67P/Churyumov-Gerasimenko, Physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 520 Astronomy, Leitungsbereich PF, Planetengeodäsie, Astronomy and Astrophysics, 620 Engineering, 13. Climate action, Space and Planetary Science, Water ice, Surface water
Abstract

Numerous water-ice-rich deposits surviving more than several months on comet 67P/Churyumov-Gerasimenko were observed during the Rosetta mission. We announce the first-time detection of water-ice features surviving up to 2 yr since their first observation via OSIRIS (Optical, Spectroscopic, and Infrared Remote Imaging System) NAC (narrow angle camera). Their existence on the nucleus of comet 67P at the arrival of the Rosetta spacecraft suggests that they were exposed to the surface during the comet's previous orbit. We investigated the temporal variation of large water-ice patches to understand the long-term sustainability of water ice on cometary nuclei on time-scales of months and years. Large clusters are stable over typical periods of 0.5 yr and reduce their size significantly around the comet's perihelion passage, while small exposures disappear. We characterized the temporal variation of their multispectral signatures. In large clusters, dust jets were detected, whereas in large isolated ones no associated activity was detected. Our thermal analysis shows that the long-term sustainability of water-ice-rich features can be explained by the scarce energy input available at their locations over the first half year. However, the situation reverses for the period lasting several months around perihelion passage. Our two end-member mixing analysis estimates a pure water-ice equivalent thickness up to 15 cm within one isolated patch, and up to 2 m for the one still observable through the end of the mission. Our spectral modelling estimates up to 48 per cent water-ice content for one of the large isolated feature, and up to 25 per cent water ice on the large boulders located within clusters.

Published
2017
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6. Close-up images of the final Philae landing site on comet 67P/Churyumov-Gerasimenko acquired by the ROLIS camera

Author

Jean-Pierre Bibring, Alexander Koncz, Katharina A. Otto, Ralf Jaumann, Stefano Mottola, B. Dolives, Gabriele Arnold, H. U. Keller, Harald Michaelis, Ivanka Pelivan, Stefan Schröder, H.-G. Grothues, F. Souvannavong, and Emile Remetean

Subjects
Asteroiden und Kometen, Brightness, 010504 meteorology & atmospheric sciences, Comet, FOS: Physical sciences, Image processing, Surface finish, 01 natural sciences, Photometry, Photometry (optics), Optics, 0103 physical sciences, Comets, 010303 astronomy & astrophysics, Image resolution, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Pixel, business.industry, Stray light, nucleus, Leitungsbereich PF, Astronomy and Astrophysics, Planetengeologie, Comet 67P/Churyumov-Gerasimenko, Space and Planetary Science, Planetare Sensorsysteme, business, Geology, Astrophysics - Earth and Planetary Astrophysics
Abstract

After coming to rest on the night side of comet 67P/Churyumov-Gerasimenko, the ROLIS camera on-board Rosetta’s Philae lander acquired five images of the surface below the lander, four of which were with the aid of LED illumination of different colors. The images confirm that Philae was perched on a sloped surface. A local horizon is visible in one corner of the image, beyond which we can see the coma. Having spent a full day on the surface Philae was commanded to lift and rotate, after which a final, sixth, LED image was acquired. The change in perspective allowed us to construct a shape model of the surface. The distance to the foreground was about 80 cm, much larger than the nominal 30 cm. This caused stray light, rather than directly reflected LED light, to dominate the image signal, complicating the analysis. The images show a lumpy surface with a roughness of apparently fractal nature. Its appearance is completely different from that of the first landing site, which was characterized by centimeter to meter-sized debris (Mottola et al., 2015). We recognize neither particles nor pores at the image resolution of 0.8 mm per pixel and large color variations are absent. The surface has a bi-modal brightness distribution that can be interpreted in terms of the degree of consolidation, a hypothesis that we support with experimental evidence. We propose the surface below the lander to consist of smooth, cracked plates with unconsolidated edges, similar to terrain seen in CIVA images.

Published
2017
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7. Magnetic Properties of Asteroid (162173) Ryugu

Author

Christian Krause, Frank Scholten, Jürgen Blum, Carsten Güttler, D. Constantinescu, Andreas Hördt, Kaname Sasaki, Karl-Heinz Glassmeier, Benjamin P. Weiss, Hans-Ulrich Auster, Laurence Lorda, Uwe Motschmann, Masaki Fujimoto, Tra-Mi Ho, J. T. Grundmann, Ayako Matsuoka, Olaf Hillenmaier, Kathrin Gebauer, Ekkehard Kührt, Aurelie Moussi-Soffys, Karl-Heinz Fornacon, David Hercik, Ingo Richter, B. Stoll, and Friederike Wolff

Subjects
Asteroiden und Kometen, asteroids, asteroid, MASCOT, Planetengeodäsie, Astronomy, Systementwicklung und Projektbüro, magnetic field, magnetization, Magnetic field, Magnetization, Geophysics, Space and Planetary Science, Geochemistry and Petrology, Asteroid, Hayabusa2 mission, Earth and Planetary Sciences (miscellaneous), Planetare Sensorsysteme, Ryugu, magnetic properties, Mechanik und Thermalsysteme, Institut für Optische Sensorsysteme, Geology, Hayabusa2
Abstract

Observations of the magnetization state of asteroids indicate diverse properties. Values between 1.9 × 10 −6 Am 2/kg (Eros) and 10 −2 Am 2/kg (Braille) have been reported. A more detailed understanding of asteroidal magnetic properties allows far-reaching conclusions of the magnetization mechanism as well as the strength of the magnetic field of the solar system regions the asteroid formed in. The Hayabusa2 mission with its lander Mobile Asteroid Surface Scout is equipped with a magnetometer experiment, MasMag. MasMag is a state-of-the-art three-axis fluxgate magnetometer, successfully operated also on Philae, the Rosetta mission lander. MasMag has enabled, after Eros for the second time ever, to determine the magnetic field of an asteroid during descent and on-surface operations. The new observations show that Ryugu, a low-albedo C-type asteroid, has no detectable global magnetization, and any local magnetization is either small (

Published
2020

8. Design, Kalibrierung und Betrieb der HP3 Wärmeflusssonde für die InSight Mars Mission

Author

Grott, Matthias, Spohn, Tilman, Knollenberg, Jörg, Müller, Nils, and Krause, Christian

Subjects
Asteroiden und Kometen, Wärmefluss, Planetenphysik, Institut für Planetenforschung, HP3, Mars, Nutzerzentrum für Weltraumexperimente (MUSC), InSight
Abstract

Die InSight Mission der NASA ist am 26. November 2018 in der Elysium Region des Mars gelandet und hat dort das erste geophysikalische Observatorium auf dem roten Planeten in Betrieb genommen. Die wissenschaftliche Nutzlast beinhaltet das sogenannte Heat Flow and Physical Properties Package (HP3), eine Wäremeflusssonde, die Temperatursensoren bis in eine Tiefe von 5 m in den Marsboden einbringen soll. Dort sollen dann der Temperaturgradient sowie die Wärmeleitfähigkeit im Marsboden gemessen werden, um daraus den oberflächennahen planetaren Wärmefluss abzuleiten. Darüber hinaus beinhaltet HP3 ein Radiometer, das die Oberflächentemperatur an der Landestelle überwacht. HP3 wurde am Deutschen Zentrum für Luft- und Raumfahrt entwickelt und wird in Zusammenarbeit mit dem Jet Propulsion Laboratory der NASA betrieben.

Published
2020

9. Near-perihelion activity of comet 67P/Churyumov-Gerasimenko. A first attempt of non-static analysis

Author

Yuri V. Skorov, Stefano Mottola, Paul Hartogh, and Horst Uwe Keller

Subjects
Area fraction, Physics, 67P/Churyumov-Gerasimenko, Asteroiden und Kometen, 010504 meteorology & atmospheric sciences, Planetengeodäsie, food and beverages, Astronomy and Astrophysics, Mechanics, Penetration (firestop), Sunset, Static analysis, Heat wave, 01 natural sciences, Space and Planetary Science, 0103 physical sciences, Thermal, numerical methods, Polar, Sublimation (phase transition), comets, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

The observed rate of water production of comet 67P/Churyumov–Gerasimenko near its perihelion can be approximated by a very steep power function of the heliocentric distance. Widely used thermophysical models based on a static dust layer on top of the icy/refractory matrix are poorly consistent with these observations. We analyse published model results and demonstrate that thermophysical models with a uniform and static ice free layer do not reproduce the observed steep water production rates of 67P near perihelion. Based on transient thermal modeling we conclude that the accelerated gas activity can be explained assuming that the active area fraction near the south pole is increased. The deeper penetration of the heat wave during polar day (no sunset) can activate sublimation through thicker inert dust layers. This can also lead to removal of thicker dust layers and consequently to an expansion of the active area.

Published
2020
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10. Asymmetric Craters on the Dwarf Planet Ceres—Results of Second Extended Mission Data Analysis

Author

Krohn, Katrin, Jaumann, Ralf, Wickhusen, Kai, Otto, Katharina A., Kersten, Elke, Stephan, Katrin, Wagner, Roland, Raymond, Carol A., and Russell, Christopher T.

Subjects
Asteroiden und Kometen, asteroids, subsurface ice, dwarf planets, asymmetrical cratering, Planetengeodäsie, Dawn, cratering processes, Planetengeologie, XM2, influence of slopes, Ceres, crater formation, asymmetric craters, crater formation on small bodies
Abstract

After almost three years of successful operation on Ceres, the Dawn spacecraft entered its last orbits around the dwarf planet and obtained a set of high-resolution images of 3 to 5 m/pixel. These images reveal a variety of morphologic features, including a set of asymmetric crater morphologies as observed earlier in the mission on the asteroid Vesta. We identified 269 craters, which are located between 60&deg, N to 60&deg, S latitude and 197&deg, E to 265&deg, E longitude, and investigated their morphological characteristics using a digital terrain model (DTM). These craters range in diameter from 0.30 to 4.2 km, and exhibit a sharp crater rim on the uphill side and a smooth one on the downhill side. We found that all asymmetric craters are formed on a sloping surface with the majority appearing at slope angles between 5 and 20 degrees. This implies that, as observed on Vesta, the topography is the main cause for these asymmetries.

