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

Keller, H.U. and Küppers, M. and Fornasier, S. and Gutierrez, P. J. and Hviid, S. F. and Jorda, L. and Knollenberg, J. and Lowry, S. C. and Rengel, M. and Bertini, I. and Cremonese, G. and Ip, W.-H. and Koschny, D. and Kramm, R. and Kührt, E. and Lara, L.-M. and Sierks, H. and Thomas, N. and Barbieri, C. and Lamy, Ph. and Rickman, H. and Rodrigo, R. and A´Hearn, M. F. and Angrilli, F. and Barucci, M.-A. and Bertaux, J.-L. and da Deppo, V. and Davidsson, B. J. R. and de Cecco, M. and Debei, St. and Fulle, M. and Gliem, F. and Groussin, O. and Lopez Moreno, J. J. and Marzari, F. and Naletto, G. and Sabau, L. and Andrés, S. A. and Wenzel, K.-P. (2006) Observations of Comet 9P/Tempel 1 around the Deep Impact event by the OSIRIS cameras onboard Rosetta. Icarus: International Journal of Solar System Studies, 187 (1), pp. 87-103. Elsevier. DOI: doi:10.1016/j.icarus.2006.09.023. ISSN 0019-1035.

Full text not available from this repository.

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 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 no new coma structures created by the impact. Instead, material from the impact cloud may have enhanced existing structures. Most of the material moves with ~200 m/s and is preferably pushed into existing coma structures of Tempel 1. The light curve of the comet after the impact and the amount of material leaving the comet (4.5-9 x 106 kg of water ice and a presumably larger amount of dust) suggest that the impact ejecta were quickly accelerated by collisions with gas molecules. Much of the material left the comet in the form of icy grains which sublimated and fragmented within the first hour after the impact. Na D-line emission was detected in the impact ejecta. If the source of the sodium is evaporation of hot dust grains, approximately 3800 kg of hot dust have been created in the impact, consistent with measurements from the Deep Impact spacecraft. The impact ejecta are quickly accelerated by gas in the near-nucleus region. The motion of the ejecta cannot be described by ballistic trajectories. Therefore, density and tensile strength of the nucleus of Tempel 1 cannot be determined with models using ballistic ejection of particles.

Document Type:Article
Title:Observations of Comet 9P/Tempel 1 around the Deep Impact event by the OSIRIS cameras onboard Rosetta
Authors:
AuthorsInstitution or Email of Authors
Keller, H.U.Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, Germany
Küppers, M.Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, Germany
Fornasier, S.Dipartimento di Astronomia and CISAS, Università di Padova, Padova, Italy
Gutierrez, P. J.Instituto de Astrofísica de Andalucía – CSIC, Granada, Spain
Hviid, S. F.Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, Germany
Jorda, L.Laboratoire d'Astrophysique de Marseille, Marseille, France
Knollenberg, J.UNSPECIFIED
Lowry, S. C.Queen's University, Astrophysics Research Centre, Department of Physics and Astronomy, Belfast, United Kingdom
Rengel, M.Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, Germany
Bertini, I.Dipartimento di Astronomia and CISAS, Università di Padova, Padova, Italy
Cremonese, G.INAF – Astronomical Observatory of Padova, Padova, Italy
Ip, W.-H.Institute of Space Science, National Central University, Chung Li, Taiwan
Koschny, D.Research and Scientific Support Department of the European Space Agency, ESTEC, Noordwijk, The Netherlands
Kramm, R.Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, Germany
Kührt, E.UNSPECIFIED
Lara, L.-M.Instituto de Astrofísica de Andalucía – CSIC, Granada, Spain
Sierks, H.Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, Germany
Thomas, N.Physikalisches Institut, Abteilung Weltraumforschung und Planetologie, Universität Bern, Bern, Switzerland
Barbieri, C.Dipartimento di Astronomia and CISAS, Università di Padova, Padova, Italy
Lamy, Ph.Laboratoire d'Astrophysique de Marseille, Marseille, France
Rickman, H.Department of Astronomy a. Space Physics, Uppsala
Rodrigo, R.Instituto de Astrofísica de Andalucía – CSIC, Granada, Spain
A´Hearn, M. F.Department of Astronomy, University of Maryland, USA
Angrilli, F.Dipartimento di Ingegneria Meccanica, Padova
Barucci, M.-A.Observatoire de Paris,Section de Meudon, Meudon, France
Bertaux, J.-L.Service d'Aéronomie du CNRS, Verrières-le-Buisson, France
da Deppo, V.CNR-INFM Luxor, Padova, Italy
Davidsson, B. J. R.Department of Astronomy a. Space Physics, Uppsala
de Cecco, M.Dipartimento di Ingegneria Meccanica, Padova; Universita degli Studi di Trento
Debei, St.Facultà Ingegneria, Università degli Studi di Trento, Trento, Italy
Fulle, M.INAF – Osservatorio Astronomico de Trieste, Trieste, Italy
Gliem, F.Institutut für Datentechnik und Kommunikationsnetzt, Technische Universität Braunschweig, Braunschweig, Germany
Groussin, O.Department of Astronomy, University of Maryland, USA
Lopez Moreno, J. J.Instituto de Astrofísica de Andalucía – CSIC, Granada, Spain
Marzari, F.Department of Physics “G. Galilei", Padova, Italy
Naletto, G.DEIDepartment of Information Engineering (DEI), University of Padova, Padova, Italy
Sabau, L.Instituto Nacional de Técnica Aerospacial, Torrejon de Ardoz (Madrid), Spain
Andrés, S. A.Universidad Politécnica de Madrid, Instituto Ignacio D'Riva, Madrid, Spain
Wenzel, K.-P.Research and Scientific Support Department of the European Space Agency, ESTEC, Noordwijk, The Netherlands
Date:13 April 2006
Journal or Publication Title:Icarus: International Journal of Solar System Studies
Refereed publication:Yes
In ISI Web of Science:Yes
Volume:187
DOI:doi:10.1016/j.icarus.2006.09.023
Page Range:pp. 87-103
Publisher:Elsevier
ISSN:0019-1035
Status:Published
Keywords:comets, impact processes, surfaces, dust, Osiris
HGF - Research field:Aeronautics, Space and Transport (old)
HGF - Program:Space (old)
HGF - Program Themes:W EW - Erforschung des Weltraums
DLR - Research area:Space
DLR - Program:W EW - Erforschung des Weltraums
DLR - Research theme (Project):W - Projekt ROSETTA Instrumente (old)
Location: Berlin-Adlershof
Institutes and Institutions:Institute of Planetary Research > Asteroids and Comets
Deposited By: Dr.rer.nat. Ekkehard Kührt
Deposited On:14 Mar 2007
Last Modified:14 Jan 2010 23:16

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