{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:XYWMXYNLZNCACJ7L55UA6L6ZMY","short_pith_number":"pith:XYWMXYNL","schema_version":"1.0","canonical_sha256":"be2ccbe1abcb440127ebef680f2fd96619d026f93e5748374990d156435da619","source":{"kind":"arxiv","id":"1410.6332","version":1},"attestation_state":"computed","paper":{"title":"Consistent neutron star models with magnetic field dependent equations of state","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["nucl-th"],"primary_cat":"astro-ph.HE","authors_text":"Debarati Chatterjee, Jerome Novak, Micaela Oertel, Thomas Elghozi","submitted_at":"2014-10-23T12:01:16Z","abstract_excerpt":"We present a self-consistent model for the study of the structure of a neutron star in strong magnetic fields. Starting from a microscopic Lagrangian, this model includes the effect of the magnetic field on the equation of state, the interaction of the electromagnetic field with matter (magnetisation), and anisotropies in the energy-momentum tensor, as well as general relativistic aspects. We build numerical axisymmetric stationary models and show the applicability of the approach with one example quark matter equation of state (EoS) often employed in the recent literature for studies of stron"},"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":"1410.6332","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2014-10-23T12:01:16Z","cross_cats_sorted":["nucl-th"],"title_canon_sha256":"aaffbaba96f8074b39d7e3749f58d68384ea2416d12e2de45b72407370eaad9b","abstract_canon_sha256":"05d9ccfb25c468231acd6348e776934bacc2cda6826e5457c2c57748c525a049"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:41:40.564765Z","signature_b64":"5XbRMyAYh5knbI5ZCrYNXjKyhOkg9K9QVGRWk29Pa1sxt82Hw9D9LhTAmme1EV/oPGxZB+bqnxvJ1iWSXRLYDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"be2ccbe1abcb440127ebef680f2fd96619d026f93e5748374990d156435da619","last_reissued_at":"2026-05-18T01:41:40.564144Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:41:40.564144Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Consistent neutron star models with magnetic field dependent equations of state","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["nucl-th"],"primary_cat":"astro-ph.HE","authors_text":"Debarati Chatterjee, Jerome Novak, Micaela Oertel, Thomas Elghozi","submitted_at":"2014-10-23T12:01:16Z","abstract_excerpt":"We present a self-consistent model for the study of the structure of a neutron star in strong magnetic fields. Starting from a microscopic Lagrangian, this model includes the effect of the magnetic field on the equation of state, the interaction of the electromagnetic field with matter (magnetisation), and anisotropies in the energy-momentum tensor, as well as general relativistic aspects. We build numerical axisymmetric stationary models and show the applicability of the approach with one example quark matter equation of state (EoS) often employed in the recent literature for studies of stron"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1410.6332","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":"1410.6332","created_at":"2026-05-18T01:41:40.564220+00:00"},{"alias_kind":"arxiv_version","alias_value":"1410.6332v1","created_at":"2026-05-18T01:41:40.564220+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1410.6332","created_at":"2026-05-18T01:41:40.564220+00:00"},{"alias_kind":"pith_short_12","alias_value":"XYWMXYNLZNCA","created_at":"2026-05-18T12:28:57.508820+00:00"},{"alias_kind":"pith_short_16","alias_value":"XYWMXYNLZNCACJ7L","created_at":"2026-05-18T12:28:57.508820+00:00"},{"alias_kind":"pith_short_8","alias_value":"XYWMXYNL","created_at":"2026-05-18T12:28:57.508820+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2605.23021","citing_title":"Finite-Size Effects on the Critical End Point of Magnetized Quark Matter in the Nonlocal PNJL Model","ref_index":5,"is_internal_anchor":true},{"citing_arxiv_id":"2605.19761","citing_title":"Magnetized neutron stars: perturbative versus fully-numerical approaches","ref_index":63,"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":22,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/XYWMXYNLZNCACJ7L55UA6L6ZMY","json":"https://pith.science/pith/XYWMXYNLZNCACJ7L55UA6L6ZMY.json","graph_json":"https://pith.science/api/pith-number/XYWMXYNLZNCACJ7L55UA6L6ZMY/graph.json","events_json":"https://pith.science/api/pith-number/XYWMXYNLZNCACJ7L55UA6L6ZMY/events.json","paper":"https://pith.science/paper/XYWMXYNL"},"agent_actions":{"view_html":"https://pith.science/pith/XYWMXYNLZNCACJ7L55UA6L6ZMY","download_json":"https://pith.science/pith/XYWMXYNLZNCACJ7L55UA6L6ZMY.json","view_paper":"https://pith.science/paper/XYWMXYNL","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1410.6332&json=true","fetch_graph":"https://pith.science/api/pith-number/XYWMXYNLZNCACJ7L55UA6L6ZMY/graph.json","fetch_events":"https://pith.science/api/pith-number/XYWMXYNLZNCACJ7L55UA6L6ZMY/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XYWMXYNLZNCACJ7L55UA6L6ZMY/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XYWMXYNLZNCACJ7L55UA6L6ZMY/action/storage_attestation","attest_author":"https://pith.science/pith/XYWMXYNLZNCACJ7L55UA6L6ZMY/action/author_attestation","sign_citation":"https://pith.science/pith/XYWMXYNLZNCACJ7L55UA6L6ZMY/action/citation_signature","submit_replication":"https://pith.science/pith/XYWMXYNLZNCACJ7L55UA6L6ZMY/action/replication_record"}},"created_at":"2026-05-18T01:41:40.564220+00:00","updated_at":"2026-05-18T01:41:40.564220+00:00"}