Published
2019
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11. Pinnacles on the surface of the comet 67P/Churyumov-Gerasimenko: regional distribution and morphology

Author

Alexander T. Basilevsky, Urs Mall, Horst Uwe Keller, Stubbe F. Hviid, Yuri V. Skorov, and S. S. Krasilnikov

Subjects
Physics, Surface (mathematics), Asteroiden und Kometen, Morphology (linguistics), Distribution (number theory), Space and Planetary Science, Asteroid, Comet, Astronomy and Astrophysics, 67P/Churyumov-Gerasimenko Comets Rosetta, Astrobiology
Abstract

Pinnacles are local topographic promontories of different shapes considered to be formed due to uneven surface erosion. In the case of comets, areal changes in the degree of erosion could be related to inhomogeneities of the nucleus. However, the amount of solar radiation and the thermal gradient is different across the orbit for geomorphological regions, which can result in different erosion and shape for a similar composition among two differently illuminated areas. Therefore, a study of the areal distribution of pinnacles on the nucleus surface and their morphology may help to understand the structure and properties of the nucleus material. We mapped 166 pinnacles on the comet nucleus surface of 67P/Churyumov-Gerasimenko. About a third of them have planimetrically rounded shape (rounded pinnacles) and the rest are planimetrically elongated (local ridges). In the southern hemisphere, number of both round pinnacles and local ridges is larger than in the northern hemisphere. This difference possibly indicates the higher effectiveness of the pinnacles’ formation in the southern hemisphere. At the same time the mean values of the measured parameters, including the height, show no statistically reliable difference between the north and south. We found that the maximum height of the pinnacles is about a hundred meters. Suggesting that they have been formed by sublimational erosion, this value allows estimating the minimum thickness of the eroded material and thus the degree of the evolutionary changes of the nucleus. In our future study, we will model pinnacles formation based on the here presented analysis of observations.

Published
2019
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12. Revisiting the Analysis of the MARA Measurements on Ryugu’s Surface with a Multi-Scale Shape Model

Author

Hamm, Maximilian, Grott, Matthias, DeWiljes, J., Knollenberg, Jörg, Scholten, Frank, Matz, K-D, Preusker, Frank, Biele, Jens, Elgner, Stephan, Ogawa, Kazunori, Sakatani, N., Senshu, H., Okada, Junpei, Jaumann, R., Sugita, S., and Tanaka, S.

Subjects
Planetengeologie, Asteroiden und Kometen, Planetenphysik, Institut für Planetenforschung, Planetengeodäsie, MASCOT MARA Hayabusa2 Asteroids Ryugu Thermal Modeling Regolith, Nutzerzentrum für Weltraumexperimente (MUSC)
Abstract

The measurents of the MASCOT Radiometer MARA are revisited and a detailed thermal model of the MASCOT environment is presented.

Published
2019

13. Analysis of night-side dust activity on comet 67P observed by VIRTIS-M: a new method to constrain the thermal inertia on the surface

Author

Rinaldi, G., Formisano, M., Kappel, D., Capaccioni, F., Bockelée-Morvan, D., Cheng, Y.-C., Vincent, J.-B., Deshapriya, P., Arnold, G., Capria, M., Ciarniello, M., D’Aversa, E., D'aversa, E, De Sanctis, M., Doose, L., Erard, S., Federico, C., Filacchione, G., Fink, U., Leyrat, C., Longobardo, A., Magni, G., Migliorini, A., Mottola, S., Naletto, G., Raponi, A., Taylor, F., Tosi, F., Tozzi, G., Salatti, M., IASI (IASI), Consiglio Nazionale delle Ricerche (CNR), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), 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), Institute of Astronomy [Taiwan] (IANCU), National Central University [Taiwan] (NCU), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique et Mécanique Textiles (LPMT), ENSITM-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Matériaux et nanosciences d'Alsace (FMNGE), Institut de Chimie du CNRS (INC)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), IASF-Roma - Istituto di Astrofisica Spaziale e Fisica cosmica - Roma, Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Instituto de Estudos Avançados (IEAV), Institut, DLR Institute of Planetary Research, German Aerospace Center (DLR), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Universita degli Studi di Padova, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto di Fisica dello Spazio Interplanetario (IFSI), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-ENSITM-Matériaux et Nanosciences Grand-Est (MNGE), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Padova = University of Padua (Unipd), and Bockelée-Morvan, Dominique

Subjects
Asteroiden und Kometen, 67P/Churyumov-Gerasimenko -infrared, 010504 meteorology & atmospheric sciences, Comet, Imaging spectrometer, Coma (optics), Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, general -comets, Mantle (geology), [SDU] Sciences of the Universe [physics], comet, 0103 physical sciences, Thermal, comets, individual, infrared: planetary systems, 010303 astronomy & astrophysics, planetary systems, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], Jet (fluid), Range (particle radiation), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], comets: general, Leitungsbereich PF, comets: individual: 67P/Churyumov-Gerasimenko, Astronomy and Astrophysics, Plume, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

On 2015 July 18, near perihelion at a heliocentric distance of 1.28 au, the Visible InfraRed Thermal Imaging Spectrometer (VIRTIS-M) on board the Rosetta spacecraft had the opportunity of observing dust activity in the inner coma with a view of the night side (shadowed side) of comet 67P/Churyumov-Gerasimenko. At the time of the measurements we present here, we observe a dust plume that originates on the far side of the nucleus. We are able to identify the approximate location of its source at the boundary between the Hapi and Anuket regions, and we find that it has been in darkness for some hours before the observation. Assuming that this time span is equal to the conductive time scale, we obtain a thermal inertia in the range 25–36 W K−1 m−2 s−1/2. These thermal inertia values can be used to verify with a 3D finite-element method (FEM) numerical code whether the surface and subsurface temperatures agree with the values found in the literature. We explored three different configurations: (1) a layer of water ice mixed with dust beneath a dust mantle of 5 mm with thermal inertia of 36 J m−2 K−1 s−0.5; (2) the same structure, but with thermal inertia of 100 J m−2 K−1 s−0.5; (3) an ice-dust mixture that is directly exposed. Of these three configurations, the first seems to be the most reasonable, both for the low thermal inertia and for the agreement with the surface and subsurface temperatures that have been found for the comet 67P/Churyumov-Gerasimenko. The spectral properties of the plume show that the visible dust color ranged from 16 ± 4.8%/100 nm to 13 ± 2.6%/100 nm, indicating that this plume has no detectable color gradient. The morphology of the plume can be classified as a narrow jet that has an estimated total ejected mass of between 6 and 19 tons when we assume size distribution indices between −2.5 and −3.

Published
2019
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14. Geometric preprocessing for Rosetta/VIRTIS-M measurements of comet 67P/C-G

Author

Kappel, David, Arnold, Gabriele, Moroz, Liubov, Raponi, A., Ciarniello, M., Tosi, F., Erard, S., Leyrat, C., Blecka, M., Filacchione, G., and Capaccioni, F.

Subjects
Asteroiden und Kometen, Leitungsbereich PF, Rosetta, Comet 67P, Geometry, VIRTIS
Abstract

Following earlier surface spectrophotometric analyses of Rosetta/VIRTIS-M measurements of comet 67P/Churyumov-Gerasimenko (hereafter 67P), we refine the instrument's geometric registration model and spatial consistency of the radiometric calibration. For this purpose we compare measured 67P nucleus images from the entire mission to corresponding photometric simulations and determine an optical distortion map between them. The refinements will allow us to improve the retrieval of physical and compositional surface properties of the comet's nucleus.

Published
2019

15. Dust composition in the innermost coma of comet 67P from the VIRTIS-M spectra: Organic features detection

Author

Rinaldi, G., D'Aversa, E., Bockelee-Morvan, D., Raponi, A, Capaccioni, F., Ciarniello, M., Filacchione, G., De Sanctis, M. C., Oliva, F., Kappel, David, Longobardo, A, Tosi, F., Capria, M., and Taylor, F.

Subjects
Asteroiden und Kometen, Rosetta, Comet 67P, Dust, VIRTIS
Abstract

The Rosetta/ESA spacecraft followed the comet 67P/Churyumov-Gerasimenko from 2014 August (3.6 au pre-perihelion) to 2016 September (3.6 au post-perihelion). This offered a unique opportunity to analyze the time evolution of the dust properties in the inner coma. Onboard Rosetta, the Visual Infrared and Thermal Imaging Spectrometer (VIRTIS-M) acquired spectra of the dust coma in the spectral range 0.25 to 5 μm.

Published
2019

16. The HP³ Radiometer on InSight

Author

Mueller, N., Grott, M., Piqueux, S., Spohn, T., Smrekar, S.E., Knollenberg, J., Hudson, T.L., Spiga, A., Forget, F., Millour, E., Lemmon, M.T., Maki, J., Golombek, M., and Banerdt, W.B.

Subjects
Asteroiden und Kometen, Planetenphysik, Leitungsbereich PF, Astrophysics::Solar and Stellar Astrophysics, Mars, Messung, Astrophysics::Earth and Planetary Astrophysics, Oberflächentemperatur, Astrophysics::Galaxy Astrophysics, Physics::Atmospheric and Oceanic Physics, Physics::Geophysics
Abstract

The Heat Flow and Physical Properties Package (HP³) includes an infrared Radiometer attached to the deck of the InSight lander. The radiometer will observe the seasonal temperature variation over the course of the mission. Fitting of diurnal temperature curves and of the response to eclipses provides an estimate of thermophysical properties of the near surface, and possibly constrains atmospheric variables such as the ratio of visible to infrared dust opacity.

Published
2019

17. Bouncing boulders on comet 67P

Author

Vincent, Jean-Baptiste, Birch, S., Hayes, A., Zacny, K., Oklay, N., and Cambianica, P.

Subjects
Asteroiden und Kometen, boulders, 67P, comets
Published
2019

18. The HP3 Radiometer on InSight

Author

Müller, Nils, Grott, Matthias, Piqueux, S., Spohn, Tilman, Smrekar, S., Knollenberg, Jörg, Hudson, T.L., Spiga, Aymeric, Forget, F., Millour, Ehouarn, Lemmon, M. T., Maki, J., Golombek, M., and Banerdt, W.B.

Subjects
Asteroiden und Kometen, Planetenphysik, Institutsplanung / Zentrale Aufgaben PF, Mars, Messung, Oberflächentemperatur
Abstract

Introduction: The Heat Flow and Physical Properties Package (HP³) includes an infrared Radiometer attached to the deck of the InSight lander. The main objective of this part of the instrument is to con-strain the surface thermal boundary condition for the heat flow derivation by the instrumented tether de-ployed into the subsurface. The heat flow in the subsurface can be affected by seasonal and diurnal temperature variations, by radiation from the lander, its shadow, and the change in surface albedo caused by dust removal during landing and later deposition. The radiometer will observe the seasonal variation over the course of the mission. Fitting of diurnal temperature curves provides an estimate of albedo and other thermophysical properties of the near surface.

