{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:VTTCNWX47KJAE32LSIIQM3QDMK","short_pith_number":"pith:VTTCNWX4","schema_version":"1.0","canonical_sha256":"ace626dafcfa92026f4b9211066e0362ba36685ee02d29ad59020215035eec81","source":{"kind":"arxiv","id":"1807.02598","version":1},"attestation_state":"computed","paper":{"title":"Axial Quasi-Normal Modes of Scalarized Neutron Stars with Realistic Equations of State","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Burkhard Kleihaus, Jose Luis Bl\\'azquez-Salcedo, Jutta Kunz, Zahra Altaha Motahar","submitted_at":"2018-07-07T01:01:36Z","abstract_excerpt":"We compute the axial quasi-normal modes of static neutron stars in scalar tensor theory. In particular, we employ various realistic equations of state including nuclear, hyperonic and hybrid matter. We investigate the fundamental curvature mode and compare the results with those of General Relativity. We find that the frequency of the modes and the damping time are reduced for the scalarized neutron stars. In addition, we confirm and extend the universal relations for quasi-normal modes known in General Relativity to this wide range of realistic equations of state for scalarized neutron stars "},"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":"1807.02598","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2018-07-07T01:01:36Z","cross_cats_sorted":[],"title_canon_sha256":"a8d918dcf4ee289779c7fd018c2ed6388f244e36b805200307052e7e2459c5b9","abstract_canon_sha256":"e018fe0ae23baff3729e9d58708d20142a5ffdbaa9253c42fa85f181282a0e7b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:06:59.173688Z","signature_b64":"DhVDP/r/0U+c/tnDKBmkwJoegDIyc9FokvRQT8akfLGFFh4DaLEpgjqdJGc3dTHFADfaslWCkzHC6q3B/VvwBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ace626dafcfa92026f4b9211066e0362ba36685ee02d29ad59020215035eec81","last_reissued_at":"2026-05-18T00:06:59.173104Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:06:59.173104Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Axial Quasi-Normal Modes of Scalarized Neutron Stars with Realistic Equations of State","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Burkhard Kleihaus, Jose Luis Bl\\'azquez-Salcedo, Jutta Kunz, Zahra Altaha Motahar","submitted_at":"2018-07-07T01:01:36Z","abstract_excerpt":"We compute the axial quasi-normal modes of static neutron stars in scalar tensor theory. In particular, we employ various realistic equations of state including nuclear, hyperonic and hybrid matter. We investigate the fundamental curvature mode and compare the results with those of General Relativity. We find that the frequency of the modes and the damping time are reduced for the scalarized neutron stars. In addition, we confirm and extend the universal relations for quasi-normal modes known in General Relativity to this wide range of realistic equations of state for scalarized neutron stars "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1807.02598","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":"1807.02598","created_at":"2026-05-18T00:06:59.173188+00:00"},{"alias_kind":"arxiv_version","alias_value":"1807.02598v1","created_at":"2026-05-18T00:06:59.173188+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1807.02598","created_at":"2026-05-18T00:06:59.173188+00:00"},{"alias_kind":"pith_short_12","alias_value":"VTTCNWX47KJA","created_at":"2026-05-18T12:32:59.047623+00:00"},{"alias_kind":"pith_short_16","alias_value":"VTTCNWX47KJAE32L","created_at":"2026-05-18T12:32:59.047623+00:00"},{"alias_kind":"pith_short_8","alias_value":"VTTCNWX4","created_at":"2026-05-18T12:32:59.047623+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.01737","citing_title":"Axial $w$-modes of anisotropic neutron stars","ref_index":35,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/VTTCNWX47KJAE32LSIIQM3QDMK","json":"https://pith.science/pith/VTTCNWX47KJAE32LSIIQM3QDMK.json","graph_json":"https://pith.science/api/pith-number/VTTCNWX47KJAE32LSIIQM3QDMK/graph.json","events_json":"https://pith.science/api/pith-number/VTTCNWX47KJAE32LSIIQM3QDMK/events.json","paper":"https://pith.science/paper/VTTCNWX4"},"agent_actions":{"view_html":"https://pith.science/pith/VTTCNWX47KJAE32LSIIQM3QDMK","download_json":"https://pith.science/pith/VTTCNWX47KJAE32LSIIQM3QDMK.json","view_paper":"https://pith.science/paper/VTTCNWX4","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1807.02598&json=true","fetch_graph":"https://pith.science/api/pith-number/VTTCNWX47KJAE32LSIIQM3QDMK/graph.json","fetch_events":"https://pith.science/api/pith-number/VTTCNWX47KJAE32LSIIQM3QDMK/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/VTTCNWX47KJAE32LSIIQM3QDMK/action/timestamp_anchor","attest_storage":"https://pith.science/pith/VTTCNWX47KJAE32LSIIQM3QDMK/action/storage_attestation","attest_author":"https://pith.science/pith/VTTCNWX47KJAE32LSIIQM3QDMK/action/author_attestation","sign_citation":"https://pith.science/pith/VTTCNWX47KJAE32LSIIQM3QDMK/action/citation_signature","submit_replication":"https://pith.science/pith/VTTCNWX47KJAE32LSIIQM3QDMK/action/replication_record"}},"created_at":"2026-05-18T00:06:59.173188+00:00","updated_at":"2026-05-18T00:06:59.173188+00:00"}