Probing the Flare Atmospheres of M dwarfs Using Infrared Emission Lines

TL;DR

This study uses infrared spectroscopy to monitor M dwarf flares, detecting multiple emission lines and modeling their atmospheres, revealing new insights into flare energetics and atmospheric conditions.

Contribution

It presents the first infrared detections of specific emission lines during M dwarf flares and models flare atmospheres with a hotter chromosphere to match observations.

Findings

Detected 16 flares with infrared emission lines.

First infrared detections of Pβ, Pγ, He I 10830Å, and Brγ during M dwarf flares.

Modeled flare atmospheres with a hotter chromosphere, matching observed line ratios.

Abstract

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 hours of observations on EV Lac, AD Leo, YZ CMi, and VB8. The three most energetic flares also showed infrared emission, including the first reported detections of P\beta, P\gamma, He I 10830\AA 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, He I 4471\AA, and Ca II K in the UV/blue and P\beta, P\gamma, P\delta, Br\gamma, and He I 10830\AA 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 He I 10830\AA. The strongest infrared emission line, P\beta, occurred in the active mid-M dwarfs with a duty cycle of ~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.