Comparative Study of the Gas and Dust in Disks Around Sun-like and Cool Stars

Details Comparative Study of the Gas and Dust in Disks Around Sun-like and Cool Stars Comparative Study of the Gas and Dust in Disks Around Sun-like and Cool Stars

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21537404p&link_type=abstract

American Astronomical Society, AAS Meeting #215, #374.04; Bulletin of the American Astronomical Society, Vol. 42, p.583

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I will present the first comprehensive, comparative Spitzer/IRS study of the dust and gas properties of disks around young Sun-like stars (K1-M5) and cool stars/brown dwarfs (M5-M9). The comparison of these two large samples of over 60 sources reveals major differences in both the dust and gas components. Cool stars and brown dwarfs show weaker 10 micron silicate emission features arising from more processed grains in the disk atmosphere. These findings complement previous indications of flatter disk structures and longer disk lifetimes around cool stars. We report the first detections of organic molecules in disks around brown dwarfs. The detection rate statistics and the line flux ratios of the molecules HCN and C2H2 show a striking difference between the two samples, demonstrating a significant underabundance of HCN relative to C2H2 in the disk surface of cool stars. We propose this to originate from the large difference in the UV irradiation around the two types of sources. Our results highlight important differences in the chemical and physical evolution of protoplanetary disks as a function of stellar mass, temperature, and radiation field which should be taken into account in planet formation models.

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