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Rapid Formation of Gas-giant Planets via Collisional Coagulation from Dust Grains to Planetary Cores. II. Dependence on Pebble Bulk Density and Disk Temperature

  • Authors: Hiroshi Kobayashi, Hidekazu Tanaka

Hiroshi Kobayashi and Hidekazu Tanaka 2023 The Astrophysical Journal 954 .

  • Provider: AAS Journals

Caption: Figure 1.

Results of DTPS with ρ m = 10−3 g cm−3 and T 1 = 100 K. Left: (a) solid surface density, ﹩{\rm{\Delta }}{{\rm{\Sigma }}}_{{\rm{s}}}/{\rm{\Delta }}\mathrm{ln}m﹩ at t = 2.3 × 105 yr, as a function of the mass of bodies and the distance from the host star. The values of the solid surface density are shown in the color bar. Right: protoplanet mass (b) and total solid surface density (c), as a function of the distance from the host star.

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