Published
2019

19. Ryugu's Parent-Body Processes Estimated from Hayabusa2 Multi-Band Optical Observations

Author

Sugita, S., Honda, R., Morota, T., Kameda, S., Sawada, H., Tatsumi, E., Honda, C., Yokota, Y., Yamada, M., Kouyama, T., Sakatani, N., Suzuki, H., Yoshioka, K., Hayakawa, M., Cho, Y., Matsuoka, M., Hirata, N., Domingue, D. L., Miyamoto, H., Kikuchi, H., Hemmi, R., Michikami, T., Barnouin, O.S., Ernst, C. M., Palmer, E., Gaskell, R., Michel, P., Hirabayashi, M., Jaumann, R, Otto, K., Schroeder, S., Hiroi, T., Nakamura, T., Komatsu, G., Yoshikawa, M., Tanaka, S., Shirai, K., Watanabe, S, Tsuda, Y., Schmitz, N., and Ogawa, K.

Subjects
Planetengeologie, Asteroiden und Kometen, surface boulders, Ryugu, meteorites, Hayabusa2
Published
2019

20. Multidisciplinary analysis of the Hapi region located on Comet 67P/Churyumov–Gerasimenko

Author

Wing-Huen Ip, Philippe Lamy, Carsten Güttler, F. La Forgia, Nilda Oklay, R. Rodrigo, Z. Y. Lin, Dennis Bodewits, Stefano Debei, V. Da Deppo, H. U. Keller, Luca Penasa, Jakob Deller, Maurizio Pajola, Alice Lucchetti, Gabriele Cremonese, Giampiero Naletto, Sonia Fornasier, Detlef Koschny, Marco Fulle, P. J. Gutierrez, M. De Cecco, Holger Sierks, J. J. Lopez Moreno, Francesco Marzari, J.-C. Lee, Matteo Massironi, F. Preusker, Ivano Bertini, Stubbe F. Hviid, Sabrina Ferrari, Imre Tóth, Jessica Agarwal, Pamela Cambianica, Xian Shi, Frank Scholten, Lorenza Giacomini, Jean-Loup Bertaux, M. A. Barucci, Stefano Mottola, Luisa Lara, Björn Davidsson, M. R. El Maarry, Clement Feller, Cecilia Tubiana, Monica Lazzarin, Jean-Baptiste Vincent, INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Department of Atmospheric Sciences [Taoyuan City], National Central University [Taiwan] (NCU), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Universita degli Studi di Padova, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Dipartimento di Geoscienze [Padova], Dipartimento di Fisica e Astronomia 'Galileo Galilei', CNR Istituto di Fotonica e Nanotecnologie [Padova] (IFN), Consiglio Nazionale delle Ricerche [Roma] (CNR), Institute of Space Science [Taiwan], Space Science Institute [Macau] (SSI), Macau University of Science and Technology (MUST), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centro de Astrobiologia [Madrid] (CAB), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), International Space Science Institute [Bern] (ISSI), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Department of Physics [Auburn], Auburn University (AU), Department of Mechanical Engineering [Padova], Department of Industrial Engineering [Padova], Universita degli Studi di Padova-Universita degli Studi di Padova, University of Trento [Trento], Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], INAF - Osservatorio Astronomico di Trieste (OAT), Institut d'Astronomie et d'Astrophysique [Bruxelles] (IAA), Université Libre de Bruxelles [Bruxelles] (ULB), Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), European Space Agency, Swedish National Space Board, Ministerio de Educación y Ciencia (España), Centre National D'Etudes Spatiales (France), Agenzia Spaziale Italiana, German Centre for Air and Space Travel, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Pajola, M. [0000-0002-3144-1277], Penasa, L. [0000-0002-6394-3108], Fornasier, S. [0000-0001-7678-3310], Lucchetti, A. [0000-0001-7413-3058], Vicent, J. B. [0000-0001-6575-3079], Naletto, G. [0000-0003-2007-3138], Barucci, M. A. [0000-0002-1345-0890], Bertaux, J. L. [0000-0003-0333-229X], Deller, J. [0000-0001-8341-007X], Fulle, M. [0000-0001-8435-5287], Güttler, C. [0000-0003-4277-1738], Tubiana, C. [0000-0001-8475-9898], Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH)-NASA, PLANETO - LATMOS, Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Université libre de Bruxelles (ULB), Agenzia Spaziale Italiana (ASI), Swedish National Space Agency (SNSA), Deutsches Zentrum für Luft- und Raumfahrt (DLR), and Centre National D'Etudes Spatiales (CNES)

Subjects
Asteroiden und Kometen, statistical [Methods], Comet, individual (67P C-G) [Comets], Comets: individual (67P C-G), Methods: data analysis, Methods: statistical, 01 natural sciences, Methods statistical, Gravitational potential, 0103 physical sciences, data analysis [Methods], 010303 astronomy & astrophysics, Southern Hemisphere, Physics, geography, geography.geographical_feature_category, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Multidisciplinary analysis, Planetengeodäsie, 67P/Churyumov–Gerasimenko Comets Rosetta Hapi, Northern Hemisphere, Astronomy, Astronomy and Astrophysics, methods: data analysis –methods: statistical – comets: individual (67P C-G), Space and Planetary Science, Ridge, individual: 67P C-G [Comets], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

By using the Rosetta/OSIRIS-NAC data set taken in 2014 August, we focus on the neck region, called Hapi, located on 67P Churyumov-Gerasimenko's Northern hemisphere. The gravitational potential and slopes of Hapi, coupled with the geological unit identification and the boulder size-frequency distributions, support the interpretation that both taluses and gravitational accumulation deposits observable on Hapi are the result of multiple cliff collapses that occurred at different times. By contrast, the fine-particle deposits observable in the central part of the study area are made of aggregates coming from the Southern hemisphere and deposited during each perihelion passage. Both the consolidated terrains on the western part of Hapi, as well as the centrally aligned ridge made of boulder-like features, suggest that Hapi is in structural continuity with the onion-like structure of the main lobe of 67P. Despite the dusty blanket observable on Hapi, its terrains are characterized by water-ice-rich components that, once repeatedly and rapidly illuminated, sublimate, hence resulting in the strong jet activity observed in 2014 August.© 2019 The Author(s)., The support of the national funding agencies of Germany (DLR), Italy (ASI), France (CNES), Spain (MEC), Sweden (SNSB), and the ESA Technical Directorate is gratefully acknowledged.

Published
2019
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21. Local Manifestations of Cometary Activity

Author

Ekkehard Kührt, Raphael Marschall, N. Oklay, Tony L. Farnham, Mohamed Ramy El-Maarry, Horst Uwe Keller, Jean-Baptiste Vincent, and Yuri V. Skorov

Subjects
Asteroiden und Kometen, Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010504 meteorology & atmospheric sciences, Comet, FOS: Physical sciences, Gas release, Astronomy and Astrophysics, 01 natural sciences, Activity, Astrobiology, Planetary science, 13. Climate action, Space and Planetary Science, Rosetta, 0103 physical sciences, Comets, 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract

Comets are made of volatile and refractory material and naturally experience various degrees of sublimation as they orbit around the Sun. This gas release, accompanied by dust, represents what is traditionally described as activity. Although the basic principles are well established, most details remain elusive, especially regarding the mechanisms by which dust is detached from the surface and subsequently accelerated by the gas flows surrounding the nucleus. During its 2 years rendez-vous with comet 67P/Churyumov-Gerasimenko, ESA's Rosetta has observed cometary activity with unprecedented details, in both the inbound and outbound legs of the comet's orbit. This trove of data provides a solid ground on which new models of activity can be built. In this chapter, we review how activity manifests at close distance from the surface, establish a nomenclature for the different types of observed features, discuss how activity is at the same time transforming and being shaped by the topography, and finally address several potential mechanisms., This paper is a review chapter in the upcoming book "Comets: Post 67P Perspectives" edited by ISSI and Space Science Reviews. Accepted on 08 April 2019

Published
2019
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22. Effects of dust layers on thermal Emission from airless bodies

Author

Biele, Jens, Kuehrt, Ekkehard, Senshu, Hiroki, Sakatani, Naoya, Ogawa, Kazunori, Hamm, Maximilian, Grott, Matthias, Okada, Tatsuaki, and Arai, Takehiko

Subjects
Asteroiden und Kometen, lcsh:QE1-996.5, lcsh:Geography. Anthropology. Recreation, Small bodies, Nutzerzentrum für Weltraumexperimente (MUSC), lcsh:Geology, Surfaces, Dust cover, lcsh:G, Planetenphysik, Thermophysical models, Solar System, Thermal inertia, Layering
Abstract

We have investigated the influence of thin thermally opaque dust layers on the thermal emission of rocks and regolith and determined the thermal response of these dust-covered surfaces to diurnal insolation cycles. Results are computed for Hayabusa2’s target asteroid (162173) Ryugu, which was observed by thermal infrared instruments on the orbiter and in situ. We show that even a very thin (10..100 μm) fine-grained porous dust layer with thermal inertia of 25 J m−2 K−1 s−1/2 can have a significant influence on surface temperatures and alter the apparent thermal inertia of the underlying material derived under the simplified assumption of a homogenous half space by more than 20%. The masking of the underlying material is complete at about 1 diurnal skin depth, corresponding to ~ 10 mm on Ryugu. Between 0.1 and 1 diurnal skin depths, we find a thermal lag smaller than what would be predicted for a surface consisting of dust only. If a dust cover were present on Ryugu, this should be clearly visible in the data returned by the orbiter’s thermal infrared imager (TIR) and the MASCOT lander’s radiometer (MARA), which observed a single boulder at the landing site. However, this appears not to be the case, and dust seems to play a minor role in the thermal emission from the asteroid.

Published
2019

23. Surface physical properties from HP³ radiometer measurements on the Mars mission InSight

Author

Mueller, N., Grott, M., Piqueux, S., Kopp, E., Spohn, T., Smrekar, S.E., Knollenberg, J., Hudson, T.L., Krause, C., Siegler, M., Spiga, A., Morgan, P., Golombek, M., and Banerdt, W.B.

