AST 341 Lecture Notes - Lecture 12: Hans Kramers, Compton Scattering, Electron Scattering

• School: Stony Brook University
• Department: Astronomy
• Course: AST 341
• Professor: Rosalba Perna

Document Summary

Let"s gather the equations that we have rived so far: dm dr = 4 r2 dr = 4 r2 q dr = gm r2 dr = 3. These are four equations with ve variables: m(r), p (r), t (r), l(r), (r). Therefore, we need another equation relating some of them. This is the so-called equation of state, i. e. a relation between pressure, density, and temperature. Furthermore, we also need an expression for the opacity and for the energy equation q in terms of our basic variables: equation of state. The interior of a star contains a mixture of ions, electrons and radiation (photons). For most stars (except very low mass stars and stellar remnants) the ions and electrons can be treated as an ideal gas and quantum e ects can be neglected. P = pgas + prad (1) where pgas = pion + pel.