Computer Science
Scientific paper
May 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006sptz.prop30239p&link_type=abstract
Spitzer Proposal ID #30239
Computer Science
Scientific paper
The first steps of planet formation are marked by the growth and crystallization of sub-micrometer-sized dust grains. These steps have been identified in disks around young stars of different masses and, recently, even in disks around brown dwarfs. Although models suggest that stellar age and luminosity alone shall determine the extent of dust processing, recent observations show that grain growth and crystallinity can be very different even for coeval disks around stars of similar spectral type. This indicates the presence of at least a third important parameter. A number of studies in the past pointed out that multiplicity could play a major role in the disk evolution. But theoretical models have not yet reached a consensus on the efficiency of planet formation in the presence of companions. We propose here to investigate the effects of stellar companions on the initial steps of planet formation in protoplanetary disks. Our work will provide fundamental constraints on theoretical models of planet formation in multiple systems as well set the frame for the correct interpretation of the numerous Spitzer studies of dust in circumstellar disks. We selected a statistically significant sample of coeval disks around low-mass stars with well-known multiplicity to test the hypothesis that multiple systems have more processed dust disks (micron-sized grains and crystals). We have identified 59 spectra in the Spitzer archive from three different programs that have sufficient signal-to-noise to meet our goals. We will reduce and analyze these spectra in the same manner and determine the amount of large-to-small grains and crystals via the spectral decomposition of the 10 micron silicate emission feature. Our Monte Carlo simulations and Kolmogorov-Smirnov tests show that we will be able, for example, to discriminate between two populations with 10% and 20% crystalline mass fractions at a confidence level of 99%.
Apai Daniel
Bouwman Jeroen
Meyer Michael
Pascucci Ilaria
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