Subjects
Asteroiden und Kometen, Weltrauminstrumente, Institut für Planetenforschung, Leitungsbereich PF, Mars, Messung, Oberflächentemperatur, Nutzerzentrum für Weltraumexperimente (MUSC)
Published
2019

24. The geomorphology, color, and thermal properties of Ryugu: Implications for parent-body processes

Author

Axel Hagermann, Yuri Shimaki, Makoto Yoshikawa, Masateru Ishiguro, Osamu Mori, Takehiko Arai, Masahiro Hayakawa, Takahiro Hiroi, Robert Gaskell, Manabu Yamada, Kei Shirai, N. Takaki, Takanao Saiki, Moe Matsuoka, Yuto Takei, Hirotaka Sawada, Naru Hirata, Fuyuto Terui, Yoshiaki Ishihara, Yoshiyuki Tsuda, Seiichi Tazawa, Hiroaki Kamiyoshihara, Ryodo Hemmi, Deborah L. Domingue, Rina Noguchi, Shinsuke Abe, Nicole Schmitz, Masanao Abe, Ralf Jaumann, Satoru Nakazawa, L. Le Corre, Kazuyoshi Asari, Takanobu Shimada, Shogo Tachibana, Yusuke Oki, M. Ozaki, R. Yamada, Katharina A. Otto, Hiroshi Araki, Faith Vilas, S. Oshigami, Toshimichi Otsubo, Patrick Michel, C. Sugimoto, K. Ogawa, Hideaki Kikuchi, Sei-ichiro Watanabe, Hiroki Senshu, Florian Thuillet, Yutaka Suzuki, T. Fukuhara, Sunao Hasegawa, K. Yamamoto, Ronald-Louis Ballouz, Satoshi Tanaka, Naoya Sakatani, Hirohide Demura, Paul A. Abell, Yuya Mimasu, T. G. Müller, Yoshiko Ogawa, Hideaki Miyamoto, Goro Komatsu, Shota Kikuchi, Carolyn M. Ernst, Fumi Yoshida, Olivier S. Barnouin, Eric Palmer, Rie Honda, Tomoki Nakamura, Yasuhiro Yokota, Yuki Takao, Tomohiko Sekiguchi, Kosuke Yoshioka, Shingo Kameda, Satoshi Hosoda, Eri Tatsumi, Kenji Nagata, Hajime Yano, Takahiro Iwata, Stefan Schröder, Yukio Yamamoto, Makoto Taguchi, Tatsuhiro Michikami, Kent Yoshikawa, J. Kimura, H. Suzuki, Seiji Sugita, Noriyuki Namiki, Yuichiro Cho, Go Ono, C. Honda, Hikaru Yabuta, Tomokatsu Morota, Ryudo Tsukizaki, A. Higuchi, Masatoshi Hirabayashi, Masato Okada, T. Takahashi, M. Shizugami, Chikako Hirose, Kazutaka Nishiyama, Takahide Mizuno, Hirotomo Noda, M. A. Barucci, Sho Sasaki, Masaki Fujimoto, Atsushi Fujii, Seiitsu Tsuruta, Tatsuaki Okada, Stefania Soldini, H. Ikeda, Tomohiro Yamaguchi, Michael E. Zolensky, Toru Kouyama, Koji Matsumoto, Naoko Ogawa, Yuichi Iijima, Hiroshi Takeuchi, Institute of Ecology, Tallinn University-Tallinn University, Institute of Space and Astronautical Science (ISAS), Department of Physics, Tokyo, Waseda University, Institute for Research on Earth Evolution [Yokosuka] (IFREE), Japan Agency for Marine-Earth Science and Technology (JAMSTEC), Institute of Observational Research for Global Change, Department of Applied Physics, The University of Tokyo, University of Electro-Communications [Tokyo] (UEC), Seoul National University [Seoul] (SNU), Tsukuba Space Center (TKSC), Japan Aerospace Exploration Agency [Tokyo] (JAXA), National Institute of Polar Research [Tokyo] (NiPR), Brown University, Service d'hépato-gastro-entérologie [Hôpital Saint-Louis], Groupe Hospitalier Saint Louis - Lariboisière - Fernand Widal [Paris], Assistance publique - Hôpitaux de Paris (AP-HP) (APHP)-Assistance publique - Hôpitaux de Paris (AP-HP) (APHP), Max-Planck-Institut für Quantenoptik (MPQ), Max-Planck-Gesellschaft, College of Industrial Technology, Nihon University, The Open University [Milton Keynes] (OU), Hiroshima University, Electronic Navigation Research Institute (ENRI), Ministry of Land, Infrastructure, Transport and Tourism, Dept Anim & Dairy Sci, University of Gerogia, National Institute of Agro-Environmental Sciences (NIAES), Mitsubishi Research Institute, Inc., Department of Natural History Sciences, Hokkaido University, Planetary Science Institute [Tucson] (PSI), Sol Agro et hydrosystème Spatialisation (SAS), Institut National de la Recherche Agronomique (INRA)-AGROCAMPUS OUEST, Max-Planck-Institut für Sonnensystemforschung (MPS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), 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), GEOMA, Université de Vigo, Universidate de Vigo, Plasma Research Center, University of Tsukuba, IHP Microelctronics, Advanced Materials Institute and Department of Chemistry, Fukuoka University, Department of Applied Mathematics and Physics, Graduate school of Mathematics, Kyoto-Kyoyo University, Department of Environmental and Materials Engineering, Nagoya Institute, Graduate School of Science and Engineering, Tokyo Metropolitan University [Tokyo], Institute of Environmental Systems (SUIKO), Kyushu University [Fukuoka], Graduate School of Science and Technology, Keio University, Rikkyo University [Tokyo], Dept. of Electronics Engineering, University of Electro-Communication, Institute for Sustainable Humanosphere (RISH), Kyoto University [Kyoto], Graduate School of Pharmaceutical Sciences, Tohoku, Tohoku University [Sendai], SolarTerrestrial Environment Laboratory, Nagoya University, Department of Geology and Geophysics, Ministry of Land, Infrastructure, Transport and Tourism (MLIT), Hokkaido University [Sapporo, Japan], DLR Institute of Planetary Research, German Aerospace Center (DLR), 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), Universidade de Vigo, Department of Advanced Technology and Development, BML, Matoba, Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Department of Physics, University of California [Irvine] (UCI), University of California-University of California, Biomécanique et génie biomédical (BIM), Centre National de la Recherche Scientifique (CNRS), University of Alaska [Fairbanks] (UAF), Information Science Laboratory, Department of Electronics and Electrical Engineering, Faculty of Science and Technology, Keio University, Department of Earth and Planetary Sciences [Kobe], Kobe University, ANR: 15-IDEX-0001,UCA JEDI,Idex UCA JEDI(2015), The University of Tokyo (UTokyo), 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), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and ANR-15-IDEX-0001,UCA JEDI,Idex UCA JEDI(2015)

Subjects
Asteroiden und Kometen, Physics, Multidisciplinary, 010504 meteorology & atmospheric sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Stereochemistry, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], 01 natural sciences, Article, Planetengeologie, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Ryugu, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

著者人数: 120名(所属. 宇宙航空研究開発機構宇宙科学研究所 (JAXA)(ISAS): 澤田, 弘崇; 横田, 康弘; 坂谷, 尚哉; 岡田, 達明; 田中, 智; 飯島, 祐一; 早川, 雅彦; 松岡, 萌; R.-L. Ballouz; 嶌生, 有理; 水野, 貴秀; 石原, 吉明; 長谷川, 直; 藤本, 正樹; 吉川, 真; 山本, 幸生; 白井, 慶; R. Noguchi; 尾川, 順子; 照井, 冬人; 菊地, 翔太; 山口, 智宏; 竹内, 央, 三桝, 裕也; 高橋, 忠輝; 竹井, 洋; 藤井, 淳; 中澤, 暁; 細田, 聡史; 森, 治; 嶋田, 貴信; Soldini, Stefania; 岩田, 隆浩; 安部, 正真; 矢野, 創; 月崎, 竜童; 尾崎, 正伸; 西山, 和孝; 佐伯, 孝尚; 渡邊, 誠一郎; 津田, 雄一), Accepted: 2019-03-12, 資料番号: SA1180387000

Published
2019
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25. Solar Sails for Planetary Defense & High-Energy Missions

Author

Waldemar Bauer, Tobias Mikschl, Kai Borchers, Siebo Reershemius, Michael Ruffer, Dominik Quantius, Sergio Montenegro, Federico Cordero, Friederike Wolff, David Hercik, Simon Tardivel, Norbert Toth, Christian Ziach, Ralf Boden, Tom Spröwitz, Maciej Sznajder, Matteo Ceriotti, Christian Grimm, Johannes Riemann, Etienne Dumont, Jens Biele, Nicole Schmitz, Patric Seefeldt, Ivanka Pelivan, Jan-Gerd Mess, Kaname Sasaki, Rico Jahnke, Elisabet Wejmo, Tra-Mi Ho, Alexander Koncz, Aaron Koch, Thomas Renger, Colin R. McInnes, Bernd Dachwald, Jan Thimo Grundmann, Peter Spietz, Eugen Mikulz, Christian Krause, Volker Maiwald, Alessandro Peloni, Roy Lichtenheldt, Wolfgang Seboldt, and Caroline Lange

Subjects
Asteroiden und Kometen, 010504 meteorology & atmospheric sciences, Computer science, Systemanalyse Raumtransport, Space weather, multiple NEA rendezvous, 01 natural sciences, MASCOT2, law.invention, Jupiter, Orbiter, law, 0103 physical sciences, Aerospace engineering, solar sail, 010303 astronomy & astrophysics, planetary defense, 0105 earth and related environmental sciences, Gossamer-1, Raumfahrt-Systemdynamik, Spacecraft, Payload, business.industry, MASCOT, Rendezvous, Systementwicklung und Projektbüro, Solar sail, Systemanalyse Raumsegment, Nutzerzentrum für Weltraumexperimente (MUSC), small spacecraft, Planetengeologie, Orbit, Asteroid, nanolander, Avioniksysteme, Polar, Land und Explorationstechnologie, Planetare Sensorsysteme, business, Mechanik und Thermalsysteme
Abstract

20 years after the successful ground deployment test of a (20 m)2 solar sail at DLR Cologne, and in the light of the upcoming U.S. NEAscout mission, we provide an overview of the progress made since in our mission and hardware design studies as well as the hardware built in the course of our solar sail technology development. We outline the most likely and most efficient routes to develop solar sails for useful missions in science and applications, based on our developed ‘now-term’ and near-term hardware as well as the many practical and managerial lessons learned from the DLR-ESTEC Gossamer Roadmap. Mission types directly applicable to planetary defense include single and Multiple NEA Rendezvous ((M)NR) for precursor, monitoring and follow-up scenarios as well as sail-propelled head-on retrograde kinetic impactors (RKI) for mitigation. Other mission types such as the Displaced L1 (DL1) space weather advance warning and monitoring or Solar Polar Orbiter (SPO) types demonstrate the capability of near-term solar sails to achieve asteroid rendezvous in any kind of orbit, from Earth-coorbital to extremely inclined and even retrograde orbits. Some of these mission types such as SPO, (M)NR and RKI include separable payloads. For one-way access to the asteroid surface, nanolanders like MASCOT are an ideal match for solar sails in micro-spacecraft format, i.e. in launch configurations compatible with ESPA and ASAP secondary payload platforms. Larger landers similar to the JAXA-DLR study of a Jupiter Trojan asteroid lander for the OKEANOS mission can shuttle from the sail to the asteroids visited and enable multiple NEA sample-return missions. The high impact velocities and re-try capability achieved by the RKI mission type on a final orbit identical to the target asteroid's but retrograde to its motion enables small spacecraft size impactors to carry sufficient kinetic energy for deflection.

