Dust and Gas in Planet-Forming Disks: Tracing the Grains in Transitional and Evolved Systems

Details Dust and Gas in Planet-Forming Disks: Tracing the Grains in Transitional and Evolved Systems Dust and Gas in Planet-Forming Disks: Tracing the Grains in Transitional and Evolved Systems

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006sptz.prop30523s&link_type=abstract

Spitzer Proposal ID #30523

Computer Science

Scientific paper

DWe present a sample of low-mass stars with disks in the Cep OB2 region, members of the young clusters Tr 37 (~4 Myr) and NGC 7160 (~12 Myr). These stars have been studied in detail using optical photometry and spectroscopy, determining membership for stars with and without disks, spectral types, ages, the presence of accretion, and the accretion rate and/or its upper limits. Because of their critical ages for planet formation, they were included in a GTO program with IRAC and MIPS. These observations revealed disk fractions of ~45% for Tr 37, and ~4% for NGC 7160, evidence of inner disk evolution in about 95% of the disks, and inner gaps in about 10% of them. Given that the dust composition and sizes, as well as the most detailed disk structure (presence of gaps and walls, dust temperatures) cannot be derived from the SEDs only, we propose to obtain IRS spectra of a large (statistically significant) and unbiased sample of these stars with well-known accretion and stellar properties. This relatively short program is crucial to study the dust characteristics in stars that are probably ongoing active planet formation, the dust settling/grain growth, the opening of gaps at few AU distances, the possible correlation between dust and gas (accretion) evolution, and it will complete our understanding of disks evolution by constraining the parameters involved in disk models.

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