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201. Characterization of OSIRIS NAC filters for the interpretation of multispectral data of comet 67P/Churyumov-Gerasimenko

Author

Oklay, N., primary, Vincent, J.-B., additional, Sierks, H., additional, Besse, S., additional, Pajola, M., additional, Bertini, I., additional, Rickman, H., additional, La Forgia, F., additional, Barucci, A. M., additional, Fornasier, S., additional, Barbieri, C., additional, Koschny, D., additional, Lamy, P. L., additional, Rodrigo, R., additional, Agarwal, J., additional, A’Hearn, M. F., additional, Bertaux, J.-L., additional, Cremonese, G., additional, Da Deppo, V., additional, Davidsson, B., additional, Debei, S., additional, De Cecco, M., additional, Fulle, M., additional, Groussin, O., additional, Gutiérrez, P. J., additional, Güttler, C., additional, Hviid, S. F., additional, Ip, W.-H., additional, Jorda, L., additional, Keller, H. U., additional, Knollenberg, J., additional, Kramm, J.-R., additional, Kührt, E., additional, Küppers, M., additional, Lara, L. M., additional, Lazzarin, M., additional, Lopez-Moreno, J. J., additional, Marzari, F., additional, Michalik, H., additional, Naletto, G., additional, Thomas, N., additional, and Tubiana, C., additional

Published
2015
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202. Redistribution of particles across the nucleus of comet 67P/Churyumov-Gerasimenko

Author

Thomas, N., primary, Davidsson, B., additional, El-Maarry, M. R., additional, Fornasier, S., additional, Giacomini, L., additional, Gracia-Berná, A. G., additional, Hviid, S. F., additional, Ip, W.-H., additional, Jorda, L., additional, Keller, H. U., additional, Knollenberg, J., additional, Kührt, E., additional, La Forgia, F., additional, Lai, I. L., additional, Liao, Y., additional, Marschall, R., additional, Massironi, M., additional, Mottola, S., additional, Pajola, M., additional, Poch, O., additional, Pommerol, A., additional, Preusker, F., additional, Scholten, F., additional, Su, C. C., additional, Wu, J. S., additional, Vincent, J.-B., additional, Sierks, H., additional, Barbieri, C., additional, Lamy, P. L., additional, Rodrigo, R., additional, Koschny, D., additional, Rickman, H., additional, A’Hearn, M. F., additional, Barucci, M. A., additional, Bertaux, J.-L., additional, Bertini, I., additional, Cremonese, G., additional, Da Deppo, V., additional, Debei, S., additional, de Cecco, M., additional, Fulle, M., additional, Groussin, O., additional, Gutierrez, P. J., additional, Kramm, J.-R., additional, Küppers, M., additional, Lara, L. M., additional, Lazzarin, M., additional, Lopez Moreno, J. J., additional, Marzari, F., additional, Michalik, H., additional, Naletto, G., additional, Agarwal, J., additional, Güttler, C., additional, Oklay, N., additional, and Tubiana, C., additional

Published
2015
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203. Scientific assessment of the quality of OSIRIS images

Author

Tubiana, C., primary, Güttler, C., additional, Kovacs, G., additional, Bertini, I., additional, Bodewits, D., additional, Fornasier, S., additional, Lara, L., additional, La Forgia, F., additional, Magrin, S., additional, Pajola, M., additional, Sierks, H., additional, Barbieri, C., additional, Lamy, P. L., additional, Rodrigo, R., additional, Koschny, D., additional, Rickman, H., additional, Keller, H. U., additional, Agarwal, J., additional, A’Hearn, M. F., additional, Barucci, M. A., additional, Bertaux, J.-L., additional, Besse, S., additional, Boudreault, S., additional, Cremonese, G., additional, Da Deppo, V., additional, Davidsson, B., additional, Debei, S., additional, De Cecco, M., additional, El-Maarry, M. R., additional, Fulle, M., additional, Groussin, O., additional, Gutiérrez-Marques, P., additional, Gutiérrez, P. J., additional, Hoekzema, N., additional, Hofmann, M., additional, Hviid, S. F., additional, Ip, W.-H., additional, Jorda, L., additional, Knollenberg, J., additional, Kramm, J.-R., additional, Kührt, E., additional, Küppers, M., additional, Lazzarin, M., additional, Lopez Moreno, J. J., additional, Marzari, F., additional, Massironi, M., additional, Michalik, H., additional, Moissl, R., additional, Naletto, G., additional, Oklay, N., additional, Scholten, F., additional, Shi, X., additional, Thomas, N., additional, and Vincent, J.-B., additional

Published
2015
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204. Large-scale dust jets in the coma of 67P/Churyumov-Gerasimenko as seen by the OSIRIS instrument onboard Rosetta

Author

Lara, L. M., primary, Lowry, S., additional, Vincent, J.-B., additional, Gutiérrez, P. J., additional, Rożek, A., additional, La Forgia, F., additional, Oklay, N., additional, Sierks, H., additional, Barbieri, C., additional, Lamy, P. L., additional, Rodrigo, R., additional, Koschny, D., additional, Rickman, H., additional, Keller, H. U., additional, Agarwal, J., additional, Auger, A.-T., additional, A’Hearn, M. F., additional, Barucci, M. A., additional, Bertaux, J.-L., additional, Bertini, I., additional, Besse, S., additional, Bodewits, D., additional, Cremonese, G., additional, Davidsson, B., additional, Da Deppo, V., additional, Debei, S., additional, De Cecco, M., additional, El-Maarry, M. R., additional, Ferri, F., additional, Fornasier, S., additional, Fulle, M., additional, Groussin, O., additional, Gutiérrez–Marques, P., additional, Güttler, C., additional, Hviid, S. F., additional, Ip, W.-H., additional, Jorda, L., additional, Knollenberg, J., additional, Kovacs, G., additional, Kramm, J.-R., additional, Kührt, E., additional, Küppers, M., additional, Lazzarin, M., additional, Lin, Z.-Y., additional, López-Moreno, J. J., additional, Magrin, S., additional, Marzari, F., additional, Michalik, H., additional, Moissl–Fraund, R., additional, Moreno, F., additional, Mottola, S., additional, Naletto, G., additional, Pajola, M., additional, Pommerol, A., additional, Thomas, N., additional, Sabau, M. D., additional, and Tubiana, C., additional

