Dynamical Modeling of the Deep Impact Dust Ejecta Cloud View Full Text


Ontology type: schema:Chapter      Open Access: True


Chapter Info

DATE

2009-01-01

AUTHORS

T. Bonev , N. Ageorges , S. Bagnulo , L. Barrera , H. Böhnhardt , O. Hainaut , E. Jehin , H. U. Käufl , F. Kerber , G. LoCurto , J. Manfroid , O. Marco , E. Pantin , E. Pompei , I. Saviane , F. Selman , C. Sterken , H. Rauer , G. P. Tozzi , M. Weiler

ABSTRACT

The collision of Deep Impact with comet 9P/Tempel 1 generated a bright cloud of dust which dissipated during several days after the impact. The brightness variations of this cloud and the changes of its position and shape are governed by the physical properties of the dust grains. We use a Monte Carlo model to describe the evolution of the post-impact dust plume. The results of our dynamical simulations are compared to the data obtained with FORS2\footnote{FORS stands for \underline{FO}cal \underline{R}educer and low dispersion \underline{S}pectrograph for the \underline{V}ery \underline{L}arge \underline{T}elescope (VLT) of the \underline{E}uropean \underline{S}outhern \underline{O}bservatory (ESO).} to derive the particle size distribution and the total amount of material contained in the dust ejecta cloud. More... »

PAGES

177-184

Identifiers

URI

http://scigraph.springernature.com/pub.10.1007/978-3-540-76959-0_22

DOI

http://dx.doi.org/10.1007/978-3-540-76959-0_22

DIMENSIONS

https://app.dimensions.ai/details/publication/pub.1041168631


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