[mesa-users] Calculating oscillation modes of higher degree

[Bill Paxton]

Hi Wiebke,

On Nov 25, 2014, at 11:31 AM, Wiebke Herzberg wrote:

> Is it indeed a problem with the hydrostatic equilibrium that hampers the mode calculation? 



Pieter Degroote has repeatedly told me that the hydrostatic equilibrium solutions in mesa/star were not a problem.
This quote is from a 2013 email from Pieter to me on the topic of numerical issues including hydrostatic equilibrium in mesa/star models for asteroseisomology:

On Feb 25, 2013, at 5:48 AM, Pieter Degroote wrote:

> In real applications, people still interpolate the model themselves to have a higher mesh density in the center (for gravity modes) or envelope (for pressure modes). So they will interpolate the model anyway, breaking numerical hydrostatic equilibrium anyway unless this is forced. Joergen actually prefers to  reintegrate the models to satisfy (his definition of) equilibrium (but in the process changing their mass or radius slightly)



I don't understand what Rich had in mind when he suggested that hydrostatic balance in the model might be the problem.  Perhaps he can elaborate on that -- and provide us with a good solution too!   I certainly hope so.   And perhaps there are also other users who can also comment on this issue.  I'd be interested to hear more.


-Bill


 
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