Locating the Dust in A Star Debris Discs. Issue Volume 8:Issue S299(2013) (6th January 2014)

• Record Type: Journal Article
• Authors: Booth, Mark; Kennedy, Grant; Sibthorpe, Bruce; Matthews, Brenda C.; Wyatt, Mark C.; Duchêne, Gaspard; Kavelaars, J. J.; Rodriguez, David; Greaves, Jane S.; Koning, Alice; Vican, Laura; Rieke, George H.; Su, Kate Y. L.; Moro-Martín, Amaya; Kalas, Paul
• Is Part Of: Proceedings of the International Astronomical Union. Volume 8:Issue S299(2013)
• Page Start: 330
• Page End: 331
• Publication Date: 2014-01-06
• Subjects: circumstellar matter, -- planetary systems, -- infrared: stars; Astronomy -- Congresses; Astronomy -- Periodicals; 520
• DOI: 10.1017/S1743921313008806
• Languages: English
• ISSNs: 1743-9213

Abstract

Abstract: Using photometry at just two wavelengths it is possible to fit a blackbody to the spectrum of infrared excess that is the signature of a debris disc. From this the location of the dust can be inferred. However, it is well known that dust in debris discs is not a perfect blackbody. By resolving debris discs we can find the actual location of the dust and compare this to that inferred from the blackbody fit. Using the Herschel Space Observatory we resolved many systems as part of the DEBRIS survey. Here we discuss a sample of 9 discs surrounding A stars and find that the discs are actually located between 1 and 2.5 times further from their star than predicted by blackbody fits to the spectral energy distribution (SED). The variation in this ratio is due to differences in stellar luminosities, location of the dust, size distribution and composition of the dust.