X-raying the AU Microscopii debris disk

Details X-raying the AU Microscopii debris disk X-raying the AU Microscopii debris disk

2010-03-29

arxiv.org/abs/1003.5562v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

11 pages, 10 figures, accepted for publication in A&A

Scientific paper

AU Mic is a young, nearby X-ray active M-dwarf with an edge-on debris disk. Debris disk are the successors of the gaseous disks usually surrounding pre-main sequence stars which form after the first few Myrs of their host stars' lifetime, when - presumably - also the planet formation takes place. Since X-ray transmission spectroscopy is sensitive to the chemical composition of the absorber, features in the stellar spectrum of AU Mic caused by its debris disk can in principle be detected. The upper limits we derive from our high resolution Chandra LETGS X-ray spectroscopy are on the same order as those from UV absorption measurements, consistent with the idea that AU Mic's debris disk possesses an inner hole with only a very low density of sub-micron sized grains or gas.

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