[mesa-users] Implementation of shellular rotation

[Bill Paxton]

Hi Leo,

It would be wonderful to have someone do an update to the hydro_rotation.f90 code along the lines you suggest.  Is that something you might be interested in doing as a contribution to the development of mesa/star?  Perhaps you could start with the specific issue you mention -- you've tracked down the site of the problem, can you now propos changes to the relevant lines of code to implement what you would like to have?  If so great.  If not, that's okay too; it will just take longer to happen.

Cheers,
Bill


On Oct 12, 2015, at 7:59 AM, Oe orst wrote:

> Hi all,
> I have a question concerning the implementation of shellular rotation in MESA.
> In your second instrumental paper you refer to Endal&Sofia 1976 for
> calculating the modified equations of stellar structure.
> In this paper they use for the effective local gravity
>  
> g = dPsi/dn
>  
> where dn is the distance between surfaces of Psi=const and
> Psi is the total potential.
>  
> But this isn't true for shellular rotation since in that case
> g can't be derived from a potential (e.g.  Meynet&Maeder 1996 A1.1.1).
> Looking into 'mesa/star/private/hydro_rotation.f90' I wasn't able to
> find any modifications of the method of Endal&Sofia as for example proposed in
> A.8 of Meynet&Maeder 1996 (e.g. at line 607 of your code).
>  
> Is there something I am missing? 
>  
> Many greetings
> Leo
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