Mass-luminosity Relation
Related Category: Astronomy: General
in astronomy, law stating that the luminosity of a star is proportional to some power of the mass of the star. More massive stars are in general more luminous.
mass-luminosity relation
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Mass-Luminosity Relation Explained
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mass-luminosity relation The dependence of the luminosity of a main-sequence star on its mass. The luminosity increases roughly as the mass raised to the third power.
mass-luminosity relation: The more massive a star is, the more luminous it is.
Maunder butterfly diagram: A graph showing the latitude of sunspots versus time; first plotted by W. W. Maunder in 1904.
Mass-Luminosity Relation - The relationship between luminosity and mass for stars. More massive stars have greater luminosities
Maunder Minimum - A period of few sunspots and low solar activity that occurred between 1640 and 1700 ...
mass-luminosity relation - (n.)
A well-defined relation between the mass and luminosity for main sequence stars.
mass number A - (n.) ...
Mass-Luminosity relation for Main Sequence stars
L ~ M 3.5, eg M0 = 0.5 Msun; A0 = 4Msun
MS lifetime shorter for higher Mass
Luminosity Function (census by brightness) ...
Mass-Luminosity Relation - used for Main Sequence stars to estimate their luminosity.
Formula:L = M3.5 where: ...
Using the mass-luminosity relationship for main sequence stars:
L ∼ M3.5
and substituting for L, we have the expression for main sequence lifetime in terms of stellar mass: ...
The exact mass-luminosity relationship depends on how efficiently energy can be transported from the core to the surface.
Answer: Using the mass-luminosity relationship, valid for stars along the main sequence, Star X's mass is 1001/3.5 solar masses. This is equal to 3.7 solar masses.
An astrophysicist, discovered the stellar mass-luminosity relationship, explained Cepheid variable pulsations and very high densities of white dwarfs, formulated the Eddington Limit which relates star’ ...
Relating these masses to the luminosity of the galaxy, we develop a mass-luminosity relation for galaxies that is applied to estimate masses of galaxies too distance to obtain a rotation curve or velocity dispersion.
This is an incredibly useful relationship, called the mass-luminosity relation. If we know where on the main sequence a star is we can infer its mass.
With these assumptions, he demonstrated that the interior temperature of stars must be millions of degrees. He discovered the mass-luminosity relationship for stars, ...
Eddington also investigated the interior of stars, and calculated their temperature based on what would be necessary to withstand the pressure of the higher-laying layers. He discovered the mass-luminosity relationship for stars, ...
Arthur S. Eddington
1882-1944
British
first to confirm Einstein's prediction that light will bend near a star; discovered the mass-luminosity relation for stars; theoretically explained the pulsation of Cepheid variables ...
The ``parallax" (i.e., distance) for a binary star whose orbit is well known, derived by using the mass-luminosity relation and Newton's generalization of Kepler's third law.
Dynamical Time ...
where N(M) the number of stars of mass M within a specified volume of space is proportional to M^{-alpha} where alpha is a dimensionless exponent. The IMF can be estimated from the initial luminosity function by using the mass-luminosity relation.
 See also: Luminosity, Mass, Star, Sun, Astronomy
  
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