What is the relationship of mass luminosity?
The relationship of bulk luminosity is an astrophysical law that concerns the luminosity or brightness of the star to its mass. For the main sequential stars, the average relationship is given l = m 3.5
and Hertzsprung-Russell Diagram (HRD) is a graph where the clay of the star is brightness due to its surface temperature. The vast majority of well -known stars fall into the hot stars with high luminous intensity to cold stars with low luminosity. This band is referred to as the main sequence. Although it was found that it had evolved before the nuclear fusion source of the energy of the star, the throat gave the theoretical traces to derive the thermodynamic properties of the star.
English astrophysicist Arthur Eddington founded his development relationship of mass luminosity on the throat. His shelterP considered the stars as if they were composed of an ideal gas, a theoretical construct that simplifies the calculation. The star was also considered a black body or a perfect radiation emitter. Using the Stefan-Boltzmann law, the stars' luminosity can be estimated with respect to its surface area and therefore its volume can be estimated.
In the hydrostatic balance, the compression of the star of the star due to gravity is balanced by the internal pressure of the gas and creates a ball. For the spherical volume of the same mass objects as the star composed of ideal gas, the virial sentence provides an estimate of the overall potential energy of the body. This value can be used to derive the approximate weight of the star and this value with its luminosity.
Theoretical approximation of Eddington for the relationship of bulk luminosity was verified by the independent of nearby binary stars. Stars mass can be determined from the exploration of their orbit and their distanceestablished by Kepler's laws. Once their distance and obvious brightness are known, luminosity can be calculated.
The weight luminosity relationship can be used to find the distance of binary files that are too far for optical measurement. Iteration technique is used, where the approximation of matter is used in Kepler's laws to obtain the distance between the stars. The arc of the body subtend in the sky and the approximate distance separating both brings the initial value for their distance from the ground. From this value and their apparent size it is possible to determine their luminosity and by the relationship of material luminosity of their mas. The weight value is then used to convert the distance separating the star and the process is repeated until the required accuracy