Published
2019

26. HP³ Radiometer Measurements from the Mars Mission InSight

Author

Mueller, N., Grott, M., Piqueux, S., Kopp, Emanuel, Spohn, T., Smrekar, S.E., Knollenberg, J., Hudson, T.L., Krause, C., Plesa, A.-C., Siegler, M.A., Spiga, Aymeric, Forget, F., Millour, E., Morgan, P., Golombek, M., and Banerdt, W.B.

Subjects
Asteroiden und Kometen, Weltrauminstrumente, Planetenphysik, Leitungsbereich PF, Mars, Messung, Oberflächentemperatur, Nutzerzentrum für Weltraumexperimente (MUSC)
Published
2019

28. Spatial Distribution an Morphology of Craters on Ryugu: Implications for Surface Processes on the C-Type Asteroid

Author

Cho, Y., Morota, T., Kanamaru, M., Ernst, C. M., Barnouin, Olivier S., Tatsumi, E., Hirabayashi, M., Otto, Katharina A., Schmitz, Nicole, Wagner, Roland, Jaumann, Ralf, Miyamoto, H., Kikuchi, H., Hemmi, R., Honda, R., Kameda, S., Yokota, Y., Kouyama, Toru, Suzuki, H., Yamada, M., Sakatani, N., Honda, C., Hayakawa, M., Yoshioka, K., Matsuoka, Moe, Michikami, T., Hirata, N., Sawada, H., and Sugita, Seiji

Subjects
Planetengeologie, Asteroiden und Kometen, Craters, asteroid, morphology, Ryugu, surface processes, Hayabusa2, ONC
Published
2019

29. In-Situ Determination of Thermal Inertia on Near Earth Asteroid (162173) Ryugu using MARA - The MASCOT Radiometer

Author

Grott, Matthias, Knollenberg, Jörg, Hamm, Maximilian, Ogawa, Kazunori, Jaumann, R., Otto, Katharina A., Matz, K-D, Schmitz, Nicole, Koncz, Alexander, Trauthan, Frank, Senshu, Hiroki, Sakatani, N., Tanaka, Satoshi, Arai, T., Mottola, Stefano, Pelivan, Ivanka, Drube, Line, Vincent, Jean-Baptiste, Delbo, M, Michel, P., Yano, H., Pilorget, C., Schlotterer, Markus, Krause, Christian, Ho, Tra-Mi, and Moussi-Soffys, A.

Subjects
Asteroiden und Kometen, Planetenphysik, Thermische Trägheit, Land und Explorationstechnologie, Ryugu, Systementwicklung und Projektbüro, Navigations- und Regelungssysteme
Published
2019

30. The Heat Flow and Physical Properties Package HP3 on InSight - First Results

Author

Spohn, Tilman, Grott, Matthias, Smrekar, S., Knollenberg, Jörg, Hudson, T.L., Krause, Christian, Müller, Nils, Wippermann, Torben, Krömer, Olaf, Lichtenheldt, Roy, Wiśniewski, Lukasz, Grygorczuk, J., Reershemius, Siebo, Spröwitz, Tom, Scharringhausen, Marco, Kopp, Emanuel, Morgan, P., Plesa, Ana-Catalina, Breuer, Doris, and Hagermann, A.

Subjects
Asteroiden und Kometen, Raumfahrt-Systemdynamik, Weltrauminstrumente, Planetenphysik, HP3, Mars, Land und Explorationstechnologie, Heat Flow, InSight, Nutzerzentrum für Weltraumexperimente (MUSC)
Published
2019

31. The Evolution of Ryugu's Parent Body Constrained by Hayabusa2 Imaging Observations

Author

Sugita, S., Honda, R., Kameda, S., Honda, C., Yokota, Y., Yamada, M., Kouyama, T., Sakatani, N., Suzuki, H., Yoshioka, K., Cho, Y., Matsuoka, M., Ogawa, K., Domingue, D.L., Miyamoto, H., Barnouin, O.S., Michel, P., Ernst, C. M., Hiroi, T., Nakamura, T., Sawada, H., Hayakawa, M., Hirata, N., Kikuchi, H., Hemmi, R., Michikami, T., Palmer, E., Gaskell, R., Hirabayashi, M., Jaumann, R, Otto, K., Schmitz, N., Schröder, S.E., Komatsu, G., Tanaka, S., Shirai, K., Yoshikawa, M., Watanabe, S, and Tsuda, Y.

Subjects
Planetengeologie, Asteroiden und Kometen, Ryugu, Hayabusa2
Published
2019

32. Thermal Evolution Modeling of (162173) Ryugu and its precursors

Author

Neumann, Wladimir, Grott, Matthias, Hamm, Maximilian, Biele, Jens, Jaumann, R, Otto, Katharina A., and Kührt, Ekkehard

Subjects
Planetengeologie, Asteroiden und Kometen, Planetenphysik, Evolution, Ryugu, Nutzerzentrum für Weltraumexperimente (MUSC), Asteroiden, Hayabusa2
Published
2019

33. Generation of photoclinometric DTMs for application to transient changes on the surface of comet 67P/Churyumov-Gerasimenko

Author

J.-B. Vincent, R. L. Kirk, Y. Tang, S. P. D. Birch, S. Squyres, N. W. Kutsop, and A. G. Hayes

Subjects
Physics, Asteroiden und Kometen, 010504 meteorology & atmospheric sciences, Comets: individual: 67P/Churyumov-Gerasimenko – Methods: data analysis – Techniques: image processing, Comet, Astronomy, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Space and Planetary Science, 0103 physical sciences, Transient (oscillation), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

Context. The wide spatial and temporal coverage of 67P/Churyumov-Gerasimenko (67P) by the Rosetta mission has revealed a surface created by scattered large-scale changes and numerous small-scale changes. The many small-scale changes are of particular interest because they are unexpected and ubiquitous. As their topographic relief is often smaller than one meter, which is below the resolution of any shape models, we need higher resolution topography to analyze them properly. Aims. We describe a photoclinometry method that is able to retrieve surface elevations for a single OSIRIS image of the surface of 67P. With this method, we can provide accurate measures, along with error estimates, of the centimeter-scale topography of observed transient changes. Methods. Photoclinometry, or shape-from-shading, estimates heights by examining the light reflection of the surface as dictated by a photometric model under a specified set of viewing geometries. Assuming a standard photometric model for 67P, we can recreate the shading of a surface under specified viewing geometries. The output is a high-resolution height map that matches the original image pixel by pixel. We then provide estimates of the error in the retrieved heights and ensure that our method is valid with a series of checks. Results. We generate digital terrain models (DTMs) with a vertical resolution comparable to or smaller than the pixel scale. This allows us to accurately measure changes in the surface topography on centimeter scales. We find that most changes within the smooth terrains involve the transport or removal of material thinner than one meter.

Published
2019

34. The Camera of the MASCOT Asteroid Lander on Board Hayabusa 2

Author

Jaumann, R., Schmitz, N., Koncz, A., Michaelis, H., Schroeder, S. E., Mottola, S., Trauthan, F., Hoffmann, H., Roatsch, T., Jobs, D., Kachlicki, J., Pforte, B., Terzer, R., Tschentscher, M., Weisse, S., Mueller, U., Perez-Prieto, L., Broll, B., Kruselburger, A., Ho, T.-M., Biele, J., Ulamec, S., Krause, C., Grott, M., Bibring, J.-P., Watanabe, Seiichiro, Sugita, Seiji, Okada, Tatsuaki, Yoshikawa, Makoto, and Yabuta, Hikaru

Subjects
Hayabusa 2, Asteroiden und Kometen, Asteroid Lander, In-situ science, 010504 meteorology & atmospheric sciences, Institut für Planetenforschung, Context (language use), 01 natural sciences, law.invention, Orbiter, Optics, Planetenphysik, Sample return mission, law, 0103 physical sciences, Depth of field, Asteroid (162173) Ryugu, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing, Radiometer, Spectrometer, business.industry, Systementwicklung und Projektbüro, Astronomy and Astrophysics, Planetary Data System, Nutzerzentrum für Weltraumexperimente (MUSC), Planetengeologie, Space and Planetary Science, Asteroid, Planetare Sensorsysteme, Camera, Mascot, business, Geology
Abstract

著者人数: 30名, Accepted: 2016-06-02, 資料番号: SA1160334000

Published
2016
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35. Small Scale Surface Roughness of Ryugu

Author

Otto, Katharina A., Parekh, Rutu, Matz, K-D, Jaumann, R, Krohn, Katrin, Stephan, Katrin, Schmitz, Nicole, Ho, Tra-Mi, Elgner, Stephan, Hamm, Maximilian, Honda, Rie, Kameda, Shingo, Preusker, Frank, Scholten, Frank, Schröder, Stefan, Senshu, Hiroki, Sugita, Seiji, and Trauthan, Frank

Subjects
Planetengeologie, Asteroiden und Kometen, Planetenphysik, Planetengeodäsie, Surface Structure, Systementwicklung und Projektbüro, Asteroid Ryugu, Roughness, Regolith
Published
2019

37. Studying the boulder morphology on comet 67P using discrete element simulations

Author

Sachse, Manuel, Kappel, David, Haack, David, and Otto, Katharina A.

Subjects
Asteroiden und Kometen, boulders, discrete element simulations, 67P, cliffs
Abstract

Our overall aim is to investigate the physics of volatile-related surface features on asteroids and comets. In the present work, we focus on studying the morphology of boulders and cliff collapses on comet 67P/Churyumov-Gerasimenko’s surface (Fig. 1). This study continues and complements previous work, where we have been investigating dynamical processes that are implied by surface features on comet 67P [1] and on asteroid Vesta[2].

