Physics
Scientific paper
Jul 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009atnf.prop.2471m&link_type=abstract
ATNF proposal C1800, Semester: July, 2009
Physics
Stellar, Atca
Scientific paper
Debris disks represent the final evolutionary phase of protoplanetary disks around young stars. While large planetesimals are undetected, visible and near infrared emission from short-lived grains produced by collisions between these asteroid-sized bodies can reveal the distribution of the planetesimal population. Understanding the spatial and size distribution of the grains sheds light on the physical conditions and dynamics of debris disk, which is the basic information needed to understand the physics of disks when planets are forming. At least two grain populations are believed to exist in the nearby southern debris disk beta Pic disk: large dark particles that dominate the thermal emission, and much smaller grains responsible for the optical and near infrared scattered light observations. The slope of the sub-mm to mm part of the spectral energy distribution provides strong constraints on the grain size. Our 7mm upper limit has helped constrain the mm SED slope of beta Pic. Here be propose to to use CABB to now determine the 7mm flux, as well as the 3mm flux, to better understand the grain population. We will also attempt to image the beta Pic disk at 3mm for the first time.
Maddison Sarah
Wright Christopher
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