{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:YYHXSR2SH5Z7F42NT5C7MP4SFH","short_pith_number":"pith:YYHXSR2S","schema_version":"1.0","canonical_sha256":"c60f7947523f73f2f34d9f45f63f9229f2e3369caf74c55462643ce3105861e8","source":{"kind":"arxiv","id":"1207.4035","version":2},"attestation_state":"computed","paper":{"title":"Equilibrium models of relativistic stars with a toroidal magnetic field","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"gr-qc","authors_text":"Joachim Frieben, Luciano Rezzolla","submitted_at":"2012-07-17T15:42:13Z","abstract_excerpt":"We have computed models of rotating relativistic stars with a toroidal magnetic field and investigated the combined effects of magnetic field and rotation on the apparent shape (i.e. the surface deformation), which could be relevant for the electromagnetic emission, and on the internal matter distribution (i.e. the quadrupole distortion), which could be relevant for the emission of gravitational waves. Using a sample of eight different cold nuclear physics equations of state, we have computed models of maximum field strength, as well as the distortion coefficients for the surface and the quadr"},"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":"1207.4035","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2012-07-17T15:42:13Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"b33b539ac88320511f5da77c7858d03844b8679ac2c36c04b713bd5c0089d503","abstract_canon_sha256":"6ea16d774ef5e555ef39ed8be1071525f2d0b68f1f7f4cfaea94bddab70718f1"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:59:08.899642Z","signature_b64":"5shEnnM6oM1SOwkj7qVvkQLnBIIwH8nwuf/IybC2Mw47DhWVzsaiQ5hvjj2vHKN7pn/SpMJ6i8UhpLMwKbjTCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c60f7947523f73f2f34d9f45f63f9229f2e3369caf74c55462643ce3105861e8","last_reissued_at":"2026-05-18T02:59:08.899147Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:59:08.899147Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Equilibrium models of relativistic stars with a toroidal magnetic field","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"gr-qc","authors_text":"Joachim Frieben, Luciano Rezzolla","submitted_at":"2012-07-17T15:42:13Z","abstract_excerpt":"We have computed models of rotating relativistic stars with a toroidal magnetic field and investigated the combined effects of magnetic field and rotation on the apparent shape (i.e. the surface deformation), which could be relevant for the electromagnetic emission, and on the internal matter distribution (i.e. the quadrupole distortion), which could be relevant for the emission of gravitational waves. Using a sample of eight different cold nuclear physics equations of state, we have computed models of maximum field strength, as well as the distortion coefficients for the surface and the quadr"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1207.4035","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":"1207.4035","created_at":"2026-05-18T02:59:08.899225+00:00"},{"alias_kind":"arxiv_version","alias_value":"1207.4035v2","created_at":"2026-05-18T02:59:08.899225+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1207.4035","created_at":"2026-05-18T02:59:08.899225+00:00"},{"alias_kind":"pith_short_12","alias_value":"YYHXSR2SH5Z7","created_at":"2026-05-18T12:27:30.460161+00:00"},{"alias_kind":"pith_short_16","alias_value":"YYHXSR2SH5Z7F42N","created_at":"2026-05-18T12:27:30.460161+00:00"},{"alias_kind":"pith_short_8","alias_value":"YYHXSR2S","created_at":"2026-05-18T12:27:30.460161+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2512.24194","citing_title":"Impact of Anisotropy on Neutron Star Structure and Curvature","ref_index":22,"is_internal_anchor":true},{"citing_arxiv_id":"2605.06418","citing_title":"On the non-radial oscillations of realistic anisotropic neutron stars: Axial modes","ref_index":13,"is_internal_anchor":false},{"citing_arxiv_id":"2409.10508","citing_title":"General-relativistic resistive-magnetohydrodynamics simulations of self-consistent magnetized rotating neutron stars","ref_index":21,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/YYHXSR2SH5Z7F42NT5C7MP4SFH","json":"https://pith.science/pith/YYHXSR2SH5Z7F42NT5C7MP4SFH.json","graph_json":"https://pith.science/api/pith-number/YYHXSR2SH5Z7F42NT5C7MP4SFH/graph.json","events_json":"https://pith.science/api/pith-number/YYHXSR2SH5Z7F42NT5C7MP4SFH/events.json","paper":"https://pith.science/paper/YYHXSR2S"},"agent_actions":{"view_html":"https://pith.science/pith/YYHXSR2SH5Z7F42NT5C7MP4SFH","download_json":"https://pith.science/pith/YYHXSR2SH5Z7F42NT5C7MP4SFH.json","view_paper":"https://pith.science/paper/YYHXSR2S","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1207.4035&json=true","fetch_graph":"https://pith.science/api/pith-number/YYHXSR2SH5Z7F42NT5C7MP4SFH/graph.json","fetch_events":"https://pith.science/api/pith-number/YYHXSR2SH5Z7F42NT5C7MP4SFH/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/YYHXSR2SH5Z7F42NT5C7MP4SFH/action/timestamp_anchor","attest_storage":"https://pith.science/pith/YYHXSR2SH5Z7F42NT5C7MP4SFH/action/storage_attestation","attest_author":"https://pith.science/pith/YYHXSR2SH5Z7F42NT5C7MP4SFH/action/author_attestation","sign_citation":"https://pith.science/pith/YYHXSR2SH5Z7F42NT5C7MP4SFH/action/citation_signature","submit_replication":"https://pith.science/pith/YYHXSR2SH5Z7F42NT5C7MP4SFH/action/replication_record"}},"created_at":"2026-05-18T02:59:08.899225+00:00","updated_at":"2026-05-18T02:59:08.899225+00:00"}