Formation of Giant Planets by Disk Instability on Wide Orbits Around Protostars with Varied Masses

Details Formation of Giant Planets by Disk Instability on Wide Orbits Around Protostars with Varied Masses Formation of Giant Planets by Disk Instability on Wide Orbits Around Protostars with Varied Masses

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.5201b&link_type=abstract

American Astronomical Society, DPS meeting #42, #52.01; Bulletin of the American Astronomical Society, Vol. 42, p.1070

Astronomy and Astrophysics

Astronomy

Scientific paper

Doppler surveys have shown that more massive stars have significantly higher frequencies of giant planets inside 3 AU than lower mass stars, consistent with giant planet formation by core accretion. Direct imaging searches have begun to discover significant numbers of giant planet candidates around stars with masses of 1 solar mass to 2 solar masses at orbital distances of 20 AU to 120 AU. Given the inability of core accretion to form giant planets at such large distances, gravitational instabilities of the gas disk leading to clump formation have been suggested as the more likely formation mechanism for gas giants on wide orbits. Here we present five new models of the evolution of disks with inner radii of 20 AU and outer radii of 100 AU, for central protostars with masses of 0.1, 0.5, 1.0, 1.5, and 2.0 solar masses, in order to assess the likelihood of planet formation on wide orbits around stars with varied masses. The disk masses range from 0.042 to 0.30 solar masses, with initial Toomre Q stability values ranging from 1 in the inner disks to 2 in the outer disks. These five models show that disk instability is capable of forming giant planets initially on orbits with semimajor axes of 35 AU to 60 AU and eccenticities of 0 to 0.3, with initial masses of 1 Jupiter mass to 3 Jupiter masses around solar-type stars, with more protoplanets forming as the mass of the protostar (and protoplanetary disk) are increased.

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