Published
2019

38. Imaging Inclusion Spectral Diversity in Carbonaceous Chondrites with MASCam

Author

Schröder, Stefan, Otto, Katharina A., Schmitz, Nicole, Scharf, Hannah, Greshake, Ansgar, Scholten, Frank, Trauthan, Frank, and Jaumann, Ralf

Subjects
Planetengeologie, Asteroiden und Kometen, MasCam, Inclusions, Planetengeodäsie, Asteroid Ryugu, Laboratory experiment, Carbonaceous Chondrites, Regolith, meteorites
Published
2019

40. A comparison of multiple Rosetta data sets and 3D model calculations of 67P/Churyumov-Gerasimenko coma around equinox (May 2015)

Author

F. Preusker, Ladislav Rezac, Laurent Jorda, Martin Rubin, P. Theologou, Jong-Shinn Wu, O. Pinzón-Rodríguez, Kathrin Altwegg, Clémence Herny, David Marshall, S. K. Dadzie, Nicolas Thomas, Selina-Barbara Gerig, Stefano Mottola, David Kappel, C. C. Su, Ekkehard Kührt, Chariton Christou, Gabriele Arnold, Y. Liao, Raphael Marschall, Paul Hartogh, Rafael Rodrigo, Frank Scholten, Olivier Groussin, O. Mousis, Laboratoire d'Astrophysique de Marseille (LAM), and 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)

Subjects
67P/Churyumov-Gerasimenko, Asteroiden und Kometen, 010504 meteorology & atmospheric sciences, 530 Physics, Comet, 3d model, Equinox, Astrophysics, 01 natural sciences, 0103 physical sciences, Rosetta, Comets, Coma, DSMC, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Spacecraft, biology, business.industry, 520 Astronomy, Leitungsbereich PF, Planetengeodäsie, Comet 67P, Astronomy and Astrophysics, Dust, biology.organism_classification, 620 Engineering, Dynamics, Outgassing, Comets 67P/Churyumov-Gerasimenko Coma Dust Dynamics, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Outflow, Bulk velocity, Osiris, business
Abstract

International audience; We have used the latest available shape model for gas and dust simulations of the inner coma of comet 67P/Churyumov-Gerasimenko for the period around May 2015 (equinox). We compare results from a purely insolation-driven model with a complementary set of observations made by ROSINA, VIRTIS, MIRO, and OSIRIS within the same period. The observations include - for the first time - inverted MIRO measurements of gas density, temperature and bulk velocity to constrain the model. The comparisons show that, as in November 2014 (Marschall et al., 2016), insolation-driven activity does not provide an adequate fit to the data. Both VIRTIS and MIRO observations indicate that emissions from the Hatmehit and Imhotep regions of the nucleus are strongly depleted in total gas, H2O, and dust emissions in this case. The MIRO inversion provides a challenging constraint to the models as a consequence of the terminator orbit and nucleus pointing of the spacecraft. Nonetheless a consistent picture with a dominance of outgassing from the Hapi region, even at equinox, is clearly evident. An inhomogeneous model consistent with models proposed for the November 2014 time-frame was constructed and provides a better fit to the data. As far as we are aware this is the first time comae data from four Rosetta instruments have been used to constrain within one self-contained model the emission distribution at the nucleus surface and study the dynamics of the gas and dust outflow.

Published
2019
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42. Experimental simulation of cometary surfaces using volatile-rich analogue materials

Author

Haack, David, Otto, Katharina A., Kührt, E., Gundlach, Bastian, Kreuzig, Christopher, and Blum, Jürgen

Subjects
Asteroiden und Kometen, sublimation, cometary surfaces
Abstract

Cometary surfaces are shaped through the process of activity when the comet approaches the sun and the sublimation of volatiles removes dust and gases. Recently, the ESA Rosetta mission showed the geomorphologic diversity of comet 67P/Churyumov-Gerasimenko in great detail (Fig. 1), giving us the opportunity to investigate the sublimation processes on small Solar System bodies by means of geomorphologic analyses of the surface . In order to understand how these processes alter the surface appearance, we investigate the morphologic evolution of sublimating cometary surfaces in the laboratory of the IGEP department at TU Braunschweig. The focus lies on the evolution of different morphologies that were found on comet 67P/Churyumov-Gerasimenko, such as fractur es and debris deposits [1,2]. We consider the composition and initial geometry of the samples and variable insolation flux. Different sample compositions and geometries are prepared to model the interaction of volatile-dust mixtures with vacuum conditions. The results will not only provide information on the material properties and parameters (e.g. cohesion, tensile strength) of comets, but will also enable us to Analyse the morphologic evolution of cometary surfaces.

Published
2019

43. The backscattering ratio of comet 67P/Churyumov-Gerasimenko dust coma as seen by OSIRIS onboard Rosetta

Author

Pamela Cambianica, F. La Forgia, Jean-Loup Bertaux, P. J. Gutierrez, Alice Lucchetti, E. Frattin, Alessandra Rotundi, Detlef Koschny, Pedro Hasselmann, Xian Shi, Wing-Huen Ip, Giovanna Rinaldi, Philippe Lamy, Carsten Güttler, Giampiero Naletto, Stefano Mottola, Monica Lazzarin, Marco Fulle, J. J. Lopez Moreno, Sabrina Ferrari, Nafiseh Masoumzadeh, M. A. Barucci, H. U. Keller, D. Guirado, Imre Toth, V. Petropoulou, Gábor L. Kovács, Holger Sierks, Gabriele Cremonese, M. De Cecco, Cesare Barbieri, L. M. Lara, Björn Davidsson, Jakob Deller, Dennis Bodewits, S. Ivanovsky, Francesca Ferri, Cecilia Tubiana, Luca Penasa, Jessica Agarwal, Stefano Debei, Ivano Bertini, Maurizio Pajola, Olga Muñoz, Francesco Marzari, S. Fornasier, Matteo Massironi, F. Moreno, R. Rodrigo, V. Da Deppo, German Centre for Air and Space Travel, Centre National D'Etudes Spatiales (France), Agenzia Spaziale Italiana, Ministerio de Educación y Ciencia (España), Swedish National Space Agency, European Space Agency, Dipartimento di Fisica e Astronomia 'Galileo Galilei', Universita degli Studi di Padova, INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Dipartimento di Scienze e Tecnologie [Napoli] (DIST), Universita degli studi di Napoli 'Parthenope' [Napoli], INAF - Osservatorio Astronomico di Padova (OAPD), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Department of Physics [Auburn], Auburn University (AU), Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), 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), CNR Istituto di Fotonica e Nanotecnologie [Padova] (IFN), Consiglio Nazionale delle Ricerche [Roma] (CNR), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), International Space Science Institute [Bern] (ISSI), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), CNR Institute for Photonics and Nanotechnologies (IFN), Department of Industrial Engineering [Padova], University of Trento [Trento], Institute of Astronomy [Taiwan] (IANCU), National Central University [Taiwan] (NCU), Space Science Institute [Macau] (SSI), Macau University of Science and Technology (MUST), Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Dipartimento di Geoscienze [Padova], Fulle, M. [0000-0001-8435-5287], Tubiana, C. [0000-0001-8475-9898], Güttler, C. [0000-0003-4277-1738], Pajola, M. [0000-0002-3144-1277], Rinaldi, G. [0000-0002-2968-0455], Naletto, G. [0000-0003-2007-3138], Barucci, M. A. [0000-0002-1345-0890], Bertaux, J. L. [0000-0003-0333-229X], Deller, J. [0000-0001-8341-007X], Fornasier, S. [0000-0001-7678-3310], Penasa, L. [0000-0002-6394-3108], Consejo Superior de Investigaciones Científicas [Spain] (CSIC), 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), IMPEC - LATMOS, Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), NASA-California Institute of Technology (CALTECH), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Technische Universität Braunschweig [Braunschweig], Università degli Studi di Padova = University of Padua (Unipd), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Università degli Studi di Napoli 'Parthenope' = University of Naples (PARTHENOPE), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Agence Spatiale Européenne = European Space Agency (ESA), and Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737

Subjects
67P/Churyumov-Gerasimenko, Asteroiden und Kometen, 010504 meteorology & atmospheric sciences, photometry, Comet, data analysis, scattering –methods: data analysis – techniques: image processing – techniques: photometric – comets: individual: 67P/Churyumov-Gerasimenko, techniques: image processing, Astrophysics, 01 natural sciences, Photometry (optics), Scattering, techniques: photometric, individual: 67P/Churyumov-Gerasimenko [Comets], 0103 physical sciences, Churyumov–Gerasimenko, image processing [Techniques], data analysis [Methods], 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, biology, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], scattering, methods: data analysis, techniques: image processing, techniques: photometric, comets: individual: 67P/Churyumov-Gerasimenko, Phase angle, scattering, photometric [Techniques], comets: individual: 67P/Churyumov-Gerasimenko, Astronomy and Astrophysics, biology.organism_classification, methods: data analysis, image processing, 13. Climate action, Space and Planetary Science, Drag, Temporal resolution, Inverse scattering problem, Osiris, individual: 67P [Comets], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Remote sensing observations of dust particles ejected from comets provide important hints on the intimate nature of the materials composing these primitive objects. The measurement of dust coma backscattering ratio, BSR, defined as the ratio of the reflectance at phase angle 0 ◦ and 30 ◦ , helps tuning theoretical models aimed at solving the inverse scattering problem deriving information on the nature of the ejected particles. The Rosetta/OSIRIS camera sampled the coma phase function of comet 67P, with four series acquired at low phase angles from 2015 January to 2016 May. We also added previously published data to our analysis to increase the temporal resolution of our findings. We measured a BSR in the range ∼ [1.7-3.6], broader than the range found in literature from ground-based observations of other comets. We found that during the post-perihelion phase, the BSR is systematically larger than the classical cometary dust values only for nucleocentric distances smaller than ∼ 100 km. We explain this trend in terms of a cloud of chunks orbiting the nucleus at distances < 100 km ejected during perihelion and slowly collapsing on the nucleus over a few months because of the coma gas drag. This also implies that the threshold particle size for the dust phase function to become similar to the nucleus phase function is between 2.5 mm and 0.1 m, taking into account previous Rosetta findings. © 2018 The Author(s)., The support of the national funding agencies of Germany (DLR: Deutschen Zentrums fur Luft-und Raumfahrt), France (CNES: Centre national d' etudes spatiales), Italy (ASI: Agenzia Spaziale Italiana), Spain (MEC: Ministry of Education& Science), Sweden (SNSB: Swedish National Space Board), and the European Space Agency (ESA) Technical Directorate is gratefully acknowledged.

