The Mass and Radius of the Unseen M-Dwarf Companion in the Single-Lined Eclipsing Binary HAT-TR-205-013

Abstract

We derive masses and radii for both components in the single-lined eclipsing binary HAT-TR-205-013, which consists of a F7V primary and a late M-dwarf secondary. The system's period is short, $P=2.230736\pm 0.000010$ days, with an orbit indistinguishable from circular, $e=0.012\pm 0.021$. We demonstrate generally that the surface gravity of the secondary star in a single-lined binary undergoing total eclipses can be derived from characteristics of the light curve and spectroscopic orbit. This constrains the secondary to a unique line in the mass-radius diagram with $M/R^2$ = constant. For HAT-TR-205-013, we assume the orbit has been tidally circularized, and that the primary's rotation has been synchronized and aligned with the orbital axis. Our observed line broadening, $V_{\mathrm{rot}}\sin i_{\mathrm{rot}}=28.9\pm 1.0$ \kms, gives a primary radius of $R_{\mathrm{A}}=1.28\pm 0.04$ \rsun. Our light curve analysis leads to the radius of the secondary, $R_{\mathrm{B}}=0.167\pm 0.006$ \rsun, and the semimajor axis of the orbit, $a = 7.54 \pm 0.30 \rsun = 0.0351 \pm 0.0014$ AU. Our single-lined spectroscopic orbit and the semimajor axis then yield the individual masses, $M_{\mathrm{B}}=0.124\pm 0.010$ \msun and $M_{\mathrm{A}}=1.04\pm 0.13$ \msun. Our result for HAT-TR-205-013 B lies above the theoretical mass-radius models from the Lyon group, consistent with results from double-lined eclipsing binaries. The method we describe offers the opportunity to study the very low end of the stellar mass-radius relation.

arXiv comment18 pages, 9 tables and 6 figures; accepted by ApJ. Added a reference and corrected a typo

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