ON THE USE OF EMPIRICAL BOLOMETRIC CORRECTIONS FOR STARS

By G. Torres. 2010

322 citations recorded by the source corpus.

When making use of tabulations of empirical bolometric corrections for stars (BCV), a commonly overlooked fact is that while the zero point is arbitrary, the bolometric magnitude of the Sun (Mbol,☉) that is used in combination with such tables cannot be chosen arbitrarily. It must be consistent with the zero point of BCV so that the apparent brightness of the Sun is reproduced. The latter is a measured quantity, for which we adopt the value V☉ = −26.76 ±  0.03. Inconsistent values of Mbol,☉ are listed in many of the most popular sources of BCV. We quantify errors that are introduced by failure to pay attention to this detail. We also take the opportunity to reprint the BCV coefficients of the often used polynomial fits by Flower, which were misprinted in the original publication.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/bb6fc36e99b28c1db242039ed76cf12a2a1749d8

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Citations in the corpus

• Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems (2014, background): “Therefore, any value of MBol, is equally legitimate, on the condition that once chosen, all BCs are rescaled accordingly (e.g., Torres 2010).”
• A UNIFORM ASTEROSEISMIC ANALYSIS OF 22 SOLAR-TYPE STARS OBSERVED BY KEPLER (2012, methodology): “We applied the bolometric correction of Flower (1996) as tabulated in Torres (2010), adopting a solar bolometric absolute magnitude Mbol,⊙ = 4.73± 0.03 to ensure internal consistency.”
• A Guide to Realistic Uncertainties on the Fundamental Properties of Solar-type Exoplanet Host Stars (2020, methodology): “…photometry in combination with model atmospheres (SED fitting, e.g. van Belle & von Braun 2009; Huber et al. 2012; Mann et al. 2013; Stassun & Torres 2016) or by applying bolometric corrections derived from model atmospheres (e.g. Alonso et al. 2004; Torres 2010; Casagrande & VandenBerg 2018).”
• FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROM KEPLER AND CoRoT AND INTERFEROMETRY FROM THE CHARA ARRAY (2012, methodology): “…determined effective temperatures and metallicities to estimate a bolometric correction for each star using the calibrations by Flower (1996) and Alonso et al. (1999) with appropriate zero-points as discussed in Torres (2010), yielding the stellar luminosity given in the last column of Table 1.”
• MaGICC discs: matching observed galaxy relationships over a wide stellar mass range (2012, methodology): “To model the luminosity of stars, a simple fit of the mass–luminosity relationship observed in binary star systems by Torres (2010) is used: L L = ⎧⎪⎪⎪⎨ ⎪⎪⎪⎩ ( M M )4 , M < 10 M 100 ( M M )2 , M > 10 M .”
• INTRINSIC COLORS, TEMPERATURES, AND BOLOMETRIC CORRECTIONS OF PRE-MAIN-SEQUENCE STARS (2013, background): “Young Stellar Colors and Temperatures 11 Though the zero point of the bolometric correction scale is arbitrary, the combination of bolometric correction and solar absolute bolometric magnitude is not (see Torres 2010 and Appendix D of Bessell et al. 1998).”
• NOMINAL VALUES FOR SELECTED SOLAR AND PLANETARY QUANTITIES: IAU 2015 RESOLUTION B3 (2016, background): “The definition of the zero point of the bolometric magnitude scale has been set (M 0bol corresponds exactly to L=3.0128×1028W; see IAU 2015 Resolution B2;E. Mamajek et al.2016, in preparation), but bolometric corrections still need to be nominalized (Torres 2010).”
• Confirmation of the Gaia DR2 Parallax Zero-point Offset Using Asteroseismology and Spectroscopy in the Kepler Field (2018, methodology): “…cm−2, and an apparent solar bolometric magnitude of mbol=−26.82 (using the visual magnitude of the Sun, Ve=−26.76, and its visual bolometric correction, BCV,e=−0.06; Torres 2010); BC is the bolometric correction, which depends on the photometric bandpass used, b, and the temperature; and Ab is…”
• The Second APOKASC Catalog: The Empirical Approach (2018, methodology): “We adopt V-band bolometric corrections from Flower (1996) with the erratum from Torres (2010), using the spectroscopic Teff values from DR13.”
• Gaia Data Release 2 (2018, methodology): “Given its distance and its measured V-band magnitude, V = −26.76 ± 0.03, the absolute magnitude MV = 4.81 is calculated and the BCV is derived: BCV = 4.74 − 4.81 = −0.07 mag (Torres 2010).”
• Thin disc, thick disc and halo in a simulated galaxy (2012, methodology): “We model the luminosity of stars using the Torres (2010) mass–luminosity relationship.”
• The dependence of dark matter profiles on the stellar-to-halo mass ratio: a prediction for cusps versus cores (2013, methodology): “The luminosity of stars is modelled with a simple fit ofhe mass-luminosity relationship observed in binary systems (Torres 2010): L L⊙ = { (M/M⊙) 4, M < 10M⊙ 100 (M/M⊙) 2, M > 10M⊙ (2) Typically, this model corresponds to the emission of2 × 1050 erg perM⊙ of the entire stellar population over…”