The First Detection of Time-Variable Infrared Line Emission During M Dwarf Flares

Details The First Detection of Time-Variable Infrared Line Emission During M Dwarf Flares The First Detection of Time-Variable Infrared Line Emission During M Dwarf Flares

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21832604s&link_type=abstract

American Astronomical Society, AAS Meeting #218, #326.04; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

M dwarfs are notorious for their active chromospheres, characterized by quiescent line emission at optical wavelengths in addition to dramatic flare events. These flares have been well-studied at X-ray, radio, UV, and optical wavelengths, but so far there is only one single-epoch detection of high-order Paschen emission lines in a red optical spectrum (Schmidt et al. 2007). In order to investigate infrared line emission during flares, we have conducted a monitoring campaign totaling about 60 hours on 5 active M dwarfs. We have obtained infrared (0.9 to 2.4 micron) spectroscopy using the TripleSpec instrument on the Apache Point Observatory 3.5-m, simultaneous optical/UV photometry on the NMSU 1-m and ARC 0.8-m, and optical spectroscopy on the DAO 1.8-m for one run. During the three brightest flares observed on EV Lac and YZ CMi (> 2 magnitudes in U), we observed emission from Hydrogen Paschen beta, gamma, and delta; Brackett gamma, and Helium 10830A. We characterize the strength and time variation of these lines and investigate the heating needed to produce infrared emission during flares.

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