The stationary size distribution of main-belt asteroids: comparing recent observations with theory

Details The stationary size distribution of main-belt asteroids: comparing recent observations with theory The stationary size distribution of main-belt asteroids: comparing recent observations with theory

Nov 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.500..839d&link_type=abstract

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

Astronomy and Astrophysics

Astrophysics

Minor Planets, Sizes, Distribution

Scientific paper

Recent observations of main-belt asteroids (Jedicke and Metcalfe, 1998; Ivecic et al., 2001) help to extend theoretical understanding of collisional evolution to sub-kilometer sizes. Previous theoretical models treated the collisional evolution as a stochastic process where the outcome of pairwise collisions between asteroids is sampled using Monte-Carlo techniques (Davis et al., 1985; Davis et al., 1989; Davis et al., 1994; Campo Bagatin, 1994), leading to a time-dependent model which depends on assumption about the initial state. Alternative theoretical investigations (Dohnanyi, 1969; Williams and Wetherill, 1994) for the stationary case have been restricted to simplified functional relationships for the outcome of collisions and for the critical specific energy of catastrophic fragmentation, and in these cases a power law as analytical solution has been found. The present model solved the quasi-stationary form of the collisional balance of mass, assuming the size distribution of very large asteroids as given.

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