[mesa-users] Learning stellar evolution and asteroseismology using MESA

[Francis Timmes]

you’re welcome cyrus.

> I realized that obtaining a RRL star which would pulsate in its fundamental
> and first overtone wasn't easy, and the parameters had to be chosen carefully.


mesa is akin to concert grand piano. 
a pianist needs practice with it to make beautiful music.

fxt





> On Mar 5, 2015, at 4:14 PM, Cyrus Zalian <thebigkiwi2003 at yahoo.fr> wrote:
> 
> Thanks a lot for your help Aaron.
> 
> Once again, I learnt more (and memorized more) with Mesa than I did in years.
> 
> As you've suggested, I've based my stopping condition on he4 and ran the calculation with at the same time an HR diagram where the flag for the theoretic instability strip was on. Once finished, I've looked back to the save diagrams and choose which model I would use with Gyre, spotting the ones in the IS (makes me re-run the program but for few steps).
> 
> I was surprised that the frequencies I obtained were relevant for two reasons.
> 
> 1) I used "naïve" inlists : nothing fancy in it (no wind, rotation, or other non default option I don't know about).
> 
> 2) I have a dramatic lack of knowledge.
> 
> Of course, there were some bad news : I realized that obtaining a RRL star which would pulsate in its fundamental and first overtone wasn't easy, and the parameters had to be chosen carefully.
> 
> All in all, I will continue pursuing my goal of plotting a Petersen diagram for RRL using mesa, but it will take me a lot more time than I taught...and in the meantime, I will have to use existing ones :(
> 
> However, thank you fir your help Aaron, and also once again Josiah and Francis.
> 
> 
> Le 27 févr. 2015 02:16, "Aaron Dotter" <aaron.dotter at gmail.com> a écrit :
> Hi Cyrus, 
> 
> 1) Find a stopping condition or a selecting condition for RR Lyrae. I'll have to jump in books and papers to find (and as I'm one a tight schedule, any help would be welcomed)
> 
> RR Lyrae stars have, generally speaking, low mass (M_initial < 0.9 Msun), low metallicity ([Fe/H] < -1), and old ages ( > 10 Gyr).
> 
> They are core He-burning stars so you can stop with something like
> 
>     xa_central_lower_limit_species(1) = 'he4'
>     xa_central_lower_limit(1) = 1d-5
> 
> You might also find it useful to identify when the star enters and exits the instability strip.  See this paper for some suggestions on the identification of the RRL instability strip in terms of effective temperature.
> 
> Aaron
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