Publikace ÚTF

Shock revival in core-collapse supernovae (CCSNe) may be due to the neutrino mechanism.
While it is known that in a neutrino-powered CCSN, explosion begins when the neutrino
luminosity of the protoneutron star exceeds a critical value, the physics of this condition in
time-dependent, multidimensional simulations is not fully understood. Pejcha & Thompson
found that an ‘antesonic condition’ exists for time-steady spherically symmetric models,
potentially giving a physical explanation for the critical curve observed in simulations. In this
paper, we extend that analysis to time-dependent, spherically symmetric polytropic models.
We verify the critical antesonic condition in our simulations, showing that models exceeding
it drive transonic winds whereas models below it exhibit steady accretion. In addition, we
find that (1) high spatial resolution is needed for accurate determination of the antesonic
ratio and shock radius at the critical curve, and that low-resolution simulations systematically
underpredict these quantities, making explosion more difficult at lower resolution; (2) there
is an important physical connection between the critical mass accretion rate at explosion and
the mass-loss rate of the post-explosion wind: the two are directly proportional at criticality,
implying that, at criticality, the wind kinetic power is tied directly to the accretion power; (3)
the value of the post-shock adiabatic index  has a large effect on the length and time-scales
of the post-bounce evolution of the explosion, larger values of  result in a longer transition
from the accretion to wind phases