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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 1.

Object’s bulk density against equivalent sphere diameter. All lines show the relation for dust aggregates (Equation (4)). The blue and orange lines show ice and silicate dust aggregates, whose material densities are 1.45 and 2.65 g cm−3, respectively. The solid and dashed lines show monomer radii of 0.1 and 1.0 μm, respectively. The markers with error bars show MBAs (very light gray dots), NEAs (light gray dots), TNOs (medium gray circles; Table 2), and comets (dark gray triangles; Table 3). The black crosses show a comet (67P; Table 3) and three asteroids (Itokawa, Bennu, and Ryugu; Table 4) that are investigated by in situ measurements.

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