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.