Hot debris dust around HD 106797

Abstract

Photometry of the A0 V main-sequence star HD 106797 with AKARI and Gemini/T-ReCS is used to detect excess emission over the expected stellar photospheric emission between 10 and 20 micron, which is best attributed to hot circumstellar debris dust surrounding the star. The temperature of the debris dust is derived as Td ~ 190 K by assuming that the excess emission is approximated by a single temperature blackbody. The derived temperature suggests that the inner radius of the debris disk is ~ 14 AU. The fractional luminosity of the debris disk is 1000 times brighter than that of our own zodiacal cloud. The existence of such a large amount of hot dust around HD 106797 cannot be accounted for by a simple model of the steady state evolution of a debris disk due to collisions, and it is likely that transient events play a significant role. Our data also show a narrow spectral feature between 11 and 12 micron attributable to crystalline silicates, suggesting that dust heating has occurred during the formation and evolution of the debris disk of HD 106797.

Accepted to ApJ Letters, 8 pages, 2 figures

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• Spitzer Evidence for a Late Heavy Bombardment and the Formation of Urelites in η Corvi at ~1 Gyr
• A Comprehensive Census of Nearby Infrared Excess Stars
• The short-lived production of exozodiacal dust in the aftermath of a dynamical instability in planetary systems
• Solar System Physics for Exoplanet Research
• A large moving group within the Lower Centaurus Crux association
• AKARI/IRC 18 Micron Survey of Warm Debris Disks
• Bright Debris Disk Candidates Observed with AKARI/Far-Infrared Surveyor (FIS)
• Faint warm debris disks around nearby bright stars explored by AKARI and IRSF
• A WISE View of IRAS Debris Disks: Revising the Dust Properties
• V488 Per revisited: no strong mid-infrared emission features and no evidence for stellar/sub-stellar companions
• Can the dustiest main sequence stars tell us about the rocky planet formation process?