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|Abstract:||We report the discovery by the HATNet survey of HAT-TR-318-007, a P = 3.34395390 0.00000020 day period detached double-lined M dwarf binary with total secondary eclipses. We combine radial velocity (RV) measurements from TRES/FLWO 1.5 m and time-series photometry from HATNet, FLWO 1.2 m, BOS 0.8 m, and NASA K2 Campaign 5, to determine the masses and radii of the component stars: MA 0.448 0.011N = , MB 0.2721 0.0042 = - +0.0041 N , RA 0.4548 0.0036 = - +0.0035 N , and RB 0.2913 0.0024 = - +0.0023 N . We obtained a FIRE/Magellan near-infrared spectrum of the primary star during a total secondary eclipse, and we use this to obtain disentangled spectra of both components. We determine spectral types of ST M3.71 0.69 A = and ST M5.01 0.73 B = and effective temperatures of Teff,A = 3190 110 K and Teff,B = 3100 110 K for the primary and secondary star, respectively. We also measure a metallicity of [Fe/H]=+ 0.298 0.080 for the system. We find that the system has a small, but significant, nonzero eccentricity of 0.0136 0.0026 . The K2 light curve shows a coherent variation at a period of 3.41315 0.00032 0.00030 - + days, which is slightly longer than the orbital period, and which we demonstrate comes from the primary star. We interpret this as the rotation period of the primary. We perform a quantitative comparison between the Dartmouth stellar evolution models and the seven systems, including HATTR-318-007, that contain M dwarfs with 0.2 0.5 N N < < M , have metallicity measurements, and have masses and radii determined to better than 5% precision. Discrepancies between the predicted and observed masses and radii are found for three of the systems.|
|Electronic Publication Date:||14-Feb-2018|
|Citation:||Hartman, JD, Quinn, SN, Bakos, GÁ, Torres, G, Kovács, G, Latham, DW, Noyes, RW, Shporer, A, Fulton, BJ, Esquerdo, GA, Everett, ME, Penev, K, Bhatti, W, Csubry, Z. (2018). HAT-TR-318-007: A Double-lined M Dwarf Binary with Total Secondary Eclipses Discovered by HATNet and Observed by K2. \aj, 155 (114 - 114. doi:10.3847/1538-3881/aaa844|
|Type of Material:||Journal Article|
|Journal/Proceeding Title:||Astronomical Journal|
|Version:||Final published version. This is an open access article.|
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