[Mesa-users] Convection velocities prior to CC (make_pre_ccsn)

[Francis Timmes]

hi dmitry,

without any details provided its challenging to say why convection in 
the innermost si-shell burning convective region ceases a few hundred 
seconds before core-collapse in your 15 msun model. it might even by physical. 

i will refer you to a lovely article comparing mesa and 3d flash simulations 
of a 15 msun model in the ~500 s prior to core-collapse:

https://ui.adsabs.harvard.edu/abs/2020ApJ...901...33F/abstract
https://youtu.be/2WFiPincS1I 

with section 2.1, among others, being relevant.

fxt







> On Dec 28, 2020, at 10:26 AM, Dmitry Shishkin via Mesa-users <mesa-users at lists.mesastar.org> wrote:
> 
> Hello,
> 
> Working on MESA r10398.
> Based on the "make_pre_ccsn" example, I'm trying to evolve a 15 solar mass, solar metallicity star and examine the convection velocity around the core just before CC. While initially (several minutes before collapse) convection is present at the silicon burning layer, it seems to completely disappear when collapse begins, as iron core infall velocities start exceeding a few hundred of km/s.
> Is there a numerical reason for convection to disappear at the onset of collapse?
> Could these be solved by modifications on the example?
> 
> Any help on the matter would be greatly appreciated.
> 
> Thanks in advance for any reply,
> Dmitry Shishkin
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