Hα Emission From Active Equal-Mass, Wide M Dwarf Binaries1 1 This publication is partially based on observations obtained with the Apache Point Observatory 3.5-meter telescope, which is owned and operated by the Astrophysical Research Consortium

• Published in: Publications of the Astronomical Society of the Pacific Vol. 126; no. 946; pp. 1081 - 1091
• Main Authors: Gunning, Heather C., Schmidt, Sarah J., Davenport, James R. A., Dhital, Saurav, Hawley, Suzanne L., West, Andrew A.
• Format: Journal Article
• Language: English
• Published: University of Chicago Press 01-12-2014
• ISSN: 0004-6280; 1538-3873
• DOI: 10.1086/679329

We identify a sample of near-equal mass wide binary M dwarf systems from the SLoWPoKES catalog of common proper-motion binaries and obtain follow-up observations of their chromospheric activity as measured by the Hα emission line. We present optical spectra for both components of 48 candidate M dwarf binaries, confirming their mid-M spectral types. Of those 48 coeval pairs, we find eight with Hα emission from both components, three with weak emission in one component and no emission in the other, and 37 with two inactive components. We find that of the 11 pairs with at least one active component, only three follow the net trend of decreasing activity strength (LHα/Lbol) with later spectral type. The difference in quiescent activity strength between the A and B components is larger than what would be expected based on the small differences in color (mass). For five binaries with two active components, we present 47 hr of time-resolved spectroscopy, observed on the ARC 3.5-m over 12 different nights. For four of the five pairs, the slightly redder (B) component exhibits a higher level of Hα emission during the majority of the observations and the redder objects are the only components to flare. The full range of Hα emission observed on these variable mid-M dwarfs is comparable to the scatter in Hα emission found in single-epoch surveys of mid-M dwarfs, indicating that variability could be a major factor in the spread of observed activity strengths. We also find that variability is independent of both activity strength and spectral type.