Circumstellar Dust Created by Terrestrial Planet Formation Processes Around HD 113766A

Details Circumstellar Dust Created by Terrestrial Planet Formation Processes Around HD 113766A Circumstellar Dust Created by Terrestrial Planet Formation Processes Around HD 113766A

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.3201l&link_type=abstract

American Astronomical Society, DPS meeting #39, #32.01; Bulletin of the American Astronomical Society, Vol. 39, p.473

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We present an analysis of the circumstellar disk material in the HD 113766 binary system (F3/F5, 16 Myr), recently observed by the Spitzer Space Telescope. For our study we have used the infrared mineralogical model derived from observations of the Deep Impact experiment. We find the dust dominated by warm, fine ( 1 um) particles, abundant in Mg-rich olivine, crystalline pyroxenes, amorphous silicates, Fe-rich sulfides, amorphous carbon, and water ice. The material mix is akin to an inner main belt asteroid of S- or V-type composition, and is dissimilar to the organic- and water-rich comet systems 9P/Tempel 1, C/Hale-Bopp 1995 O1, or the comet-dominated YSO HD 100546. The 440 K effective temperature of the warm dust implies that the bulk of the observed material is at 1.8 AU from the 4.4 Lsolar central source, in the terrestrial planet-forming region and habitable zone of the system (equivalent to 0.9 AU in the solar system). The icy dust lies in 2 belts, at 9 AU and at 60-80 AU. The amount of mass responsible for the warm dust emission in dn/da a-3.5 particles is very large, 3 x 1023 kg, or 0.5 MMars. The persistence of the strong IR excess over the last two decades argues for a mechanism to provide replenishment of the circumstellar material on yearly timescales. The disk around HD 113766A appears to arise from collisions in a young, extremely dense asteroid belt, or from catastrophic disruption of terrestrial planet embryo(s) and subsequent grinding of the fragments.

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