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  Modelling the large particle environment of comet 67P/Churyumov–Gerasimenko

Agarwal, J., Müller, M., Böhnhardt, H., & Grün, E. (2006). Modelling the large particle environment of comet 67P/Churyumov–Gerasimenko. Advances in Space Research, 38(9), 2049-2053. doi:10.1016/j.asr.2005.04.046.

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Item Permalink: http://hdl.handle.net/11858/00-001M-0000-0011-86D0-B Version Permalink: http://hdl.handle.net/11858/00-001M-0000-0011-86D1-9
Genre: Journal Article

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 Creators:
Agarwal, Jessica1, Author              
Müller, M.2, Author              
Böhnhardt, H.3, Author
Grün, Eberhard1, Author              
Affiliations:
1Ralf Srama - Heidelberg Dust Group, Research Groups, MPI for Nuclear Physics, Max Planck Society, ou_907558              
2Division Prof. Dr. Manfred Lindner, MPI for Nuclear Physics, Max Planck Society, ou_904549              
3European Space Operations Centre, Robert-Bosch-Str. 5, 64293 Darmstadt, Germany Hawaii Institute of Geophysics and Planetology, University of Hawaii, 1680 East West Road, POST 512c, Honolulu, HI 96822, USA, ou_persistent22              

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Free keywords: Comet dust; Comet tail; Comet trail; Trail model; Large particles; 67P; Churyumov–Gerasimenko
 Abstract: A method is presented to simulate images of a cometary dust trail in consistency with observed gas and dust production rates. It is also applicable to dust tails including neckline and antitail phenomena. Our main objective is to analyse the amount of mm-sized and larger particles within a given image. These are interesting to us because their emission by comets may constitute a major source of interplanetary dust. The model is applied to 67P/Churyumov–Gerasimenko, the target of ESA’s Rosetta mission. The employed parameters are consistent with a hydrodynamic coma model. Dust emitted during all apparitions of 67P since the Jupiter encounter in 1959 is taken into account. We compare simulated images with two images taken in May 2003 and April 2004. Both of these show a bright feature close to the projected orbit of the comet. We analyse the simulated images with respect to the age of the dust in this feature. We find that, within our model, the feature in 2003 is dominated by particles emitted during the same apparition. For 2004 we estimate that 25% of the intensity in the bright feature can be attributed to dust emitted during previous apparitions and 29% to particles emitted at true anomalies of (180 ± 5)° before observation. Concerning the sizes of dust grains in the bright feature, we find that in 2003, particles with radii between about 10 μm and 1 cm contribute nearly equally to the total intensity. In 2004 however, the structure is dominated by particles having sizes of 100 μm to 1 mm.

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Language(s): eng - English
 Dates: 2006
 Publication Status: Published in print
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Method: Peer
 Identifiers: eDoc: 276613
DOI: 10.1016/j.asr.2005.04.046
 Degree: -

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Title: Advances in Space Research
Source Genre: Journal
 Creator(s):
Affiliations:
Publ. Info: -
Pages: - Volume / Issue: 38 (9) Sequence Number: - Start / End Page: 2049 - 2053 Identifier: -