Their great stellar luminosities are determined from various spectral features, which are sensitive to surface gravity, such as H? line widths in hot stars or a strong Balmer discontinuity in cooler stars.
12.
For perspective, the overall range of stellar luminosities runs from dwarfs less than 1 / 10, 000th as luminous as the Sun, to supergiants over 1, 000, 000 times more luminous.
13.
This led to systematic differences in bolometric corrections scales, which when combined with incorrect assumed absolute bolometric magnitudes for the Sun could lead to systematic errors in estimated stellar luminosities ( and stellar properties calculated which rely on stellar luminosity, such as radii, ages, and so on ).
14.
This led to systematic differences in bolometric corrections scales, which when combined with incorrect assumed absolute bolometric magnitudes for the Sun could lead to systematic errors in estimated stellar luminosities ( and stellar properties calculated which rely on stellar luminosity, such as radii, ages, and so on ).
15.
In the current system of stellar classification, stars are grouped according to temperature, with the massive, very young and energetic Class M stars exhibit temperatures less than 3, 500 K . Because luminosity is proportional to temperature to the fourth power, the large variation in stellar temperatures produces an even vaster variation in stellar luminosity.
