{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2000:J46GRMF7G7EB44T3YGTAZIMQK2","short_pith_number":"pith:J46GRMF7","schema_version":"1.0","canonical_sha256":"4f3c68b0bf37c81e727bc1a60ca19056867d28d20c33d84bc8df3e68a8830404","source":{"kind":"arxiv","id":"astro-ph/0012306","version":1},"attestation_state":"computed","paper":{"title":"Thermal Relaxation in Young Neutron Stars","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Alexander Y. Potekhin, Dmitry G. Yakovlev, Oleg Y. Gnedin","submitted_at":"2000-12-14T00:01:46Z","abstract_excerpt":"The internal properties of the neutron star crust can be probed by observing the epoch of thermal relaxation. After the supernova explosion, powerful neutrino emission quickly cools the stellar core, while the crust stays hot. The cooling wave then propagates through the crust, due to its finite thermal conductivity. When the cooling wave reaches the surface (age 10-100 yr), the effective temperature drops sharply from 250 eV to 30 or 100 eV, depending on the cooling model. The crust relaxation time is sensitive to the (poorly known) microscopic properties of matter of subnuclear density, such"},"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":"astro-ph/0012306","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2000-12-14T00:01:46Z","cross_cats_sorted":[],"title_canon_sha256":"d003934b0370a4d094aff675c2711ce702d55e1d3dd90d8ef266be8085e98166","abstract_canon_sha256":"0f63ef523542b3eadae2b1fadaf7b3b99b3d2e3e521dc4f6cd08e5a0beeb02c8"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:17:48.032931Z","signature_b64":"y+l0YXF0NfULGjppCRoKuzcBmKEuFz6+9ZJdW0lWpIRP0kEDv+zJwKzxd9AWjLB6fIsNmMtwGqtK0b9XwMTeDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"4f3c68b0bf37c81e727bc1a60ca19056867d28d20c33d84bc8df3e68a8830404","last_reissued_at":"2026-07-04T16:17:48.032484Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:17:48.032484Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Thermal Relaxation in Young Neutron Stars","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Alexander Y. Potekhin, Dmitry G. Yakovlev, Oleg Y. Gnedin","submitted_at":"2000-12-14T00:01:46Z","abstract_excerpt":"The internal properties of the neutron star crust can be probed by observing the epoch of thermal relaxation. After the supernova explosion, powerful neutrino emission quickly cools the stellar core, while the crust stays hot. The cooling wave then propagates through the crust, due to its finite thermal conductivity. When the cooling wave reaches the surface (age 10-100 yr), the effective temperature drops sharply from 250 eV to 30 or 100 eV, depending on the cooling model. The crust relaxation time is sensitive to the (poorly known) microscopic properties of matter of subnuclear density, such"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0012306","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/astro-ph/0012306/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":"astro-ph/0012306","created_at":"2026-07-04T16:17:48.032541+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0012306v1","created_at":"2026-07-04T16:17:48.032541+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0012306","created_at":"2026-07-04T16:17:48.032541+00:00"},{"alias_kind":"pith_short_12","alias_value":"J46GRMF7G7EB","created_at":"2026-07-04T16:17:48.032541+00:00"},{"alias_kind":"pith_short_16","alias_value":"J46GRMF7G7EB44T3","created_at":"2026-07-04T16:17:48.032541+00:00"},{"alias_kind":"pith_short_8","alias_value":"J46GRMF7","created_at":"2026-07-04T16:17:48.032541+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2604.21652","citing_title":"Constraining dark matter self-interaction from kinetic heating in neutron stars","ref_index":102,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/J46GRMF7G7EB44T3YGTAZIMQK2","json":"https://pith.science/pith/J46GRMF7G7EB44T3YGTAZIMQK2.json","graph_json":"https://pith.science/api/pith-number/J46GRMF7G7EB44T3YGTAZIMQK2/graph.json","events_json":"https://pith.science/api/pith-number/J46GRMF7G7EB44T3YGTAZIMQK2/events.json","paper":"https://pith.science/paper/J46GRMF7"},"agent_actions":{"view_html":"https://pith.science/pith/J46GRMF7G7EB44T3YGTAZIMQK2","download_json":"https://pith.science/pith/J46GRMF7G7EB44T3YGTAZIMQK2.json","view_paper":"https://pith.science/paper/J46GRMF7","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0012306&json=true","fetch_graph":"https://pith.science/api/pith-number/J46GRMF7G7EB44T3YGTAZIMQK2/graph.json","fetch_events":"https://pith.science/api/pith-number/J46GRMF7G7EB44T3YGTAZIMQK2/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/J46GRMF7G7EB44T3YGTAZIMQK2/action/timestamp_anchor","attest_storage":"https://pith.science/pith/J46GRMF7G7EB44T3YGTAZIMQK2/action/storage_attestation","attest_author":"https://pith.science/pith/J46GRMF7G7EB44T3YGTAZIMQK2/action/author_attestation","sign_citation":"https://pith.science/pith/J46GRMF7G7EB44T3YGTAZIMQK2/action/citation_signature","submit_replication":"https://pith.science/pith/J46GRMF7G7EB44T3YGTAZIMQK2/action/replication_record"}},"created_at":"2026-07-04T16:17:48.032541+00:00","updated_at":"2026-07-04T16:17:48.032541+00:00"}