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89 results on '"Kuehrt, E."'

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

Author

Marschall, R., Rezac, L., Kappel, D., Su, C.C., Gerig, S.-B., Rubin, M., Pinzón-Rodríguez, O., Marshall, D., Liao, Y., Herny, C., Arnold, G., Christou, C., Dadzie, S.K., Groussin, O., Hartogh, P., Jorda, L., Kührt, E., Mottola, S., Mousis, O., Preusker, F., Scholten, F., Theologou, P., Wu, J.-S., Altwegg, K., Rodrigo, R., and Thomas, N.

Published
2019
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3. Regional unit definition for the nucleus of comet 67P/Churyumov-Gerasimenko on the SHAP7 model

Author

Thomas, N., El Maarry, M.R., Theologou, P., Preusker, F., Scholten, F., Jorda, L., Hviid, S.F., Marschall, R., Kührt, E., Naletto, G., Sierks, H., Lamy, P.L., Rodrigo, R., Koschny, D., Davidsson, B., Barucci, M.A., Bertaux, J.L., Bertini, I., Bodewits, D., Cremonese, G., Da Deppo, V., Debei, S., De Cecco, M., Fornasier, S., Fulle, M., Groussin, O., Gutièrrez, P.J., Güttler, C., Ip, W.H., Keller, H.U., Knollenberg, J., Lara, L.M., Lazzarin, M., Lòpez-Moreno, J.J., Marzari, F., Tubiana, C., and Vincent, J.B.

Published
2018
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4. On deviations from free-radial outflow in the inner coma of comet 67P/Churyumov–Gerasimenko

Author

Gerig, S.-B., Marschall, R., Thomas, N., Bertini, I., Bodewits, D., Davidsson, B., Fulle, M., Ip, W.-H., Keller, H.U., Küppers, M., Preusker, F., Scholten, F., Su, C.C., Toth, I., Tubiana, C., Wu, J.-S., Sierks, H., Barbieri, C., Lamy, P.L., Rodrigo, R., Koschny, D., Rickman, H., Agarwal, J., Barucci, M.A., Bertaux, J.-L., Cremonese, G., Da Deppo, V., Debei, S., De Cecco, M., Deller, J., Fornasier, S., Groussin, O., Gutierrez, P.J., Güttler, C., Hviid, S.F., Jorda, L., Knollenberg, J., Kramm, J.-R., Kührt, E., Lara, L.M., Lazzarin, M., Lopez Moreno, J.J., Marzari, F., Mottola, S., Naletto, G., Oklay, N., and Vincent, J.-B.

Published
2018
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5. Meter-scale thermal contraction crack polygons on the nucleus of comet 67P/Churyumov-Gerasimenko

Author

Auger, A.-T., Groussin, O., Jorda, L., El-Maarry, M.R., Bouley, S., Séjourné, A., Gaskell, R., Capanna, C., Davidsson, B., Marchi, S., Höfner, S., Lamy, P.L., Sierks, H., Barbieri, C., Rodrigo, R., Koschny, D., Rickman, H., Keller, H.U., Agarwal, J., A’Hearn, M.F., Barucci, M.A., Bertaux, J.-L., Bertini, I., Cremonese, G., Da Deppo, V., Debei, S., De Cecco, M., Fornasier, S., Fulle, M., Gutiérrez, P.J., Güttler, C., Hviid, S., Ip, W.-H., Knollenberg, J., Kramm, J.-R., Kührt, E., Küppers, M., Lara, L.M., Lazzarin, M., Lopez Moreno, J.J., Marzari, F., Massironi, M., Michalik, H., Naletto, G., Oklay, N., Pommerol, A., Sabau, L., Thomas, N., Tubiana, C., Vincent, J.-B., and Wenzel, K.-P.

Published
2018
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7. Surface changes on comet 67P/Churyumov-Gerasimenko suggest a more active past

Author

El-Maarry, M. Ramy, Groussin, O., Thomas, N., Pajola, M., Auger, A.-T., Davidsson, B., Hu, X., Hviid, S. F., Knollenberg, J., Güttler, C., Tubiana, C., Fornasier, S., Feller, C., Hasselmann, P., Vincent, J.-B., Sierks, H., Barbieri, C., Lamy, P., Rodrigo, R., Koschny, D., Keller, H. U., Rickman, H., A’Hearn, M. F., Barucci, M. A., Bertaux, J.-L., Bertini, I., Besse, S., Bodewits, D., Cremonese, G., Da Deppo, V., Debei, S., De Cecco, M., Deller, J., Deshapriya, J. D. P., Fulle, M., Gutierrez, P. J., Hofmann, M., Ip, W.-H., Jorda, L., Kovacs, G., Kramm, J.-R., Kührt, E., Küppers, M., Lara, L. M., Lazzarin, M., Lin, Z.-Yi, Moreno, J. J. Lopez, Marchi, S., Marzari, F., Mottola, S., Naletto, G., Oklay, N., Pommerol, A., Preusker, F., Scholten, F., and Shi, X.

Published
2017

8. Rosetta's comet 67P/Churyumov-Gerasimenko sheds its dusty mantle to reveal its icy nature

Author

Fornasier, S., Mottola, S., Keller, H. U., Barucci, M. A., Davidsson, B., Feller, C., Deshapriya, J. D. P., Sierks, H., Barbieri, C., Lamy, P. L., Rodrigo, R., Koschny, D., Rickman, H., A'Hearn, M., Agarwal, J., Bertaux, J.-L., Bertini, I., Besse, S., Cremonese, G., Da Deppo, V., Debei, S., De Cecco, M., Deller, J., EI-Maarry, M. R., Fulle, M., Groussin, O., Gutierrez, P. J., Güttler, C., Hofmann, M., Hviid, S. F., Ip, W.-H., Jorda, L., Knollenberg, J., Kovacs, G., Kramm, R., Kührt, E., Küppers, M., Lara, M. L., Lazzarin, M., Moreno, J. J. Lopez, Marzari, F., Massironi, M., Naletto, G., Oklay, N., Pajola, M., Pommerol, A., Preusker, F., Scholten, F., Shi, X., Thomas, N., Toth, I., Tubiana, C., and Vincent, J.-B.

Published
2016

9. Seasonal exposure of carbon dioxide ice on the nucleus of comet 67P/Churyumov-Gerasimenko

Author

Filacchione, G., Raponi, A., Capaccioni, F., Ciarniello, M., Tosi, F., Capria, M. T., De Sanctis, M. C., Migliorini, A., Piccioni, G., Cerroni, P., Barucci, M. A., Fornasier, S., Schmitt, B., Quirico, E., Erard, S., Bockelee-Morvan, D., Leyrat, C., Arnold, G., Mennella, V., Ammannito, E., Bellucci, G., Benkhoff, J., Bibring, J. P., Blanco, A., Blecka, M. I., Carlson, R., Carsenty, U., Colangeli, L., Combes, M., Combi, M., Crovisier, J., Drossart, P., Encrenaz, T., Federico, C., Fink, U., Fonti, S., Fulchignoni, M., Ip, W.-H., Irwin, P., Jaumann, R., Kuehrt, E., Langevin, Y., Magni, G., McCord, T., Moroz, L., Mottola, S., Palomba, E., Schade, U., Stephan, K., Taylor, F., Tiphene, D., Tozzi, G. P., Beck, P., Biver, N., Bonal, L., Combe, J.-Ph., Despan, D., Flamini, E., Formisano, M., Frigeri, A., Grassi, D., Gudipati, M. S., Kappel, D., Longobardo, A., Mancarella, F., Markus, K., Merlin, F., Orosei, R., Rinaldi, G., Cartacci, M., Cicchetti, A., Hello, Y., Henry, F., Jacquinod, S., Reess, J. M., Noschese, R., Politi, R., and Peter, G.

