[mesa-users] The Cepheid phase

[RICHARD H D TOWNSEND]

Hi Earl —

> On Jul 29, 2016, at 9:33 AM, Earl Bellinger <earlbellinger at gmail.com> wrote:
> 
> Hello everybody,
> 
> In Dziembowski's 2012 paper [1] the claim is made that:
> 
>> "BaSTI (Pietrinferni et al. 2006) models at M = 4 and 5 do not rich the instability strip but the maximum values of L in this evolutionary phase are in a good agreement with the relation given by Eq. (2). Similar conclusion was reached by Smolec (private communication), who used public domain code MESA (Paxton et al. 2011). Apparently, new evolutionary codes do not describe well the Cepheid phase."
> 
> Can anyone corroborate/evaluate this claim for me please? That is: is
> MESA suitable for investigating Cepheid stars? If not, why not?
> 

Yes, absolutely it is!

> For example, can a theoretical Cepheid Period-Luminosity relation be
> derived using MESA plus a pulsation code (ADIPLS/GYRE/etc)?
> 

See figure 14 of Paxton et al. (2015) (the third instrument paper) — there, we reproduce the blue edge of the instability strip using MESA and GYRE.

cheers,

Rich

> Thanks for any insights.
> 
> [1] http://acta.astrouw.edu.pl/Vol62/n4/pdf/pap_62_4_1.pdf
> 
> Best regards,
> Earl Bellinger
> Stellar Ages & Galactic Evolution Group
> Max-Planck-Institut für Sonnensystemforschung
> 
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