Published
2015
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205. Search for satellites near comet 67P/Churyumov-Gerasimenko using Rosetta/OSIRIS images

Author

Bertini, I., primary, Gutiérrez, P. J., additional, Lara, L. M., additional, Marzari, F., additional, Moreno, F., additional, Pajola, M., additional, La Forgia, F., additional, Sierks, H., additional, Barbieri, C., additional, Lamy, P., additional, Rodrigo, R., additional, Koschny, D., additional, Rickman, H., additional, Keller, H. U., additional, Agarwal, J., additional, A’Hearn, M. F., additional, Barucci, M. A., additional, Bertaux, J.-L., additional, Cremonese, G., additional, Da Deppo, V., additional, Davidsson, B., additional, Debei, S., additional, De Cecco, M., additional, Ferri, F., additional, Fornasier, S., additional, Fulle, M., additional, Giacomini, L., additional, Groussin, O., additional, Güttler, C., additional, Hviid, S. F., additional, Ip, W.-H., additional, Jorda, L., additional, Knollenberg, J., additional, Kramm, J. R., additional, Kührt, E., additional, Küppers, M., additional, Lazzarin, M., additional, Lopez Moreno, J. J., additional, Magrin, S., additional, Massironi, M., additional, Michalik, H., additional, Mottola, S., additional, Naletto, G., additional, Oklay, N., additional, Thomas, N., additional, Tubiana, C., additional, and Vincent, J.-B., additional

Published
2015
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206. THERMAP: a mid-infrared spectro-imager for space missions to small bodies in the inner solar system

Author

Groussin, O., primary, Licandro, J., additional, Helbert, J., additional, Reynaud, J. L., additional, Levacher, P., additional, Reyes García-Talavera, M., additional, Alí-Lagoa, V., additional, Blanc, P. E., additional, Brageot, E., additional, Davidsson, B., additional, Delbó, M., additional, Deleuze, M., additional, Delsanti, A., additional, Diaz Garcia, J. J., additional, Dohlen, K., additional, Ferrand, D., additional, Green, S. F., additional, Jorda, L., additional, Joven Álvarez, E., additional, Knollenberg, J., additional, Kührt, E., additional, Lamy, P., additional, Lellouch, E., additional, Le Merrer, J., additional, Marty, B., additional, Mas, G., additional, Rossin, C., additional, Rozitis, B., additional, Sunshine, J., additional, Vernazza, P., additional, and Vives, S., additional

Published
2015
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207. The rotation state of 67P/Churyumov-Gerasimenko from approach observations with the OSIRIS cameras on Rosetta

Author

Mottola, S., Lowry, S., Snodgrass, C., Lamy, P.L., Toth, I., Rożek, A., Sierks, H., A'Hearn, M.F., Angrilli, F., Barbieri, C., Barucci, M.A., Bertaux, J.-L., Cremonese, G., Da Deppo, V., Davidsson, B., De Cecco, M., Debei, S., Fornasier, S., Fulle, M., Groussin, O., Gutiérrez, P., Hviid, S.F., Ip, W., Jorda, L., Keller, H.U., Knollenberg, J., Koschny, D., Kramm, R., Kührt, E., Küppers, M., Lara, L., Lazzarin, M., Lopez Moreno, J.J., Marzari, F., Michalik, H., Naletto, G., Rickman, H., Rodrigo, R., Sabau, L., Thomas, N., Wenzel, K.-P., Agarwal, J., Bertini, I., Ferri, F., Güttler, C., Magrin, S., Oklay, N., Tubiana, C., Vincent, J.-B., Mottola, S., Lowry, S., Snodgrass, C., Lamy, P.L., Toth, I., Rożek, A., Sierks, H., A'Hearn, M.F., Angrilli, F., Barbieri, C., Barucci, M.A., Bertaux, J.-L., Cremonese, G., Da Deppo, V., Davidsson, B., De Cecco, M., Debei, S., Fornasier, S., Fulle, M., Groussin, O., Gutiérrez, P., Hviid, S.F., Ip, W., Jorda, L., Keller, H.U., Knollenberg, J., Koschny, D., Kramm, R., Kührt, E., Küppers, M., Lara, L., Lazzarin, M., Lopez Moreno, J.J., Marzari, F., Michalik, H., Naletto, G., Rickman, H., Rodrigo, R., Sabau, L., Thomas, N., Wenzel, K.-P., Agarwal, J., Bertini, I., Ferri, F., Güttler, C., Magrin, S., Oklay, N., Tubiana, C., and Vincent, J.-B.

Abstract

Aims. Approach observations with the Optical, Spectroscopic, and Infrared Remote Imaging System (OSIRIS) experiment onboard Rosetta are used to determine the rotation period, the direction of the spin axis, and the state of rotation of comet 67P's nucleus. Methods. Photometric time series of 67P have been acquired by OSIRIS since the post wake-up commissioning of the payload in March 2014. Fourier analysis and convex shape inversion methods have been applied to the Rosetta data as well to the available ground-based observations. Results. Evidence is found that the rotation rate of 67P has significantly changed near the time of its 2009 perihelion passage, probably due to sublimation-induced torque. We find that the sidereal rotation periods P1 = 12.76129 ± 0.00005 h and P2 = 12.4043 ± 0.0007 h for the apparitions before and after the 2009 perihelion, respectively, provide the best fit to the observations. No signs of multiple periodicity are found in the light curves down to the noise level, which implies that the comet is presently in a simple rotation state around its axis of largest moment of inertia. We derive a prograde rotation model with spin vector J2000 ecliptic coordinates ? = 65° ± 15°, ? = + 59° ± 15°, corresponding to equatorial coordinates RA = 22°, Dec = + 76°. However, we find that the mirror solution, also prograde, at ? = 275° ± 15°, ? = + 50° ± 15° (or RA = 274°, Dec = + 27°), is also possible at the same confidence level, due to the intrinsic ambiguity of the photometric problem for observations performed close to the ecliptic plane. © 2014 ESO.