Published
2016

10. The global shape, density and rotation of Comet 67P/Churyumov-Gerasimenko from preperihelion Rosetta/OSIRIS observations

Author

Jorda, L., Gaskell, R., Capanna, C., Hviid, S., Lamy, P., Ďurech, J., Faury, G., Groussin, O., Gutiérrez, P., Jackman, C., Keihm, S.J., Keller, H.U., Knollenberg, J., Kührt, E., Marchi, S., Mottola, S., Palmer, E., Schloerb, F.P., Sierks, H., Vincent, J.-B., A’Hearn, M.F., Barbieri, C., Rodrigo, R., Koschny, D., Rickman, H., Barucci, M.A., Bertaux, J.L., Bertini, I., Cremonese, G., Da Deppo, V., Davidsson, B., Debei, S., De Cecco, M., Fornasier, S., Fulle, M., Güttler, C., Ip, W.-H., Kramm, J.R., Küppers, M., Lara, L.M., Lazzarin, M., Lopez Moreno, J.J., Marzari, F., Naletto, G., Oklay, N., Thomas, N., Tubiana, C., and Wenzel, K.-P.

Published
2016
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12. The nonmagnetic nucleus of comet 67P/Churyumov-Gerasimenko

Author

Auster, H.-U., Apathy, I., Berghofer, G., Fornacon, K.-H., Remizov, A., Carr, C., Güttler, C., Haerendel, G., Heinisch, P., Hercik, D., Hilchenbach, M., Kührt, E., Magnes, W., Motschmann, U., Richter, I., Russell, C. T., Przyklenk, A., Schwingenschuh, K., Sierks, H., and Glassmeier, K.-H.

Published
2015

13. The landing(s) of Philae and inferences about comet surface mechanical properties

Author

Biele, J., Ulamec, S., Maibaum, M., Roll, R., Witte, L., Jurado, E., Muñoz, P., Arnold, W., Auster, H.-U., Casas, C., Faber, C., Fantinati, C., Finke, F., Fischer, H.-H., Geurts, K., Güttler, C., Heinisch, P., Herique, A., Hviid, S., Kargl, G., Knapmeyer, M., Knollenberg, J., Kofman, W., Kömle, N., Kührt, E., Lommatsch, V., Mottola, S., de Santayana, R. Pardo, Remetean, E., Scholten, F., Seidensticker, K. J., Sierks, H., and Spohn, T.

Published
2015

15. On the nucleus structure and activity of comet 67P/Churyumov-Gerasimenko

Author

Sierks, H., Barbieri, C., Lamy, P. L., Rodrigo, R., Koschny, D., Rickman, H., Keller, H. U., Agarwal, J., A'Hearn, M. F., Angrilli, F., Auger, A.-T., Barucci, M. A., Bertaux, J.-L., Bertini, I., Besse, S., Bodewits, D., Capanna, C., Cremonese, G., Da Deppo, V., Davidsson, B., Debei, S., De Cecco, M., Ferri, F., Fornasier, S., Fulle, M., Gaskell, R., Giacomini, L., Groussin, O., Gutierrez-Marques, P., Gutiérrez, P. J., Güttler, C., Hoekzema, N., Hviid, S. F., Ip, W.-H., Jorda, L., Knollenberg, J., Kovacs, G., Kramm, J.-R., Kührt, E., Küppers, M., La Forgia, F., Lara, L. M., Lazzarin, M., Leyrat, C., Moreno, J. J. Lopez, Magrin, S., Marchi, S., Marzari, F., Massironi, M., Michalik, H., Moissl, R., Mottola, S., Naletto, G., Oklay, N., Pajola, M., Pertile, M., Preusker, F., Sabau, L., Scholten, F., Snodgrass, C., Thomas, N., Tubiana, C., Vincent, J.-B., Wenzel, K.-P., Zaccariotto, M., and Pätzold, M.

Published
2015

16. The morphological diversity of comet 67P/Churyumov-Gerasimenko

Author

Thomas, N., Sierks, H., Barbieri, C., Lamy, P. L., Rodrigo, R., Rickman, H., Koschny, D., Keller, H. U., Agarwal, J., A'Hearn, M. F., Angrilli, F., Auger, A.-T., Barucci, M. A., Bertaux, J.-L., Bertini, I., Besse, S., Bodewits, D., Cremonese, G., Da Deppo, V., Davidsson, B., De Cecco, M., Debei, S., El-Maarry, M. R., Ferri, F., Fornasier, S., Fulle, M., Giacomini, L., Groussin, O., Gutierrez, P. J., Güttler, C., Hviid, S. F., Ip, W.-H., Jorda, L., Knollenberg, J., Kramm, J.-R., Kührt, E., Küppers, M., La Forgia, F., Lara, L. M., Lazzarin, M., Moreno, J. J. Lopez, Magrin, S., Marchi, S., Marzari, F., Massironi, M., Michalik, H., Moissl, R., Mottola, S., Naletto, G., Oklay, N., Pajola, M., Pommerol, A., Preusker, F., Sabau, L., Scholten, F., Snodgrass, C., Tubiana, C., Vincent, J.-B., and Wenzel, K.-P.

Published
2015

17. Time variability and heterogeneity in the coma of 67P/Churyumov-Gerasimenko

Author

Hässig, M., Altwegg, K., Balsiger, H., Bar-Nun, A., Berthelier, J. J., Bieler, A., Bochsler, P., Briois, C., Calmonte, U., Combi, M., De Keyser, J., Eberhardt, P., Fiethe, B., Fuselier, S. A., Galand, M., Gasc, S., Gombosi, T. I., Hansen, K. C., Jäckel, A., Keller, H. U., Kopp, E., Korth, A., Kührt, E., Le Roy, L., Mall, U., Marty, B., Mousis, O., Neefs, E., Owen, T., Rème, H., Rubin, M., Sémon, T., Tornow, C., Tzou, C.-Y., Waite, J. H., and Wurz, P.

Published
2015

18. Dust measurements in the coma of comet 67P/Churyumov-Gerasimenko inbound to the Sun

Author

Rotundi, A., Sierks, H., Corte, V. Della, Fulle, M., Gutierrez, P. J., Lara, L., Barbieri, C., Lamy, P. L., Rodrigo, R., Koschny, D., Rickman, H., Keller, H. U., López-Moreno, J. J., Accolla, M., Agarwal, J., A'Hearn, M. F., Altobelli, N., Angrilli, F., Barucci, M. A., Bertaux, J.-L., Bertini, I., Bodewits, D., Bussoletti, E., Colangeli, L., Cosi, M., Cremonese, G., Crifo, J.-F., Da Deppo, V., Davidsson, B., Debei, S., De Cecco, M., Esposito, F., Ferrari, M., Fornasier, S., Giovane, F., Gustafson, B., Green, S. F., Groussin, O., Grün, E., Güttler, C., Herranz, M. L., Hviid, S. F., Ip, W., Ivanovski, S., Jerónimo, J. M., Jorda, L., Knollenberg, J., Kramm, R., Kührt, E., Küppers, M., Lazzarin, M., Leese, M. R., López-Jiménez, A. C., Lucarelli, F., Lowry, S. C., Marzari, F., Epifani, E. Mazzotta, McDonnell, J. A. M., Mennella, V., Michalik, H., Molina, A., Morales, R., Moreno, F., Mottola, S., Naletto, G., Oklay, N., Ortiz, J. L., Palomba, E., Palumbo, P., Perrin, J.-M., Rodríguez, J., Sabau, L., Snodgrass, C., Sordini, R., Thomas, N., Tubiana, C., Vincent, J.-B., Weissman, P., Wenzel, K.-P., Zakharov, V., and Zarnecki, J. C.

