Infalling Planetesimals in Pre-Main Sequence Stellar Systems

Details Infalling Planetesimals in Pre-Main Sequence Stellar Systems Infalling Planetesimals in Pre-Main Sequence Stellar Systems

Jan 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999stin...9964010g&link_type=abstract

Technical Report, Jet Propulsion Lab., California Inst. of Tech. Pasadena, CA United States

Physics

Imaging Techniques, Infrared Radiation, Planetary Systems, Planetary Evolution, Stellar Systems, Stellar Mass, Stellar Envelopes, Debris, Dust, Gas Giant Planets, Inventories, Light Emission, Main Sequence Stars, Pre-Main Sequence Stars, Protoplanets

Scientific paper

These are exciting times in the study of planetary system formation with a steadily expanding inventory of exo-planet detections, and imaging of dust disks around nearby young and main sequence stars. While these discoveries imply that our Solar System is far from unique, linking the data for the protoplanetary and debris disks to mature planetary systems requires a demonstration that disk evolution proceeds via planetesimal production and growth to the formation of planets. Theoretical studies of planet formation indicate that planetesimals grow, via runaway accretion, to lunar-sized (approx. = 2000 km) embryos in 105 years. Recent gas giant planet formation studies have suggested that most of the action in planet formation occurs over 1-16 Myr, with formation of planets similar to Jupiter in t less than 10 Myr, within the time interval that infrared (IR) and optical emission line studies have demonstrated that circumstellar material remains detectable around both solar mass and intermediate mass stars. Direct imaging of exo-planetesimals is not feasible with current and foreseeable technology, since such bodies have substantially less surface area than micron-sized grains distributed in a disk, and thus are inefficient IR emitters. However, such bodies may be indirectly detectable.

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