{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1999:EYUYYMTDPJWO67FX3NKMVMQ43W","short_pith_number":"pith:EYUYYMTD","schema_version":"1.0","canonical_sha256":"26298c32637a6cef7cb7db54cab21cdd99edbc1c490f5cd3091e06be54449b29","source":{"kind":"arxiv","id":"astro-ph/9903127","version":3},"attestation_state":"computed","paper":{"title":"Transport properties of degenerate electrons in neutron star envelopes and white dwarf cores","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Y. Potekhin (1), D. A. Baiko (1), D. G. Yakovlev (1) ((1) Ioffe Phys.-Tech. Inst., P. Haensel (2), St.Petersburg; (2) CAMK, Warsaw)","submitted_at":"1999-03-09T13:15:32Z","abstract_excerpt":"New calculations of the thermal and electrical electron conductivities are performed for a broad range of physical parameters typical for envelopes of neutron stars and cores of white dwarfs. We consider stellar matter composed of astrophysically important chemical elements from H to Fe in the density range from 10^2-10^4 g/ccm up to 10^7-10^{10} g/ccm, where atoms are fully ionized and electrons are strongly degenerate. We have used modified ion structure factors suggested in physics/9811052. In the ion liquid, these modifications take into account, in an approximate way, instantaneous electr"},"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/9903127","kind":"arxiv","version":3},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1999-03-09T13:15:32Z","cross_cats_sorted":[],"title_canon_sha256":"3e3b15c428be60c9aa95847fb761b5db84c940b612b45bfde9de79eda3e5462c","abstract_canon_sha256":"c24734c50ef08eee0ce7b4f239385098fc6baaa3b5d77753e77c4f74e9750e3e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:21:32.367619Z","signature_b64":"Oc0qb1DE54WBdVqyw8yQszFG4zXeHAU2yPon+//QD0xtauvSCxWS7U2D3JdS/aYDCZUnqI8QiZvmrHKscN9dBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"26298c32637a6cef7cb7db54cab21cdd99edbc1c490f5cd3091e06be54449b29","last_reissued_at":"2026-05-18T04:21:32.367199Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:21:32.367199Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Transport properties of degenerate electrons in neutron star envelopes and white dwarf cores","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Y. Potekhin (1), D. A. Baiko (1), D. G. Yakovlev (1) ((1) Ioffe Phys.-Tech. Inst., P. Haensel (2), St.Petersburg; (2) CAMK, Warsaw)","submitted_at":"1999-03-09T13:15:32Z","abstract_excerpt":"New calculations of the thermal and electrical electron conductivities are performed for a broad range of physical parameters typical for envelopes of neutron stars and cores of white dwarfs. We consider stellar matter composed of astrophysically important chemical elements from H to Fe in the density range from 10^2-10^4 g/ccm up to 10^7-10^{10} g/ccm, where atoms are fully ionized and electrons are strongly degenerate. We have used modified ion structure factors suggested in physics/9811052. In the ion liquid, these modifications take into account, in an approximate way, instantaneous electr"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9903127","kind":"arxiv","version":3},"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":"astro-ph/9903127","created_at":"2026-05-18T04:21:32.367257+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9903127v3","created_at":"2026-05-18T04:21:32.367257+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9903127","created_at":"2026-05-18T04:21:32.367257+00:00"},{"alias_kind":"pith_short_12","alias_value":"EYUYYMTDPJWO","created_at":"2026-05-18T12:25:49.631198+00:00"},{"alias_kind":"pith_short_16","alias_value":"EYUYYMTDPJWO67FX","created_at":"2026-05-18T12:25:49.631198+00:00"},{"alias_kind":"pith_short_8","alias_value":"EYUYYMTD","created_at":"2026-05-18T12:25:49.631198+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.15857","citing_title":"Tracing the outburst decay of soft X-ray transients Aql X-1 and 4U 1608-52 with XSPECT","ref_index":122,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/EYUYYMTDPJWO67FX3NKMVMQ43W","json":"https://pith.science/pith/EYUYYMTDPJWO67FX3NKMVMQ43W.json","graph_json":"https://pith.science/api/pith-number/EYUYYMTDPJWO67FX3NKMVMQ43W/graph.json","events_json":"https://pith.science/api/pith-number/EYUYYMTDPJWO67FX3NKMVMQ43W/events.json","paper":"https://pith.science/paper/EYUYYMTD"},"agent_actions":{"view_html":"https://pith.science/pith/EYUYYMTDPJWO67FX3NKMVMQ43W","download_json":"https://pith.science/pith/EYUYYMTDPJWO67FX3NKMVMQ43W.json","view_paper":"https://pith.science/paper/EYUYYMTD","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9903127&json=true","fetch_graph":"https://pith.science/api/pith-number/EYUYYMTDPJWO67FX3NKMVMQ43W/graph.json","fetch_events":"https://pith.science/api/pith-number/EYUYYMTDPJWO67FX3NKMVMQ43W/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/EYUYYMTDPJWO67FX3NKMVMQ43W/action/timestamp_anchor","attest_storage":"https://pith.science/pith/EYUYYMTDPJWO67FX3NKMVMQ43W/action/storage_attestation","attest_author":"https://pith.science/pith/EYUYYMTDPJWO67FX3NKMVMQ43W/action/author_attestation","sign_citation":"https://pith.science/pith/EYUYYMTDPJWO67FX3NKMVMQ43W/action/citation_signature","submit_replication":"https://pith.science/pith/EYUYYMTDPJWO67FX3NKMVMQ43W/action/replication_record"}},"created_at":"2026-05-18T04:21:32.367257+00:00","updated_at":"2026-05-18T04:21:32.367257+00:00"}