Published
2014

208. 67P/Churyumov-Gerasimenko: Activity between March and June 2014 as observed from Rosetta/OSIRIS

Author

Tubiana, C., primary, Snodgrass, C., additional, Bertini, I., additional, Mottola, S., additional, Vincent, J.-B., additional, Lara, L., additional, Fornasier, S., additional, Knollenberg, J., additional, Thomas, N., additional, Fulle, M., additional, Agarwal, J., additional, Bodewits, D., additional, Ferri, F., additional, Güttler, C., additional, Gutierrez, P. J., additional, La Forgia, F., additional, Lowry, S., additional, Magrin, S., additional, Oklay, N., additional, Pajola, M., additional, Rodrigo, R., additional, Sierks, H., additional, A’Hearn, M. F., additional, Angrilli, F., additional, Barbieri, C., additional, Barucci, M. A., additional, Bertaux, J.-L., additional, Cremonese, G., additional, Da Deppo, V., additional, Davidsson, B., additional, De Cecco, M., additional, Debei, S., additional, Groussin, O., additional, Hviid, S. F., additional, Ip, W., additional, Jorda, L., additional, Keller, H. U., additional, Koschny, D., additional, Kramm, R., additional, Kührt, E., additional, Küppers, M., additional, Lazzarin, M., additional, Lamy, P. L., additional, Lopez Moreno, J. J., additional, Marzari, F., additional, Michalik, H., additional, Naletto, G., additional, Rickman, H., additional, Sabau, L., additional, and Wenzel, K.-P., additional

Published
2014
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209. Triple F--a comet nucleus sample return mission

Author

Küppers, Michael, Keller, H. U., Kührt, E., A'Hearn, M. F., Altwegg, K., Bertrand, R., Busemann, H., Capria, M. T., Colangeli, L., Davidsson, B., Ehrenfreund, P., Knollenberg, J., Mottola, S., Rathke, A., Weiss, P., Zolensky, M., Akim, E., Basilevsky, A., Galimov, E., Gerasimov, M., Korablev, O., Lomakin, I., Marov, M., Martynov, M., Nazarov, M., Zakharov, A., Zelenyi, L., Aronica, A., Ball, A. J., Barbieri, C., Bar-Nun, A., Benkhoff, J., Biele, J., Biver, N., Blum, J., Bockelée-Morvan, D., Botta, O., Bredehöft, J. H., Capaccioni, F., Charnley, S., Cloutis, E., Cottin, H., Cremonese, G., Crovisier, J., Crowther, S. A., Epifani, E. M., Esposito, F., Ferrari, A. C., Ferri, F., Fulle, M., Gilmour, J., Goesmann, F., Gortsas, N., Green, S. F., Groussin, O., Grün, E., Gutiérrez, P. J., Hartogh, P., Henkel, T., Hilchenbach, M., Ho, T. M., Horneck, G., Hviid, S. F., Ip, W. H., Jäckel, A., Jessberger, E., Kallenbach, R., Kargl, G., Kömle, N. I., Korth, A., Kossacki, K., Krause, C., Krüger, H., Li, Z. Y., Licandro, J., Lopez-Moreno, J. J., Lowry, S. C., Lyon, I., Magni, G., Mall, U., Mann, I., Markiewicz, W., Martins, Z., Maurette, M., Meierhenrich, U., Mennella, V., Ng, T. C., Nittler, L. R., Palumbo, P., Pätzold, M., Prialnik, D., Rengel, M., Rickman, H., Rodriguez, J., Roll, R., Rost, D., Rotundi, A., Sandford, S., Schönbächler, M., Sierks, H., Srama, R., Stroud, R. M., Szutowicz, S., Tornow, C., Ulamec, S., Wallis, M., Waniak, W., Weissman, P., Wieler, R., Wurz, P., Yung, K. L., Zarnecki, J. C., Schonbachler, Maria, Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), 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), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Solar System, Cosmic Vision, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Comet, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], sample return, Sample return, space mission, 7. Clean energy, 01 natural sciences, Space mission, Astrobiology, Interplanetary dust cloud, Sample return mission, Comet nucleus, 0103 physical sciences, Comets, comets, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Spacecraft, business.industry, Astronomy, Astronomy and Astrophysics, Cosmogony, 13. Climate action, Space and Planetary Science, cosmogony, Formation and evolution of the Solar System, business
Abstract

The Triple F (Fresh From the Fridge) mission, a Comet Nucleus Sample Return, has been proposed to ESA's Cosmic Vision program. A sample return from a comet enables us to reach the ultimate goal of cometary research. Since comets are the least processed bodies in the solar system, the proposal goes far beyond cometary science topics (like the explanation of cometary activity) and delivers invaluable information about the formation of the solar system and the interstellar molecular cloud from which it formed. The proposed mission would extract three sample cores of the upper 50cm from three locations on a cometary nucleus and return them cooled to Earth for analysis in the laboratory. The simple mission concept with a touch-and-go sampling by a single spacecraft was proposed as an M-class mission in collaboration with the Russian space agency ROSCOSMOS. © The Author(s) 2008.

Published
2009

210. Motivation of young people for studying SET. The gender perspective

Author

Sagebiel, F., Dahmen, J., Davidsson, B., Godfroy-Genin, A.S., Rommes, E.W.M., Thaler, A., and Urbancíková, N.

Subjects
Dynamics of gender, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), Developing normativity in education
Abstract

Contains fulltext : 73538.pdf (Publisher’s version ) (Open Access)

Published
2008

212. Observations of the outer belt

Author

Lagerkvist, C-.I., Moroz, L., Karlsson, O., Nathues, A., Erikson, A., Lahulla, F., Dahlgren, M., and Davidsson, B.

Published
2004

213. The rotation state of 67P/Churyumov-Gerasimenko from approach observations with the OSIRIS cameras on Rosetta

Author

Mottola, S., primary, Lowry, S., additional, Snodgrass, C., additional, Lamy, P. L., additional, Toth, I., additional, Rożek, A., additional, Sierks, H., additional, A’Hearn, M. F., additional, Angrilli, F., additional, Barbieri, C., additional, Barucci, M. A., additional, Bertaux, J.-L., additional, Cremonese, G., additional, Da Deppo, V., additional, Davidsson, B., additional, De Cecco, M., additional, Debei, S., additional, Fornasier, S., additional, Fulle, M., additional, Groussin, O., additional, Gutiérrez, P., additional, Hviid, S. F., additional, Ip, W., additional, Jorda, L., additional, Keller, H. U., additional, Knollenberg, J., additional, Koschny, D., additional, Kramm, R., additional, Kührt, E., additional, Küppers, M., additional, Lara, L., additional, Lazzarin, M., additional, Lopez Moreno, J. J., additional, Marzari, F., additional, Michalik, H., additional, Naletto, G., additional, Rickman, H., additional, Rodrigo, R., additional, Sabau, L., additional, Thomas, N., additional, Wenzel, K.-P., additional, Agarwal, J., additional, Bertini, I., additional, Ferri, F., additional, Güttler, C., additional, Magrin, S., additional, Oklay, N., additional, Tubiana, C., additional, and Vincent, J.-B., additional

