From Gas to Satellitesimals: Disk Formation and Evolution

Abstract

The subject of satellite formation is strictly linked to the one of planetary formation. Giant planets strongly shape the evolution of the circum-planetary disks during their formation and thus, indirectly, influence the initial conditions for the processes governing satellite formation. In order to fully understand the present features of the satellite systems of the giant planets, we need to take into account their formation environments and histories and the role of the different physical parameters. In particular, the pressure and temperature profiles in the circum-planetary nebulae shaped their chemical gradients by allowing the condensation of ices and noble gases. These chemical gradients, in turn, set the composition of the satellitesimals, which represent the building blocks of the present regular satellites.

JIRAM, the Jovian Infrared Auroral Mapper

“…The formation of Jupiter, in fact, changes the local conditions existing at its formation region (Coradini et al 2010). The gas accretion causes the forming planet to acquire an accretion luminosity that heats up the disk and causes the vaporization of most volatile species (Coradini et al 2010).…”

“…The formation of Jupiter, in fact, changes the local conditions existing at its formation region (Coradini et al 2010). The gas accretion causes the forming planet to acquire an accretion luminosity that heats up the disk and causes the vaporization of most volatile species (Coradini et al 2010). Moreover, the accretion process also affects the gas density and velocity in the feeding zone of the giant planet and thus influences its pressure and the possibility for volatile species (H 2 O, NH 3 , CO, CO 2 , CH 4 ) to condense (or re-condense) as solids (Coradini et al 2010).…”

“…The gas accretion causes the forming planet to acquire an accretion luminosity that heats up the disk and causes the vaporization of most volatile species (Coradini et al 2010). Moreover, the accretion process also affects the gas density and velocity in the feeding zone of the giant planet and thus influences its pressure and the possibility for volatile species (H 2 O, NH 3 , CO, CO 2 , CH 4 ) to condense (or re-condense) as solids (Coradini et al 2010). Finally, the evolution of the circum-Jovian environment would influence also the formation of the satellite system of the giant planet (by affecting the capture and migration rates of planetesimals in the circum-planetary disk) and the abundance of volatile elements in their bulk composition.…”

Vesta and Ceres: Crossing the History of the Solar System

“…According to Lissauer et al (2009), the gas-accretion time of Jupiter varies between several 10 4 to a few 10 5 years. Coradini et al (2010) measured the gas-accretion time-scales for Jupiter and Saturn, which vary between a few 10 3 to about 10 5 years depending on the physical parameters of the Solar Nebula. The agreement between these values indicates that the time over which Jupiter accreted its gaseous envelope (i.e.…”

“…The rapid changes in the gravitational potential across the circumsolar disk due to Jupiter's accretion and migration should have strongly affected the mass and velocity distribution of all the bodies present at that time in the Solar Nebula (see e.g. Coradini et al 2010;Turrini et al 2011).…”