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Extensions of the main belt collisional model
Vávra, Michael ; Brož, Miroslav (advisor) ; Scheirich, Petr (referee)
The Main Belt, the region between the orbits of Mars and Jupiter, is the home to more than 1 million asteroids. These asteroids form orbital groups, i.e., asteroid families formed by collisions; and also spectral groups (taxonomies) with different chemical composition, in particular, carbonaceous (C-types) and silicate (S-types). In this thesis, we extend the existing collisional model by finding appropriate dependence of the strength vs. size (also known as the scaling law) for these two groups. We used color indices and geometric albedos of 56 and 72 spectroscopically confirmed C- and S-types (control samples) and statistical methods on 1 065 054 asteroids, to assign C-, S- or other-types (neither C- nor S-type). This allowed us to construct the observed size-frequency distributions (SFDs) for several sub-populations constrained either in the semi-major axis (inner, middle, outer) or taxonomy (C, S, other). Then we used the Monte-Carlo code Boulder (Morbidelli et al. 2009). to compute the long-term collisional evolution (4.5 billion years) and derive synthetic SFDs. We find that the scaling laws for C- and S-types disagree with the ones proposed by Holsapple & Housen (2019). Our best-fit scaling laws indicate that S-types must be weakened below approximately 1 km compared to C-types, to explain a...
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