# Models of a protoplanetary disk forming in-situ the Galilean and smaller nearby satellites before Jupiter is formed

## TL;DR

This paper models Jupiter's early protoplanetary disk to understand the formation conditions of its satellites, revealing a stable, low-rotation disk with a density profile akin to the solar nebula.

## Contribution

It introduces an isothermal oscillatory density model fitting Jupiter's disk to explain satellite formation prior to Jupiter's formation.

## Key findings

- Disk had low rotational support, ensuring stability.
- Density profile similar to the solar nebula.
- Disk parameters derived from satellite data.

## Abstract

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 stability against self-gravity induced instabilities for millions of years.