{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2007:7XSSICRLEHTGRJDNSN6TH5CR3S","short_pith_number":"pith:7XSSICRL","schema_version":"1.0","canonical_sha256":"fde5240a2b21e668a46d937d33f451dc94c53050913b609890bbfc1d86f2da9d","source":{"kind":"arxiv","id":"0705.4594","version":1},"attestation_state":"computed","paper":{"title":"Two branches of neutron stars - reconciling a 2M_sun pulsar and SN1987A","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"J.L. Zdunik, M. Bejger, P. Haensel","submitted_at":"2007-05-31T13:12:44Z","abstract_excerpt":"The analysis of SN1987A led Brown and Bethe (1995) to conclusion, that the maximum mass of cold neutron stars is low, M_max ~ 1.5M_sun. Such a low M_max, due to a kaon condensation in the stellar core, implies collapse of a too massive deleptonized protoneutron star into a black hole. This would naturally explain the lack of a neutron star in the SN1987A remnant. On the other hand, recent evaluation of mass of PSR J0751+1807 gives M_max > 2M_sun. This contradicts the original Bethe-Brown model, but can be reconciled within scenarios proposed in the present Letter. We consider two types of dens"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"0705.4594","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2007-05-31T13:12:44Z","cross_cats_sorted":[],"title_canon_sha256":"504c35634ec667d504ac903d2e0bf4c061025ecfc983f14d32492ffda8a78384","abstract_canon_sha256":"a4e2b0ed637a9868e771396e8f6bf23c562820ef10d0094decade00a30eb879f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:01:36.604915Z","signature_b64":"FTrRBCGbcF12rCCGWTEi51klREr0S0K27q7hEfY27ZFaPMlzrjkX87m3KEcsdYB/Aq4xCmaNQ+i4LpAzBUT9DA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"fde5240a2b21e668a46d937d33f451dc94c53050913b609890bbfc1d86f2da9d","last_reissued_at":"2026-07-04T15:01:36.604499Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:01:36.604499Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Two branches of neutron stars - reconciling a 2M_sun pulsar and SN1987A","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"J.L. Zdunik, M. Bejger, P. Haensel","submitted_at":"2007-05-31T13:12:44Z","abstract_excerpt":"The analysis of SN1987A led Brown and Bethe (1995) to conclusion, that the maximum mass of cold neutron stars is low, M_max ~ 1.5M_sun. Such a low M_max, due to a kaon condensation in the stellar core, implies collapse of a too massive deleptonized protoneutron star into a black hole. This would naturally explain the lack of a neutron star in the SN1987A remnant. On the other hand, recent evaluation of mass of PSR J0751+1807 gives M_max > 2M_sun. This contradicts the original Bethe-Brown model, but can be reconciled within scenarios proposed in the present Letter. We consider two types of dens"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0705.4594","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/0705.4594/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"},"aliases":[{"alias_kind":"arxiv","alias_value":"0705.4594","created_at":"2026-07-04T15:01:36.604561+00:00"},{"alias_kind":"arxiv_version","alias_value":"0705.4594v1","created_at":"2026-07-04T15:01:36.604561+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0705.4594","created_at":"2026-07-04T15:01:36.604561+00:00"},{"alias_kind":"pith_short_12","alias_value":"7XSSICRLEHTG","created_at":"2026-07-04T15:01:36.604561+00:00"},{"alias_kind":"pith_short_16","alias_value":"7XSSICRLEHTGRJDN","created_at":"2026-07-04T15:01:36.604561+00:00"},{"alias_kind":"pith_short_8","alias_value":"7XSSICRL","created_at":"2026-07-04T15:01:36.604561+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2412.01426","citing_title":"Simultaneous explanation of XTE J1814-338 and HESS J1731-347 objects using ${K^{-}}$ and ${\\bar{K}^{0}}$ condensates","ref_index":19,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/7XSSICRLEHTGRJDNSN6TH5CR3S","json":"https://pith.science/pith/7XSSICRLEHTGRJDNSN6TH5CR3S.json","graph_json":"https://pith.science/api/pith-number/7XSSICRLEHTGRJDNSN6TH5CR3S/graph.json","events_json":"https://pith.science/api/pith-number/7XSSICRLEHTGRJDNSN6TH5CR3S/events.json","paper":"https://pith.science/paper/7XSSICRL"},"agent_actions":{"view_html":"https://pith.science/pith/7XSSICRLEHTGRJDNSN6TH5CR3S","download_json":"https://pith.science/pith/7XSSICRLEHTGRJDNSN6TH5CR3S.json","view_paper":"https://pith.science/paper/7XSSICRL","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0705.4594&json=true","fetch_graph":"https://pith.science/api/pith-number/7XSSICRLEHTGRJDNSN6TH5CR3S/graph.json","fetch_events":"https://pith.science/api/pith-number/7XSSICRLEHTGRJDNSN6TH5CR3S/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/7XSSICRLEHTGRJDNSN6TH5CR3S/action/timestamp_anchor","attest_storage":"https://pith.science/pith/7XSSICRLEHTGRJDNSN6TH5CR3S/action/storage_attestation","attest_author":"https://pith.science/pith/7XSSICRLEHTGRJDNSN6TH5CR3S/action/author_attestation","sign_citation":"https://pith.science/pith/7XSSICRLEHTGRJDNSN6TH5CR3S/action/citation_signature","submit_replication":"https://pith.science/pith/7XSSICRLEHTGRJDNSN6TH5CR3S/action/replication_record"}},"created_at":"2026-07-04T15:01:36.604561+00:00","updated_at":"2026-07-04T15:01:36.604561+00:00"}