mass-luminosity relation

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• Mass–luminosity relation — In astrophysics, the mass–luminosity relation is an equation giving the relationship between a star s mass and its luminosity. The relationship is represented by the equation: where L⊙ and M⊙ are the luminosity and mass of the sun and… …   Wikipedia

• Initial mass function — The initial mass function (IMF) is an empirical function that describes the mass distribution (the histogram of stellar masses) of a population of stars in terms of their theoretical initial mass (the mass they were formed with). The properties… …   Wikipedia

• Tully-Fisher relation — In astronomy, the Tully Fisher relation, published by astronomers R. Brent Tully and J. Richard Fisher in 1977, is an empirical relationship between the intrinsic luminosity (proportional to the stellar mass) of a spiral galaxy and its velocity… …   Wikipedia

• Faber-Jackson relation — The Faber Jackson relation is an early empirical power law relation between the luminosity L and the central stellar velocity dispersion sigma of elliptical galaxies, first noted by the astronomers Sandra M. Faber and Robert Earl Jackson in 1976 …   Wikipedia

• M-sigma relation — The M sigma (or MBH σ) relation is an empirical correlation between the stellar velocity dispersion σ of a galaxy bulge and the mass M of the supermassive black hole at the galaxy s center. The relation can be expressed mathematically as A recent …   Wikipedia

• Planetary nebula luminosity function — (PNLF) is a secondary distance indicator used in astronomy. It makes use of the [O III| [O III] λ5007 forbidden line found in all planetary nebula which are members of the old stellar populations (Population… …   Wikipedia

• Intermediate-mass black hole — An Intermediate mass black hole (IMBH) is a black hole whose mass is significantly more than stellar black holes (a few tens of the mass of the Sun) yet far less than supermassive black holes (a few millions of the mass of the Sun). There is less …   Wikipedia

• Main sequence — A Hertzsprung Russell diagram plots the actual brightness (or absolute magnitude) of a star against its color index (represented as B V). The main sequence is visible as a prominent diagonal band that runs from the upper left to the lower right.… …   Wikipedia

• Cosmic distance ladder — * Light green boxes: Technique applicable to star forming galaxies. * Light blue boxes: Technique applicable to Population II galaxies. * Light Purple boxes: Geometric distance technique. * Light Red box: The planetary nebula luminosity function… …   Wikipedia

• Séquence principale — Le diagramme de Hertzsprung Russell figure les étoiles. En abscisse, l indice de couleur (B V) ; en ordonnée, la magnitude absolue. La séquence principale se voit comme une bande diagonale marquée allant du haut à gauche au bas à droite. Ce… …   Wikipédia en Français

• Dynamical parallax — In astronomy, the distance to a visual binary star may be estimated from the masses of its two components, the size of their orbit, and the period of their revolution around one another.[1] A dynamical parallax is an (annual) parallax which is… …   Wikipedia