http://arxiv.org/abs/1901.05131
We fit an isothermal oscillatory density model of Jupiter’s protoplanetary disk to the present-day Galilean and other nearby satellites and we determine the radial scale length of the disk, the equation of state and the central density of the primordial gas, and the rotational state of the Jovian nebula. Although the radial density profile of Jupiter’s disk was similar to that of the solar nebula, its rotational support against self-gravity was very low, a property that also guaranteed its long-term dynamical stability against self-gravity induced instabilities for millions of years.
D. Christodoulou and D. Kazanas
Thu, 17 Jan 19
23/51
Comments: RAA, submitted