Growth of Jupiter: Formation in Disks of Gas and Solids and Evolution to the Present Epoch
arXiv:2009.05575 · doi:10.1016/j.icarus.2020.114087
Abstract
[Abridged] The formation of Jupiter is modeled via core-nucleated accretion, and the planet's evolution is simulated up to the present epoch. The growth from a small embryo until gas accretion overtakes solids' accretion was presented by D'Angelo et al. (Icarus 2014, 241, 298). Those calculations followed the formation for years, until the heavy-element and H/He masses were and Earth's masses (), respectively, and . The calculation is continued through the phase when , at which age, about years, the planet mass is . About years later, is approximately and . Around this epoch, the contraction of the envelope dictates gas accretion rates a few times per year, initiating the regime of disk-limited accretion, when the planet's evolution is tied to disk's evolution. Growth is continued by constructing simplified models of accretion disks that evolve through viscous diffusion, winds, and accretion on the planet. Jupiter's formation ends after - Myr, when nebula gas disperses. The young Jupiter is - times as voluminous as it is presently and thousands of times as luminous, . The heavy-element mass is . The evolution proceeds through the cooling and contraction phase, in isolation except for solar irradiation. After Myr, radius and luminosity of the planet are within % of current values. During formation, and soon thereafter, the planet exhibits features, e.g., luminosity and effective temperature, that may probe aspects of the latter stages of formation, if observable. These possibly distinctive features, however, seem to disappear within a few tens of Myr.
23 pages, 19 figures. Published in the journal Icarus
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