{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1998:VXD3G7JETCBZM4BRH6BVNGLMFR","short_pith_number":"pith:VXD3G7JE","schema_version":"1.0","canonical_sha256":"adc7b37d2498839670313f8356996c2c753386eab7856d1a5733dcb1e1179f72","source":{"kind":"arxiv","id":"gr-qc/9803053","version":1},"attestation_state":"computed","paper":{"title":"Gravitational Radiation Instability in Hot Young Neutron Stars","license":"","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Benjamin J. Owen, Lee Lindblom, Sharon M. Morsink","submitted_at":"1998-03-13T22:09:33Z","abstract_excerpt":"We show that gravitational radiation drives an instability in hot young rapidly rotating neutron stars. This instability occurs primarily in the l=2 r-mode and will carry away most of the angular momentum of a rapidly rotating star by gravitational radiation. On the timescale needed to cool a young neutron star to about T=10^9 K (about one year) this instability can reduce the rotation rate of a rapidly rotating star to about 0.076\\Omega_K, where \\Omega_K is the Keplerian angular velocity where mass shedding occurs. In older colder neutron stars this instability is suppressed by viscous effect"},"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":"gr-qc/9803053","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"gr-qc","submitted_at":"1998-03-13T22:09:33Z","cross_cats_sorted":[],"title_canon_sha256":"fe95e8fd69742f72e858d262bf12d9900ae7bee37b219b19b35dde5603e5abf2","abstract_canon_sha256":"8e7626335a4a203def2517b3a3856df110c7f675cfb12460f5932c3b589583b6"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:35:33.813916Z","signature_b64":"Cnh7DuxCRRmCVIPcOHlslZCW2GJ2Cgwpd4zZngXjRXjdkKvF+axdlu8PkKYZF7upQKbmB4oU/Dg2E1RS6z+rCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"adc7b37d2498839670313f8356996c2c753386eab7856d1a5733dcb1e1179f72","last_reissued_at":"2026-05-18T04:35:33.813289Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:35:33.813289Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Gravitational Radiation Instability in Hot Young Neutron Stars","license":"","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Benjamin J. Owen, Lee Lindblom, Sharon M. Morsink","submitted_at":"1998-03-13T22:09:33Z","abstract_excerpt":"We show that gravitational radiation drives an instability in hot young rapidly rotating neutron stars. This instability occurs primarily in the l=2 r-mode and will carry away most of the angular momentum of a rapidly rotating star by gravitational radiation. On the timescale needed to cool a young neutron star to about T=10^9 K (about one year) this instability can reduce the rotation rate of a rapidly rotating star to about 0.076\\Omega_K, where \\Omega_K is the Keplerian angular velocity where mass shedding occurs. In older colder neutron stars this instability is suppressed by viscous effect"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"gr-qc/9803053","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":""},"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":"gr-qc/9803053","created_at":"2026-05-18T04:35:33.813389+00:00"},{"alias_kind":"arxiv_version","alias_value":"gr-qc/9803053v1","created_at":"2026-05-18T04:35:33.813389+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.gr-qc/9803053","created_at":"2026-05-18T04:35:33.813389+00:00"},{"alias_kind":"pith_short_12","alias_value":"VXD3G7JETCBZ","created_at":"2026-05-18T12:25:49.038998+00:00"},{"alias_kind":"pith_short_16","alias_value":"VXD3G7JETCBZM4BR","created_at":"2026-05-18T12:25:49.038998+00:00"},{"alias_kind":"pith_short_8","alias_value":"VXD3G7JE","created_at":"2026-05-18T12:25:49.038998+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"1907.04654","citing_title":"Phase transitions in neutron stars and their links to gravitational waves","ref_index":273,"is_internal_anchor":true},{"citing_arxiv_id":"gr-qc/9909058","citing_title":"Quasi-Normal Modes of Stars and Black Holes","ref_index":142,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/VXD3G7JETCBZM4BRH6BVNGLMFR","json":"https://pith.science/pith/VXD3G7JETCBZM4BRH6BVNGLMFR.json","graph_json":"https://pith.science/api/pith-number/VXD3G7JETCBZM4BRH6BVNGLMFR/graph.json","events_json":"https://pith.science/api/pith-number/VXD3G7JETCBZM4BRH6BVNGLMFR/events.json","paper":"https://pith.science/paper/VXD3G7JE"},"agent_actions":{"view_html":"https://pith.science/pith/VXD3G7JETCBZM4BRH6BVNGLMFR","download_json":"https://pith.science/pith/VXD3G7JETCBZM4BRH6BVNGLMFR.json","view_paper":"https://pith.science/paper/VXD3G7JE","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=gr-qc/9803053&json=true","fetch_graph":"https://pith.science/api/pith-number/VXD3G7JETCBZM4BRH6BVNGLMFR/graph.json","fetch_events":"https://pith.science/api/pith-number/VXD3G7JETCBZM4BRH6BVNGLMFR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/VXD3G7JETCBZM4BRH6BVNGLMFR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/VXD3G7JETCBZM4BRH6BVNGLMFR/action/storage_attestation","attest_author":"https://pith.science/pith/VXD3G7JETCBZM4BRH6BVNGLMFR/action/author_attestation","sign_citation":"https://pith.science/pith/VXD3G7JETCBZM4BRH6BVNGLMFR/action/citation_signature","submit_replication":"https://pith.science/pith/VXD3G7JETCBZM4BRH6BVNGLMFR/action/replication_record"}},"created_at":"2026-05-18T04:35:33.813389+00:00","updated_at":"2026-05-18T04:35:33.813389+00:00"}