Formation of Large Regular Satellites of Giant Planets in an Extended Gaseous Nebula: Subnebula Model and Accretion of Satellites

Details Formation of Large Regular Satellites of Giant Planets in an Extended Gaseous Nebula: Subnebula Model and Accretion of Satellites Formation of Large Regular Satellites of Giant Planets in an Extended Gaseous Nebula: Subnebula Model and Accretion of Satellites

Jan 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000stin...0229887m&link_type=abstract

Technical Report, NASA Ames Research Center Moffett Field, CA United States

Mathematics

Nebulae, Saturn Satellites, Protoplanets, Planetary Evolution, Mathematical Models, Accretion Disks, Galilean Satellites, Callisto, Ganymede, Iapetus, Titan

Scientific paper

We model the subnebulae of Jupiter and Saturn wherein satellite accretion took place. We expect a giant planet subnebula to be composed of an optically thick (given gaseous opacity) inner region inside of the planet's centrifugal radius (located at r(sub c, sup J) = l5RJ for Jupiter and r(sub c, sup S) = 22RS for Saturn), and an optically thin, extended outer disk out to a fraction of the planet's Roche lobe, which we choose to be Rroche/5 (located at approximately 150RJ near the inner irregular satellites for Jupiter, and approximately 200RS near Phoebe for Saturn). This places Titan and Ganymede in the inner disk, Callisto and Iapetus in the outer disk, and Hyperion in the transition region. The inner disk is the leftover of the gas accreted by the protoplanet. The outer disk results from the solar torque on nebula gas flowing into the protoplanet during the time of giant planet gap opening. For the sake of specificity, we use a cosmic mixture 'minimum mass' model to constrain the gas densities of the inner disks of Jupiter and Saturn (and also Uranus). For the total mass of the outer disk we use the simple scaling Mdisk = MPtaugap/tauacc, where MP is the mass of the giant planet, taugap is the gap opening timescale, and tauacc is the giant planet accretion time. This gives a total outer disk mass of approximately 100MCallisto for Jupiter and possibly approximately 200MIapetus for Saturn (which contain enough condensables to form Callisto and Iapetus respectively). Our model has Ganymede at a subnebula temperature of approximately 250 K and Titan at approximately 100 K. The outer disks of Jupiter and Saturn have constant temperatures of 130 K and 90 K respectively.

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