Do first-principles 3D models reproduce observed supernova energies? · revision history

Revision 2

Accepted · core change · record

Changes against revision 1:

Title
Do first-principles 3D models reproduce observed supernova energies?
Plain · changed
Revision 1: Typical supernovae release about $1e51\,\mathrm{erg}$ as motion of the ejected gas; models must show that neutrino heating supplies this much.
Revision 2: Typical supernovae release about $10^{51}\,\mathrm{erg}$ as motion of the ejected gas; models must show that neutrino heating supplies this much.
Precise · changed · core
Revision 1: In $3\mathrm{D}$ neutrino-radiation hydrodynamics with general relativity and energy-dependent neutrino transport, determine whether the delayed neutrino-heating mechanism reaches asymptotic explosion energies $\sim 1e51\,\mathrm{erg}$ and Ni-56 masses $\sim 0.01\ \text{to}\ 0.1\,M_{\mathrm{sun}}$ (median $\sim 0.03\,M_{\mathrm{sun}}$) for progenitors of $9\ \text{to}\ 25\,M_{\mathrm{sun}}$, as observed in Type II-P supernovae. Answer: converged energies and Ni-56 masses versus progenitor, with dependence on resolution and transport method quantified.
Revision 2: In $3\mathrm{D}$ neutrino-radiation hydrodynamics with general relativity and energy-dependent neutrino transport, determine whether the delayed neutrino-heating mechanism reaches asymptotic explosion energies $\sim 10^{51}\,\mathrm{erg}$ and Ni-56 masses $\sim 0.01\ \text{to}\ 0.1\,M_{\mathrm{sun}}$ (median $\sim 0.03\,M_{\mathrm{sun}}$) for progenitors of $9\ \text{to}\ 25\,M_{\mathrm{sun}}$, as observed in Type II-P supernovae. Answer: converged energies and Ni-56 masses versus progenitor, with dependence on resolution and transport method quantified.
Settled by
Long-duration (more than 5 s after bounce) 3D simulations by independent codes agreeing on energies within about 20 percent and matching observed distributions.
Kind
well-posed
Answer type
value
References
(empty)
Literature status
partially-resolved
Status note · changed
Revision 1: 2024: $3\mathrm{D}$ simulations followed for several seconds reach energies approaching $1e51\ \mathrm{erg}$ for some progenitors; code-to-code agreement is not established.
Revision 2: 2024: $3\mathrm{D}$ simulations followed for several seconds reach energies approaching $10^{51}\ \mathrm{erg}$ for some progenitors; code-to-code agreement is not established.
Posed since
1985

Decisions