Convective vortices in collapsing stars
Telman Y. Abdikamalov E. Foglizzo T.
1 December 2024Oxford University Press
Monthly Notices of the Royal Astronomical Society
2024#535Issue 21388 - 1393 pp.
Recent studies show that non-radial structures arising from massive star shell convection play an important role in shaping core-collapse supernova explosions. During the collapse phase, convective vortices generate acoustic waves that interact with the supernova shock. This amplifies turbulence in the post-shock region, contributing to explosion. We study how various physical parameters influence the evolution of these convective vortices during stellar collapse using simplified simulations. We model the collapsing star with a transonic Bondi flow and represent convection as solenoidal velocity perturbations. Our results are consistent with previous studies, demonstrating that the peak perturbation amplitude scales linearly with the pre-collapse convective Mach number and inversely with the angular wavenumber of convection. While the shell radius and width primarily determine the time-scale of accretion, they have little impact on the peak perturbation amplitudes. Finally, we show that when the convective Mach number is below approximately 0.2, the dynamics remain within the linear regime.
convection , hydrodynamics , instabilities , supernovae: general
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Department of Physics, Nazarbayev University, 53 Kabanbay Batyr ave, Astana, 010000, Kazakhstan
Energetic Cosmos Laboratory, Nazarbayev University, 53 Kabanbay Batyr ave, Astana, 010000, Kazakhstan
AIM, CEA, CNRS, Universite Paris-Saclay, Universite Paris Diderot, Sorbonne Paris Cite, Gif-sur-Yvette, F-91191, France
Department of Physics
Energetic Cosmos Laboratory
AIM
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