Debris Disk Evolution around A Stars

The Astrophysical Journal (Impact Factor: 5.99). 12/2008; 653(1):675. DOI: 10.1086/508649
Source: arXiv


We report 24 and/or 70 μm measurements of ~160 A-type main-sequence stars using the Multiband Imaging Photometer for Spitzer (MIPS). Their ages range from 5 to 850 Myr, based on estimates from the literature (cluster or moving group associations) or from the H-R diagram and isochrones. The thermal infrared excess is identified by comparing the deviation (~3% and ~15% at the 1 σ level at 24 and 70 μm, respectively) between the measurements and the synthetic Kurucz photospheric predictions. Stars showing excess infrared emission due to strong emission lines or extended nebulosity seen at 24 μm are excluded from our sample; therefore, the remaining infrared excesses are likely to arise from circumstellar debris disks. At the 3 σ confidence level, the excess rate at 24 and 70 μm is 32% and ≥33% (with an uncertainty of 5%), considerably higher than what has been found for old solar analogs and M dwarfs. Our measurements place constraints on the fractional dust luminosities and temperatures in the disks. We find that older stars tend to have lower fractional dust luminosity than younger ones. While the fractional luminosity from the excess infrared emission follows a general 1/t relationship, the values at a given stellar age vary by at least 2 orders of magnitude. We also find that (1) older stars possess a narrow range of temperature distribution peaking at colder temperatures, and (2) the disk emission at 70 μm persists longer than that at 24 μm. Both results suggest that the debris disk clearing process is more effective in the inner regions.

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Available from: James Muzerolle, Jun 10, 2014
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    • "The debris disc around Vega was the first debris disc discovered in this way (Aumann et al. 1984) and after that more than 100 discs have been subsequently discovered. Observations from recent surveys indicate that at least 15 per cent of FGK stars and 32 per cent of A stars have a detectable amount of circumstellar debris (Bonsor et al. (2014), Bryden et al. (2006), Moro-Martín et al. (2007), Hillenbrand et al. (2008),Greaves et al. (2009) and Su et al. (2006)). "
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