I need some guidance to understand and properly use MESA.

My ultimate goal is to modify it such that I can use a variable G.

I saw a video using it to predict the evolution of a main-sequence star. I don't quite understand how it is used to predict observations (Stellar Population).

I am familiar with the Kennicutt-Schmidt Law, relating the rate of galaxy formation and gas surface density

https://en.wikipedia.org/wiki/Kennicutt%E2%80%93Schmidt_law

The Tolman surface brightness test (surface brightness versus z), might be used together with wavelength information to determine star population as a function of z.

Then there is the initial mass function

It is not clear how this initial mass function would be changed in an epoch-dependent G.

IN SUMMARY

This is a very early stage of exploration of the issue of Stellar Population Modeling, Star Evolution under MESA.

Advice and comments are welcomed.

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