Published
2015

19. The organic-rich surface of comet 67P/Churyumov-Gerasimenko as seen by VIRTIS/Rosetta

Author

Capaccioni, F., Coradini, A., Filacchione, G., Erard, S., Arnold, G., Drossart, P., De Sanctis, M. C., Bockelee-Morvan, D., Capria, M. T., Tosi, F., Leyrat, C., Schmitt, B., Quirico, E., Cerroni, P., Mennella, V., Raponi, A., Ciarniello, M., MeCord, T., Moroz, L., Palomba, E., Ammannito, E., Barucci, M. A., Bellucci, G., Benkhoff, J., Bibring, J. P., Blanco, A., Blecka, M., Carlson, R., Carsenty, U., Colangeli, L., Combes, M., Combi, M., Crovisier, J., Encrenaz, T., Federico, C., Fink, U., Fonti, S., Ip, W. H., Irwin, P., Jaumann, R., Kuehrt, E., Langevin, Y., Magni, G., Mottola, S., Orofino, V., Palumbo, P., Piccioni, G., Schade, U., Taylor, F., Tiphene, D., Tozzi, G. P., Beck, P., Biver, N., Bonal, L., Combe, J.-Ph., Despan, D., Flamini, E., Fornasier, S., Frigeri, A., Grassi, D., Gudipati, M., Longobardo, A., Markus, K., Merlin, F., Orosei, R., Rinaldi, G., Stephan, K., Cartacci, M., Cicchetti, A., Giuppi, S., Hello, Y., Henry, F., Jacquinod, S., Noschese, R., Peter, G., Politi, R., Reess, J. M., and Semery, A.

Published
2015

24. The diurnal cycle of water ice on comet 67P/Churyumov-Gerasimenko

Author

De Sanctis, M. C., Capaccioni, F., Ciarniello, M., Filacchione, G., Formisano, M., Mottola, S., Raponi, A., Tosi, F., Bockelée-Morvan, D., Erard, S., Leyrat, C., Schmitt, B., Ammannito, E., Arnold, G., Barucci, M. A., Combi, M., Capria, M. T., Cerroni, P., Ip, W.-H., Kuehrt, E., McCord, T. B., Palomba, E., Beck, P., Quirico, E., Piccioni, G., Bellucci, G., Fulchignoni, M., Jaumann, R., Stephan, K., Longobardo, A., Mennella, V., Migliorini, A., Benkhoff, J., Bibring, J. P., Blanco, A., Blecka, M., Carlson, R., Carsenty, U., Colangeli, L., Combes, M., Crovisier, J., Drossart, P., Encrenaz, T., Federico, C., Fink, U., Fonti, S., Irwin, P., Langevin, Y., Magni, G., Moroz, L., Orofino, V., Schade, U., Taylor, F., Tiphene, D., Tozzi, G. P., Biver, N., Bonal, L., Combe, J.-Ph., Despan, D., Flamini, E., Fornasier, S., Frigeri, A., Grassi, D., Gudipati, M. S., Mancarella, F., Markus, K., Merlin, F., Orosei, R., Rinaldi, G., Cartacci, M., Cicchetti, A., Giuppi, S., Hello, Y., Henry, F., Jacquinod, S., Reess, J. M., Noschese, R., Politi, R., and Peter, G.

Subjects
Water cycle -- Natural history -- Observations, Comets -- Natural history -- Observations, Environmental issues, Science and technology, Zoology and wildlife conservation
Abstract

Author(s): M. C. De Sanctis (corresponding author) [1]; F. Capaccioni [1]; M. Ciarniello [1]; G. Filacchione [1]; M. Formisano [1]; S. Mottola [2]; A. Raponi [1]; F. Tosi [1]; D. [...]

Published
2015
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26. The geomorphology of (21) Lutetia: Results from the OSIRIS imaging system onboard ESA's Rosetta spacecraft

Author

Thomas, N., Barbieri, C., Keller, H.U., Lamy, P., Rickman, H., Rodrigo, R., Sierks, H., Wenzel, K.P., Cremonese, G., Jorda, L., Küppers, M., Marchi, S., Marzari, F., Massironi, M., Preusker, F., Scholten, F., Stephan, K., Barucci, M.A., Besse, S., El-Maarry, M.R., Fornasier, S., Groussin, O., Hviid, S.F., Koschny, D., Kührt, E., Martellato, E., Moissl, R., Snodgrass, C., Tubiana, C., and Vincent, J.-B.

Published
2012
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27. 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., Kührt, E., Küppers, M., Lara, L., Lazzarin, M., Leyrat, C., Moreno, J. J. Lopez, 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., Pätzold, M., and Weiss, B. P.

Published
2011

28. The Surface Composition and Temperature of Asteroid 21 Lutetia As Observed by Rosetta/VIRTIS

Author

Coradini, A., Capaccioni, F., Erard, S., Arnold, G., De Sanctis, M. C., Filacchione, G., Tosi, F., Barucci, M. A., Capria, M. T., Ammannito, E., Grassi, D., Piccioni, G., Giuppi, S., Bellucci, G., Benkhoff, J., Bibring, J. P., Blanco, A., Blecka, M., Bockelee-Morvan, D., Carraro, F., Carlson, R., Carsenty, U., Cerroni, P., Colangeli, L., Combes, M., Combi, M., Crovisier, J., Drossart, P., Encrenaz, E. T., Federico, C., Fink, U., Fonti, S., Giacomini, L., Ip, W. H., Jaumann, R., Kuehrt, E., Langevin, Y., Magni, G., McCord, T., Mennella, V., Mottola, S., Neukum, G., Orofino, V., Palumbo, P., Schade, U., Schmitt, B., Taylor, F., Tiphene, D., and Tozzi, G.

Published
2011

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

Author

Keller, H. U., Barbieri, C., Koschny, D., Lamy, P., Rickman, 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., Gutierrez, P. J., Hviid, S. F., Ip, W.-H., Jorda, L., Knollenberg, J., Kramm, J. R., Kührt, E., Küppers, M., Lara, L.-M., Lazzarin, M., Moreno, J. Lopez, Marzari, F., Michalik, H., Naletto, G., Sabau, L., Wenzel, K.-P., Bertini, I., Besse, S., Ferri, F., Kaasalainen, M., Lowry, S., Marchi, S., Mottola, S., Sabolo, W., Schröder, S. E., Spjuth, S., and Vernazza, P.

