Numerical simulations of cometary dust tail brightnesses

Details Numerical simulations of cometary dust tail brightnesses Numerical simulations of cometary dust tail brightnesses

Nov 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.500..597m&link_type=abstract

In: Proceedings of Asteroids, Comets, Meteors - ACM 2002. International Conference, 29 July - 2 August 2002, Berlin, Germany. Ed

Computer Science

Comets, Dust Tail, Numerical Simulations

Scientific paper

A numerical method to compute cometary dust tail brightnesses has been developed. The method, analogous in many ways to the inverse Monte Carlo method proposed by Fulle (1989), has been applied to one image of comet C/1999 T1 McNaught-Hartley. The time and size dependence of the particle terminal velocities, the size distribution functions, and the dependence with time of the power index of the size distribution have been derived. The best fits to the observed isophote field are obtained for highly anisotropic dust grain ejection velocities. The dependence with time of the power index of the size distribution of grains show small values. These results are in line with previous results by Fulle relating systematic decrease of size distribution power index and dust ejection isotropy as the comet age increases.

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