{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1996:6OS6Y72ACT3EDDDTWC6IT2W4I5","short_pith_number":"pith:6OS6Y72A","schema_version":"1.0","canonical_sha256":"f3a5ec7f4014f6418c73b0bc89eadc477583cd4fc05e391b2197fa1b28d9155f","source":{"kind":"arxiv","id":"astro-ph/9604072","version":1},"attestation_state":"computed","paper":{"title":"Model neutron star atmospheres with low magnetic fields. 1. Atmospheres in radiative equilibrium","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Garching, Germany), G.G. Pavlov (Pennsylvania State University, Russia), Technology, USA), V.E. Zavlin (Max-Planck-Institut fuer Extrater. Physik, Yu.A. Shibanov (Ioffe Institute of Physics","submitted_at":"1996-04-13T12:08:55Z","abstract_excerpt":"We present a detailed investigation of neutron star atmospheres with low magnetic fields, $B < 10^8 -10^{10}$ G, which do not affect opacities and equation of state of the atmospheric matter. We compute the atmospheric structure, emergent spectral fluxes and specific intensities for hydrogen, helium and iron atmospheres in a wide domain of effective temperatures and gravitational accelerations expected for neutron stars. The iron atmospheres are computed with the opacities and equations of state from the OPAL opacity library. We show that the model atmosphere spectra are substantially differen"},"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/9604072","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1996-04-13T12:08:55Z","cross_cats_sorted":[],"title_canon_sha256":"d6ec17751e8b58f0e7d5160abfc23f704c014901cf5c7516d0867ae67ff7f814","abstract_canon_sha256":"97f1b2f3a89f149065dce7485be0c3d34ab65bf4959986f711b98631bb701f1c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T14:14:43.877176Z","signature_b64":"lYd6WPnSRQEtpzmnIisB/ctHzh0PWR8QHNA90jXC8W0LXjPGtrA56WGa+bkC4C6JExt6XLaQP0Z4QDVPzbtNBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"f3a5ec7f4014f6418c73b0bc89eadc477583cd4fc05e391b2197fa1b28d9155f","last_reissued_at":"2026-07-04T14:14:43.876736Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T14:14:43.876736Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Model neutron star atmospheres with low magnetic fields. 1. Atmospheres in radiative equilibrium","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Garching, Germany), G.G. Pavlov (Pennsylvania State University, Russia), Technology, USA), V.E. Zavlin (Max-Planck-Institut fuer Extrater. Physik, Yu.A. Shibanov (Ioffe Institute of Physics","submitted_at":"1996-04-13T12:08:55Z","abstract_excerpt":"We present a detailed investigation of neutron star atmospheres with low magnetic fields, $B < 10^8 -10^{10}$ G, which do not affect opacities and equation of state of the atmospheric matter. We compute the atmospheric structure, emergent spectral fluxes and specific intensities for hydrogen, helium and iron atmospheres in a wide domain of effective temperatures and gravitational accelerations expected for neutron stars. The iron atmospheres are computed with the opacities and equations of state from the OPAL opacity library. We show that the model atmosphere spectra are substantially differen"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9604072","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/9604072/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/9604072","created_at":"2026-07-04T14:14:43.876794+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9604072v1","created_at":"2026-07-04T14:14:43.876794+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9604072","created_at":"2026-07-04T14:14:43.876794+00:00"},{"alias_kind":"pith_short_12","alias_value":"6OS6Y72ACT3E","created_at":"2026-07-04T14:14:43.876794+00:00"},{"alias_kind":"pith_short_16","alias_value":"6OS6Y72ACT3EDDDT","created_at":"2026-07-04T14:14:43.876794+00:00"},{"alias_kind":"pith_short_8","alias_value":"6OS6Y72A","created_at":"2026-07-04T14:14:43.876794+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2510.07764","citing_title":"GPU-Accelerated X-ray Pulse Profile Modeling","ref_index":97,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/6OS6Y72ACT3EDDDTWC6IT2W4I5","json":"https://pith.science/pith/6OS6Y72ACT3EDDDTWC6IT2W4I5.json","graph_json":"https://pith.science/api/pith-number/6OS6Y72ACT3EDDDTWC6IT2W4I5/graph.json","events_json":"https://pith.science/api/pith-number/6OS6Y72ACT3EDDDTWC6IT2W4I5/events.json","paper":"https://pith.science/paper/6OS6Y72A"},"agent_actions":{"view_html":"https://pith.science/pith/6OS6Y72ACT3EDDDTWC6IT2W4I5","download_json":"https://pith.science/pith/6OS6Y72ACT3EDDDTWC6IT2W4I5.json","view_paper":"https://pith.science/paper/6OS6Y72A","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9604072&json=true","fetch_graph":"https://pith.science/api/pith-number/6OS6Y72ACT3EDDDTWC6IT2W4I5/graph.json","fetch_events":"https://pith.science/api/pith-number/6OS6Y72ACT3EDDDTWC6IT2W4I5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/6OS6Y72ACT3EDDDTWC6IT2W4I5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/6OS6Y72ACT3EDDDTWC6IT2W4I5/action/storage_attestation","attest_author":"https://pith.science/pith/6OS6Y72ACT3EDDDTWC6IT2W4I5/action/author_attestation","sign_citation":"https://pith.science/pith/6OS6Y72ACT3EDDDTWC6IT2W4I5/action/citation_signature","submit_replication":"https://pith.science/pith/6OS6Y72ACT3EDDDTWC6IT2W4I5/action/replication_record"}},"created_at":"2026-07-04T14:14:43.876794+00:00","updated_at":"2026-07-04T14:14:43.876794+00:00"}