NOAO > Observing Info > Approved Programs > 2011A-0106
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NOAO > Observing Info > Approved Programs > 2011A-0106 |
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PI: John Wisniewski, University of Washington, jwisnie@u.washington.edu
Address: Astronomy Department, Box 351580, Seattle, WA 98195, USA
CoI: Adam Kowalski, University of Washington
CoI: Sarah Schmidt, University of Washington
CoI: Praveen Kundurthy, University of Washington
CoI: Suzanne Hawley, University of Washington
CoI: Ben Tofflemire, University of Washington
CoI: Jon Holtzman, New Mexico State University
Title: M Dwarf Flares: Exoplanet Implications
Abstract: M dwarfs are attractive stars for exoplanet transit research as their low luminosities and small stellar radii could enable detection of super-Earths residing in their habitable zones. M dwarf flare events can cause <0.1 to 6.0 magnitude flux enhancements in the optical U- band, which is significantly higher than the predicted transit depths of super-Earths (~0.005 magnitude flux decrease). While Solar flares have been observed to cause infrared continuum enhancements (Xu et al 2006); surprisingly, it is not known whether energetic flares associated with M dwarfs can induce IR variability in filters relevant to future transiting exoplanet characterization studies (e.g. using JWST). We propose to monitor the optical & IR flux of a M dwarf known to regularly flare, to determine what effect flares could have on future IR characterization studies of M dwarf exoplanets. This proposal represents a resubmission of our approved 2009B program, which lost >80% of its on-sky time due to Tropical Storm Olaf (but did demonstrate the ability to achieve 5 milli-mag IR photometry with the KPNO 2.1m). We request 5 nights in 2011A to complete our science goals.
National Optical Astronomy Observatory, 950 North Cherry Avenue, P.O. Box 26732, Tucson, Arizona 85726, Phone: (520) 318-8000, Fax: (520) 318-8360
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NOAO > Observing Info > Approved Programs > 2011A-0106 |
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