PROBING THE FLARE ATMOSPHERES OF M DWARFS USING INFRARED EMISSION LINES

We present the results of a campaign to monitor active M dwarfs using infrared spectroscopy, supplemented with optical photometry and spectroscopy. We detected 16 flares during nearly 50 hr of observations on EV Lac, AD Leo, YZ CMi, and VB 8. The three most energetic flares also showed infrared emission, including the first reported detections of P beta, P gamma, HeI lambda 10830, and Br gamma during an M dwarf flare. The strongest flare (Delta u = 4.02 on EV Lac) showed emission from H gamma, H delta, HeI lambda 4471, and CaII K in the UV/blue and P beta, P gamma, P delta, Br gamma, and HeI lambda 10830 in the infrared. The weaker flares (Delta u = 1.68 on EV Lac and Delta U = 1.38 on YZ CMi) were only observed with photometry and infrared spectroscopy; both showed emission from P beta, P gamma, and HeI lambda 10830. The strongest infrared emission line, P beta, occurred in the active mid-M dwarfs with a duty cycle of similar to 3%-4%. To examine the most energetic flare, we used the static NLTE radiative transfer code RH to produce model spectra based on a suite of one-dimensional model atmospheres. Using a hotter chromosphere than previous one-dimensional atmospheric models, we obtain line ratios that match most of the observed emission lines.