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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.

Item URL in elib:https://elib.dlr.de/43596/
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 AuthorsAuthors ORCID iD
Keller, H.U.Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, GermanyUNSPECIFIED
Küppers, M.Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, GermanyUNSPECIFIED
Fornasier, S.Dipartimento di Astronomia and CISAS, Università di Padova, Padova, ItalyUNSPECIFIED
Gutierrez, P. J.Instituto de Astrofísica de Andalucía – CSIC, Granada, SpainUNSPECIFIED
Hviid, S. F.Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, GermanyUNSPECIFIED
Jorda, L.Laboratoire d'Astrophysique de Marseille, Marseille, FranceUNSPECIFIED
Knollenberg, J.UNSPECIFIEDUNSPECIFIED
Lowry, S. C.Queen's University, Astrophysics Research Centre, Department of Physics and Astronomy, Belfast, United KingdomUNSPECIFIED
Rengel, M.Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, GermanyUNSPECIFIED
Bertini, I.Dipartimento di Astronomia and CISAS, Università di Padova, Padova, ItalyUNSPECIFIED
Cremonese, G.INAF – Astronomical Observatory of Padova, Padova, ItalyUNSPECIFIED
Ip, W.-H.Institute of Space Science, National Central University, Chung Li, TaiwanUNSPECIFIED
Koschny, D.Research and Scientific Support Department of the European Space Agency, ESTEC, Noordwijk, The NetherlandsUNSPECIFIED
Kramm, R.Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, GermanyUNSPECIFIED
Kührt, E.UNSPECIFIEDUNSPECIFIED
Lara, L.-M.Instituto de Astrofísica de Andalucía – CSIC, Granada, SpainUNSPECIFIED
Sierks, H.Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, GermanyUNSPECIFIED
Thomas, N.Physikalisches Institut, Abteilung Weltraumforschung und Planetologie, Universität Bern, Bern, SwitzerlandUNSPECIFIED
Barbieri, C.Dipartimento di Astronomia and CISAS, Università di Padova, Padova, ItalyUNSPECIFIED
Lamy, Ph.Laboratoire d'Astrophysique de Marseille, Marseille, FranceUNSPECIFIED
Rickman, H.Department of Astronomy a. Space Physics, UppsalaUNSPECIFIED
Rodrigo, R.Instituto de Astrofísica de Andalucía – CSIC, Granada, SpainUNSPECIFIED
A´Hearn, M. F.Department of Astronomy, University of Maryland, USAUNSPECIFIED
Angrilli, F.Dipartimento di Ingegneria Meccanica, PadovaUNSPECIFIED
Barucci, M.-A.Observatoire de Paris,Section de Meudon, Meudon, FranceUNSPECIFIED
Bertaux, J.-L.Service d'Aéronomie du CNRS, Verrières-le-Buisson, FranceUNSPECIFIED
da Deppo, V.CNR-INFM Luxor, Padova, ItalyUNSPECIFIED
Davidsson, B. J. R.Department of Astronomy a. Space Physics, UppsalaUNSPECIFIED
de Cecco, M.Dipartimento di Ingegneria Meccanica, Padova; Universita degli Studi di TrentoUNSPECIFIED
Debei, St.Facultà Ingegneria, Università degli Studi di Trento, Trento, ItalyUNSPECIFIED
Fulle, M.INAF – Osservatorio Astronomico de Trieste, Trieste, ItalyUNSPECIFIED
Gliem, F.Institutut für Datentechnik und Kommunikationsnetzt, Technische Universität Braunschweig, Braunschweig, GermanyUNSPECIFIED
Groussin, O.Department of Astronomy, University of Maryland, USAUNSPECIFIED
Lopez Moreno, J. J.Instituto de Astrofísica de Andalucía – CSIC, Granada, SpainUNSPECIFIED
Marzari, F.Department of Physics “G. Galilei", Padova, ItalyUNSPECIFIED
Naletto, G.DEIDepartment of Information Engineering (DEI), University of Padova, Padova, ItalyUNSPECIFIED
Sabau, L.Instituto Nacional de Técnica Aerospacial, Torrejon de Ardoz (Madrid), SpainUNSPECIFIED
Andrés, S. A.Universidad Politécnica de Madrid, Instituto Ignacio D'Riva, Madrid, SpainUNSPECIFIED
Wenzel, K.-P.Research and Scientific Support Department of the European Space Agency, ESTEC, Noordwijk, The NetherlandsUNSPECIFIED
Date:13 April 2006
Journal or Publication Title:Icarus: International Journal of Solar System Studies
Refereed publication:Yes
Open Access:No
Gold Open Access:No
In SCOPUS:No
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: Kührt, Dr.rer.nat. Ekkehard
Deposited On:14 Mar 2007
Last Modified:14 Jan 2010 23:16

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