[Mesa-users] Adds all the absolute magnitudes to the output in profiles

[Josiah Schwab]

Hi Richard,

The ultimate aim is to translate the features of the observed light curve
> into the internal physics. The observed light curve varies as a function of
> wavelength because the variation of the black body curve as a function of
> temperature is dependent on wavelength. Various things like opacity vary
> with wavelength and also with the spatial position in the star. This is why
> I would like to get the magnitudes in each zone.
>

This suggests to me that you may not understand the assumptions
underpinning stellar models like MESA.

- the radiation transport in the stellar interior/MESA model is treated in
the diffusion approximation and the opacity is the Rosseland mean (e.g.,
MESA I, Section 6.2)
- the outer boundary condition of the stellar model is typically applied
around the photosphere using an atmospheric model provided by the atm
module (e.g., MESA I, Section 5.3)
- the calculation of an absolute magnitude uses a bolometric correction
that comes from a pre-computed atmospheric model/stellar spectrum (i.e.,
MESA IV, Appendix A)

If, for instance, you are interested in learning about how photons of
different wavelengths come from different depths, you want a stellar
atmosphere model and not a MESA model.

Josiah
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