Published
2014
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215. Search for satellites near (21) Lutetia using OSIRIS/Rosetta images

Author

Bertini, I., Sabolo, W., Gutierrez, P.J., Marzari, F., Snodgrass, C., Tubiana, C., Moissl, R., Pajola, M., Lowry, S.C., Barbieri, C., Ferri, F., Davidsson, B., Sierks, H., Bertini, I., Sabolo, W., Gutierrez, P.J., Marzari, F., Snodgrass, C., Tubiana, C., Moissl, R., Pajola, M., Lowry, S.C., Barbieri, C., Ferri, F., Davidsson, B., and Sierks, H.

Abstract

On 2010 July 10 the ESA Rosetta mission flew by the large asteroid (21) Lutetia. One of the scientific goals of the onboard OSIRIS instrument was the search for satellites of the asteroid, with more than 20 images specifically dedicated to this topic. An observational campaign was devised with a selection of filters and exposure times tailored to maximize the possibility of detecting small companions and determining their bound orbits. Data were analyzed with suitable methods to remove cosmic ray hits and known background objects, in order to search for persistent detections of potential interesting flux sources. We found no unambiguous detections of a satellite larger than ?160m inside the entire sphere of gravitational influence. Our search confirmed the absence of bound companions larger than â?¼30m inside 20 primary radii. These limits are a factor of ?30 smaller than the values reported so far from large ground-based telescopes using adaptive optics and from the Hubble Space Telescope. © 2011 Elsevier Ltd.

Published
2012

217. Images of Asteroid 21 Lutetia: A Remnant Planetesimal from the Early Solar System

Author

Sierks, H., Lamy, P., Barbieri, C., Koschny, D., Rickman, H., Rodrigo, R., A'Hearn, M. F., Angrilli, F., Barucci, M. A., Bertaux, J. -L., Bertini, I., Besse, S., Carry, B., Cremonese, G., Da Deppo, V., Davidsson, B., Debei, S., De Cecco, M., De Leon, J., Ferri, F., Fornasier, S., Fulle, M., Hviid, S. F., Gaskell, R. W., Groussin, O., Gutierrez, P., Ip, W., Jorda, L., Kaasalainen, M., Keller, H. U., Knollenberg, J., Kramm, R., Kuehrt, E., Kueppers, M., Lara, L., Lazzarin, M., Leyrat, C., Lopez Moreno, J. J., Magrin, S., Marchi, S., Marzari, F., Massironi, M., Michalik, H., Moissl, R., Naletto, G., Preusker, F., Sabau, L., Sabolo, W., Scholten, F., Snodgrass, C., Thomas, N., Tubiana, C., Vernazza, P., Vincent, J. -B., Wenzel, K. -P., Andert, T., Paetzold, M., Weiss, B. P., Sierks, H., Lamy, P., Barbieri, C., Koschny, D., Rickman, H., Rodrigo, R., A'Hearn, M. F., Angrilli, F., Barucci, M. A., Bertaux, J. -L., Bertini, I., Besse, S., Carry, B., Cremonese, G., Da Deppo, V., Davidsson, B., Debei, S., De Cecco, M., De Leon, J., Ferri, F., Fornasier, S., Fulle, M., Hviid, S. F., Gaskell, R. W., Groussin, O., Gutierrez, P., Ip, W., Jorda, L., Kaasalainen, M., Keller, H. U., Knollenberg, J., Kramm, R., Kuehrt, E., Kueppers, M., Lara, L., Lazzarin, M., Leyrat, C., Lopez Moreno, J. J., Magrin, S., Marchi, S., Marzari, F., Massironi, M., Michalik, H., Moissl, R., Naletto, G., Preusker, F., Sabau, L., Sabolo, W., Scholten, F., Snodgrass, C., Thomas, N., Tubiana, C., Vernazza, P., Vincent, J. -B., Wenzel, K. -P., Andert, T., Paetzold, M., and Weiss, B. P.

Abstract

Images obtained by the Optical, Spectroscopic, and Infrared Remote Imaging System (OSIRIS) cameras onboard the Rosetta spacecraft reveal that asteroid 21 Lutetia has a complex geology and one of the highest asteroid densities measured so far, 3.4 +/- 0.3 grams per cubic centimeter. The north pole region is covered by a thick layer of regolith, which is seen to flow in major landslides associated with albedo variation. Its geologically complex surface, ancient surface age, and high density suggest that Lutetia is most likely a primordial planetesimal. This contrasts with smaller asteroids visited by previous spacecraft, which are probably shattered bodies, fragments of larger parents, or reaccumulated rubble piles.

Published
2011

218. The Cratering History of Asteroid (2867) Steins

Author

Marchi, S., Barbieri, C., Kueppers, M., Marzari, F., Davidsson, B., Keller, H. U., Besse, S., Lamy, P., Mottola, S., Massironi, M., Cremonese, G., Marchi, S., Barbieri, C., Kueppers, M., Marzari, F., Davidsson, B., Keller, H. U., Besse, S., Lamy, P., Mottola, S., Massironi, M., and Cremonese, G.

