TY - JOUR
T1 - HAT-TR-318-007
T2 - A Double-lined M Dwarf Binary with Total Secondary Eclipses Discovered by HATNet and Observed by K2
AU - Hartman, J. D.
AU - Quinn, S. N.
AU - Bakos, G. A.
AU - Torres, G.
AU - Kovács, G.
AU - Latham, D. W.
AU - Noyes, R. W.
AU - Shporer, A.
AU - Fulton, B. J.
AU - Esquerdo, G. A.
AU - Everett, M. E.
AU - Penev, K.
AU - Bhatti, W.
AU - Csubry, Z.
N1 - Funding Information:
Partial support for the work reported here was provided by NASA grants NNX09AB29G, NNX13AJ15G, NNX14AE87G, and NNX17AB61G and NSF grant AST-1108686. G.T. acknowledges partial support for this work from NSF grant AST-1509375. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts.
Publisher Copyright:
© 2018. The American Astronomical Society. All rights reserved.
PY - 2018/3
Y1 - 2018/3
N2 - 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 ± 0.011M⊙N, MB 0.2721-0.0042+0.0041 M⊙N, RA 0.4548-0.0036+0.0035R⊙N, and RB 0.2913-0.0024+0.0023R⊙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 STA = M3.71 ± 0.69 and STB = M5.01 ± 0.73 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 0.2M⊙N < M < 0.5M⊙N, 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.
AB - 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 ± 0.011M⊙N, MB 0.2721-0.0042+0.0041 M⊙N, RA 0.4548-0.0036+0.0035R⊙N, and RB 0.2913-0.0024+0.0023R⊙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 STA = M3.71 ± 0.69 and STB = M5.01 ± 0.73 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 0.2M⊙N < M < 0.5M⊙N, 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.
KW - binaries: eclipsing
KW - stars: fundamental parameters
KW - stars: individual (HAT-TR-318-007, EPIC 211432946)
KW - stars: late-type
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U2 - 10.3847/1538-3881/aaa844
DO - 10.3847/1538-3881/aaa844
M3 - Article
AN - SCOPUS:85043501852
SN - 0004-6256
VL - 155
JO - Astronomical Journal
JF - Astronomical Journal
IS - 3
M1 - 114
ER -