Published
2010
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31. Exposed water ice on the nucleus of comet 67P/Churyumov–Gerasimenko

Author

Filacchione, G., De Sanctis, M. C., Capaccioni, F., Raponi, A., Tosi, F., Ciarniello, M., Cerroni, P., Piccioni, G., Capria, M. T., Palomba, E., Bellucci, G., Erard, S., Bockelee-Morvan, D., Leyrat, C., Arnold, G., Barucci, M. A., Fulchignoni, M., Schmitt, B., Quirico, E., Jaumann, R., Stephan, K., Longobardo, A., Mennella, V., Migliorini, A., Ammannito, E., Benkhoff, J., Bibring, J. P., Blanco, A., Blecka, M. I., Carlson, R., Carsenty, U., Colangeli, L., Combes, M., Combi, M., Crovisier, J., Drossart, P., Encrenaz, T., Federico, C., Fink, U., Fonti, S., Ip, W. H., Irwin, P., Kuehrt, E., Langevin, Y., Magni, G., McCord, T., Moroz, L., Mottola, S., Orofino, V., Schade, U., Taylor, F., Tiphene, D., Tozzi, G. P., Beck, P., Biver, N., Bonal, L., Combe, J-Ph., Despan, D., Flamini, E., Formisano, M., Fornasier, S., Frigeri, A., Grassi, D., Gudipati, M. S., Kappel, D., Mancarella, F., Markus, K., Merlin, F., Orosei, R., Rinaldi, G., Cartacci, M., Cicchetti, A., Giuppi, S., Hello, Y., Henry, F., Jacquinod, S., Reess, J. M., Noschese, R., Politi, R., and Peter, G.

Published
2016
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32. Virtis: An Imaging Spectrometer for the Rosetta Mission

Author

Coradini, A, Capaccioni, F., Drossart, P., Arnold, G., Ammannito, E., Angrilli, F., Barucci, A., Bellucci, G., Benkhoff, J., Bianchini, G., Bibring, J. P., Blecka, M., Bockelee-Morvan, D., Capria, M. T., Carlson, R., Carsenty, U., Cerroni, P., Colangeli, L., Combes, M., Combi, M., Crovisier, J., Desanctis, M. C., Encrenaz, E. T., Erard, S., Federico, C., Filacchione, G., Fink, U., Fonti, S., Formisano, V., Ip, W. H., Jaumann, R., Kuehrt, E., Langevin, Y., Magni, G., Mccord, T., Mennella, V., Mottola, S., Neukum, G., Palumbo, P., Piccioni, G., Rauer, H., Saggin, B., Schmitt, B., Tiphene, D., and Tozzi, G.

Published
2007
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34. A collision in 2009 as the origin of the debris trail of asteroid P/2010 A2

Author

Snodgrass, Colin, Tubiana, Cecilia, Vincent, Jean-Baptiste, Sierks, Holger, Hviid, Stubbe, Moissl, Richard, Boehnhardt, Hermann, Barbieri, Cesare, Koschny, Detlef, Lamy, Philippe, Rickman, Hans, Rodrigo, Rafael, Carry, Benoît, Lowry, Stephen C., Laird, Ryan J. M., Weissman, Paul R., Fitzsimmons, Alan, Marchi, Simone, 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.

Published
2010
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35. Composition of LHB Comets and Their Influence on the Early Earth Atmosphere Composition

Author

Tornow, C, Kupper, S, Ilgner, M, Kuehrt, E, and Motschmann, U

Subjects
Space Sciences (General)
Abstract

Two main processes were responsible for the composition of this atmosphere: chemical evolution of the volatile fraction of the accretion material forming the planet and the delivery of gasses to the planetary surface by impactors during the late heavy bombardment (LHB). The amount and composition of the volatile fraction influences the outgassing of the Earth mantle during the last planetary formation period. A very weakened form of outgassing activity can still be observed today by examining the composition of volcanic gasses. An enlightenment of the second process is based on the sparse records of the LHB impactors resulting from the composition of meteorites, observed cometary comas, and the impact material found on the Moon. However, for an assessment of the influence of the outgassing on the one hand and the LHB event on the other, one has to supplement the observations with numerical simulations of the formation of volatiles and their incorporation into the accretion material which is the precursors of planetary matter, comets and asteroids. These simulations are performed with a combined hydrodynamic-chemical model of the solar nebula (SN). We calculate the chemical composition of the gas and dust phase of the SN. From these data, we draw conclusions on the upper limits of the water content and the amount of carbon and nitrogen rich volatiles incorporated later into the accretion material. Knowing these limits we determine the portion of major gas compounds delivered during the LHB and compare it with the related quantities of the outgassed species.

Published
2011

36. Triple F - A Comet Nucleus Sample Return Mission

Author

Kueppers, Michael, Keller, H. U, Kuehrt, E, A'Hearn, M. F, Altwegg, K, Bertrand, R, Busemann, H, Capria, M. T, Colangeli, L, Davidsson, B, Ehrenfreund, P, Knollenberg, J, Mottola, S, Weiss, P, Zolensky, M, Akim, E, Basilevsky, A, Galimov, E, Gerasimov, M, Korablev, O, Charnley, S, Nittler, L. R, Sandford, S, and Weissman, P

Subjects
Astronomy
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 50 cm 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-andgo sampling by a single spacecraft was proposed as an M-class mission in collaboration with the Russian space agency ROSCOSMOS.

Published
2008
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37. On understanding multi-instrument Rosetta data of the innermost dust and gas coma of comet 67P/Churyumov-Gerasimenko - results, strengths, and limitations of models

Author

Marschall, R., Rezac, L., Kappel, David, Marshall, D., Su, Chin-Chia, Gerig, S.B., Pinzon, O., Liao, Y., Rubin, M., Herny, C., Hartogh, P., Kuehrt, E., Mottola, Stefano, Preusker, Frank, Scholten, Frank, Jorda, L, Theologou, Panagiotis, Groussin, Olivier, Dadzie, S Kokou, Christou, C., Arnold, Gabriele, Wu, Jong-Shinn, Altwegg, Kathrin, Sierks, H., Rodrigo, R., and Thomas, N.

Subjects
Asteroiden und Kometen, MIRO, 520 Astronomy, Leitungsbereich PF, Planetengeodäsie, Comet 67P, OSIRIS, Coma, VIRTIS, ROSINA, DSMC, 620 Engineering
Abstract

Numerical models are powerful tools for understanding the connection between the emitted gas and dust from the surface of comets and the subsequent expansion into space where remote sensing instruments can perform measurements. We will present such a predictive model which can provide synthetic measurements for multiple instruments on board ESA's Rosetta mission to comet 67P/Churyumov-Gerasimenko (hereafter 67P). We will demonstrate why a multi instrument approach is essential and how models can be used to constrain the gas and dust source distribution on the surface.

Published
2018
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38. Physical properties of the regolith of Phobos

Author

Ksanofomaliti, L, Moroz, V, Goroshkova, N, Zhukov, B, Nikitin, G, Murchie, S, Britt, D, Duxbury, T, Kuehrt, E, and Murray, B

Subjects
Lunar And Planetary Exploration
Abstract

Results of two experiments performed onboard the Phobos spacecraft are presented: spectrophotometry in the 300-600 nm range and thermal radiometry, i.e., intrinsic thermal emission in the 6-50 micron range. The thermophysical characteristics of the Phobos regolith are indicated by a thermal inertia coefficient which is similar to that of the moon. The reflectivity of the regolith is inhomogeneous in the region investigated and depends mostly on the relief features, primarily craters and their age. The expected similarity of the reflection spectra with those of carbonacenous chondrites was not confirmed.

