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

Cyrus Zalian thebigkiwi2003 at yahoo.fr
Mon Jan 25 18:15:04 EST 2016


Thanks for the answer !

I was actually reading Deupree paper when I got your answer. Well, then I
think that I've gone as far as I could for the moment with MESA. Thanks
once again to everyone for their help...Hope I can be the one that helps
next time.

Cheers.

2016-01-25 15:51 GMT+01:00 Ehsan Moravveji <e.moravveji at gmail.com>:

> 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
> 2. The GraCo code:
>     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
>
> 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>:
>
>> 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
>>
>> 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>:
>> > Hi folks —
>> >
>> >> On Jan 24, 2016, at 7:32 PM, Hideyuki Saio <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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