Abstract

The cratering history of main belt asteroid (2867) Steins has been investigated using OSIRIS imagery acquired during the Rosetta flyby that took place on the 5th of September 2008. For this purpose, we applied current models describing the formation and evolution of main belt asteroids, that provide the rate and velocity distributions of impactors. These models coupled with appropriate crater scaling laws, allow the cratering history to be estimated. Hence, we derive Steins' cratering retention age, namely the time lapsed since its formation or global surface reset. We also investigate the influence of various factors -like bulk structure and crater erasing- on the estimated age, which spans from a few hundred Myrs to more than 1Gyr, depending on the adopted scaling law and asteroid physical parameters. Moreover, a marked lack of craters smaller than about 0.6km has been found and interpreted as a result of a peculiar evolution of Steins cratering record, possibly related either to the formation of the 2.1km wide impact crater near the south pole or to YORP reshaping., Comment: Accepted by Planetary and Space Science

Published
2010
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219. E-type asteroid (2867) steins as imaged by OSIRIS on board rosetta

Author

Keller, H.U., Barbieri, C., Koschny, D., Lamy, P., Rkkman, H., Rodrigo, R., Sierks, H., A'Hearn, M.F., Angrilli, F., Barucci, M.A., Bertaux, J.-L., Cremonese, G., Da Deppo, V., Davidsson, B., De Cecco, M., Debei, S., Fornasier, S., Fulle, M., Groussin, O., Gutiérrez, P.J., Hviid, S.F., Ip, W.-H., Jorda, L., Knollenberg, J., Kramm, J.R., Kührt, E., Küppers, M., Lara, L.-M., Lazzarin, M., Lopez Moreno, J., Marzari, F., Michalik, H., Naletto, G., Sabau, L., Thomas, N., Wenzel, K.-P., Bertini, I., Besse, S., Ferri, F., Kaasalainen, M., Lowry, S.C., Marchi, S., Mottola, S., Sabolo, W., Schröder, S.E., Spjuth, S., Vernazza, P., Keller, H.U., Barbieri, C., Koschny, D., Lamy, P., Rkkman, H., Rodrigo, R., Sierks, H., A'Hearn, M.F., Angrilli, F., Barucci, M.A., Bertaux, J.-L., Cremonese, G., Da Deppo, V., Davidsson, B., De Cecco, M., Debei, S., Fornasier, S., Fulle, M., Groussin, O., Gutiérrez, P.J., Hviid, S.F., Ip, W.-H., Jorda, L., Knollenberg, J., Kramm, J.R., Kührt, E., Küppers, M., Lara, L.-M., Lazzarin, M., Lopez Moreno, J., Marzari, F., Michalik, H., Naletto, G., Sabau, L., Thomas, N., Wenzel, K.-P., Bertini, I., Besse, S., Ferri, F., Kaasalainen, M., Lowry, S.C., Marchi, S., Mottola, S., Sabolo, W., Schröder, S.E., Spjuth, S., and Vernazza, P.

Abstract

The European Space Agency's Rosetta mission encountered the main-belt asteroid (2867) Steins while on its way to rendezvous with comet 67P/Churyumov-Gerasimenko. Images taken with the OSIRIS (optical, spectroscopic, and infrared remote imaging system) cameras on board Rosetta show that Steins is an oblate body with an effective spherical diameter of 5.3 kilometers. Its surface does not show color variations. The morphology of Steins is dominated by linear faults and a large 2.1-kilometer-diameter crater near its south pole. Crater counts reveal a distinct lack of small craters. Steins is not solid rock but a rubble pile and has a conical appearance that is probably the result of reshaping due to Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) spin-up. The OSIRIS images constitute direct evidence for the YORP effect on a main-belt asteroid.

Published
2010

220. A collision in 2009 as the origin of the debris trail of asteroid P/2010 A2

Author

Snodgrass, C., Tubiana, C., Vincent, J.-B., Sierks, H., Hviid, S., Moissl, R., Boehnhardt, H., Barbieri, C., Koschny, D., Lamy, P., Rickman, H., Rodrigo, R., Carry, B., Lowry, S.C., Laird, R.J.M., Weissman, P.R., Fitzsimmons, A., Marchi, S., A'Hearn, M., Angrilli, F., Barucci, A., Bertaux, J.-L., Cremonese, G., Da Deppo, V., Davidsson, B., Debei, S., De Cecco, M., Fornasier, S., Gutiérrez, P., Ip, W.-H., Keller, H.U., Knollenberg, J., Kramm, J.R., Kuehrt, E., Kueppers, M., Lara, L.M., Lazzarin, M., López-Moreno, J.J., Marzari, F., Michalik, H., Naletto, G., Sabau, L., Thomas, N., Wenzel, K.P., Snodgrass, C., Tubiana, C., Vincent, J.-B., Sierks, H., Hviid, S., Moissl, R., Boehnhardt, H., Barbieri, C., Koschny, D., Lamy, P., Rickman, H., Rodrigo, R., Carry, B., Lowry, S.C., Laird, R.J.M., Weissman, P.R., Fitzsimmons, A., Marchi, S., A'Hearn, M., Angrilli, F., Barucci, A., Bertaux, J.-L., Cremonese, G., Da Deppo, V., Davidsson, B., Debei, S., De Cecco, M., Fornasier, S., Gutiérrez, P., Ip, W.-H., Keller, H.U., Knollenberg, J., Kramm, J.R., Kuehrt, E., Kueppers, M., Lara, L.M., Lazzarin, M., López-Moreno, J.J., Marzari, F., Michalik, H., Naletto, G., Sabau, L., Thomas, N., and Wenzel, K.P.

Abstract

The peculiar object P/2010 A2 was discovered1 in January 2010 and given a cometary designation because of the presence of a trail of material, although there was no central condensation or coma. The appearance of this object, in an asteroidal orbit (small eccentricity and inclination) in the inner main asteroid belt attracted attention as a potential new member of the recently recognized2 class of main-belt comets. If confirmed, this new object would expand the range in heliocentric distance over which main-belt comets are found. Here we report observations of P/2010 A2 by the Rosetta spacecraft. We conclude that the trail arose from a single event, rather than a period of cometary activity, in agreement with independent results3. The trail is made up of relatively large particles of millimetre to centimetre size that remain close to the parent asteroid. The shape of the trail can be explained by an initial impact ejecting large clumps of debris that disintegrated and dispersed almost immediately. We determine that this was an asteroid collision that occurred around 10 February 2009. © 2010 Macmillan Publishers Limited. All rights reserved.

Published
2010

221. Outburst activity in comets - I. Continuous monitoring of comet 29P/Schwassmann-Wachmann 1

Author

Trigo-Rodriguez, J. M., Garcia-Melendo, E., Davidsson, B. J. R., Sanchez, A., Rodriguez, D., Lacruz, J., Reyes, J. A. De los, Pastor, S., Trigo-Rodriguez, J. M., Garcia-Melendo, E., Davidsson, B. J. R., Sanchez, A., Rodriguez, D., Lacruz, J., Reyes, J. A. De los, and Pastor, S.

