{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2000:ZOONAQX6KDJC3I7BJXAVAATXFH","short_pith_number":"pith:ZOONAQX6","schema_version":"1.0","canonical_sha256":"cb9cd042fe50d22da3e14dc150027729cdbacb81d668c3400486e756aba6cee4","source":{"kind":"arxiv","id":"astro-ph/0001341","version":2},"attestation_state":"computed","paper":{"title":"Radio Pulsar Death Line Revisited: Is PSR J2144-3933 Anomalous?","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"2), (2) NRC research associate, (3) SM&A Corporation), Alexander G. Muslimov (3) ((1) NASA/GSFC, Alice K. Harding (1), Bing Zhang (1","submitted_at":"2000-01-19T18:49:47Z","abstract_excerpt":"We reinvestigate the radio pulsar ``death lines'' within the framework of two different types of polar cap acceleration models, i.e., the vacuum gap model and the space-charge-limited flow model, with either curvature radiation or inverse Compton scattering photons as the source of pairs. General relativistic frame-dragging is taken into account in both models. We find that the inverse Compton scattering induced space-charge-limited flow model can sustain strong pair production in some long-period pulsars, which allows the newly detected 8.5s pulsar PSR J2144-3933 to be radio loud, without ass"},"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/0001341","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2000-01-19T18:49:47Z","cross_cats_sorted":[],"title_canon_sha256":"2062540528619c5eb06d96e55d06715af9774791ac64574a8ee0fbced9478ae2","abstract_canon_sha256":"bbd39b76fa5668f0578304fcad895cd39578cfd221392d9b33bd4fc8e9c3c550"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:15:56.644651Z","signature_b64":"Dbg/+6owa2a1i0XReYCus65MX2IGMUHZCnJMLfeAikjSQUvmUD4K5baAUzKYyGSmYjNzDfWAAyt6QSTet2D4Cw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"cb9cd042fe50d22da3e14dc150027729cdbacb81d668c3400486e756aba6cee4","last_reissued_at":"2026-07-04T16:15:56.644203Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:15:56.644203Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Radio Pulsar Death Line Revisited: Is PSR J2144-3933 Anomalous?","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"2), (2) NRC research associate, (3) SM&A Corporation), Alexander G. Muslimov (3) ((1) NASA/GSFC, Alice K. Harding (1), Bing Zhang (1","submitted_at":"2000-01-19T18:49:47Z","abstract_excerpt":"We reinvestigate the radio pulsar ``death lines'' within the framework of two different types of polar cap acceleration models, i.e., the vacuum gap model and the space-charge-limited flow model, with either curvature radiation or inverse Compton scattering photons as the source of pairs. General relativistic frame-dragging is taken into account in both models. We find that the inverse Compton scattering induced space-charge-limited flow model can sustain strong pair production in some long-period pulsars, which allows the newly detected 8.5s pulsar PSR J2144-3933 to be radio loud, without ass"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0001341","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/0001341/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/0001341","created_at":"2026-07-04T16:15:56.644275+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0001341v2","created_at":"2026-07-04T16:15:56.644275+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0001341","created_at":"2026-07-04T16:15:56.644275+00:00"},{"alias_kind":"pith_short_12","alias_value":"ZOONAQX6KDJC","created_at":"2026-07-04T16:15:56.644275+00:00"},{"alias_kind":"pith_short_16","alias_value":"ZOONAQX6KDJC3I7B","created_at":"2026-07-04T16:15:56.644275+00:00"},{"alias_kind":"pith_short_8","alias_value":"ZOONAQX6","created_at":"2026-07-04T16:15:56.644275+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.03087","citing_title":"Understanding the Neutron Star Population with the SKAO Telescopes","ref_index":254,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ZOONAQX6KDJC3I7BJXAVAATXFH","json":"https://pith.science/pith/ZOONAQX6KDJC3I7BJXAVAATXFH.json","graph_json":"https://pith.science/api/pith-number/ZOONAQX6KDJC3I7BJXAVAATXFH/graph.json","events_json":"https://pith.science/api/pith-number/ZOONAQX6KDJC3I7BJXAVAATXFH/events.json","paper":"https://pith.science/paper/ZOONAQX6"},"agent_actions":{"view_html":"https://pith.science/pith/ZOONAQX6KDJC3I7BJXAVAATXFH","download_json":"https://pith.science/pith/ZOONAQX6KDJC3I7BJXAVAATXFH.json","view_paper":"https://pith.science/paper/ZOONAQX6","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0001341&json=true","fetch_graph":"https://pith.science/api/pith-number/ZOONAQX6KDJC3I7BJXAVAATXFH/graph.json","fetch_events":"https://pith.science/api/pith-number/ZOONAQX6KDJC3I7BJXAVAATXFH/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ZOONAQX6KDJC3I7BJXAVAATXFH/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ZOONAQX6KDJC3I7BJXAVAATXFH/action/storage_attestation","attest_author":"https://pith.science/pith/ZOONAQX6KDJC3I7BJXAVAATXFH/action/author_attestation","sign_citation":"https://pith.science/pith/ZOONAQX6KDJC3I7BJXAVAATXFH/action/citation_signature","submit_replication":"https://pith.science/pith/ZOONAQX6KDJC3I7BJXAVAATXFH/action/replication_record"}},"created_at":"2026-07-04T16:15:56.644275+00:00","updated_at":"2026-07-04T16:15:56.644275+00:00"}