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Having derived the four differential equations of stellar structure, we turn now to the three associated relations for P, and we introduced earlier.

P = P (, T, composition) pressure (the equation of state)
= (, T, composition) opacity
= (, T, composition) energy release per unit mass per unit time

In this part of the course we will see how P, and can be calculated if the density, , temperature, T, and chemical composition of the stellar material are known. In order to do this, we will have to look at the physics of stellar interiors, including nuclear physics, atomic physics and thermodynamics. This is a complex subject and hence only the basic physical processes which determine P, and will be described here.

©Vik Dhillon, 27th September 2010