Evolution of Gaseous Disks and the Formation of Giant and Terrestrial Planets

Details Evolution of Gaseous Disks and the Formation of Giant and Terrestrial Planets Evolution of Gaseous Disks and the Formation of Giant and Terrestrial Planets

Sep 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004sptz.prop.2300c&link_type=abstract

Spitzer Proposal ID #2300

Computer Science

Scientific paper

The remarkable diversity in the properties of the extrasolar planets shows that planet formation can lead to a wide variety of outcomes, including planetary systems very different from our own. This diversity raises a fundamental question: What is the likelihood of forming solar systems like ours? One way to address this issue is by studying the planet formation process as it occurs around nearby young stars. We propose to explore the gaseous component of planet-forming disks from the onset of giant planet formation through the epoch of the assembly of terrestrial planets (ages 1--10 Myr). Our observations, which will probe the gas content of disks over the range of radii relevant to planet formation (< 10 AU), will address issues that bear on the possibility of forming solar systems like our own. The proposed observations will [1] determine the timescale available to form giant planets and therefore identify dominant pathways for giant planet formation; [2] identify systems in which giant planets may be forming through core accretion; [3] measure the gas mass and dissipation timescale in the terrestrial planet region of the disk, an important factor in determining the likelihood of forming Earth-like planets.

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