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.
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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.
|Title:||Observations of Comet 9P/Tempel 1 around the Deep Impact event by the OSIRIS cameras onboard Rosetta|
|Date:||13 April 2006|
|Journal or Publication Title:||Icarus: International Journal of Solar System Studies|
|In ISI Web of Science:||Yes|
|Page Range:||pp. 87-103|
|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)|
|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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