Published
1991

40. Continued activity in P/2013 P5 PANSTARRS - The comet that should not be

Author

Hainaut, O. R., Boehnhardt, H., Snodgrass, C., Meech, K. J., Deller, J., Gillon, M., Jehin, E., Kuehrt, E., Lowry, S. C., Manfroid, J., Micheli, M., Mottola, S., Opitom, C., Vincent, J. -B., and Wainscoat, R.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

P/2013 P5 PANSTARRS was discovered in Aug. 2013, displaying a cometary tail, but with orbital elements typical for a member of the inner asteroid Main Belt. We monitored the object from 2013 Aug. 30 until Oct. 05 using the CFHT, NTT, CA 1.23m, Perkins 1.8m (Lowell), and the 0.6m TRAPPIST telescopes. We measured its nuclear radius to be r < 0.25-0.29km, and its colours g-r = 0.58+/-0.05 and r-i = 0.23+/-0.06, typical for an S-class asteroid. We failed to detect any rotational light curve, with an amplitude < 0.05mag and a double-peaked rotation period < 20h. A detailed Finson-Probstein analysis of deep NTT and CFHT images indicated that the object was active since at least late January 2013 until the time of the latest observations in 2013 September, with at least two peaks of activity around 2013 June 14+/-10d and 2013 July 22+/-3d. The changes of activity level and the activity peaks were extremely sharp and short, shorter than the temporal resolution of our observations (about 1d). The dust distribution was similar during these two events, with dust grains covering at least the 1-1000��m range. The total mass ejected in grains, A&A, accepted

Published
2014

41. Spectrophotometric investigation of Phobos with the Rosetta OSIRIS-NAC camera and implications for its collisional capture

Author

Pajola, M, Lazzarin, M, Bertini, I, Marzari, F, Turrini, D., Magrin, S, La Forgia, F, Thomas, N, Küppers, M, Moissl, R, Ferri, F, Barbieri, C, Rickman, H, Sierks, H, A’Hearn, Osiris Team (M., Angrilli, F., Barucci, A., Bertaux, J. -L., Cremonese, G., Davidsson, B., Da Deppo, V., Debei, S., De Cecco, M., Fornasier, S., Fulle, M., Groussin, O., Gutierrez, P., Hviid, S., W. -H., Ip, Jorda, L., Keller, H. U., Knollenberg, J., Koschny, D., Kramm, J. R., Kuehrt, E., Lamy, P., Lara, L. M., Lopez-Moreno, J. J., Michalik, H., Naletto, G., Rodrigo, R., Sabau, L., and Wenzel), K. -P.

Subjects
Solar System, 530 Physics, Mars, Context (language use), Individual, Spectral line, Rosetta Space Mission, Phobos, Phase angle (astronomy), Planet, Spectral slope, Formation -planets and satellites, Imaging spectroscopy -planets and satellites, Phobos -planets and satellites, Surfaces, Techniques, Physics, 520 Astronomy, Astronomy, Osiris images, Astronomy and Astrophysics, Mars Exploration Program, 620 Engineering, Space and Planetary Science, Asteroid
Abstract

The Martian satellite Phobos has been observed on 2007 February 24 and 25, during the pre- and post-Mars closest approach (CA) of the ESA Rosetta spacecraft Mars swing-by. The goal of the observations was the determination of the surface composition of different areas of Phobos, in order to obtain new clues regarding its nature and origin. Near-ultraviolet, visible and near-infrared (263.5–992.0 nm) images of Phobos's surface were acquired using the Narrow Angle Camera of the OSIRIS instrument onboard Rosetta. The six multi-wavelength sets of observations allowed a spectrophotometric characterization of different areas of the satellite, belonging respectively to the leading and trailing hemisphere of the anti-Mars hemisphere, and also of a section of its sub-Mars hemisphere. The pre-CA spectrophotometric data obtained with a phase angle of 19° have a spectral trend consistent within the error bars with those of unresolved/disc-integrated measurements present in the literature. In addition, we detect an absorption band centred at 950 nm, which is consistent with the presence of pyroxene. The post-CA observations cover from NUV to NIR a portion of the surface (0° to 43°E of longitude) never studied before. The reflectance measured on our data does not fit with the previous spectrophotometry above 650 nm. This difference can be due to two reasons. First, the OSIRIS observed area in this observation phase is completely different with respect to the other local specific spectra and hence the spectrum may be different. Secondly, due to the totally different observation geometry (the phase angle ranges from 137° to 140°), the differences of spectral slope can be due to phase reddening. The comparison of our reflectance spectra, both pre- and post-CA, with those of D-type asteroids shows that the spectra of Phobos are all redder than the mean D-type spectrum, but within the spectral dispersion of other D-types. To complement this result, we performed an investigation of the conditions needed to collisionally capture Phobos in a way similar to that proposed for the irregular satellites of the giant planets. Once put in the context of the current understanding of the evolution of the early Solar system, the coupled observational and dynamical results we obtained strongly argue for an early capture of Phobos, likely immediately after the formation of Mars.

Published
2012
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42. (21) Lutetia spectrophotometry from Rosetta-OSIRIS images and comparison to ground-based observations

Author

Magrin, S., La Forgia, F., Pajola, Maurizio, Lazzarin, M., Massironi, M., Ferri, F., Da Deppo, V., Barbieri, C., Sierks, H., A’Hearn, OSIRIS Team (M., Angrilli, F., Barucci, A., Bertaux, J. -L., Cremonese, G., Davidsson, B., Debei, S., De Cecco, M., Fornasier, S., Fulle, M., Groussin, O., Gutierrez, P., Hviid, S., W. -H., Ip, Jorda, L., Keller, H. U., Knollenberg, J., Koschny, D., Kramm, J. R., Kuehrt, E., Kuppers, M., Lamy, P., Lara, L. M., Lopez-Moreno, J. J., Marzari, F., Michalik, H., Naletto, G., Rickman, H., Rodrigo, R., Sabau, L., Thomas, N., Weissman, P. r., and Wenzel), K. -P.

Subjects
Physics, medicine.diagnostic_test, biology, Data error, Minor bodies, Lutetia Asteroid, Astronomy and Astrophysics, Astrophysics, Lutetia, biology.organism_classification, Space and Planetary Science, Asteroid, Spectrophotometry, Variegation (histology), Rosetta, medicine, spectrophotometry, OSIRIS, Osiris, Remote sensing
Abstract

Here we present some preliminary results on surface variegation found on (21) Lutetia from ROSETTA-OSIRIS images acquired on 2010-07-10. The spectrophotometry obtained by means of the two cameras NAC and WAC (Narrow and Wide Angle Cameras) is consistent with ground based observations, and does not show surface diversity above the data error bars. The blue and UV images (shortward 500 nm) may, however, indicate a variegation of the optical properties of the asteroid surface on the Baetica region (Sierks et al., 2011). We also speculate on the contribution due to different illumination and to different ground properties (composition or, more probably, grain size diversity). In particular a correlation with geologic units independently defined by Massironi et al. (2012) is evident, suggesting that the variegation of the ground optical properties is likely to be real. © 2011 Elsevier Ltd.

