{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2002:6CVEL2TTXLIQTMJWLSM64S4YML","short_pith_number":"pith:6CVEL2TT","schema_version":"1.0","canonical_sha256":"f0aa45ea73bad109b1365c99ee4b9862e55814b2e0efbfdec5d4ad79cde39433","source":{"kind":"arxiv","id":"astro-ph/0212062","version":4},"attestation_state":"computed","paper":{"title":"Equation of state and opacities for hydrogen atmospheres of neutron stars with strong magnetic fields","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Y. Potekhin (Ioffe Inst., ENS-Lyon), G. Chabrier (CRAL, St.-Petersburg)","submitted_at":"2002-12-03T13:04:09Z","abstract_excerpt":"We present an equation of state and radiative opacities for a strongly magnetized hydrogen plasma at magnetic fields B, temperatures T, and densities \\rho typical for atmospheres of isolated neutron stars. The first- and second-order thermodynamic functions, monochromatic radiative opacities, and Rosseland mean opacities are calculated and tabulated, taking account of partial ionization, for 8x10^{11} G < B < 3x10^{13} G,\n  2x10^5 K < T < 10^7 K, and a wide range of \\rho. We show that bound-bound and bound-free transitions give an important contribution to the opacities at T < (1-5)x10^6 K in "},"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":"astro-ph/0212062","kind":"arxiv","version":4},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph","submitted_at":"2002-12-03T13:04:09Z","cross_cats_sorted":[],"title_canon_sha256":"4ba454931e51e81b8d2a8793d768061ba0029cf628cdf99aaae3d733883790c3","abstract_canon_sha256":"1601af806995973be36b526576d060c87db9a4b754d0b577ae42793a40778b7b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:31:20.624191Z","signature_b64":"75pTZxP1/nmrJt9Xi2V5hwqKlTyzv7smGsVEnfkMM7NRtW+TDpygHrxQFgh157u0Cyvuv592sUcapCCHQ8S7AQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"f0aa45ea73bad109b1365c99ee4b9862e55814b2e0efbfdec5d4ad79cde39433","last_reissued_at":"2026-07-04T16:31:20.623811Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:31:20.623811Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Equation of state and opacities for hydrogen atmospheres of neutron stars with strong magnetic fields","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Y. Potekhin (Ioffe Inst., ENS-Lyon), G. Chabrier (CRAL, St.-Petersburg)","submitted_at":"2002-12-03T13:04:09Z","abstract_excerpt":"We present an equation of state and radiative opacities for a strongly magnetized hydrogen plasma at magnetic fields B, temperatures T, and densities \\rho typical for atmospheres of isolated neutron stars. The first- and second-order thermodynamic functions, monochromatic radiative opacities, and Rosseland mean opacities are calculated and tabulated, taking account of partial ionization, for 8x10^{11} G < B < 3x10^{13} G,\n  2x10^5 K < T < 10^7 K, and a wide range of \\rho. We show that bound-bound and bound-free transitions give an important contribution to the opacities at T < (1-5)x10^6 K in "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0212062","kind":"arxiv","version":4},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/0212062/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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":"astro-ph/0212062","created_at":"2026-07-04T16:31:20.623874+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0212062v4","created_at":"2026-07-04T16:31:20.623874+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0212062","created_at":"2026-07-04T16:31:20.623874+00:00"},{"alias_kind":"pith_short_12","alias_value":"6CVEL2TTXLIQ","created_at":"2026-07-04T16:31:20.623874+00:00"},{"alias_kind":"pith_short_16","alias_value":"6CVEL2TTXLIQTMJW","created_at":"2026-07-04T16:31:20.623874+00:00"},{"alias_kind":"pith_short_8","alias_value":"6CVEL2TT","created_at":"2026-07-04T16:31:20.623874+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.10342","citing_title":"Magnetospheric flows in X-ray pulsars II: Heating, cooling and ionization degree at sub-critical accretion","ref_index":61,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/6CVEL2TTXLIQTMJWLSM64S4YML","json":"https://pith.science/pith/6CVEL2TTXLIQTMJWLSM64S4YML.json","graph_json":"https://pith.science/api/pith-number/6CVEL2TTXLIQTMJWLSM64S4YML/graph.json","events_json":"https://pith.science/api/pith-number/6CVEL2TTXLIQTMJWLSM64S4YML/events.json","paper":"https://pith.science/paper/6CVEL2TT"},"agent_actions":{"view_html":"https://pith.science/pith/6CVEL2TTXLIQTMJWLSM64S4YML","download_json":"https://pith.science/pith/6CVEL2TTXLIQTMJWLSM64S4YML.json","view_paper":"https://pith.science/paper/6CVEL2TT","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0212062&json=true","fetch_graph":"https://pith.science/api/pith-number/6CVEL2TTXLIQTMJWLSM64S4YML/graph.json","fetch_events":"https://pith.science/api/pith-number/6CVEL2TTXLIQTMJWLSM64S4YML/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/6CVEL2TTXLIQTMJWLSM64S4YML/action/timestamp_anchor","attest_storage":"https://pith.science/pith/6CVEL2TTXLIQTMJWLSM64S4YML/action/storage_attestation","attest_author":"https://pith.science/pith/6CVEL2TTXLIQTMJWLSM64S4YML/action/author_attestation","sign_citation":"https://pith.science/pith/6CVEL2TTXLIQTMJWLSM64S4YML/action/citation_signature","submit_replication":"https://pith.science/pith/6CVEL2TTXLIQTMJWLSM64S4YML/action/replication_record"}},"created_at":"2026-07-04T16:31:20.623874+00:00","updated_at":"2026-07-04T16:31:20.623874+00:00"}