A chemical model of the coma of 19P/ Comet Borrelly

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It is generally believed that the chemical composition of cometary nuclei is representive of the most primitive material in the outer solar system as well as the end product of interstellar grains. It is therefore of great interest to study the physical structures and chemical abundances of different classes of comets ( i.e., short-period comets from the Kuiper belt and long-period comets from the Oort cloud ) so that more information on their origins and physicochemical conditions can be obtained. The encounter of Comet Borrelly by the Deep Space 1 spacecraft in September 2001 provided the first opportunity for in-situ measurements of the coma of a short-period comet. The plasma instrument (Pepe) obtained important information on the chemical abundances of the water-group and other ions as functions of distance from the cometary nucleus ( Reisenfeld et al., 2002 ). As a part of a systematic effort to build up the chemical modeling in cometary comas, molecular clouds, and interstellar medium, we will use the updated molecular abundances from ground based observations ( Hamane et al., 2002 ) to construct models of the neutral gas coma and ionosphere of Comet Borrelly during the Deep Space 1 encounter. In addition, a 2-dimensional cometary plasma flow field is adopted to examine the chemical compositional changes of the water-group ions.

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