Abstract

Aims. We carried out a continuous monitoring of comet 29P/Schwassmann-Wachmann 1 by using medium aperture telescopes with the aim of studying the activity and outburst mechanisms of this comet on the basis of photometric variations. Methods. We used a standardized method to obtain the coma photometry in the R filter of the Johnson-Kron-Cousins system. Some abrupt changes observed in the brightness of SW1 suggest important variations in surface activity with time. Results. During our 2002-2007 observational campaign we detected 28 outbursts (of 1 mag or larger) in 29P/Schwassmann-Wachmann 1. A typical outburst is characterized by a rapid increase towards maximum (in a few hours) and a slower decrease toward the quiescent level (in 3-4 days). Given the effective observing time, the average outburst rate is 7.3 events per year. Despite well-sampled data, no signs of a clear periodicity in the outburst occurrence has been found, thus confirming the unpredictability of the activity of this comet.

Published
2008
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222. Observations of Comet 9P/Tempel 1 around the Deep Impact event by the OSIRIS cameras onboard Rosetta

Author

Keller, H.U., Küppers, Michael, Fornasier, S., Gutiérrez, Pedro J., Hviid, Stubbe F., Jorda, Laurent, Knollenberg, Jörg, Lowry, Stephen C., Rengel, Miriam, Bertini, Ivano, Cremonese, G., Wing, Ip, Koschny, Detlef, Kramm, Rainer, Kührt, E., Lara, Luisa María, Sierks, Holger, Thomas, Nicolas, Barbieri, Cesare, Lamy, Philoppe, Rickman, Hans, Rodrigo Montero, Rafael, A’Hearn, Michael F., Angrilli, Francesco, Barucci, M.A., Bertaux, Jean-Loup, Deppo, Vania da, Davidsson, B., Cecco, Mariolino de, Debei, Stefano, Fulle, Marco, Gliem, Fritz, Groussin, Olivier, López-Moreno, José Juan, Marzari, Francesco, Naletto, Giampiero, Sabau-Graziati, Lola, Sanz Andrés, Ángel, Wenzel, Klaus-Peter, Keller, H.U., Küppers, Michael, Fornasier, S., Gutiérrez, Pedro J., Hviid, Stubbe F., Jorda, Laurent, Knollenberg, Jörg, Lowry, Stephen C., Rengel, Miriam, Bertini, Ivano, Cremonese, G., Wing, Ip, Koschny, Detlef, Kramm, Rainer, Kührt, E., Lara, Luisa María, Sierks, Holger, Thomas, Nicolas, Barbieri, Cesare, Lamy, Philoppe, Rickman, Hans, Rodrigo Montero, Rafael, A’Hearn, Michael F., Angrilli, Francesco, Barucci, M.A., Bertaux, Jean-Loup, Deppo, Vania da, Davidsson, B., Cecco, Mariolino de, Debei, Stefano, Fulle, Marco, Gliem, Fritz, Groussin, Olivier, López-Moreno, José Juan, Marzari, Francesco, Naletto, Giampiero, Sabau-Graziati, Lola, Sanz Andrés, Ángel, and Wenzel, Klaus-Peter

Abstract

The OSIRIS cameras on the Rosetta spacecraft observed Comet 9P/Tempel 1 from 5 days before to 10 days after it was hit by the Deep Impact projectile. The Narrow Angle Camera (NAC) monitored the cometary dust in 5 different filters. The Wide Angle Camera (WAC) observed through filters sensitive to emissions from OH, CN, Na, and OI together with the associated continuum. Before and after the impact the comet showed regular variations in intensity. The period of the brightness changes is consistent with the rotation period of Tempel 1. The overall brightness of Tempel 1 decreased by about 10% during the OSIRIS observations. The analysis of the impact ejecta shows that no new permanent coma structures were created by the impact. Most of the material moved with ~ 200 m/s. Much of it left the comet in the form of icy grains which sublimated and fragmented within the first hour after the impact. The light curve of the comet after the impact and the amount of material leaving the comet (4.5 - 9 x 10e6 of water ice and a presumably larger amount of dust) suggest that the impact ejecta were quickly accelerated by collisions with gas molecules. Therefore, the motion of the bulk of the ejecta cannot be described by ballistic trajectories, and the validity of determinations of the density and tensile strength of the nucleus of Tempel 1 with models using ballistic ejection of particles is uncertain.

Published
2007

223. THERMAP: a mid-infrared spectro-imager for space missions to small bodies in the inner solar system.

Author

Groussin, O., Licandro, J., Helbert, J., Reynaud, J., Levacher, P., Reyes García-Talavera, M., Alí-Lagoa, V., Blanc, P., Brageot, E., Davidsson, B., Delbó, M., Deleuze, M., Delsanti, A., Diaz Garcia, J., Dohlen, K., Ferrand, D., Green, S., Jorda, L., Joven Álvarez, E., and Knollenberg, J.

Subjects
SOLAR system, ASTEROIDS, SPECTRUM analysis, TEMPERATURE measurements, BOLOMETERS
Abstract

We present THERMAP, a mid-infrared spectro-imager for space missions to small bodies in the inner solar system, developed in the framework of the MarcoPolo-R asteroid sample return mission. THERMAP is very well suited to characterize the surface thermal environment of a NEO and to map its surface composition. The instrument has two channels, one for imaging and one for spectroscopy: it is both a thermal camera with full 2D imaging capabilities and a slit spectrometer. THERMAP takes advantage of the recent technological developments of uncooled microbolometer arrays, sensitive in the mid-infrared spectral range. THERMAP can acquire thermal images (8-18 μm) of the surface and perform absolute temperature measurements with a precision better than 3.5 K above 200 K. THERMAP can acquire mid-infrared spectra (8-16 μm) of the surface with a spectral resolution Δλ of 0.3 μm. For surface temperatures above 350 K, spectra have a signal-to-noise ratio >60 in the spectral range 9-13 μm where most emission features occur. [ABSTRACT FROM AUTHOR]

Published
2016
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224. Images of Asteroid 21 Lutetia: A Remnant Planetesimal from the Early Solar System

