A 0.24+0.18 M double-lined eclipsing binary from the HATSouth survey

Abstract

We report the discovery and characterization of a new M-dwarf binary, with component masses and radii of M<inf>1</inf> = 0.244+0.003<inf>-0.003</inf> M<inf>⊙</inf>, R<inf>1</inf> = 0.261+0.006<inf>-0.009</inf> R<inf>⊙</inf>, M<inf>2</inf> = 0.179+0.002<inf>-0.001</inf> M<inf>⊙</inf>, R<inf>2</inf> = 0.218+0.007<inf>-0.011</inf> R<inf>⊙</inf>, and orbital period of ~4.1 d. The M-dwarf binary HATS551Š027 (LP 837Š20) was identified as an eclipsing binary by the HATSouth survey, and characterized by a series of high-precision photometric observations of the eclipse events, and spectroscopic determinations of the atmospheric parameters and radial velocity orbits. HATS551-027 is one of few systems with both stellar components lying in the fully convective regime of very low mass stars, and can serve as a test for stellar interior models. The radius of HATS551-027A is consistent with models to 1σ, whilst HATS551-027B is inflated by 9 per cent at 2σ significance. We measure the effective temperatures for the two stellar components to be T<inf>eff, 1</inf> = 3190 ± 100 K and T<inf>eff, 2</inf> = 2990 ± 110 K; both are slightly cooler than theoretical models predict, but consistent with other M-dwarfs of similar masses that have previously been studied. We also measure significant H α emission from both components of the binary system, and discuss this in the context of the correlation between stellar activity and the discrepancies between the observed and model temperatures.