The Origin of Warm Debris Disks around Solar Analogues

Details The Origin of Warm Debris Disks around Solar Analogues The Origin of Warm Debris Disks around Solar Analogues

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007sptz.prop40566a&link_type=abstract

Spitzer Proposal ID #40566

Computer Science

Scientific paper

The Origin of Warm Debris Disks Around Solar Analogues One of the major discoveries of the IRAS mission was that many main-sequence stars are accompanied by circumstellar dust disks. Since the lifetime of dust grains in such disks is rather short, one assumes a planetesimal belt around the star, where collisions replenish the dust. Most known extrasolar debris disks are cold (50-90 K), and can be considered as the extrasolar analogues of our Kuiper belt. Warmer disks of 200-300 K are, however, rare: surveys of solar analogue main-sequence F,G or K stars discovered only about a dozen stars (2% of the observed systems) which harbour such kind of debris disks. These disks may be the closest - though somewhat brighter - analogues of our inner solar system. Many open questions are related to these spectacular objects, but perhaps the most interesting is their origin: were they formed via steady state evolution, or they are the product of transient dust-producing events, like collision of large asteroids, or a Late Heavy Bombardment (LHB)-like period. The answers may help to better understand the formation of the inner solar system, too. We propose to carry out detailed IRAC, IRS and MIPS observations of a well-selected large sample of 35 warm-disk candidates around F-G-K stars. Each system will be characterized in terms of disk structure and grain properties, and its most likely formation scenario will be outlined. Performing such an analysis on our whole sample we will give the first hints on how common are LHB-type events among Solar-analogue stars?

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