[mesa-users] oscillation data
Bill Paxton
paxton at kitp.ucsb.edu
Sun Jun 23 17:44:51 EDT 2013
Hi Rich,
So you suggest caution --- but what do you want me to "cautiously" write in the star code that produces data for GYRE?
Should I leave it as is (without the eps_grav) or change it to be like the FGONG/OSC output?
-B
On Jun 23, 2013, at 2:40 PM, Richard Townsend wrote:
>
> On Jun 23, 2013, at 10:17 PM, Bill Paxton wrote:
>
>>
>> On Jun 23, 2013, at 2:12 PM, Ehsan Moravveji wrote:
>>
>>> SIGH,
>>> I am all safe now.
>>>
>>> Thanks Bill for the clarification regarding the extra source heats.
>>> Are you also going to update /star/private/pulsation_info.f in this regard?
>>
>> I don't think there is anything that needs to be changed in the code --- unless Rich tells me differently.
>> The FGONG/OSC VAR(9) assignments in the code match the documentation.
>> Of course, I'm naively assuming that matching the documentation is a good thing in this case.
>>
>> Now we'll wait to see if Rich wants to change epsilon for GYRE to be like epsilon in FGONG/OSC files.
>> The GYRE documentation says epsilon = "energy generation rate (ers/s/gm)", so I may need to add on the eps_grav term.
>>
>
> I'm not sure myself what the best approach is here. It's worth remarking that the eps_grav term is only appreciably non-zero when a star *isn't* in thermal equilibrium; yet the non-adiabatic pulsation equations are typically derived under the assumption of thermal equilibrium. So some caution is definitely in order in including/neglecting the eps_grav term.
>
> cheers,
>
> Rich
>
>>> It will be very fruitful to discuss with the mesa-user community how to write the epsilon term.
>>> I also do not know the observational status of mode excitation in binaries beyond the canonical kappa driven instability.
>>>
>>> Best regards
>>> Ehsan.
>>
>>
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