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

[Dmitry Shishkin]

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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