A low-mass eclipsing binary within the fully convective zone from the Next Generation Transit Survey

2018/08/08 by S. L. Casewell, L. Raynard, Liam Raynard +35 · 18 citations
Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Astrophysics and Star Formation Studies #Binary number #Binary star #Brown dwarf #Eclipse #Low Mass #Main sequence #Physics #RADIUS #Star formation #Stars #Stellar mass #Stellar, planetary, and galactic studies #Transit (satellite) #astro-ph.SR

paper · pdf · open access · doi:10.1093/mnras/sty2183

published in Monthly Notices of the Royal Astronomical Society 481(2), 1897-1907 (Oxford University Press) · 12 pages, 9 Figures, Accepted for publication in MNRAS

arxiv created 2018/08/08 · openalex publication_date 2018/08/13 · openalex created_date 2018/08/22 · arxiv updated 2018/09/19 · openalex updated_date 2026/08/05

Abstract

We have discovered a new, near-equal-mass, eclipsing M dwarf binary from the Next Generation Transit Survey. This system is only one of three field-age (>1 Gyr), late M dwarf eclipsing binaries known, and has a period of 1.74774 d, similar to that of CM Dra and KOI126. Modelling of the eclipses and radial velocities shows that the component masses are Mpri =|0.17391 ^+0.00153_-0.00099| M⊙, Msec = |0.17418 ^+0.00193_-0.00059| M⊙; and the radii are Rpri = |0.2045 ^+0.0038_-0.0058| R⊙, Rsec= |0.2168 ^+0.0047_-0.0048| R⊙. The effective temperatures are |T_{\rm pri}=2995 ⁺⁸⁵_-105| K and |T_{\rm sec}=2997 ⁺⁶⁶_-101|K, consistent with M5 dwarfs and broadly consistent with main-sequence models. This pair represents a valuable addition that can be used to constrain the mass–radius relationship at the low-mass end of the stellar sequence.

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