{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2004:FVKWTJ6PQWYPSAFHFRVRZBW5DP","short_pith_number":"pith:FVKWTJ6P","schema_version":"1.0","canonical_sha256":"2d5569a7cf85b0f900a72c6b1c86dd1bfd28c55739ccaf640a2ab655bf1ee93e","source":{"kind":"arxiv","id":"astro-ph/0408538","version":3},"attestation_state":"computed","paper":{"title":"High Energy Emission from Magnetars","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A.M. Beloborodov, C. Thompson","submitted_at":"2004-08-30T19:46:36Z","abstract_excerpt":"The recently discovered soft gamma-ray emission from the anomalous X-ray pulsar 1E 1841-045 has a luminosity L_g ~ 10^{36} ergs/s. This luminosity exceeds the spindown power by three orders of magnitude and must be fed by an alternative source of energy such as an ultrastrong magnetic field. A gradual release of energy in the stellar magnetosphere is expected if it is twisted and a strong electric current is induced on the closed field lines. We examine two mechanisms of gamma-ray emission associated with the gradual dissipation of this current. (1) A thin surface layer of the star is heated b"},"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/0408538","kind":"arxiv","version":3},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2004-08-30T19:46:36Z","cross_cats_sorted":[],"title_canon_sha256":"30d50ca5718c45ad4940a843bc696739838411a4371eb9c4306a0aa708129a76","abstract_canon_sha256":"fb1d0feceac890dedd44f2b3a921ea71b63b1447fcf09c649bb0b8e64dbd62c0"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:44:34.886449Z","signature_b64":"hgPx7DwYGRy52w2go1pcwj7paeEVTPDf0CRWmwIiueMuZB1Dg0wr1ACt8V2ztT4Fmt6lgeedacsjsbft6p2gBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2d5569a7cf85b0f900a72c6b1c86dd1bfd28c55739ccaf640a2ab655bf1ee93e","last_reissued_at":"2026-07-04T16:44:34.886084Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:44:34.886084Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"High Energy Emission from Magnetars","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A.M. Beloborodov, C. Thompson","submitted_at":"2004-08-30T19:46:36Z","abstract_excerpt":"The recently discovered soft gamma-ray emission from the anomalous X-ray pulsar 1E 1841-045 has a luminosity L_g ~ 10^{36} ergs/s. This luminosity exceeds the spindown power by three orders of magnitude and must be fed by an alternative source of energy such as an ultrastrong magnetic field. A gradual release of energy in the stellar magnetosphere is expected if it is twisted and a strong electric current is induced on the closed field lines. We examine two mechanisms of gamma-ray emission associated with the gradual dissipation of this current. (1) A thin surface layer of the star is heated b"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0408538","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/0408538/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/0408538","created_at":"2026-07-04T16:44:34.886144+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0408538v3","created_at":"2026-07-04T16:44:34.886144+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0408538","created_at":"2026-07-04T16:44:34.886144+00:00"},{"alias_kind":"pith_short_12","alias_value":"FVKWTJ6PQWYP","created_at":"2026-07-04T16:44:34.886144+00:00"},{"alias_kind":"pith_short_16","alias_value":"FVKWTJ6PQWYPSAFH","created_at":"2026-07-04T16:44:34.886144+00:00"},{"alias_kind":"pith_short_8","alias_value":"FVKWTJ6P","created_at":"2026-07-04T16:44:34.886144+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2508.19801","citing_title":"On Ultra-long Period (53.8 min) Pulsar ASKAP J1935+2148: Coherent Radio Emission Triggered by Local Superstrong Magnetic Reconnection","ref_index":83,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/FVKWTJ6PQWYPSAFHFRVRZBW5DP","json":"https://pith.science/pith/FVKWTJ6PQWYPSAFHFRVRZBW5DP.json","graph_json":"https://pith.science/api/pith-number/FVKWTJ6PQWYPSAFHFRVRZBW5DP/graph.json","events_json":"https://pith.science/api/pith-number/FVKWTJ6PQWYPSAFHFRVRZBW5DP/events.json","paper":"https://pith.science/paper/FVKWTJ6P"},"agent_actions":{"view_html":"https://pith.science/pith/FVKWTJ6PQWYPSAFHFRVRZBW5DP","download_json":"https://pith.science/pith/FVKWTJ6PQWYPSAFHFRVRZBW5DP.json","view_paper":"https://pith.science/paper/FVKWTJ6P","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0408538&json=true","fetch_graph":"https://pith.science/api/pith-number/FVKWTJ6PQWYPSAFHFRVRZBW5DP/graph.json","fetch_events":"https://pith.science/api/pith-number/FVKWTJ6PQWYPSAFHFRVRZBW5DP/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/FVKWTJ6PQWYPSAFHFRVRZBW5DP/action/timestamp_anchor","attest_storage":"https://pith.science/pith/FVKWTJ6PQWYPSAFHFRVRZBW5DP/action/storage_attestation","attest_author":"https://pith.science/pith/FVKWTJ6PQWYPSAFHFRVRZBW5DP/action/author_attestation","sign_citation":"https://pith.science/pith/FVKWTJ6PQWYPSAFHFRVRZBW5DP/action/citation_signature","submit_replication":"https://pith.science/pith/FVKWTJ6PQWYPSAFHFRVRZBW5DP/action/replication_record"}},"created_at":"2026-07-04T16:44:34.886144+00:00","updated_at":"2026-07-04T16:44:34.886144+00:00"}