Debris Disk Evolution Around A Stars

Details Debris Disk Evolution Around A Stars Debris Disk Evolution Around A Stars

2006-08-25

arxiv.org/abs/astro-ph/0608563v1

Astrophys.J.653:675-689,2006

Astronomy and Astrophysics

Astrophysics

17 pages, accepted for publication in ApJ

Scientific paper

10.1086/508649

We report 24 and/or 70 um 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-\sigma level at 24 and 70 um, 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 um are excluded from our sample; therefore, the remaining infrared excesses are likely to arise from circumstellar debris disks. At the 3-sigma confidence level, the excess rate at 24 and 70 um is 32% and >=33% (with an uncertainty of 5%), considerably higher than 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 two 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 um persists longer than that at 24 um. Both results suggest that the debris-disk clearing process is more effective in the inner regions.

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