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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 3.

Top: internal density profiles of ice dust aggregates (solid lines) when r m = 0.1 μm and ρ c = 0.35 (left) and 0.002 g cm−3 (right). The other parameters except for the material density are listed in Table 1. We assume that each ice monomer has a silicate core whose mass equals the mass of an ice mantle, so that ρ m = 1.45 g cm−3. The orange dotted lines show polytropes with a constant polytropic index of 0.5. The dashed lines show the numerically obtained bulk densities. The green dotted lines show the bulk densities obtained analytically from Equation (4). Bottom: internal pressure profiles.

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