Author

Sierks, H., primary, Lamy, P., additional, Barbieri, C., additional, Koschny, D., additional, Rickman, H., additional, Rodrigo, R., additional, A'Hearn, M. F., additional, Angrilli, F., additional, Barucci, M. A., additional, Bertaux, J.- L., additional, Bertini, I., additional, Besse, S., additional, Carry, B., additional, Cremonese, G., additional, Da Deppo, V., additional, Davidsson, B., additional, Debei, S., additional, De Cecco, M., additional, De Leon, J., additional, Ferri, F., additional, Fornasier, S., additional, Fulle, M., additional, Hviid, S. F., additional, Gaskell, R. W., additional, Groussin, O., additional, Gutierrez, P., additional, Ip, W., additional, Jorda, L., additional, Kaasalainen, M., additional, Keller, H. U., additional, Knollenberg, J., additional, Kramm, R., additional, Kuhrt, E., additional, Kuppers, M., additional, Lara, L., additional, Lazzarin, M., additional, Leyrat, C., additional, Moreno, J. J. L., additional, Magrin, S., additional, Marchi, S., additional, Marzari, F., additional, Massironi, M., additional, Michalik, H., additional, Moissl, R., additional, Naletto, G., additional, Preusker, F., additional, Sabau, L., additional, Sabolo, W., additional, Scholten, F., additional, Snodgrass, C., additional, Thomas, N., additional, Tubiana, C., additional, Vernazza, P., additional, Vincent, J.- B., additional, Wenzel, K.- P., additional, Andert, T., additional, Patzold, M., additional, and Weiss, B. P., additional

Published
2011
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225. An investigation of errors in estimates of the cometary nuclei active area fractions

Author

Gutiérrez, Pedro J., Rodrigo Montero, Rafael, Ortiz, José Luis, Davidsson, B., Gutiérrez, Pedro J., Rodrigo Montero, Rafael, Ortiz, José Luis, and Davidsson, B.

Abstract

Active area fractions of cometary nuclei are often estimated by comparing the observed water production rates with theoretical rates obtained by applying the fast rotator or subsolar point approximations to spherical model nuclei. Any discrepancy between observed and theoretical production rates is interpreted as a certain degree of dust mantling (or in some cases hyper activity) of the object. We here investigate the typical errors introduced in such active area fraction estimates by the usage of oversimplified spherical model nuclei. This is done by first calculating the production rates of slowly rotating irregular model bodies with different activity patterns on their surfaces and arbitrary spin axis orientations, for which solar illumination is treated properly. Next, the production rates of the spherical model objects under averaged insolation are compared to the production rates of the complex model objects in an attempt to recover the known active area fraction of the latter bodies. We then find that the fast rotator and subsolar point approximations generally yield large over– and underestimates of the active area fraction, depending on the characteristics of the simulated complex nuclei. Acceptable relative errors (<100%) only occur at small heliocentric distances, and the subsolar point approximation yields somewhat better results than the fast rotator approximation.

Published
2003

226. Millimeter and submillimeter measurements of asteroid (2867) Steins during the Rosetta fly-by

Author

Gulkis, S., primary, Keihm, S., additional, Kamp, L., additional, Backus, C., additional, Janssen, M., additional, Lee, S., additional, Davidsson, B., additional, Beaudin, G., additional, Biver, N., additional, Bockelée-Morvan, D., additional, Crovisier, J., additional, Encrenaz, P., additional, Encrenaz, T., additional, Hartogh, P., additional, Hofstadter, M., additional, Ip, W., additional, Lellouch, E., additional, Mann, I., additional, Schloerb, P., additional, Spilker, T., additional, and Frerking, M., additional

Published
2010
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227. The cratering history of asteroid (2867) Steins

Author

Marchi, S., primary, Barbieri, C., additional, Küppers, M., additional, Marzari, F., additional, Davidsson, B., additional, Keller, H.U., additional, Besse, S., additional, Lamy, P., additional, Mottola, S., additional, Massironi, M., additional, and Cremonese, G., additional

Published
2010
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228. E-Type Asteroid (2867) Steins as Imaged by OSIRIS on Board Rosetta

Author

Keller, H. U., primary, Barbieri, C., additional, Koschny, D., additional, Lamy, P., additional, Rickman, H., additional, Rodrigo, R., additional, Sierks, H., additional, A’Hearn, M. F., additional, Angrilli, F., additional, Barucci, M. A., additional, Bertaux, J.-L., additional, Cremonese, G., additional, Da Deppo, V., additional, Davidsson, B., additional, De Cecco, M., additional, Debei, S., additional, Fornasier, S., additional, Fulle, M., additional, Groussin, O., additional, Gutierrez, P. J., additional, Hviid, S. F., additional, Ip, W.-H., additional, Jorda, L., additional, Knollenberg, J., additional, Kramm, J. R., additional, Kührt, E., additional, Küppers, M., additional, Lara, L.-M., additional, Lazzarin, M., additional, Moreno, J. Lopez, additional, Marzari, F., additional, Michalik, H., additional, Naletto, G., additional, Sabau, L., additional, Thomas, N., additional, Wenzel, K.-P., additional, Bertini, I., additional, Besse, S., additional, Ferri, F., additional, Kaasalainen, M., additional, Lowry, S., additional, Marchi, S., additional, Mottola, S., additional, Sabolo, W., additional, Schröder, S. E., additional, Spjuth, S., additional, and Vernazza, P., additional

Published
2010
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230. Triple F—a comet nucleus sample return mission