Published
2012

43. Shape modeling technique KOALA validated by ESA Rosetta at (21) Lutetia

Author

Carry, B., Kaasalainen, M., Merline, W. J., Müller, T. G., Jorda, L., Drummond, J. D., Berthier, J., O'Rourke, L., Urech, J., Küppers, M., Conrad, A., Tamblyn, P., Dumas, C., Sierks, A’Hearn, H. (M., Angrilli, F., Barbieri, C., Barucci, A., Bertaux, J. -L., Cremonese, G., Da Deppo, V., Davidsson, B., Debei, S., De Cecco, M., Fornasier, S., Fulle, M., Groussin, O., Gutierrez, P., W. -H., Ip, Hviid, S., Keller, H. U., Koschny, D., Knollenberg, J., Kramm, J. R., Kuehrt, E., Lamy, P., Lara, L. M., Lazzarin, M., Lopez-Moreno, J. J., Marzari, F., Michalik, H., Naletto, G., Rickman, H., Rodrigo, R., Sabau, L., Thomas, N., Wenzel), K. -P., European Space Astronomy Centre (ESAC), European Space Agency (ESA), Department of Mathematics [Tampere], Tampere University of Technology [Tampere] (TUT), Department of Space Studies [Boulder], Southwest Research Institute [Boulder] (SwRI), Max-Planck-Institut für Extraterrestrische Physik (MPE), 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), Starfire Optical Range [AFRL] (SOR), United States Air Force (USAF), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Astronomical Institute of Charles University, Charles University [Prague] (CU), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, European Southern Observatory (ESO), Max-Planck-Institut für Sonnensystemforschung (MPS), Agence Spatiale Européenne = European Space Agency (ESA), 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 de Lille-Centre National de la Recherche Scientifique (CNRS), Groupe Astrométrie et Planétologie (GAP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Tampere University of Technology (TUT), Southwest Research Institute, Max-Planck-Institut für Extraterrestriche Physik (MPE), 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), Starfire Optical Range, Directed Energy Directorate, Air Force Research Laboratory, Kirtland AFB, Astronomical Institute, Charles University, European Southern Observatory, Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), European Space Astronomy Centre, Tampere University of Technology [Tampere] ( TUT ), Southwest Research Institute [Boulder] ( SwRI ), Max-Planck-Institut für Extraterrestrische Physik ( MPE ), 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'Etudes Spatiales ( CNES ), Starfire Optical Range [AFRL] ( SOR ), United States Air Force ( USAF ), Institut de Mécanique Céleste et de Calcul des Ephémérides ( IMCCE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), Charles University [Prague], Max-Planck-Institut für Astronomie ( MPIA ), European Southern Observatory ( ESO ), and Max-Planck-Institut für Sonnensystemforschung ( MPS )

Subjects
(21) Lutetia, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Astrophysics, 01 natural sciences, Imaging data, Occultation, Space exploration, Geometric albedo, 0103 physical sciences, Rosetta, KOALA, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing, Earth and Planetary Astrophysics (astro-ph.EP), biology, Spacecraft, Asteroid, Disk-resolved imaging, Astronomy and Astrophysics, Space and Planetary Science, business.industry, Astronomy, Observable, biology.organism_classification, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [ PHYS.ASTR.EP ] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Earth and Planetary Astrophysics, Osiris, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Geology, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present a comparison of our results from ground-based observations of asteroid (21) Lutetia with imaging data acquired during the flyby of the asteroid by the ESA Rosetta mission. This flyby provided a unique opportunity to evaluate and calibrate our method of determination of size, 3-D shape, and spin of an asteroid from ground-based observations. We present our 3-D shape-modeling technique KOALA which is based on multi-dataset inversion. We compare the results we obtained with KOALA, prior to the flyby, on asteroid (21) Lutetia with the high-spatial resolution images of the asteroid taken with the OSIRIS camera on-board the ESA Rosetta spacecraft, during its encounter with Lutetia. The spin axis determined with KOALA was found to be accurate to within two degrees, while the KOALA diameter determinations were within 2% of the Rosetta-derived values. The 3-D shape of the KOALA model is also confirmed by the spectacular visual agreement between both 3-D shape models (KOALA pre- and OSIRIS post-flyby). We found a typical deviation of only 2 km at local scales between the profiles from KOALA predictions and OSIRIS images, resulting in a volume uncertainty provided by KOALA better than 10%. Radiometric techniques for the interpretation of thermal infrared data also benefit greatly from the KOALA shape model: the absolute size and geometric albedo can be derived with high accuracy, and thermal properties, for example the thermal inertia, can be determined unambiguously. We consider this to be a validation of the KOALA method. Because space exploration will remain limited to only a few objects, KOALA stands as a powerful technique to study a much larger set of small bodies using Earth-based observations., 15 pages, 8 figures, 2 tables, accepted for publication in P&SS

Published
2011

44. Continued activity in P/2013 P5 PANSTARRS; Unexpected comet, rotational break-up, or rubbing binary asteroid?

Author

Hainaut, O. R., Boehnhardt, H., Snodgrass, C., Meech, K. J., Deller, J., Gillon, M., Jehin, E., Kuehrt, E., Lowry, S. C., Manfroid, J., Micheli, M., Mottola, S., Opitom, C., Vincent, J.-B., and Wainscoat, R.

Subjects
COMETS, ASTEROID belt, IMAGE processing, ASTEROIDS, BINARY stars, COMETARY orbits
Abstract

The object P/2013 P5 PANSTARRS was discovered in August 2013, displaying a cometary tail, but its orbital elements indicated that it was a typical member of the inner asteroid main belt. We monitored the object from 2013 August 30 until 2013 October 05 using the CFHT 3.6 m telescope (Mauna Kea, HI), the NTT (ESO, La Silla), the CA 1.23 m telescope (Calar Alto), the Perkins 1.8m (Lowell) and the 0.6 m TRAPPIST telescope (La Silla). We measured its nuclear radius to be r ≲ 0.25-0.29 km, and its colours g' - r' = 0.58 ± 0.05 and r' - i' = 0.23 ± 0.06, typical for an S-class asteroid, as expected for an object in the inner asteroid belt and in the vicinity of the Flora collisional family. We failed to detect any rotational light curve with an amplitude <0.05 mag and a double-peaked rotation period <20 h. The evolution of the tail during the observations was as expected from a dust tail. A detailed Finson-Probstein analysis of deep images acquired with the NTT in early September and with the CFHT in late September indicated that the object was active since at least late January 2013 until the time of the latest observations in 2013 September, with at least two peaks of activity around 2013 June 14 ± 10 d and 2013 July 22 ± 3 d. The changes of activity level and the activity peaks were extremely sharp and short, shorter than the temporal resolution of our observations (~1 d). The dust distribution was similar during these two events, with dust grains covering at least the 1-1000 μm range. The total mass ejected in grains <1 mm was estimated to be 3.0 × 106 kg and 2.6 × 107 kg around the two activity peaks. Rotational disruption cannot be ruled out as the cause of the dust ejection. We also propose that the components of a contact binary might gently rub and produce the observed emission. Volatile sublimation might also explain what appears as cometary activity over a period of 8 months. However, while main belt comets best explained by ice sublimation are found in the outskirts of the main belt, where water ice is believed to be able to survive buried in moderately large objects for the age of the solar system deeply, the presence of volatiles in an object smaller than 300 m in radius would be very surprising in the inner asteroid belt. [ABSTRACT FROM AUTHOR]

Published
2014
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45. Rotating dust particles in the coma of comet 67P/Churyumov-Gerasimenko

Author

A'Hearn, M. F., Wenzel, K. P., Sierks, H., Guettler, C., Marzari, F., Rickman, H., Kueppers, M., Cremonese, G., Naletto, G., Keller, H. U., Michalik, H., Debei, S., Lara, L., Rotundi, A., Bodewits, D., Della Corte, V., Barbieri, C., Vincent, J. B., Agarwal, J., Lazzarin, M., Sabau, L., Barucci, M. A., Ivanovski, S. L., Thomas, Nicolas, Jorda, L., Bertini, I., Lopez-Moreno, J. J., Rodrigo, R., Tubiana, C., Lamy, P. L., Davidsson, B., Hviid, S. F., Kramm, R., De Cecco, M., Knollenberg, J., Bertaux, J. L., Koschny, D., Kuehrt, E., Oklay, N., Fornasier, S., Gutierrez, P., Zakharov, V., Fulle, M., Ip, W., Groussin, O., and Da Deppo, V.

