The distance to a star derived from comparison of its apparent magnitude with its absolute magnitude deduced from study of its position on an H-R diagram determined by observation of its spectrum (spectral type and luminosity class).
derivation of the star's distance (or parallax) from its apparent magnitude and its absolute magnitude on the basis of its luminosity and spectral characteristics.
a method of determining distances to stars from knowledge of the luminosity of their spectral types and measurement of their apparent brightness. The distances are derived from the inverse square law of light brightness.
Spectroscopic parallax uses the spectral classification and luminosity of a star (obtained from photometric observations) to place it on an HR diagram. By then comparing the apparent magnitude with the expected absolute magnitude a distance to the star can be estimated.
A parallax (or distance) of a star that is derived by comparing the apparent magnitude of the star with its absolute magnitude as deduced from its spectral characteristics.
Method of determining the distance to a star by measuring its temperature and then determining its absolute brightness by comparing with a standard H-R diagram. The absolute and apparent brightness of the star gives the star's distance from Earth.
The method of determining a star's distance by comparing its apparent magnitude with its absolute magnitude as estimated from its spectrum.
