Young debris disks at the epoch of planet formation in the Orion OB1 association

Details Young debris disks at the epoch of planet formation in the Orion OB1 association Young debris disks at the epoch of planet formation in the Orion OB1 association

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008sptz.prop50690h&link_type=abstract

Spitzer Proposal ID #50690

Computer Science

Scientific paper

Debris disks are dusty, gas-poor disks around stars, in which the grains are replenished from a reservoir, such as collisions between parents bodies. In general, observational studies of the evolution of Debris disks have been focused on long period trend (from few Myr to hundred of Myr or Gyr), where the luminosities of the debris disks decay as the reservoir of collisional parent diminishes. However, theoretical models show that for A type the time scale to produce large icy objects (1000 Km) that stir-up the solids on the disks and begin a collisional cascade is around 10 Myr, observational studies on the Orion OB1 association support this timescale showing that the debris disks around intermediate mass stars are more frequent and have larger 24{micron} excess around 10 Myr (the stellar aggregate 25 Ori); younger stellar groups could be associated to a phase between the clearing of primordial disks (<3My) and the formation of large icy object. We propose to obtain IRS spectra (short-low and long-low modules) and 70{micron} MIPS photometry in order to study in more detail 18 debris disk found in three region of the Orion Association: the stellar aggregate 25 Ori (10 Myr), the sub association Orion OB1b (5 Myr), and the stellar cluster sigma Orionis (3 Myr). The analysis of the IRS spectra and the spectral energy distribution, in combination with theoretical models, will provide us important tools to characterize the bulk of the emitting particles (e.g. grain-size distribution, composition and radial distribution of dust); besides, 70 {micron} photometry enable us to study the outer part of the disk where mechanisms for dispersing primordial optically thick disks operate less efficiently. Overall, this project will provide considerable insight into the nature of the second generation dust process at the epoch of planet formation and primordial disk dissipation

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