Subjects
13. Climate action, 530 Physics, 520 Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Context. During September and October 2014, the OSIRIS cameras onboard the ESA Rosetta mission detected millions of single particles. Many of these dust particles appear as long tracks (due to both the dust proper motion and the spacecraft motion during the exposure time) with a clear brightness periodicity. Aims. We interpret the observed periodic features as a rotational and translational motion of aspherical dust grains. Methods. By counting the peaks of each track, we obtained statistics of a rotation frequency. We compared these results with the rotational frequency predicted by a model of aspherical dust grain dynamics in a model gas flow. By testing many possible sets of physical conditions and grain characteristics, we constrained the rotational properties of dust grains. Results. We analyzed on the motion of rotating aspherical dust grains with different cross sections in flow conditions corresponding to the coma of 67P/Churyumov-Gerasimenko qualitatively and quantitatively. Based on the OSIRIS observations, we constrain the possible physical parameters of the grains.

46. Gravitational slopes, geomorphology, and material strengths of the nucleus of comet 67P/Churyumov-Gerasimenko from OSIRIS observations

Author

Lazzarin, M., Hviid, S., Jorda, L., Bertini, I., Auger, A. T., Agarwal, J., Thomas, Nicolas, Cremonese, G., Capanna, C., Pommerol, Antoine, A'Hearn, M. F., Koschny, D., Lamy, P., Gutierrez, P. J., Pajola, M., Debei, S., De Cecco, M., Marchi, S., Scholten, F., Keller, U., Davidsson, B., Vincent, J. B., Marzari, F., Rodrigo, R., Knollenberg, J., Fulle, M., Barucci, M. A., Preusker, F., Michalik, H., Sierks, H., Guettler, C., Bertaux, J. L., Kueppers, M., Kramm, J. R., Da Deppo, V., Gaske, R., Tubiana, C., Massironi, M., Groussin, O., Huettig, C., Naletto, G., Fornasier, S., Oklay, N., Ip, W. H., Kuehrt, E., Boudreault, S., Elmaarry, Mohamed Ramy, Toth, I., Rickman, H., Barbieri, C., Lopez Moreno, J. J., and Lara, L. M.

Subjects
13. Climate action, 530 Physics, 520 Astronomy
Abstract

Aims. We study the link between gravitational slopes and the surface morphology on the nucleus of comet 67P/Churyumov-Gerasimenko and provide constraints on the mechanical properties of the cometary material (tensile, shear, and compressive strengths). Methods. We computed the gravitational slopes for five regions on the nucleus that are representative of the different morphologies observed on the surface (Imhotep, Ash, Seth, Hathor, and Agilkia), using two shape models computed from OSIRIS images by the stereo-photoclinometry (SPC) and stereo-photogrammetry (SPG) techniques. We estimated the tensile, shear, and compressive strengths using different surface morphologies (overhangs, collapsed structures, boulders, cliffs, and Philae's footprint) and mechanical considerations. Results. The different regions show a similar general pattern in terms of the relation between gravitational slopes and terrain morphology: i) low-slope terrains (0-20 degrees) are covered by a fine material and contain a few large (>10 m) and isolated boulders; ii) intermediate-slope terrains (20-45 degrees) are mainly fallen consolidated materials and debris fields, with numerous intermediate-size boulders from

47. Are fractured cliffs the source of cometary dust jets? Insights from OSIRIS/Rosetta at 67P/Churyumov-Gerasimenko

Author

Hu, X., De Cecco, M., Lamy, P. L., Rickman, H., Lopez Moreno, J. J., Sierks, H., Rodrigo, R., Lowry, S., Keller, H. U., Moreno, F., Davidsson, B., Toth, I., Bodewits, D., Barucci, M. A., Lara, L. M., Lazzarin, M., Kueppers, M., Vincent, J. B., Gutierrez, P. J., Guettler, C., Tubiana, C., Barbieri, C., Da Deppo, V., Elmaarry, Mohamed Ramy, Kuehrt, E., Ip, W. H., Koschny, D., Bertaux, J. L., Kramm, J. R., Massironi, M., Gutierrez-Marquez, P., Mottola, S., Bertini, I., Cremonese, G., Oklay, N., Pajola, M., Fornasier, S., A'Hearn, M. F., Marzari, F., Besse, S., Lin, Z. Y., Scholten, F., Hofmann, M., Fulle, M., Hoefner, S., Groussin, O., Naletto, G., Knollenberg, J., Shi, X., Debei, S., Preusker, F., Kovacs, G., Hviid, S. F., Jordan, L., and Thomas, Nicolas

Subjects
13. Climate action, 530 Physics, 520 Astronomy
Abstract

Context. Dust jets (i.e., fuzzy collimated streams of cometary material arising from the nucleus) have been observed in situ on all comets since the Giotto mission flew by comet 1P/Halley in 1986, and yet their formation mechanism remains unknown. Several solutions have been proposed involving either specific properties of the active areas or the local topography to create and focus the gas and dust flows. While the nucleus morphology seems to be responsible for the larger features, high resolution imagery has shown that broad streams are composed of many smaller jets (a few meters wide) that connect directly to the nucleus surface. Aims. We monitored these jets at high resolution and over several months to understand what the physical processes are that drive their formation and how this affects the surface. Methods. Using many images of the same areas with different viewing angles, we performed a 3-dimensional reconstruction of collimated jets and linked them precisely to their sources on the nucleus. Results. We show here observational evidence that the northern hemisphere jets of comet 67P/Churyumov-Gerasimenko arise from areas with sharp topographic changes and describe the physical processes involved. We propose a model in which active cliffs are the main source of jet-like features and therefore of the regions eroding the fastest on comets. We suggest that this is a common mechanism taking place on all comets.

48. Characterization of the Abydos region through OSIRIS high-resolution images in support of CIVA measurements

Author

Debei, S., Elmaarry, Mohamed Ramy, Marzari, F., Keller, H. U., Sierks, H., Guettler, C., Preusker, F., Bertini, I., Pajola, M., A'Hearn, M. F., Kramm, J. R., Fulle, M., Bertaux, J. L., Bibring, J. P., Kuehrt, E., Barucci, M. A., Gutierrez, P. J., La Forgia, F., Lucchetti, A., Cremonese, G., Da Deppo, V., Lamy, P., Mottola, S., Davidsson, B., Lopez Moreno, J. J., Oklay, N., Kueppers, M., Agarwal, J., Rickman, H., Vincent, J. B., De Cecco, M., Scholten, F., Ip, W. H., Lara, L. M., Tubiana, C., Groussin, O., Lazzarin, M., Jorda, L., Barbieri, C., Thomas, Nicolas, Hviid, S. F., Naletto, G., Koschny, D., Fornasier, S., Rodrigo, R., Massironi, M., Poulet, F., and Knollenberg, J.

