{"record":{"author":{"account_ref":null,"orcid":null},"builds_on":[],"content_schema":"pubphys.content.revision/1","content_sha256":"abc70c2dc4f061085c0e05e1eae36c387fa9cefda7257daf46bd862ec660b03f","created":"2026-10-03T07:18:07Z","files":[],"origin":{"assisted_by":[],"kind":"seed"},"parents":["5475cf5dc5b1a72283d26dc95dc6e00d7ea4e00096a7c6492e409a1816eeb011"],"salt":"3ae3e44c93f094f5eb83460e06edf00fb03c6888fe6c82f10a72220518ea34ad","schema":"pubphys.record/2","site":"pubphys.com","target":null,"type":"revision"},"content":{"answer_type":"value","assisted_by":[],"external_id":"nuc.neutron-star-matter.maximum-mass","kind":"well-posed","literature_status":"open","n":"1","parents":[],"plain":"Above a certain mass a neutron star must collapse into a black hole. The heaviest known neutron stars weigh a little over two Suns, but the true limit is not known.","posed_since":"","precise":"Determine $M_{\\mathrm{TOV}}$, the maximum gravitational mass of a cold nonrotating neutron star (the Tolman-Oppenheimer-Volkoff limit). Lower bounds come from PSR J0740+6620 at about $2.08\\ \\text{solar masses}$ and PSR J0952-0607 at $2.35 \\pm 0.17\\ \\text{solar masses}$; arguments about the GW170817 merger remnant suggest $M_{\\mathrm{TOV}}$ below about $2.3\\ \\text{solar masses}$. Answer: $M_{\\mathrm{TOV}}$ with uncertainty below $0.1\\ \\text{solar mass}$.","problem_ref":null,"references":"","settled_by":"A radio-timed pulsar mass above 2.3 solar masses or a measured collapse time of a merger remnant, combined with equation-of-state inference.","status_note":"The 2.35 solar-mass value (Romani et al., 2022) relies on modeling of an irradiated companion star and is less secure than radio-timing masses.","title":"Maximum mass of a nonrotating neutron star","topic_ref":"dc9703fcc2930752e3222472fa4f0774fcc6cb72d19c4033b77e3e2b58d0fcb3"},"attested":{"attestation":{"batch":null,"client_id":null,"id_token_sha256":null,"kind":"platform"},"record_hash":"b41256a5c426c21d592a9319c9f4406dd94ecd8eaa10b1543448bd22ff119179","schema":"pubphys.attested/1"},"envelope":{"attested_hash":"fafbbea0ba529023922f601b127426f309e8226afb4633b3e2b53fed55346156","platform_signature":{"key_id":"c6afc19b31429869751f06879c75cd64ea92654423d15b44be775bf1310a60da","sig":"-zm9hKOGMZxgkE6tO6lhXa4rWzd65k3LBKAlSJWrTlPmYRI-N3Ye1lU4aSqp8q_tWSzpObpxCckf3a0llFxWDw"},"schema":"pubphys.envelope/1"},"record_hash":"b41256a5c426c21d592a9319c9f4406dd94ecd8eaa10b1543448bd22ff119179","leaf_index":1779}