The EBLM Project: V. Physical properties of ten fully convective, very-low-mass stars

Research output: Contribution to journalArticlepeer-review

Authors

  • Alexander von Boetticher
  • Didier Queloz
  • Sam Gill
  • Pierre F. L. Maxted
  • Yaseen Almleaky
  • David R. Anderson
  • Francois Bouchy
  • Artem Burdanov
  • Andrew Collier Cameron
  • Laetitia Delrez
  • Elsa Ducrot
  • Francesca Faedi
  • Michaël Gillon
  • Yilen Gómez Maqueo Chew
  • Leslie Hebb
  • Coel Hellier
  • Emmanuël Jehin
  • Monika Lendl
  • Maxime Marmier
  • David V. Martin
  • James McCormac
  • Francesco Pepe
  • Don Pollacco
  • Damien Ségransan
  • Barry Smalley
  • Samantha Thompson
  • Oliver Turner
  • Stéphane Udry
  • Valérie Van Grootel
  • Richard West

Colleges, School and Institutes

Abstract

Measurements of the physical properties of stars at the lower end of the main sequence are scarce. In this context we report masses, radii and surface gravities of ten very-low-mass stars in eclipsing binary systems, with orbital periods of the order of several days. The objects probe the stellar mass-radius relation in the fully convective regime, $M_\star \lesssim 0.35$ M$_\odot$, down to the hydrogen burning mass-limit, $M_{\mathrm{HB}} \sim 0.07$ M$_\odot$. The stars were detected by the WASP survey for transiting extra-solar planets, as low-mass, eclipsing companions orbiting more massive, F- and G-type host stars. We use eclipse observations of the host stars (TRAPPIST, Leonhard Euler, SPECULOOS telescopes), and radial velocities of the host stars (CORALIE spectrograph), to determine physical properties of the low-mass companions. Companion surface gravities are derived from the eclipse and orbital parameters of each system. Spectroscopic measurements of the host star effective temperature and metallicity are used to infer the host star mass and age from stellar evolution models. Masses and radii of the low-mass companions are then derived from the eclipse and orbital parameters of each system. The objects are compared to stellar evolution models for low-mass stars, to test for an effect of the stellar metallicity and orbital period on the radius of low-mass stars in close binary systems. Measurements are in good agreement with stellar models; an inflation of the radii of low-mass stars with respect to model predictions is limited to 1.6 $\pm$ 1.2% in the fully convective regime. The sample of ten objects indicates a scaling of the radius of low-mass stars with the host star metallicity. No correlation between stellar radii and orbital periods of the binary systems is determined. A combined analysis with comparable objects from the literature is consistent with this result.

Bibliographic note

19 pages

Details

Original languageEnglish
Article numberA150
Number of pages18
JournalAstronomy and Astrophysics
Volume625
Publication statusPublished - 1 May 2019

Keywords

  • astro-ph.SR, astro-ph.EP, stars: low-mass, binaries: eclipsing, binaries: spectroscopic, techniques: spectroscopic, techniques: photometric