Author

Küppers, Michael, primary, Keller, H. U., additional, Kührt, E., additional, A’Hearn, M. F., additional, Altwegg, K., additional, Bertrand, R., additional, Busemann, H., additional, Capria, M. T., additional, Colangeli, L., additional, Davidsson, B., additional, Ehrenfreund, P., additional, Knollenberg, J., additional, Mottola, S., additional, Rathke, A., additional, Weiss, P., additional, Zolensky, M., additional, Akim, E., additional, Basilevsky, A., additional, Galimov, E., additional, Gerasimov, M., additional, Korablev, O., additional, Lomakin, I., additional, Marov, M., additional, Martynov, M., additional, Nazarov, M., additional, Zakharov, A., additional, Zelenyi, L., additional, Aronica, A., additional, Ball, A. J., additional, Barbieri, C., additional, Bar-Nun, A., additional, Benkhoff, J., additional, Biele, J., additional, Biver, N., additional, Blum, J., additional, Bockelée-Morvan, D., additional, Botta, O., additional, Bredehöft, J.-H., additional, Capaccioni, F., additional, Charnley, S., additional, Cloutis, E., additional, Cottin, H., additional, Cremonese, G., additional, Crovisier, J., additional, Crowther, S. A., additional, Epifani, E. M., additional, Esposito, F., additional, Ferrari, A. C., additional, Ferri, F., additional, Fulle, M., additional, Gilmour, J., additional, Goesmann, F., additional, Gortsas, N., additional, Green, S. F., additional, Groussin, O., additional, Grün, E., additional, Gutiérrez, P. J., additional, Hartogh, P., additional, Henkel, T., additional, Hilchenbach, M., additional, Ho, T.-M., additional, Horneck, G., additional, Hviid, S. F., additional, Ip, W.-H., additional, Jäckel, A., additional, Jessberger, E., additional, Kallenbach, R., additional, Kargl, G., additional, Kömle, N. I., additional, Korth, A., additional, Kossacki, K., additional, Krause, C., additional, Krüger, H., additional, Li, Z.-Y., additional, Licandro, J., additional, Lopez-Moreno, J. J., additional, Lowry, S. C., additional, Lyon, I., additional, Magni, G., additional, Mall, U., additional, Mann, I., additional, Markiewicz, W., additional, Martins, Z., additional, Maurette, M., additional, Meierhenrich, U., additional, Mennella, V., additional, Ng, T. C., additional, Nittler, L. R., additional, Palumbo, P., additional, Pätzold, M., additional, Prialnik, D., additional, Rengel, M., additional, Rickman, H., additional, Rodriguez, J., additional, Roll, R., additional, Rost, D., additional, Rotundi, A., additional, Sandford, S., additional, Schönbächler, M., additional, Sierks, H., additional, Srama, R., additional, Stroud, R. M., additional, Szutowicz, S., additional, Tornow, C., additional, Ulamec, S., additional, Wallis, M., additional, Waniak, W., additional, Weissman, P., additional, Wieler, R., additional, Wurz, P., additional, Yung, K. L., additional, and Zarnecki, J. C., additional

Published
2008
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231. Outburst activity in comets

Author

Trigo-Rodríguez, J. M., primary, García-Melendo, E., additional, Davidsson, B. J. R., additional, Sánchez, A., additional, Rodríguez, D., additional, Lacruz, J., additional, De los Reyes, J. A., additional, and Pastor, S., additional

Published
2008
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244. Scientific Planning and Commanding of the Rosetta Payload.

Author

Koschny, D., Dhiri, V., Wirth, K., Zender, J., Solaz, R., Hoofs, R., Laureijs, R., Ho, T.-M, Davidsson, B., and Schwehm, G.

Subjects
ROCKET payloads, LIVE loads, AERODYNAMIC load, SPACE flight, SCIENTIFIC apparatus & instruments, SPACE sciences
Abstract

ESA’s Rosetta mission was launched in March 2004 and is on its way to comet 67P/Churyumov-Gerasimenko, where it is scheduled to arrive in summer 2014. It comprises a payload of 12 scientific instruments and a Lander. All instruments are provided by Principal Investigators, which are responsible for their operations. As for most ESA science missions, the ground segment of the mission consists of a Mission Operations Centre (MOC) and a Science Operations Centre (SOC). While the MOC is responsible for all spacecraft-related aspects and the final uplink of all command timelines to the spacecraft, the scientific operations of the instruments and the collection of the data and ingestion into the Planetary Science Archive are coordinated by the SOC. This paper focuses on the tasks of the SOC and in particular on the methodology and constraints to convert the scientific goals of the Rosetta mission to operational timelines. [ABSTRACT FROM AUTHOR]

Published
2006
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249. Correction to: The Thermal, Mechanical, Structural, and Dielectric Properties of Cometary Nuclei After Rosetta.

Author

Groussin, O., Attree, N., Brouet, Y., Ciarletti, V., Davidsson, B., Filacchione, G., Fischer, H.-H., Gundlach, B., Knapmeyer, M., Knollenberg, J., Kokotanekova, R., Kührt, E., Leyrat, C., Marshall, D., Pelivan, I., Skorov, Y., Snodgrass, C., Spohn, T., and Tosi, F.

Subjects
DIELECTRIC properties
Abstract

Correction to: Space Sci. Rev. (2019) 215: 2910.1007/s11214-019-0594-x The article The Thermal, Mechanical, Structural, and Dielectric Properties of Cometary Nuclei After Rosetta, written by Groussin et al., was originally published electronically on the publisher's internet portal (currently SpringerLink) on 2 May 2019 without open access. With the author(s)' decision to opt for Open Choice the copyright of the article changed to © The Author(s) 2019 and the article is forthwith distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits use, duplication, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license and indicate if changes were made. [ABSTRACT FROM AUTHOR]

Published
2019
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250. The Thermal, Mechanical, Structural, and Dielectric Properties of Cometary Nuclei After Rosetta.

Author

Groussin, O., Attree, N., Brouet, Y., Ciarletti, V., Davidsson, B., Filacchione, G., Fischer, H.-H., Gundlach, B., Knapmeyer, M., Knollenberg, J., Kokotanekova, R., Kührt, E., Leyrat, C., Marshall, D., Pelivan, I., Skorov, Y., Snodgrass, C., Spohn, T., and Tosi, F.

Subjects
DIELECTRIC properties, GRANULAR materials, TENSILE strength, PERMITTIVITY
Abstract

The physical properties of cometary nuclei observed today relate to their complex history and help to constrain their formation and evolution. In this article, we review some of the main physical properties of cometary nuclei and focus in particular on the thermal, mechanical, structural and dielectric properties, emphasising the progress made during the Rosetta mission. Comets have a low density of 480 ± 220 kg m − 3 and a low permittivity of 1.9–2.0, consistent with a high porosity of 70–80%, are weak with a very low global tensile strength < 100 Pa, and have a low bulk thermal inertia of 0 – 60 J K − 1 m − 2 s − 1 / 2 that allowed them to preserve highly volatiles species (e.g. CO, CO2, CH4, N2) into their interior since their formation. As revealed by 67P/Churyumov-Gerasimenko, the above physical properties vary across the nucleus, spatially at its surface but also with depth. The broad picture is that the bulk of the nucleus consists of a weakly bonded, rather homogeneous material that preserved primordial properties under a thin shell of processed material, and possibly covered by a granular material; this cover might in places reach a thickness of several meters. The properties of the top layer (the first meter) are not representative of that of the bulk nucleus. More globally, strong nucleus heterogeneities at a scale of a few meters are ruled out on 67P's small lobe. [ABSTRACT FROM AUTHOR]

Published
2019
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