{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2002:JBL4ARUZUTSI7CNU6LIP4SKSBZ","short_pith_number":"pith:JBL4ARUZ","schema_version":"1.0","canonical_sha256":"4857c04699a4e48f89b4f2d0fe49520e644baeca1445b3dd451c963170d83792","source":{"kind":"arxiv","id":"gr-qc/0206002","version":2},"attestation_state":"computed","paper":{"title":"Dynamical instability of differentially rotating stars","license":"","headline":"","cross_cats":["astro-ph"],"primary_cat":"gr-qc","authors_text":"Masaru Shibata, Shigeyuki Karino, Yoshiharu Eriguchi (Univ. of Tokyo)","submitted_at":"2002-06-02T08:48:10Z","abstract_excerpt":"We study the dynamical instability against bar-mode deformation of differentially rotating stars. We performed numerical simulation and linear perturbation analysis adopting polytropic equations of state with the polytropic index $n=1$. It is found that rotating stars of a high degree of differential rotation are dynamically unstable even for the ratio of the kinetic energy to the gravitational potential energy of $O(0.01)$. Gravitational waves from the final nonaxisymmetric quasistationary states are calculated in the quadrupole formula. For rotating stars of mass $1.4M_{\\odot}$ and radius se"},"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/0206002","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"gr-qc","submitted_at":"2002-06-02T08:48:10Z","cross_cats_sorted":["astro-ph"],"title_canon_sha256":"0fec8b7d4bc8ceeb04d228ddb3cac1ff9e5821f5dd4cc47b83bb5370bc20ba56","abstract_canon_sha256":"3eb00dc39403c3f257eaa5d81f7e9bb5ff68216d8b65608440f72623045fa11e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:35:34.955439Z","signature_b64":"7T1XoAsfVp9HraRXlk88lw8DjzqkRXtz1YD/XARKmioMFaosw0yJ59M0lk1XuOWx6oorBgc48B7GevlacYmICw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"4857c04699a4e48f89b4f2d0fe49520e644baeca1445b3dd451c963170d83792","last_reissued_at":"2026-05-18T04:35:34.954703Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:35:34.954703Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Dynamical instability of differentially rotating stars","license":"","headline":"","cross_cats":["astro-ph"],"primary_cat":"gr-qc","authors_text":"Masaru Shibata, Shigeyuki Karino, Yoshiharu Eriguchi (Univ. of Tokyo)","submitted_at":"2002-06-02T08:48:10Z","abstract_excerpt":"We study the dynamical instability against bar-mode deformation of differentially rotating stars. We performed numerical simulation and linear perturbation analysis adopting polytropic equations of state with the polytropic index $n=1$. It is found that rotating stars of a high degree of differential rotation are dynamically unstable even for the ratio of the kinetic energy to the gravitational potential energy of $O(0.01)$. Gravitational waves from the final nonaxisymmetric quasistationary states are calculated in the quadrupole formula. For rotating stars of mass $1.4M_{\\odot}$ and radius se"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"gr-qc/0206002","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":"gr-qc/0206002","created_at":"2026-05-18T04:35:34.954835+00:00"},{"alias_kind":"arxiv_version","alias_value":"gr-qc/0206002v2","created_at":"2026-05-18T04:35:34.954835+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.gr-qc/0206002","created_at":"2026-05-18T04:35:34.954835+00:00"},{"alias_kind":"pith_short_12","alias_value":"JBL4ARUZUTSI","created_at":"2026-05-18T12:25:50.845339+00:00"},{"alias_kind":"pith_short_16","alias_value":"JBL4ARUZUTSI7CNU","created_at":"2026-05-18T12:25:50.845339+00:00"},{"alias_kind":"pith_short_8","alias_value":"JBL4ARUZ","created_at":"2026-05-18T12:25:50.845339+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":264,"is_internal_anchor":true},{"citing_arxiv_id":"2409.10508","citing_title":"General-relativistic resistive-magnetohydrodynamics simulations of self-consistent magnetized rotating neutron stars","ref_index":81,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/JBL4ARUZUTSI7CNU6LIP4SKSBZ","json":"https://pith.science/pith/JBL4ARUZUTSI7CNU6LIP4SKSBZ.json","graph_json":"https://pith.science/api/pith-number/JBL4ARUZUTSI7CNU6LIP4SKSBZ/graph.json","events_json":"https://pith.science/api/pith-number/JBL4ARUZUTSI7CNU6LIP4SKSBZ/events.json","paper":"https://pith.science/paper/JBL4ARUZ"},"agent_actions":{"view_html":"https://pith.science/pith/JBL4ARUZUTSI7CNU6LIP4SKSBZ","download_json":"https://pith.science/pith/JBL4ARUZUTSI7CNU6LIP4SKSBZ.json","view_paper":"https://pith.science/paper/JBL4ARUZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=gr-qc/0206002&json=true","fetch_graph":"https://pith.science/api/pith-number/JBL4ARUZUTSI7CNU6LIP4SKSBZ/graph.json","fetch_events":"https://pith.science/api/pith-number/JBL4ARUZUTSI7CNU6LIP4SKSBZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/JBL4ARUZUTSI7CNU6LIP4SKSBZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/JBL4ARUZUTSI7CNU6LIP4SKSBZ/action/storage_attestation","attest_author":"https://pith.science/pith/JBL4ARUZUTSI7CNU6LIP4SKSBZ/action/author_attestation","sign_citation":"https://pith.science/pith/JBL4ARUZUTSI7CNU6LIP4SKSBZ/action/citation_signature","submit_replication":"https://pith.science/pith/JBL4ARUZUTSI7CNU6LIP4SKSBZ/action/replication_record"}},"created_at":"2026-05-18T04:35:34.954835+00:00","updated_at":"2026-05-18T04:35:34.954835+00:00"}