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## Main Question or Discussion Point

I'm trying to teach myself some of the early basics of stellar modelling and hope to write some code to calculate conditions within the star

Assuming a constant and homogenous composition and simplified calculations of pressure equation of state and opacity. Simplified assumption of adiabatic convection.

From what i've been able to figure out:

1. Use the ideal gas law and radiation pressure equation to solve for local density.

2. Use local density to determine opacity and energy generation rate of that layer.

3. Now use the differential equations for pressure, internal mass, temperature and luminosity to solve for those quanitities. Convert them to "difference equations" and solve for an outer layer and an inner layer that is very close to the outer.

4. Now use those quantities to solve for a new local density as in step one

5. Repeat process, going deeper into the star.

Is this a simplified way of doing this, or at least a decent starting point?

I'd appreciate any input, keeping in mind I am just learning the basics

Assuming a constant and homogenous composition and simplified calculations of pressure equation of state and opacity. Simplified assumption of adiabatic convection.

From what i've been able to figure out:

1. Use the ideal gas law and radiation pressure equation to solve for local density.

2. Use local density to determine opacity and energy generation rate of that layer.

3. Now use the differential equations for pressure, internal mass, temperature and luminosity to solve for those quanitities. Convert them to "difference equations" and solve for an outer layer and an inner layer that is very close to the outer.

4. Now use those quantities to solve for a new local density as in step one

5. Repeat process, going deeper into the star.

Is this a simplified way of doing this, or at least a decent starting point?

I'd appreciate any input, keeping in mind I am just learning the basics