The interior of stars (part VII)
16 Abril 2020, 14:00 • Israel Matute
During this lecture, we continued discussing how some approximations can be used for stellar models so that costly numerical solutions do not have to be computed for every single model. We saw
The advantage of parameterizing the eq. of stellar structure as a function of mass and not as a function of radius: the Vogt-Russell theorem;
We discussed the advantage of normalizing the equations as a function of mass and how this leads to the concept of homologous stars:
The homologous relations for stars under the approximation of ideal gas are introduced and discussed. The form that many of these relations (especially the one link L and effective temperature) allow a better understanding of the HR diagram;
Approximations to the computation of opacities: Kramers opacity, etc.
Stellar-mass limits in the Main-Sequence: the Eddington luminosity
Example of an extreme stellar system: Eta-Carinae