MIPS 24 micron Study of Debris Disks in Praesepe and Coma Berenices

Details MIPS 24 micron Study of Debris Disks in Praesepe and Coma Berenices MIPS 24 micron Study of Debris Disks in Praesepe and Coma Berenices

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006sptz.prop30429r&link_type=abstract

Spitzer Proposal ID #30429

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Scientific paper

Debris disks form when asteroidal-scale bodies collide or cometary objects evaporate, generating fragments that participate in cascades of further collisions, eventually producing significant amounts of dust grains that glow in the Spitzer bands. Therefore, debris disks are clear evidence that planetary objects are present, and provide a great opportunity to understand how a planetary system forms from a record of events in planetary-forming zones. Early Spitzer studies on debris disks around A-type stars show a general decline in the amount of excess emission with age; younger (age <500 Myr) stars exhibit excesses more frequently (~30%) and with higher fractional excess than do the older stars. Other results from studying the evolution of excesses around solar-type stars show a similar trend within the errors, suggestive of an independence of stellar mass and a critical transition in disk properties from 300 Myr to 1 Gyr, over which the 24 um excesses apparently disappear. Nevertheless, we do not have a good statistical significance for ages greater than 300 Myr. In this proposal, we will address the debris disk evolution in this important intermediate age (500-600 Myr) with MIPS 24 um observations of Praesepe and Coma Berenices clusters. These two clusters are ~600 Myr in age, coinciding with the era of Heavy Bombardment and settling down to set the stage for life in our Solar system. Our proposed observations will span a critical gap in debris disk studies by Spitzer, and help to understand the debris disk evolution in this important era.

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