[Mesa-users] Nonphysical behavior of outermost envelope of rapidly rotating stars

[Aldo Serenelli]

Hi Larry,

it seems to me that density inversions are possible in the framework of 
mixing length theory. Check for instance

https://ui.adsabs.harvard.edu/abs/1970A%26A.....9..277L/abstract

I hope this helps.

Aldo


On 28/07/2020 22:23, Larry Molnar wrote:
>
> Here are the plots a second time scaled to zoom in on the outer layers 
> only.
>
> *From:* Larry Molnar <lmolnar at calvin.edu>
> *Sent:* Tuesday, July 28, 2020 4:17 PM
> *To:* Tomasz Plewa <tplewa at fsu.edu>
> *Cc:* Pablo Marchant <pamarca at gmail.com>; mesa-users at lists.mesastar.org
> *Subject:* RE: [Mesa-users] Nonphysical behavior of outermost envelope 
> of rapidly rotating stars
>
> Here are some sample log(rho)-log(T) plots for the case of M = 1.0 
> Msun, Omega/Omega_crit (initial) = 0.42. The excursion to low surface 
> temperature/large radius occurred in profiles 146-225. My samples 
> include before, during and after the excursion.
>
> I see that the density briefly **increases** with increasing radius in 
> the outermost layers of the suspect profiles.
>
> *From:* Tomasz Plewa <tplewa at fsu.edu>
> *Sent:* Monday, July 27, 2020 4:58 PM
> *To:* Larry Molnar <lmolnar at calvin.edu>
> *Cc:* Pablo Marchant <pamarca at gmail.com>; mesa-users at lists.mesastar.org
> *Subject:* Re: [Mesa-users] Nonphysical behavior of outermost envelope 
> of rapidly rotating stars
>
> Larry -
>
> Can you show the log(rho)-log(T) plot, please? How the density looks 
> like in the surface layers?
>
> Tomek
>
>
>
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