The antesonic condition for the explosion of core-collapse supernovae – I. Spherically symmetric polytropic models: stability and wind emergence

Abstract

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 proto-neutron star exceeds a critical value, the physics of this condition in time-dependent, multidimensional simulations are not fully understood. Pejcha & Thompson (2012) 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 Γ has a large effect on the length and time scales of the post-bounce evolution of the explosion larger values of Γ result in a longer transition from the accretion to wind phases.

Simulating Turbulence-aided Neutrino-driven Core-collapse Supernova Explosions in One Dimension

“…Our approach is far more general, accounting for the detailed physics of the neutrino transport and time-dependent dynamics of core collapse for realistic progenitors making comparison between STIR and these other models challenging. This is also the case for other explosion criteria such as the "antesonic" condition of Pejcha & Thompson (2012) and Raives et al (2018), which does not account for turbulence or convection.…”

Binary-stripped Stars as Core-collapse Supernovae Progenitors

“…We draw attention only to the point that compactness and the critical condition focus on two distinct factors of explosion outcome: the density profile, including the presence of a strong Si/O interface (see Figure 4), and the accretion/accretion-luminosity tracks, respectively. Additionally, more detailed prescriptions for predicting explosion exist (Pejcha & Thompson 2012;Ertl et al 2016;Müller et al 2016;Murphy & Dolence 2017;Raives et al 2018). These parameterizations are in the context of one-dimensional spherically symmetric explosions, dependent on the simulation results for tuning, and beyond our scope in the context of multidimensional simulations.…”

Applications of Machine Learning to Predicting Core-collapse Supernova Explosion Outcomes

“…To circumvent this limitation, and in order to explore the explosion landscape by progenitor for final explosion energies, observational signatures, and nucleosynthetic compositions, various groups have developed CCSNe population studies using simplified prescriptions in reduced dimensions. Different such approaches include analytical approximations of protoneutron star cooling (Ugliano et al 2012), PUSH (Perego et al 2015;Curtis et al 2021), simple pistons (Sukhbold et al 2016), and spherically symmetric turbulence models (STIR; Mabanta et al 2019;Couch et al 2020), often calibrated to SN1987a and the Crab and comparing the derived explosion outcomes with various formulated predictions (e.g., the antesonic condition, Pejcha & Thompson 2012;Raives et al 2018;the Ertl criterion, Ertl et al 2016; a semianalytical pre-SN parameterization, Müller et al 2016a).…”