AU Mic Is Not Alone: New M Dwarf Debris Disks

Details AU Mic Is Not Alone: New M Dwarf Debris Disks AU Mic Is Not Alone: New M Dwarf Debris Disks

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008sptz.prop50731p&link_type=abstract

Spitzer Proposal ID #50731

Computer Science

Scientific paper

M dwarfs constitute ~70% of the stars in our local neighborhood, yet we know little about the frequency and evolution of debris disks and planetary systems for this diverse spectral class. Among the numerous M dwarfs sampled by Spitzer in the nearest 25pc, AU Mic remains a unique M dwarf with its debris disk, infrared excess, 12Myr age, flaring, and X-ray activity (Chen et al. 2005, Plavchan et al. 2005, Kalas et al. 2005, Gautier et al., 2007). Plavchan et al. (2005) proposed that stellar wind drag can account for the apparent dearth of mature M dwarf debris disks. To test this hypothesis, in Cycle-4 we have observed to date 10 of 22 X-ray saturated M dwarfs like AU Mic out to a median distance of 32pc. From these initial observations, we have discovered 3 new M dwarf debris disks (Plavchan et al. in prep.). We propose to expand our sample to a statistically robust sample size comparable to the number of observed mature M dwarfs (~40). We propose observe 15 more nearby X-ray saturated M dwarfs in Cycle-5. These late-type dwarfs have ROSAT detections indicative of saturated X-ray activity (F_X>8x10^-5 ergs/cm^2/s) and are consequently likely to both be young and lack significant radial winds. Compared to the relatively old population of nearby M dwarfs, circumstellar disks are more likely to both exist and persist around these stars. Combining our sample with previous Spitzer observations, we will constrain the age evolution, frequency, and dynamics of M dwarf debris disks to place into context disks around solar type stars.

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