Published
2019
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44. Diurnal variation of dust and gas production in comet 67P/Churyumov-Gerasimenko at the inbound equinox as seen by OSIRIS and VIRTIS-M on board Rosetta

Author

D. Bodewits, Lyn R. Doose, Giovanna Rinaldi, U. Fink, M. De Cecco, Ivano Bertini, Marco Fulle, Maria Teresa Capria, Anny Chantal Levasseur-Regourd, D. Bockelée-Morvan, Imre Toth, Luisa Lara, Sonia Fornasier, H. Krueger, Mauro Ciarniello, Vladimir E. Zakharov, Holger Sierks, Alessandra Migliorini, Gabriele Arnold, Andrea Longobardo, Carsten Güttler, X. Hu, Michelangelo Formisano, Francesco Marzari, Xian Shi, Wing-Huen Ip, Philippe Lamy, F. La Forgia, Stefano Mottola, Gabriele Cremonese, Detlef Koschny, Zhong-Yi Lin, David Kappel, Raphael Marschall, Fredric W. Taylor, V. Da Deppo, S. Ivanovski, J. J. López-Moreno, Fabrizio Capaccioni, Gianrico Filacchione, H. U. Keller, Stéphane Erard, M. C. De Sanctis, Jean-Loup Bertaux, J. Deller, Pedro J. Gutiérrez, Stefano Debei, R. Rodrigo, Jacques Crovisier, Giampiero Naletto, Björn Davidsson, Cecilia Tubiana, M. A. Barucci, Colin Snodgrass, Monica Lazzarin, Ludmilla Kolokolova, Agenzia Spaziale Italiana, German Research Foundation, Centre National de la Recherche Scientifique (France), Ministerio de Economía y Competitividad (España), Government of Sweden, European Space Agency, l'Observatoire de Paris, Science and Technology Facilities Council (UK), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Institut für Geodäsie und Geoinformationstechnik, Technische Universität Berlin (TU), International Space Science Institute [Bern] (ISSI), INAF - Osservatorio Astronomico di Trieste (OAT), Dipartimento di Fisica e Astronomia 'Galileo Galilei', Universita degli Studi di Padova, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Department of Physics [Auburn], Auburn University (AU), INAF - Osservatorio Astronomico di Padova (OAPD), CNR Institute for Photonics and Nanotechnologies (IFN), Consiglio Nazionale delle Ricerche [Roma] (CNR), Department of Industrial Engineering [Padova], University of Trento [Trento], Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institute of Astronomy [Taiwan] (IANCU), National Central University [Taiwan] (NCU), Space Science Institute [Macau] (SSI), Macau University of Science and Technology (MUST), Institut für Physik und Astrophysik [Potsdam], Universität Potsdam, Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA)-European Space Agency (ESA), Universita degli studi di Napoli 'Parthenope' [Napoli], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Physics [Oxford], University of Oxford [Oxford], Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), Technische Universität Berlin (TUB), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), IMPEC - LATMOS, Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), NASA-California Institute of Technology (CALTECH), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Technische Universität Braunschweig [Braunschweig], and Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)

Subjects
Asteroiden und Kometen, 67P/Churyumov-Gerasimenko, Brightness, 010504 meteorology & atmospheric sciences, Comet, Comets, Data analysis, General, Individual, Methods, FOS: Physical sciences, Coma (optics), Spatial distribution, Atmospheric sciences, 01 natural sciences, 7. Clean energy, Methods: data analysis, individual: 67P/Churyumov-Gerasimenko [Comets], 0103 physical sciences, data analysis [methods], ddc:530, 010303 astronomy & astrophysics, Southern Hemisphere, Comet: individual: 67P/Churyumov-Gerasimenko, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Diurnal temperature variation, Leitungsbereich PF, comets: individual: 67P/Churyumov-Gerasimenko, Institut für Physik und Astronomie, general [Comets], Astronomy and Astrophysics, Comets: general, 13. Climate action, Space and Planetary Science, astro-ph.EP, Environmental science, Spatial variability, Longitude, Astrophysics - Earth and Planetary Astrophysics
Abstract

Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Open Access funding provided by Max Planck Society., On 27 April 2015, when comet 67P/Churyumov-Gerasimenko was at 1.76 au from the Sun and moving toward perihelion, the OSIRIS and VIRTIS-M instruments on board the Rosetta spacecraft simultaneously observed the evolving dust and gas coma during a complete rotation of the comet.© C. Tubiana et al. 2019, OSIRIS was built by a consortium led by the Max-Planck-Institut fur Sonnensystemforschung, Gottingen, Germany, in collaboration with CISAS, University of Padova, Italy, the Laboratoire d'Astrophysique de Marseille, France, the Instituto de Astrofisica de Andalucia, CSIC, Granada, Spain, the Scientific Support Office of the European Space Agency, Noordwijk, The Netherlands, the Instituto Nacional de Tecnica Aeroespacial, Madrid, Spain, the Universidad Politechnica de Madrid, Spain, the Department of Physics and Astronomy of Uppsala University, Sweden, and the Institut fur Daten-technik und Kommunikationsnetze der Technischen Universitat Braunschweig, Germany. The support of the national funding agencies of Germany (DLR), France (CNES), Italy (ASI), Spain (MEC), Sweden (SNSB), and the ESA Technical Directorate is gratefully acknowledged. We thank the Rosetta Science Ground Segment at ESAC, the Rosetta Mission Operations Centre at ESOC and the Rosetta Project at ESTEC for their outstanding work enabling the science return of the Rosetta Mission. VIRTIS was built by a consortium, which includes Italy, France, and Germany, under the scientific responsibility of the Istituto di Astrofisica e Planetologia Spaziali of INAF, Italy, which also guides the scientific operations. The VIRTIS instrument development, led by the prime contractor Leonardo-Finmeccanica (Florence, Italy), has been funded and managed by ASI, with contributions from Observatoire de Meudon financed by CNES, and from DLR. We thank the Rosetta Science Ground Segment and the Rosetta Mission Operations Centre for their support throughout all the phases of the mission. The VIRTIS calibrated data will be available through the ESA's Planetary Science Archive Website (www.rssd.esa.int) and is available upon request until posted to the archive. We thank the following institutions and agencies for support of this work: Italian Space Agency (ASI, Italy) contract number I/024/12/1, Centre National d'Etudes Spatiales (CNES, France), DLR (Germany), NASA (USA) Rosetta Program, and Science and Technology Facilities Council (UK).

Published
2019
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45. Rosetta/OSIRIS observations of the 67P nucleus during the April 2016 flyby: High-resolution spectrophotometry

Author

H. U. Keller, Alice Lucchetti, M. De Cecco, Giampiero Naletto, D. Bodewits, Monica Lazzarin, Francesco Marzari, R. Rodrigo, P. J. Gutiérrez, Maurizio Pajola, Sonia Fornasier, J. D. P. Deshapriya, Stefano Debei, F. La Forgia, A. Barucci, J. J. López-Moreno, V. Da Deppo, Frank Preusker, Wing-Huen Ip, Philippe Lamy, Matteo Massironi, C. Feller, Holger Sierks, Pedro Hasselmann, Gabriele Cremonese, Björn Davidsson, Cecilia Tubiana, Luisa Lara, B. Gaskell, Carsten Güttler, Frank Scholten, Ivano Bertini, Marco Fulle, Sabrina Ferrari, Xian Shi, Stefano Mottola, Jean-Loup Bertaux, Detlef Koschny, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Universita degli Studi di Padova, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Dipartimento di Fisica e Astronomia 'Galileo Galilei', CNR Istituto di Fotonica e Nanotecnologie [Padova] (IFN), Consiglio Nazionale delle Ricerche [Roma] (CNR), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), International Space Science Institute [Bern] (ISSI), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA)-European Space Agency (ESA), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Department of Physics [Auburn], Auburn University (AU), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), CNR Institute for Photonics and Nanotechnologies (IFN), Department of Industrial Engineering [Padova], University of Trento [Trento], INAF - Osservatorio Astronomico di Trieste (OAT), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institute of Astronomy [Taiwan] (IANCU), National Central University [Taiwan] (NCU), Space Science Institute [Macau] (SSI), Macau University of Science and Technology (MUST), Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Planetary Science Institute [Tucson] (PSI), Feller, C. [0000-0002-2941-3875], Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, German Centre for Air and Space Travel, Centre National D'Etudes Spatiales (France), Agenzia Spaziale Italiana, Agencia Estatal de Investigación (España), European Space Agency, Swedish National Space Agency, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), IMPEC - LATMOS, Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), NASA-California Institute of Technology (CALTECH), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), and Technische Universität Braunschweig [Braunschweig]

Subjects
Asteroiden und Kometen, 67P/Churyumov-Gerasimenko, 010504 meteorology & atmospheric sciences, techniques: image processing, Astrophysics, 01 natural sciences, individual: 67P/Churyumov-Gerasimenko [Comets], Frost line, Spectrophotometry, Spectral slope, Methods, Churyumov–Gerasimenko, image processing [Techniques], space vehicles: instruments, data analysis [Methods], 010303 astronomy & astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Comets: individual: 67P/Churyumov-Gerasimenko, Physics, [PHYS]Physics [physics], biology, medicine.diagnostic_test, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Resolution (electron density), Comets, Data analysis, Image processing, Individual, Instruments, Space vehicles, Techniques, individual: 67P [Comets], Comet, FOS: Physical sciences, Terrain, Context (language use), instruments [Space vehicles], 0103 physical sciences, medicine, 0105 earth and related environmental sciences, Planetengeodäsie, space vehicles – space vehicles: instruments – comets: individual: 67P/Churyumov–Gerasimenko – techniques: image processing – methods: data analysis, Astronomy and Astrophysics, biology.organism_classification, methods: data analysis, 13. Climate action, Space and Planetary Science, Osiris, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract

From August 2014 to September 2016, the Rosetta spacecraft followed comet 67P/Churyumov-Gerasimenko along its orbit. After the comet passed perihelion, Rosetta performed a flyby manoeuvre over the Imhotep-Khepry transition in April 2016. The OSIRIS/Narrow-Angle-Camera (NAC) acquired 112 observations with mainly three broadband filters (centered at 480, 649, and 743 nm) at a resolution of up to 0.53 m/px and for phase angles between 0.095 degrees and 62 degrees. Aims. We have investigated the morphological and spectrophotometrical properties of this area using the OSIRIS/NAC high-resolution observations. Methods. We assembled the observations into coregistered color cubes. Using a 3D shape model, we produced the illumination conditions and georeference for each observation. We mapped the observations of the transition to investigate its geomorphology. Observations were photometrically corrected using the Lommel-Seeliger disk law. Spectrophotometric analyses were performed on the coregistered color cubes. These data were used to estimate the local phase reddening. Results. The Imhotep-Khepry transition hosts numerous and varied types of terrains and features. We observe an association between a feature's nature, its reflectance, and its spectral slopes. Fine material deposits exhibit an average reflectance and spectral slope, while terrains with diamictons, consolidated material, degraded outcrops, or features such as somber boulders present a lower-than-average reflectance and higher-than-average spectral slope. Bright surfaces present here a spectral behavior consistent with terrains enriched in water-ice. We find a phase-reddening slope of 0.064 +/- 0.001%/100 nm/degrees at 2.7 au outbound, similar to the one obtained at 2.3 au inbound during the February 2015 flyby. Conclusions. Identified as the source region of multiple jets and a host of water-ice material, the Imhotep-Khepry transition appeared in April 2016, close to the frost line, to further harbor several potential locations with exposed water-ice material among its numerous different morphological terrain units.© ESO 2019, OSIRIS was built by a consortium of the Max-Planck-Institut fur Sonnensystemforschung, Gottingen, Germany, CISAS-University of Padova, Italy, Laboratoire d'Astrophysique de Marseille, France, Instituto de Astrofisica de Andalucia, CSIC, Granada, Spain, Research and Scientific Support Department of the European Space Agency, Noordwijk, The Netherlands, Instituto Nacional de Tecnica Aeroespacial, Madrid, Spain, Universidad Politechnica de Madrid, Spain, Department of Physics and Astronomy of Uppsala University, Sweden, and Institut fur Datentechnik und Kommunikationsnetze der Technischen Universitat Braunschweig, Germany. The support of the national funding agencies of Germany (DLR), France (CNES), Italy (ASI), Spain (MEC), Sweden (SNSB), and the ESA Technical Directorate is gratefully acknowledged. Rosetta is an ESA mission with contributions from its member states and NASA. Rosetta's Philae lander is provided by a consortium led by DLR, MPS, CNES, and ASI. The SPICE libraries and PDS resources are developed and maintained by NASA. The authors thank the referee and editors for their questions, remarks, and advices for the improvement of this article.

Published
2019
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46. Phase-curve analysis of comet 67P/Churyumov-Gerasimenko at small phase angles

Author

D. Bodewits, Marco Fulle, Monica Lazzarin, Jakob Deller, Giampiero Naletto, V. Da Deppo, Nafiseh Masoumzadeh, Stefano Debei, Mohamed Ramy El-Maarry, Detlef Koschny, Björn Davidsson, H. U. Keller, Cecilia Tubiana, J. J. Lopez-Moreno, Imre Toth, W-H. Ip, M. A. Barucci, Pedro Hasselmann, Gabriele Cremonese, Ludmilla Kolokolova, Sonia Fornasier, Colin Snodgrass, M. De Cecco, Pedro J. Gutiérrez, Xian Shi, Carsten Güttler, Ivano Bertini, Francesco Marzari, L. M. Lara, Stefano Mottola, Holger Sierks, R. Rodrigo, P. L. Lamy, J. L. Bertaux, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Department of Earth and Planetary Sciences [UCL/Birkbeck], Birkbeck College [University of London], DLR Institute of Planetary Research, German Aerospace Center (DLR), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Dipartimento di Fisica e Astronomia 'Galileo Galilei', Universita degli Studi di Padova, Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), CNR Istituto di Fotonica e Nanotecnologie [Padova] (IFN), Consiglio Nazionale delle Ricerche [Roma] (CNR), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centro de Astrobiologia [Madrid] (CAB), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), International Space Science Institute [Bern] (ISSI), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Auburn], Auburn University (AU), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), CNR Institute for Photonics and Nanotechnologies (IFN), Department of Industrial Engineering [Padova], University of Trento [Trento], INAF - Osservatorio Astronomico di Trieste (OAT), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Space Science Institute [Macau] (SSI), Macau University of Science and Technology (MUST), Institute of Astronomy [Taiwan] (IANCU), National Central University [Taiwan] (NCU), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig [Braunschweig], Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), PLANETO - LATMOS, Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), California Institute of Technology (CALTECH)-NASA, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), and Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig]

Subjects
Asteroiden und Kometen, Study phase, 010504 meteorology & atmospheric sciences, publications, bibliography, Comet, comets: general – comets: individual: 67P/Churyumov-Gerasimenko – techniques: photometric – techniques: image processing, Individual, Image processing, techniques: image processing, Coherent backscattering, Astrophysics, 7. Clean energy, 01 natural sciences, photometric [techniques], techniques: photometric, individual: 67P/Churyumov-Gerasimenko [Comets], 0103 physical sciences, Comets, publications, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], Comets: individual: 67P/Churyumov-Gerasimenko, image processing [techniques], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Phase angle, bibliography - techniques, general [Comets], bibliography, Astronomy and Astrophysics, Phase curve, 67P/Churyumov-Gerasimenko - publications, bibliography - techniques, General - comets, Photometric - techniques, Computational physics, Comets: general, Wavelength, Space and Planetary Science, Phase ratio, 67P/Churyumov-Gerasimenko - publications, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Open Access funding provided by Max Planck Society., The Rosetta-OSIRIS images acquired at small phase angles in three wavelengths during the fly-by of the spacecraft on 9-10 April 2016 provided a unique opportunity to study the opposition effect on the surface of comet 67P/Churyumov-Gerasimenko (67P). Our goal is to study phase curves of the nucleus at small phase angles for a variety of surface structures to show the differences in their opposition effect and to determine which surface properties cause the differences.© N. Masoumzadeh et al. 2019, OSIRIS was built by a consortium of the Max-Planck-Institut fur Sonnensystemforschung, Gottingen, Germany; the CISAS University of Padova, Italy; the Laboratoire d'Astrophysique de Marseille, France; the Instituto de Astrofisica de Andalucia, CSIC, Granada, Spain; the Research and Scientific Support Department of the ESA, Noordwijk, Netherlands; the Instituto Nacional de Tecnica Aeroespacial, Madrid, Spain; the Universidad Politechnica de Madrid, Spain; the Department of Physics and Astronomy of Uppsala University, Sweden; and the Institut fur Datentechnik und Kommunikationsnetze der Technischen Universitat Braunschweig, Germany. The support of the national funding agencies of Germany (DLR), France (CNES), Italy (ASI), Spain (MEC), Sweden (SNSB), and the ESA Technical Directorate is gratefully acknowledged. We thank the Rosetta Science Operations Centre and the Rosetta Mission Operations Centre for the successful rendezvous with comet 67P/Churyumov-Gerasimenko. This research has made use of the USGS Integrated Software for Imagers and Spectrometers (ISIS). We gratefully acknowledge the developers of SPICE and NAIF/PDS resources. This research has made use of the scientific software shapeViewer www.comet-toolbox.com.L.K.acknowledges a support from the NASA SSW grant 80NSSC17K0731.

Published
2019
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47. Thermal Evolution Modeling of Ryugu and its Precursors

Author

Neumann, Wladimir, Grott, Matthias, Hamm, Maximilian, Biele, Jens, Jaumann, R, and Kührt, Ekkehard

Subjects
Asteroiden und Kometen, Planetengeologie, Planetenphysik, Evolution, Ryugu, Asteroiden, Hayabusa2, Nutzerzentrum für Weltraumexperimente (MUSC)
Published
2019

49. Experimental simulation of geomorphological evolution of cometary surfaces using volatile-rich analog materials

Author

Haack, David, Otto, Katharina A., Kührt, Ekkehard, Gundlach, B., Kreuzig, Christopher, Blum, J., and Jaumann, R

Subjects
Asteroiden und Kometen, cometary morphology, experimental sublimation
Abstract

The morphologic development of sublimating cometary surfaces is investigated in our study using analog laboratory experiments on Earth. The focus lies on the evolution of different morphologies, taking into account parameters such as the composition of the sample material and variable insolation flux. Different sample compositions and geometries are prepared to model the interaction of volatile-dust mixtures with vacuum conditions. We aim to study the appearance of morphologic features, such as fractures and debris, developing by insolation and sublimation. Important questions to answer are: • Under which insolation and compositional conditions do cracks form in the sample material? • Under which insolation and compositional conditions do cliffs collapse and are larger debris particles formed? • Under given environmental conditions, how long do morphologic features remain on the surface? • How do sublimating volatiles support the process of dust transport? • What are the time scales of activity under given environmental conditions? Initial investigations were conducted using cometary analogue materials. These materials are mixtures of water-ice and silica-dust particles with a diameter of few microns and in different mixing ratios. The water-ice particles are produced by freezing mist with liquid nitrogen and the silica-dust consists of angular particles of comparable size. To determine the tensile strength of the different ice-dust mixtures a series of Brazilian Disc Tests was performed. In this test, small cylinders of sample material are exposed to pressure until fracturing. The derived tensile strength can be used to determine the cohesion of the ice-dust mixtures and allows the vapour pressure that is required to entrain particles by sublimating volatiles to be estimated. In our upcoming experiments, sample mixtures of variable particle sizes and water-ice/silica-dust ratios will be shaped into various morphologies, such as a cliff, pits or boulders and placed into a vacuum sublimation chamber. During insolation, the water-ice sublimates and the altering sample morphology will be observed and analysed with cameras. Additional monitored processes will be: • mass loss during different phases of varying insolation • lateral extent of mass movements • the evolution of the temperature inside the sample material.

Published
2019

50. Surface Thermophysical Properties of Near Earth Asteroid (162173) Ryugu from in-situ Observations: First Results from the MASCOT MARA Radiometer

Author

Grott, Matthias, Knollenberg, Jörg, Hamm, Maximilian, Ogawa, Kazunori, Jaumann, R, Otto, Katharina A., Matz, K-D, Schmitz, Nicole (Admin.), Funktional, Koncz, Alexander, Trauthan, Frank, Senshu, H., Okada, T., Kührt, Ekkehard, Biele, Jens, Neumann, Wladimir, Knapmeyer, Martin, Helbert, Jörn, Maturilli, Alessandro, Müller, Nils, and Hagermann, A.

Subjects
Asteroiden und Kometen, Planetengeologie, Planetenphysik, MASCOT, Ryugu, MARA, Nutzerzentrum für Weltraumexperimente (MUSC), Asteroiden
Published
2019

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