[mesa-users] Pulsating star in the HB using GYRE

[Ehsan Moravveji]

Hi Cyrus,
I am not so sure if ADIPLS accounts for the convection-pulsation interplay.
But, I know that two other codes which are not public do so:
1. The Liege MAD code:
    http://adsabs.harvard.edu/abs/2005A%26A...434.1055G <http://adsabs.harvard.edu/abs/2005A&A...434.1055G>
    http://adsabs.harvard.edu/abs/2012MNRAS.422L..43G <http://adsabs.harvard.edu/abs/2012MNRAS.422L..43G> 
2. The GraCo code:
    http://adsabs.harvard.edu/abs/2008AN....329..541M <http://adsabs.harvard.edu/abs/2008AN....329..541M>

Going beyond 1D, the following paper can possibly give you a pointer on reading more interesting stuff:
http://adsabs.harvard.edu/abs/2015ApJ...800...35G <http://adsabs.harvard.edu/abs/2015ApJ...800...35G> 

Best regards
Ehsan.


> On 25 Jan 2016, at 15:29, Cyrus Zalian <thebigkiwi2003 at yahoo.fr> wrote:
> 
> Thank you to everybody for their help.
> 
> So, now my question would be : would ADLIPS or any other publicly available pulsationnal code implement the convection-pulsation interaction ?
> 
> Thanks again for your help (as I said before this software is the perfect tool for learning).
> 
> 2016-01-25 11:21 GMT+01:00 László Molnár <molnar.laszlo at csfk.mta.hu <mailto:molnar.laszlo at csfk.mta.hu>>:
> Ha! Turns out my first guess was right. :)
> 
> In the mean time, you can make a rough estimate for the red edge based
> on the non-linear pulsation results of Robert Szabo et al:
> http://www.aanda.org/component/article?access=bibcode&bibcode=&bibcode=2004A%2526A...425..627SFUL <http://www.aanda.org/component/article?access=bibcode&bibcode=&bibcode=2004A%2526A...425..627SFUL>
> 
> see Figure 3 there. Note that these pulsation models don't include
> stellar evolution, and actual stars not necessarily reach all of these
> parameter combinations.
> 
> Cheers,
> László
> 
> László Molnár
> -------------------------------------------
> research fellow, PhD
> IBVS editor
> Konkoly Observatory
> Budapest
> -------------------------------------------
> 
> 
> 2016-01-25 3:10 GMT+01:00 RICHARD H D TOWNSEND <townsend at astro.wisc.edu <mailto:townsend at astro.wisc.edu>>:
> > Hi folks —
> >
> >> On Jan 24, 2016, at 7:32 PM, Hideyuki Saio <saio at astr.tohoku.ac.jp <mailto:saio at astr.tohoku.ac.jp>> wrote:
> >>
> >> Hi Cyrus,
> >>
> >> Your calculation results look to me quite reasonable.
> >>
> >>> Maybe the fact that my convection zone disappear is linked to the absence of barrier on the red side for the instability strip.
> >> I guess, the disappearance of the convective core is just due to the exhaustion of helium in the center, which is nothing to do with excitation of radial pulsations.
> >>
> >> Pulsation in the red side of the instability strip should be suppressed by convection-pulsation coupling in the envelope. I guess, the effect is not included in the GYRE code, and you found many pulsation modes excited in the red side of the instability strip.
> >>
> >
> > Yes, Hideyuki is quite correct here — GYRE does not include the pulsation-convection coupling, and thus cannot set the red edge correctly. Adding in this coupling is on my to-do list for 2016.
> >
> > cheers,
> >
> > Rich
> >
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