Jean-Baptiste Vincent

MPS
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COSSIM: COma Structures SIMulator

It is important to understand the formation and evolution of dust coma structures at all scales: from tiny filaments to thousands of km large structures in the coma. Inverting their apparent source location points us to areas where we can investigate the link between activity and surface.

I developped a model which simulates the emission of these dust jets from cometary nuclei and reproduces the images acquired with ground or space based observations. It accounts for the full 3D representation of the nucleus and a physical description of the dust acceleration processes in its neighborhood. COSSIM is used to: The model has been applied to constrain the spin axis orientation and activity of several targets : 73P 3-B,C, 9P, 81P, & 67P. Our results could be directly compared with in-situ measurements from Deep Impact, Stardust, Rosetta, and were confirmed by the missions.
We have analysed and simulated the activity of 67P over the last two perihelion passages, and predicted succesfully what the Rosetta mission would observe in 2014-2015.

Note: As of 2018, the full COSSIM code is NOT available publicly. I very much wish to do so, but do not have the time to clean up and document the code.

I did release in 2014 a partial version of COSSIM: the Finson-Probstein diagram.

COma Structures SIMulator (COSSIM)
COma Structures SIMulator (COSSIM)
version 0.9.7
Dust jets of comet 9P/Tempel 1
Dust jets of comet 9P/Tempel 1
COma Structures SIMulator (COSSIM)
Simulation and observation of comet ISON's tail on 2014/10/16
COma Structures SIMulator (COSSIM)
Typical small jets seen close to a nucleus surface
(left: 9P/Tempel 1 image; right: Pi-DSMC-MPS model)
COma Structures SIMulator (COSSIM)
Large scale jets seen in enhanced ground based observations
(left: 81P/Wild 2 image; right: COSSIM model)
COma Structures SIMulator (COSSIM)
Large scale jets seen in enhanced ground based observations
(left: 67P/C-G image; right: COSSIM model)