Origins of Disks & Protoplanetesimals Using Silicate Mineralogy

Details Origins of Disks & Protoplanetesimals Using Silicate Mineralogy Origins of Disks & Protoplanetesimals Using Silicate Mineralogy

Feb 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001noao.prop...72w&link_type=abstract

NOAO Proposal ID #2001A-0072

Physics

Scientific paper

The analysis of the carbonaceous materials and silicate mineralogy of pre-main sequence Herbig Ae/Be (HAEBE) stars to main sequence (beta)- Pic systems probes the chemical and physical conditions in these potentially planet-forming environments, the condensation of dust from the gas-disk, and the aggregation and accretion of these solids into planetesimals and comets. We propose to obtain low resolution OSCIR spectra of the 9.3 µ crystalline pyroxene and 11.2 µ crystalline olivine features in HAEBE and (beta)-Pic debris disk systems. The OSCIR spectra are required to model how the grain mineralogy and size distributions vary spatially from the inner disk to the outer disk/envelope. We will synthesize dust emission spectra using grain-scattering and radiative transfer models of optically thick disks and optically thin dusty disk atmospheres. Our extensive observational and analytical modeling efforts will characterize the connections between silicate mineralogy and the origins and evolution of disks and protoplanetesimals.

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