The Structure and Evolution of Intermediate-Mass Stars
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Date
2021-01-02
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Addis Ababa University
Abstract
We explore the structure and evolution of intermediate-mass stars. Under this, we focus
on the mass-luminosity relation of the single main sequence interme diate-mass stars.
We derivate the stellar structure equations and put the fundamental stellar quantities in
terms of mass. After this, we derivate the lifetime of intermediate-mass stars in three
nuclear burning phases and relate the stellar quantities with their lifetime. Thus we
predict the relation MLR, MRR, and MTR in hydrogen core burning, hydrogen shell burning,
and helium core burning. The mass-luminosity relation is in good agreement for O.Yu.
Malkove observational work of the absolute MLR relation.In the effects of temperature
gravity and nuclear reaction, the star’s structure was varied. To determine the final
differential results of star’s structure equations, we must used the derivative of interior
stars structure equations with central radius r. This allows us to compute the M, T, P,
L, and R relations. Those are quantities derived from the stellar structure equations.
From those equations, we have obtained the mass-luminosity relation equation and using
nuclear reactions we studied the star’s mass and age relation using the simplified form
of the equations. We showed the graphical relationship of Mass to Luminosity, Mass to
Temperature, and Mass to Radius of stars in terms of a parameter of a nuclear burning
lifetime.
The lifetime equation of the star in hydrogen core burning and the mass-luminosity equation
are good ways to measure the mass-luminosity relation of B-type stars.
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Keywords
Structure, Evolution, Intermediate-Mass Stars