2007/10/04 by Grant M. Kennedy, Scott J. Kenyon · 1 citation
Physics and Astronomy · #astro-ph
paper · pdf · doi:10.1086/524130
Accepted to ApJ. 12 pages of emulateapj
arxiv created 2007/10/04 · arxiv updated 2009/12/01
We use a semi-analytic circumstellar disk model that considers movement of the snow line through evolution of accretion and the central star to investigate how gas giant frequency changes with stellar mass. The snow line distance changes weakly with stellar mass; thus giant planets form over a wide range of spectral types. The probability that a given star has at least one gas giant increases linearly with stellar mass from 0.4 Msun to 3 Msun. Stars more massive than 3 Msun evolve quickly to the main-sequence, which pushes the snow line to 10-15 AU before protoplanets form and limits the range of disk masses that form giant planet cores. If the frequency of gas giants around solar-mass stars is 6%, we predict occurrence rates of 1% for 0.4 Msun stars and 10% for 1.5 Msun stars. This result is largely insensitive to our assumed model parameters. Finally, the movement of the snow line as stars >2.5 Msun move to the main-sequence may allow the ocean planets suggested by Leger et. al. to form without migration.