http://arxiv.org/abs/2304.02466
Using high-resolution spectra from the Tillinghast Reflector Echelle Spectrograph (TRES) and photometry from sector 56 of the Transiting Exoplanet Survey Satellite (TESS), we report that the nearby M dwarf G 68-34 is a double-lined eclipsing binary. The pair is spin-orbit synchronized with a period of 0.655 days. The light curve shows significant spot modulation with a larger photometric amplitude than that of the grazing eclipses. We perform a joint fit to the spectroscopic and photometric data, obtaining masses of $0.3280\pm 0.0034$M$\odot$ and $0.3207\pm 0.0036$M$\odot$ and radii of $0.345\pm 0.014$R$\odot$ and $0.342\pm 0.014$R$\odot$ after marginalizing over unknowns in the starspot distribution. This system adds to the small but growing population of fully convective M dwarfs with precisely measured masses and radii that can be used to test models of stellar structure. The pair also has a white dwarf primary at 9″ separation, with the system known to be older than 5 Gyr from the white-dwarf cooling age. The binarity of G 68-34 confirms our hypothesis from Pass et al. (2022): in that work, we noted that G 68-34 was both rapidly rotating and old, highly unusual given our understanding of the spindown of M dwarfs, and that a close binary companion may be responsible.
E. Pass and D. Charbonneau
Thu, 6 Apr 23
32/76
Comments: Accepted for publication in ApJ, 10 pages, 5 figures, 3 tables