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The Bulk Densities of Small Solar System Bodies as a Probe of Planetesimal Formation

  • Authors: Misako Tatsuuma, Akimasa Kataoka, Hidekazu Tanaka, Tristan Guillot

Misako Tatsuuma et al 2024 The Astrophysical Journal 974 .

  • Provider: AAS Journals

Caption: Figure 6.

Top: upper limit of pressure (Equation (C1)) of dust aggregates below which monomer disruption can be neglected as a function of monomer radius. The blue and orange lines are for ice and silicate, whose material densities are 1.45 and 2.65 g cm−3, respectively. The parameters except for the material density are listed in Table 1. Bottom: upper limit of diameter of dust aggregates (Equation (C3)).

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