M Dwarfs in SDSS Stripe 82: Photometric Light Curves and Flare Rate Analysis

TL;DR

This study analyzes the flare activity of over 50,000 M dwarfs in SDSS Stripe 82, revealing correlations with spectral features, color, and galactic position, and providing estimates of flare rates and luminosities.

Contribution

It presents a comprehensive flare rate analysis of a large M dwarf sample using photometric light curves and introduces a customized variability detection method.

Findings

Flares are strongly associated with H-alpha emission.

Flaring fraction increases with redder stellar colors.

Most flares occur within 300 pc of the Galactic plane.

Abstract

We present a flare rate analysis of 50,130 M dwarf light curves in SDSS Stripe 82. We identified 271 flares using a customized variability index to search ~2.5 million photometric observations for flux increases in the u- and g-bands. Every image of a flaring observation was examined by eye and with a PSF-matching and image subtraction tool to guard against false positives. Flaring is found to be strongly correlated with the appearance of H-alpha in emission in the quiet spectrum. Of the 99 flare stars that have spectra, we classify 8 as relatively inactive. The flaring fraction is found to increase strongly in stars with redder colors during quiescence, which can be attributed to the increasing flare visibility and increasing active fraction for redder stars. The flaring fraction is strongly correlated with |Z| distance such that most stars that flare are within 300 pc of the Galactic plane. We derive flare u-band luminosities and find that the most luminous flares occur on the earlier-type M dwarfs. Our best estimate of the lower limit on the flaring rate (averaged over Stripe 82) for flares with \Delta u \ge 0.7 magnitudes on stars with u < 22 is 1.3 flares hour^-1 square degree^-1 but can vary significantly with the line-of-sight.