{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:JP44F5IBGDMSYO4FMCSX5FRLAS","short_pith_number":"pith:JP44F5IB","schema_version":"1.0","canonical_sha256":"4bf9c2f50130d92c3b8560a57e962b04959f5ed7d1e23700bf124e344db53654","source":{"kind":"arxiv","id":"2002.03300","version":1},"attestation_state":"computed","paper":{"title":"A New Approach to Mass and Radius of Neutron Stars with Supernova Neutrinos","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ph","nucl-th"],"primary_cat":"astro-ph.HE","authors_text":"Hideyuki Suzuki, Ken'ichiro Nakazato","submitted_at":"2020-02-09T06:34:27Z","abstract_excerpt":"Neutron stars are formed in core-collapse supernova explosions, where a large number of neutrinos are emitted. In this paper, supernova neutrino light curves are computed for the cooling phase of protoneutron stars, which lasts a few minutes. In the numerical simulations, 90 models of the phenomenological equation of state with different incompressibilities, symmetry energies, and nucleon effective masses are employed for a comprehensive study. It is found that the cooling timescale is longer for a model with a larger neutron star mass and a smaller neutron star radius. Furthermore, a theoreti"},"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":"2002.03300","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2020-02-09T06:34:27Z","cross_cats_sorted":["hep-ph","nucl-th"],"title_canon_sha256":"50805b1df61671981632ccfb32ac33e3e2f5f2ca3e92568ee2ddeca2268f4e6f","abstract_canon_sha256":"a4f2c6ba9cf392c865b33bd6cdcf838cb4371409d49d007f16b4eb9ebc7ff4c0"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:48:23.923296Z","signature_b64":"zo4cY6eXhx59ktkt8PqaWqAxPm8raYuslNp4ayD5wEhL0FioZLtEqYPvha46bbLUygMG3keOnCso5JgqUqZpAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"4bf9c2f50130d92c3b8560a57e962b04959f5ed7d1e23700bf124e344db53654","last_reissued_at":"2026-07-05T00:48:23.922893Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:48:23.922893Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A New Approach to Mass and Radius of Neutron Stars with Supernova Neutrinos","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ph","nucl-th"],"primary_cat":"astro-ph.HE","authors_text":"Hideyuki Suzuki, Ken'ichiro Nakazato","submitted_at":"2020-02-09T06:34:27Z","abstract_excerpt":"Neutron stars are formed in core-collapse supernova explosions, where a large number of neutrinos are emitted. In this paper, supernova neutrino light curves are computed for the cooling phase of protoneutron stars, which lasts a few minutes. In the numerical simulations, 90 models of the phenomenological equation of state with different incompressibilities, symmetry energies, and nucleon effective masses are employed for a comprehensive study. It is found that the cooling timescale is longer for a model with a larger neutron star mass and a smaller neutron star radius. Furthermore, a theoreti"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2002.03300","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/2002.03300/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":"2002.03300","created_at":"2026-07-05T00:48:23.922958+00:00"},{"alias_kind":"arxiv_version","alias_value":"2002.03300v1","created_at":"2026-07-05T00:48:23.922958+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2002.03300","created_at":"2026-07-05T00:48:23.922958+00:00"},{"alias_kind":"pith_short_12","alias_value":"JP44F5IBGDMS","created_at":"2026-07-05T00:48:23.922958+00:00"},{"alias_kind":"pith_short_16","alias_value":"JP44F5IBGDMSYO4F","created_at":"2026-07-05T00:48:23.922958+00:00"},{"alias_kind":"pith_short_8","alias_value":"JP44F5IB","created_at":"2026-07-05T00:48:23.922958+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2608.05582","citing_title":"Influence of effective mass of the relativistic mean field theory on core collapse supernovae and compact objects","ref_index":78,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/JP44F5IBGDMSYO4FMCSX5FRLAS","json":"https://pith.science/pith/JP44F5IBGDMSYO4FMCSX5FRLAS.json","graph_json":"https://pith.science/api/pith-number/JP44F5IBGDMSYO4FMCSX5FRLAS/graph.json","events_json":"https://pith.science/api/pith-number/JP44F5IBGDMSYO4FMCSX5FRLAS/events.json","paper":"https://pith.science/paper/JP44F5IB"},"agent_actions":{"view_html":"https://pith.science/pith/JP44F5IBGDMSYO4FMCSX5FRLAS","download_json":"https://pith.science/pith/JP44F5IBGDMSYO4FMCSX5FRLAS.json","view_paper":"https://pith.science/paper/JP44F5IB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2002.03300&json=true","fetch_graph":"https://pith.science/api/pith-number/JP44F5IBGDMSYO4FMCSX5FRLAS/graph.json","fetch_events":"https://pith.science/api/pith-number/JP44F5IBGDMSYO4FMCSX5FRLAS/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/JP44F5IBGDMSYO4FMCSX5FRLAS/action/timestamp_anchor","attest_storage":"https://pith.science/pith/JP44F5IBGDMSYO4FMCSX5FRLAS/action/storage_attestation","attest_author":"https://pith.science/pith/JP44F5IBGDMSYO4FMCSX5FRLAS/action/author_attestation","sign_citation":"https://pith.science/pith/JP44F5IBGDMSYO4FMCSX5FRLAS/action/citation_signature","submit_replication":"https://pith.science/pith/JP44F5IBGDMSYO4FMCSX5FRLAS/action/replication_record"}},"created_at":"2026-07-05T00:48:23.922958+00:00","updated_at":"2026-07-05T00:48:23.922958+00:00"}