Bolometric correction

Setting the correction scale

The bolometric correction scale is set by the absolute magnitude of the Sun and an adopted (arbitrary) absolute bolometric magnitude for the Sun. Hence, while the absolute magnitude of the Sun in different filters is a physical and not arbitrary quantity, the absolute bolometric magnitude of the Sun is arbitrary, and so the zero-point of the bolometric correction scale that follows from it. This explains why classic references have tabulated apparently mutually incompatible values for these quantities. The bolometric scale historically had varied somewhat in the literature, with the Sun's bolometric correction in V-band varying from -0.19 to -0.07 magnitude. It follows that any value for the absolute bolometric magnitude of the Sun is legitimate, on the condition that once chosen all bolometric corrections are rescaled accordingly. If not, this will induce systematic errors in the determination of stellar luminosities.

The XXIXth International Astronomical Union (IAU) General Assembly in Honolulu adopted in August 2015 Resolution B2 on recommended zero points for the absolute and apparent bolometric magnitude scales.

Although bolometric magnitudes have been in use for over eight decades, there have been systematic differences in the absolute magnitude-luminosity scales presented in various astronomical references with no international standardization. This has led to systematic differences in bolometric correction scales. When combined with incorrect assumed absolute bolometric magnitudes for the Sun this can lead to systematic errors in estimated stellar luminosities. Many stellar properties are calculated based on stellar luminosity, such as radii, ages, etc.

IAU 2015 Resolution B2 proposed an absolute bolometric magnitude scale where ${\displaystyle M_{\text{bol}}=0}$ corresponds to luminosity 3.0128×10²⁸ W, with the zero point luminosity chosen such that the Sun (with nominal luminosity 3.828×10²⁶ W) corresponds to absolute bolometric magnitude ${\displaystyle M_{{\text{bol}}_{\mathrm{S}\mathrm{u}\mathrm{n}}}=4.74}$. Placing a radiation source (e.g. star) at the standard distance of 10 parsecs, it follows that the zero point of the apparent bolometric magnitude scale ${\displaystyle m_{\text{bol}}=0}$ corresponds to irradiance ${\displaystyle f_o=\mathrm{2.518021002...}\times {10}^{-8}\mathrm{W}/{\mathrm{m}}^2}$, where the nominal total solar irradiance measured at 1 astronomical unit (1361 W/m²) corresponds to an apparent bolometric magnitude of the Sun of ${\displaystyle m_{{\text{bol}}_{\mathrm{S}\mathrm{u}\mathrm{n}}}=-26.832}$.

A similar IAU proposal in 1999 (with a slightly different zero point, tied to an obsolete solar luminosity estimate) was adopted by IAU Commissions 25 and 36. However it never reached a General Assembly vote, and subsequently was only adopted sporadically by astronomers in the literature.