Subjects
13. Climate action, 530 Physics, 520 Astronomy
Abstract

Context. On 12 November 2014, the European mission Rosetta delivered the Philae lander on the nucleus of comet 67P /Churyumov-Gerasimenko (67P). After the first touchdown, the lander bounced three times before finally landing at a site named Abydos. Aims. We provide a morphologically detailed analysis of the Abydos landing site to support Philae's measurements and to give context for the interpretation of the images coming from the Comet Infrared and Visible Analyser (CIVA) camera system onboard the lander. Methods. We used images acquired by the OSIRIS Narrow Angle Camera (NAC) on 6 December 2014 to perform the analysis of the Abydos landing site, which provided the geomorphological map, the gravitational slope map, the size-frequency distribution of the boulders. We also computed the albedo and spectral reddening maps. Results. The morphological analysis of the region could suggest that Philae is located on a primordial terrain. The Abydos site is surrounded by two layered and fractured outcrops and presents a 0.02 km(2) talus deposit rich in boulders. The boulder size frequency distribution gives a cumulative power-law index of 4.0 + 0.3/0.4, which is correlated with gravitational events triggered by sublimation and /or thermal fracturing causing regressive erosion. The average value of the albedo is 5.8% at lambda(1) = 480.7 nm and 7.4% at lambda(2) = 649.2 nm, which is similar to the global albedos derived by OSIRIS and CIVA, respectively.

49. Spectrophotometric properties of the nucleus of comet 67P/Churyumov-Gerasimenko from the OSIRIS instrument onboard the ROSETTA spacecraft

Author

Kramm, R., Koschny, D., Scholten, F., Thomas, Nicolas, Feller, C., Jorda, L., Shi, X., Lara, L., Vincent, J. B., Kueppers, M., Lamy, P. L., Rickman, H., Lazzarin, M., Pommerol, Antoine, Guettler, C., Davidsson, B., Preusker, F., Sierks, H., Da Deppo, V., Oklay, N., Hviid, S. F., A'Hearn, M. F., Fornasier, S., Knollenberg, J., Kovacs, G., Barucci, M. A., Rodrigo, R., Tubiana, C., Pajola, M., Fulle, M., Lopez Moreno, J. J., Kuehrt, E., Debei, S., Bertaux, J. L., Hasselmann, P. H., Barbieri, C., Gutierrez, P. J., Marzari, F., Keller, H. U., Agarwal, J., Snodgrass, C., La Forgia, F., De Cecco, M., Michalik, H., Groussin, O., Matz, K. D., Cremonese, G., Leyrat, C., Bertini, I., Naetto, G., Ip, W., Mottola, S., Besse, S., and Moreno, F.

Subjects
13. Climate action, 530 Physics, 520 Astronomy
Abstract

Context. The Rosetta mission of the European Space Agency has been orbiting the comet 67P/Churyumov-Gerasimenko (67P) since August 2014 and is now in its escort phase. A large complement of scientific experiments designed to complete the most detailed study of a comet ever attempted are onboard Rosetta. Aims. We present results for the photometric and spectrophotometric properties of the nucleus of 67P derived from the OSIRIS imaging system, which consists of a Wide Angle Camera (WAC) and a Narrow Angle Camera (NAC). The observations presented here were performed during July and the beginning of August 2014, during the approach phase, when OSIRIS was mapping the surface of the comet with several filters at different phase angles (1.3 degrees-54 degrees). The resolution reached up to 2.1 m/px. Methods. The OSIRIS images were processed with the OSIRIS standard pipeline, then converted into I/F. radiance factors and corrected for the illumination conditions at each pixel using the Lommel-Seeliger disk law. Color cubes of the surface were produced by stacking registered and illumination-corrected images. Furthermore, photometric analysis was performed both on disk-averaged photometry in several filters and on disk-resolved images acquired with the NAC orange filter, centered at 649 ran, using Hapke modeling. Results. The disk-averaged phase function of the nucleus of 67P shows a strong opposition surge with a G parameter value of -0.13 +/- 0.01 in the HG system formalism and an absolute magnitude H-v(1, 1, 0) = 15.74 +/- 0.02 mag. The integrated spectrophotometry in 20 filters covering the 250-1000 nm wavelength range shows a red spectral behavior, without clear absorption bands except for a potential absorption centered at similar to 290 rim that is possibly due to SO2 ice. The nucleus shows strong phase reddening, with disk-averaged spectral slopes increasing from 11%/( 100 nm) to 16%/(100 nm) in the 1.3 degrees-54 degrees phase angle range. The geometric albedo of the comet is 6.5 +/- 0.2% at 649 nm, with local variations of up to similar to 16% in the Hapi region. From the disk-resolved images we computed the spectral slope together with local spectrophotometry and identified three distinct groups of regions (blue, moderately red, and red). The Hapi region is the brightest, the bluest in term of spectral slope, and the most active surface on the comet. Local spectrophotometry shows an enhancement of the flux in the 700-750 nm that is associated with coma emissions.

50. Geomorphology and spectrophotometry of Philae's landing site on comet 67P/Churyumov-Gerasimenko

Author

Davidsson, B., Lara, L. M., Oklay, N., Cremonese, G., Tubiana, C., Kuehrt, E., Giacomini, L., Gutierrez, P. J., Hall, I., Besse, S., Bodewits, D., Knollenberg, J., Lamy, P., De Cecco, M., Vincent, J. B., Naletto, G., Lopez Moreno, J. J., Guettler, C., Keller, H. U., Mottola, S., Fornasier, S., Koschny, D., Sierks, H., Rickman, H., Simioni, E., Hviid, S. F., Kramm, J. R., Jorda, L., A'Hearn, M. F., Elmaarry, Mohamed Ramy, Preusker, F., Auger, A. T., Kueppers, M., Barbieri, C., Groussin, O., Ip, W. H., Lazzarin, M., Pommerol, Antoine, Agarwal, J., Marzari, F., Ferri, F., Da Deppo, V., Rodrigo, R., Barucci, M. A., Scholten, F., La Forgia, F., Debei, S., Bertaux, J. L., Fulle, M., Pajola, M., Thomas, Nicolas, Michalik, H., Bertini, I., Magrin, S., and Massironi, M.

Subjects
13. Climate action, 530 Physics, 520 Astronomy, 620 Engineering
Abstract

Context. On 12 November 2014 the European mission Rosetta succeeded in delivering a lander, named Philae, on the surface of one of the smallest, low-gravity and most primitive bodies of the solar system, the comet 67P/Churyumov-Gerasimenko (67P). Aims. The aim of this paper is to provide a comprehensive geomorphological and spectrophotometric analysis of Philae's landing site (Agilkia) to give an essential framework for the interpretation of its in situ measurements. Methods. OSIRIS images, coupled with gravitational slopes derived from the 3D shape model based on stereo-photogrammetry were used to interpret the geomorphology of the site. We adopted the Hapke model, using previously derived parameters, to photometrically correct the images in orange filter (649.2 nm). The best approximation to the Hapke model, given by the Akimov parameter-less function, was used to correct the reflectance for the effects of viewing and illumination conditions in the other filters. Spectral analyses on coregistered color cubes were used to retrieve spectrophotometric properties. Results. The landing site shows an average normal albedo of 6.7% in the orange filter with variations of similar to 15% and a global featureless spectrum with an average red spectral slope of 15.2%/100 nm between 480.7 nm (blue filter) and 882.1 nm (near-IR filter). The spatial analysis shows a well-established correlation between the geomorphological units and the photometric characteristics of the surface. In particular, smooth deposits have the highest reflectance a bluer spectrum than the outcropping material across the area. Conclusions. The featureless spectrum and the redness of the material are compatible with the results by other instruments that have suggested an organic composition. The observed small spectral variegation could be due to grain size effects. However, the combination of photometric and spectral variegation suggests that a compositional differentiation is more likely. This might be tentatively interpreted as the effect of the efficient dust-transport processes acting on 67P. High-activity regions might be the original sources for smooth fine-grained materials that then covered Agilkia as a consequence of airfall of residual material. More observations performed by OSIRIS as the comet approaches the Sun would help interpreting the processes that work at shaping the landing site and the overall nucleus.

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