Empirical bolometric correction coefficients for nearby main-sequence stars in the Gaia era

Eker Z., Soydugan F., Bilir S., Bakış V., Aliçavuş F., Özer S., ...More

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, vol.496, no.3, pp.3887-3905, 2020 (SCI-Expanded) identifier

  • Publication Type: Article / Article
  • Volume: 496 Issue: 3
  • Publication Date: 2020
  • Doi Number: 10.1093/mnras/staa1659
  • Journal Name: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
  • Journal Indexes: Science Citation Index Expanded (SCI-EXPANDED), Scopus, Academic Search Premier, Aerospace Database, Applied Science & Technology Source, Communication Abstracts, INSPEC, Metadex, zbMATH, DIALNET, Civil Engineering Abstracts
  • Page Numbers: pp.3887-3905
  • Keywords: stars: fundamental parameters, stars: binaries: eclipsing, stars: binaries: spectroscopic, Sun: general; astrophysics, solar and stellar astrophysics
  • Çanakkale Onsekiz Mart University Affiliated: Yes

Abstract

Nearby detached double-lined eclipsing binaries with most accurate data were studied and 290 systems were found with at least one main-sequence component having a metallicity of 0.008 <= Z <= 0.040. Stellar parameters, light ratios, Gaia Data Release 2 trigonometric parallaxes, extinctions and/or reddening were investigated and only 206 systems were selected as eligible to calculate empirical bolometric corrections. NASA/IPAC Galactic dustmaps were the main source of extinctions. Unreliable extinctions at low Galactic latitudes vertical bar b vertical bar <= 5 degrees were replaced with individual determinations, if they exist in the literature, else associated systems were discarded. The main-sequence stars of te remaining systems were used to calculate the bolometric corrections (BCs) and to calibrate the BC-T-eff relation, which is valid in the range 3100-36 000 K. De-reddened (B - V)(0) colours, on the other hand, allowed us to calibrate two intrinsic colour-effective temperature relations; the linear one is valid for T-eff > 10 000 K, while the quadratic relation is valid for T-eff < 10 000 K; that is, both are valid in the same temperature range in which the BC-Teff relation is valid. New BCs computed from Teff and other astrophysical parameters are tabulated, as well.