[mesa-users] The Cepheid phase

Tue Aug 30 04:10:28 EDT 2016

hear, hear!

zero default overshoot.

fxt

> On Aug 30, 2016, at 12:59 AM, Pablo Marchant <pamarca at gmail.com> wrote:
> 
> I would strongly oppose adding any kind of overshoot by default. This would likely be a source of significant confusion for many, and could possibly result in many publications inadvertently using overshooting they're unaware of. The amount of overshooting used would also be very arbitrary, and choosing a default would result in people using it just because it is a MESA default.
> 
> If you would ask me I would have everyone using the Ledoux criterion, but I think the proper approach is for users to actually understand what they're doing and turn that on themselves. 

> 
> On Tue, Aug 30, 2016 at 7:18 AM, Ehsan Moravveji <e.moravveji at gmail.com> wrote:
> Dear Hideyuki,
> 
> Regarding the choice of opacity tables, and in the light of CO sensitivity of the core, when growing, you need CO-enhanced opacities. For that purpose, you can, e.g. set the following in your star_jobs
>       kappa_CO_prefix = ‘a09_co’
> in addition to the following in the controls section:
>       use_Type2_opacities = .true.
>       Zbase = 0.014
> 
> Please read the documentation around the latter section to set other relevant options accordingly.
> 
> I hope this helps your cores consistently grow.
> 
> Best regards,
> Ehsan.
> 
> 
>> On 30 Aug 2016, at 02:37, Hideyuki Saio <saio at astr.tohoku.ac.jp> wrote:
>> 
>> Dear Ehsan,
>> 
>>> In the instrument paper II, Fig. 15, the evolution of non-degenerate convective He burning cores using Ledoux and Sch criteria are shown. Indeed, the behaviour of the core depends on two factors: the (extra) mixing at the boundary, and the CO-enhanced opacities.
>>> Fig. 15 shows that Sch with tiny little overshoot shall give you a growing core; so, the machinery is already there.
>> Thanks for indicating this. I didn’t know it.
>> 
>>> Two questions: 
>>> - For a fixed mass, how does you Mcc vs. t_He behave? Can you supply a figure comparing models with and without overshoot?
>> Sorry, I cannot produce it immediately, because I am not sufficiently familiar with MESA.
>> 
>>>   Do you use Ledoux or Schwarzschild criteria?
>> I didn’t specify it. So, probably Schwarzschild criterion.
>>> - Are you using CO-enhanced type II opacity tables?
>> About opacity, I included only the line:
>>       kappa_file_prefix = 'a09'
>> 
>> Thanks.
>> Hideyuki
>> 
>> 
>> 
>>> 
>>> 
>>> 
>>>> On 29 Aug 2016, at 11:50, Hideyuki Saio <saio at astr.tohoku.ac.jp> wrote:
>>>> 
>>>> Hi,
>>>> 
>>>> I am writing about my calculations of Cepheid loops. 
>>>> I computed some models to He-exhaustion with a default setting with X=0.72, Z=0.014; mixing length = 1.7Hp, and no mass loss.
>>>> 
>>>> For one set of calculations, no overshootings were included. 
>>>> 
>>>> For another set I included tiny overshooting from the He-burning core boundary, by just inserting following two lines in my inlist :
>>>>          overshoot_f_above_burn_he_core = 0.001
>>>>          overshoot_f0_above_burn_he_core = 0.001
>>>> 
>>>> I attach to this mail evolution tracks for the two cases, in which He-burning stages are shown by solid lines, while dotted lines are tracks before He ignition. Numbers are stellar masses. 
>>>> 
>>>> The first file show tracks without any overshooting, the second one with tiny over shooting from the He-buring core.  As you see, in the first case small cepheid loops occur in most cases, while  well developed loops were obtained for all masses in the second case.
>>>> 
>>>> Judging from the results, I guessed, which might be a wrong guess, that MESA code might be determining  convective-core boundary by using the composition just exterior to the boundary.    If that is the case, I am afraid that it would suppress the growth of convective-core size, which should be induced by the increase of C/O abundance (and hence enhanced opacity) in the core as discussed in ‘70s (e.g., Paczynski 1970, AcA 20, 195).  
>>>> 
>>>> Overshooting, even if very tiny one, enhances C/O abundance (and hence opacity) just outside the boundary, which would shift the boundary slightly outward in the next time step, so that the convective core size would increase progressively.  I speculate, that is the reason why well developed loops were obtained if even a tiny overshooting was included.
>>>> 
>>>> Although I am not familiar with  MESA code, if the core boundary is determined based on the composition (opacity) just outside of the boundary, I wish the method to be modified.    Thanks.
>>>> 
>>>> Best regards, 
>>>> Hideyuki Saio
>>>> 
>>>> 
>>>> <hrd_ceploop_noheos.pdf>
>>>> <hrd_ceploop_heos001.pdf>
>>>>      
>>>>   
>>>> 
>>>> 
>>>>>> Hi,
>>>>>> 
>>>>>> This loop is really weird. I’ve studied blue loops pretty extensively and I can’t recall seeing anything like it. You can take a look at my paper (2015, MNRAS 447, 2378). We tried to determine whether pulsating B-type supergiants can be on blue loops or not. The considered masses are higher (M >= 13 Ms) but our loops behave better. I intend to publish a paper solely focused on the blue-loop problem in massive stars but that’s that's not going to happen until the end of the year.
>>>>> 
>>>>> Thanks Jakub.    Perhaps the message is that mesa/star will do weird things if you give it weird parameters!   The real question is whether can we get reasonable blue loops by some settings -- my plot shows how easy it is to get strange results.   In my book, you're the mesa expert on this, so we'll be interested to see what you have found.   
>>>>> 
>>>>>> Anyway, the problem is extremely complicated so even the easiest questions might be difficult to answer.
>>>>> 
>>>>> that sums it up nicely!
>>>>> 
>>>>> Bill
>>>>> 
>>>> 
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>>> 
>> 
> 
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> -- 
> Pablo Marchant Campos
> M.Sc on Astrophysics, Universidad Católica de Chile
> PhD student, Argelander-Institut für Astronomie
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