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

被引:60
作者
Eker, Z. [1 ]
Soydugan, F. [2 ,3 ,4 ]
Bilir, S. [5 ]
Bakis, V [1 ]
Alicavus, F. [2 ,3 ,4 ]
Ozer, S. [2 ,3 ,4 ]
Aslan, G. [1 ]
Alpsoy, M. [1 ]
Kose, Y. [1 ]
机构
[1] Akdeniz Univ, Fac Sci, Dept Space Sci & Technol, TR-07058 Antalya, Turkey
[2] Canakkale Onsekiz Mart Univ, Fac Arts & Sci, Dept Phys, TR-17100 Canakkale, Turkey
[3] Canakkale Onsekiz Mart Univ, Astrophys Res Ctr, TR-17100 Canakkale, Turkey
[4] Canakkale Onsekiz Mart Univ, Ulupinar Observ, TR-17100 Canakkale, Turkey
[5] Istanbul Univ, Fac Sci, Dept Astron & Space Sci, TR-34119 Istanbul, Turkey
关键词
stars: fundamental parameters; stars: binaries: eclipsing; stars: binaries: spectroscopic; Sun: general; astrophysics; solar and stellar astrophysics; ECLIPSING BINARIES PROGRAM; EFFECTIVE TEMPERATURES; ABSOLUTE DIMENSIONS; APSIDAL MOTION; LOW-MASS; PHYSICAL PARAMETERS; DETACHED BINARY; SHORT-PERIOD; SYSTEM; COLORS;
D O I
10.1093/mnras/staa1659
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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.
引用
收藏
页码:3887 / 3905
页数:19
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