{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2015:6CLJKKGSHLDEXUDPQRFN2TORCC","short_pith_number":"pith:6CLJKKGS","schema_version":"1.0","canonical_sha256":"f0969528d23ac64bd06f844add4dd110a6344e6f4ff2508c4f37ece7b90c7cf8","source":{"kind":"arxiv","id":"1509.06975","version":2},"attestation_state":"computed","paper":{"title":"Growth rate of the tidal p-mode g-mode instability in coalescing binary neutron stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","gr-qc"],"primary_cat":"astro-ph.SR","authors_text":"Nevin N. Weinberg","submitted_at":"2015-09-22T00:50:45Z","abstract_excerpt":"We recently described an instability due to the nonlinear coupling of p-modes to g-modes and, as an application, we studied the stability of the tide in coalescing binary neutron stars. Although we found that the tide is p-g unstable early in the inspiral and rapidly drives modes to large energies, our analysis only accounted for three-mode interactions. Venumadhav, Zimmerman, and Hirata showed that four-mode interactions must also be accounted for as they enter into the analysis at the same order. They found a near-exact cancellation between three- and four-mode interactions and concluded tha"},"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":"1509.06975","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2015-09-22T00:50:45Z","cross_cats_sorted":["astro-ph.HE","gr-qc"],"title_canon_sha256":"25355c158cf3a4c7edb06352702a90a46a1f1ea93a8bcfe0c1cf775634524ceb","abstract_canon_sha256":"e4df9f4627d560cd4faeb8332ffa7096c78754c7ce10e866ee07bcbcf66c9314"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:19:05.792677Z","signature_b64":"3WEutwoeFYb5LpGYMAyx7Ke8GDylDXOZxRz2ak1CTmpxO8L/ROOiPeYnlnpUKKBYbHvKTFJAr8be+hFOhJyOBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"f0969528d23ac64bd06f844add4dd110a6344e6f4ff2508c4f37ece7b90c7cf8","last_reissued_at":"2026-05-18T01:19:05.792005Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:19:05.792005Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Growth rate of the tidal p-mode g-mode instability in coalescing binary neutron stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","gr-qc"],"primary_cat":"astro-ph.SR","authors_text":"Nevin N. Weinberg","submitted_at":"2015-09-22T00:50:45Z","abstract_excerpt":"We recently described an instability due to the nonlinear coupling of p-modes to g-modes and, as an application, we studied the stability of the tide in coalescing binary neutron stars. Although we found that the tide is p-g unstable early in the inspiral and rapidly drives modes to large energies, our analysis only accounted for three-mode interactions. Venumadhav, Zimmerman, and Hirata showed that four-mode interactions must also be accounted for as they enter into the analysis at the same order. They found a near-exact cancellation between three- and four-mode interactions and concluded tha"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1509.06975","kind":"arxiv","version":2},"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":"1509.06975","created_at":"2026-05-18T01:19:05.792103+00:00"},{"alias_kind":"arxiv_version","alias_value":"1509.06975v2","created_at":"2026-05-18T01:19:05.792103+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1509.06975","created_at":"2026-05-18T01:19:05.792103+00:00"},{"alias_kind":"pith_short_12","alias_value":"6CLJKKGSHLDE","created_at":"2026-05-18T12:29:07.941421+00:00"},{"alias_kind":"pith_short_16","alias_value":"6CLJKKGSHLDEXUDP","created_at":"2026-05-18T12:29:07.941421+00:00"},{"alias_kind":"pith_short_8","alias_value":"6CLJKKGS","created_at":"2026-05-18T12:29:07.941421+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2607.07943","citing_title":"Nonlinear hydrodynamics in spinning neutron stars: Theoretical universal relations and equilibrium solutions","ref_index":55,"is_internal_anchor":true},{"citing_arxiv_id":"2604.08653","citing_title":"Love numbers of black holes and compact objects","ref_index":96,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/6CLJKKGSHLDEXUDPQRFN2TORCC","json":"https://pith.science/pith/6CLJKKGSHLDEXUDPQRFN2TORCC.json","graph_json":"https://pith.science/api/pith-number/6CLJKKGSHLDEXUDPQRFN2TORCC/graph.json","events_json":"https://pith.science/api/pith-number/6CLJKKGSHLDEXUDPQRFN2TORCC/events.json","paper":"https://pith.science/paper/6CLJKKGS"},"agent_actions":{"view_html":"https://pith.science/pith/6CLJKKGSHLDEXUDPQRFN2TORCC","download_json":"https://pith.science/pith/6CLJKKGSHLDEXUDPQRFN2TORCC.json","view_paper":"https://pith.science/paper/6CLJKKGS","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1509.06975&json=true","fetch_graph":"https://pith.science/api/pith-number/6CLJKKGSHLDEXUDPQRFN2TORCC/graph.json","fetch_events":"https://pith.science/api/pith-number/6CLJKKGSHLDEXUDPQRFN2TORCC/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/6CLJKKGSHLDEXUDPQRFN2TORCC/action/timestamp_anchor","attest_storage":"https://pith.science/pith/6CLJKKGSHLDEXUDPQRFN2TORCC/action/storage_attestation","attest_author":"https://pith.science/pith/6CLJKKGSHLDEXUDPQRFN2TORCC/action/author_attestation","sign_citation":"https://pith.science/pith/6CLJKKGSHLDEXUDPQRFN2TORCC/action/citation_signature","submit_replication":"https://pith.science/pith/6CLJKKGSHLDEXUDPQRFN2TORCC/action/replication_record"}},"created_at":"2026-05-18T01:19:05.792103+00:00","updated_at":"2026-05-18T01:19:05.792103+00:00"}