{"record":{"author":{"account_ref":null,"orcid":null},"builds_on":[],"content_schema":"pubphys.content.revision/1","content_sha256":"8f004b34268f1434e115f58014cedf4f500450c3ce3db8d7bba0108ede39786e","created":"2026-10-15T23:43:22Z","files":[],"origin":{"assisted_by":[],"kind":"seed"},"parents":["ce59fb6cd812fc05906d0c60a71c75ea22bc686bcf38e7c3ef7010834d98ee7b","f975f008a8a2a0aa2f413ca255c8aee0325112b81cc38c73fe39bd1aadab4b75"],"salt":"741915bc9ee1703721db694c8b161ec372636d604ad0c02507242e7a5b9324a2","schema":"pubphys.record/2","site":"pubphys.com","target":null,"type":"revision"},"content":{"answer_type":"value","assisted_by":[],"external_id":"astro.core-collapse-supernovae.explosion-energy","kind":"well-posed","literature_status":"partially-resolved","n":"2","parents":[],"plain":"Typical supernovae release about $10^{51}\\,\\mathrm{erg}$ as motion of the ejected gas; models must show that neutrino heating supplies this much.","posed_since":"1985","precise":"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.","problem_ref":"f975f008a8a2a0aa2f413ca255c8aee0325112b81cc38c73fe39bd1aadab4b75","references":"","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.","status_note":"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.","title":"Do first-principles 3D models reproduce observed supernova energies?","topic_ref":null},"attested":{"attestation":{"batch":null,"client_id":null,"id_token_sha256":null,"kind":"platform"},"record_hash":"ea0e4fe9c0844b7b49268f3b14a8b378258229bdb8b2e37a7c7334a05721011f","schema":"pubphys.attested/1"},"envelope":{"attested_hash":"0355289153c085ded315ae225f0fc5d2cbf1c1675d15fd4e98a599eca4e907c7","platform_signature":{"key_id":"c6afc19b31429869751f06879c75cd64ea92654423d15b44be775bf1310a60da","sig":"0QsDhKGMQK-J68qxNQbmY4ZZmXYUgcwmpT6BRbqeSqHgL-sb6sJKdUBjUYkfzTiBry1JMWouPEHMxQKqtDuLCA"},"schema":"pubphys.envelope/1"},"record_hash":"ea0e4fe9c0844b7b49268f3b14a8b378258229bdb8b2e37a7c7334a05721011f","leaf_index":2320}