Models of a protoplanetary disk forming in-situ the Galilean \ and smaller nearby satellites before Jupiter is fully formed. (arXiv:1901.05131v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Christodoulou_D/0/1/0/all/0/1">D. M. Christodoulou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kazanas_D/0/1/0/all/0/1">D. Kazanas</a>
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.
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.
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