Astrophysics (index)

Stellar Luminosity Determination

(methods by which the luminosity of a star is determined)

Stellar Luminosity Determination at its most accurate and reliable, i.e., for nearby stars, is done by Stellar Radius Determination and Stellar Temperature Determination for its Effective Temperature (Teff), the Luminosity (L) determined by the relationship of the three.

When a reliable Stellar Distance Determination is available, e.g., from Parallax measurements, the distance's effect on the Apparent Magnitude (m) can be accounted for and the Absolute Magnitude (M) can be determined along with the Bolometric Magnitude (Mbol) which is just another measure of luminosity.

At further distances, the relationship of luminosity to Spectral Class is used, but this is a rough estimate and depends upon whether the star is a Main Sequence Star versus one a giant phase, which greatly affects the expected radius.


Referenced by:
Stellar Parameter Determination