{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2015:NJNACFEYF6DYOLGC2PIYAGQR3J","short_pith_number":"pith:NJNACFEY","schema_version":"1.0","canonical_sha256":"6a5a0114982f87872cc2d3d1801a11da587fed4e830f2b5c002ecc2b7a7f675d","source":{"kind":"arxiv","id":"1506.03933","version":2},"attestation_state":"computed","paper":{"title":"Magnetic field growth in young glitching pulsars with a braking index","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"Wynn C. G. Ho (Univ of Southampton)","submitted_at":"2015-06-12T08:27:15Z","abstract_excerpt":"In the standard scenario for spin evolution of isolated neutron stars, a young pulsar slows down with a surface magnetic field B that does not change. Thus the pulsar follows a constant B trajectory in the phase space of spin period and spin period time derivative. Such an evolution predicts a braking index n = 3 while the field is constant and n > 3 when the field decays. This contrasts with all nine observed values being n < 3. Here we consider a magnetic field that is buried soon after birth and diffuses to the surface. We use a model of a growing surface magnetic field to fit observations "},"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":"1506.03933","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2015-06-12T08:27:15Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"6140b0253406efb422d497925b86e369584e6398d43b86b6a60bbeb59a8de768","abstract_canon_sha256":"8dcec62ce6ae92d70e98c21ebad068b67a0f29351a7d83284e59919553d71d2e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:37:10.742262Z","signature_b64":"X3RwFhtGqSnjKbYy7anECw68r3ZBcJeTohI8xLodOFVQe7dfFZ7J9V4A1h8Z6KUQs9g1i7nKcBmsFcq3mKgKDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6a5a0114982f87872cc2d3d1801a11da587fed4e830f2b5c002ecc2b7a7f675d","last_reissued_at":"2026-05-18T01:37:10.741257Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:37:10.741257Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Magnetic field growth in young glitching pulsars with a braking index","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"Wynn C. G. Ho (Univ of Southampton)","submitted_at":"2015-06-12T08:27:15Z","abstract_excerpt":"In the standard scenario for spin evolution of isolated neutron stars, a young pulsar slows down with a surface magnetic field B that does not change. Thus the pulsar follows a constant B trajectory in the phase space of spin period and spin period time derivative. Such an evolution predicts a braking index n = 3 while the field is constant and n > 3 when the field decays. This contrasts with all nine observed values being n < 3. Here we consider a magnetic field that is buried soon after birth and diffuses to the surface. We use a model of a growing surface magnetic field to fit observations "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1506.03933","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":""},"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":"1506.03933","created_at":"2026-05-18T01:37:10.741387+00:00"},{"alias_kind":"arxiv_version","alias_value":"1506.03933v2","created_at":"2026-05-18T01:37:10.741387+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1506.03933","created_at":"2026-05-18T01:37:10.741387+00:00"},{"alias_kind":"pith_short_12","alias_value":"NJNACFEYF6DY","created_at":"2026-05-18T12:29:32.376354+00:00"},{"alias_kind":"pith_short_16","alias_value":"NJNACFEYF6DYOLGC","created_at":"2026-05-18T12:29:32.376354+00:00"},{"alias_kind":"pith_short_8","alias_value":"NJNACFEY","created_at":"2026-05-18T12:29:32.376354+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2512.17214","citing_title":"Pulsed radio emission from a Central Compact Object","ref_index":36,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/NJNACFEYF6DYOLGC2PIYAGQR3J","json":"https://pith.science/pith/NJNACFEYF6DYOLGC2PIYAGQR3J.json","graph_json":"https://pith.science/api/pith-number/NJNACFEYF6DYOLGC2PIYAGQR3J/graph.json","events_json":"https://pith.science/api/pith-number/NJNACFEYF6DYOLGC2PIYAGQR3J/events.json","paper":"https://pith.science/paper/NJNACFEY"},"agent_actions":{"view_html":"https://pith.science/pith/NJNACFEYF6DYOLGC2PIYAGQR3J","download_json":"https://pith.science/pith/NJNACFEYF6DYOLGC2PIYAGQR3J.json","view_paper":"https://pith.science/paper/NJNACFEY","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1506.03933&json=true","fetch_graph":"https://pith.science/api/pith-number/NJNACFEYF6DYOLGC2PIYAGQR3J/graph.json","fetch_events":"https://pith.science/api/pith-number/NJNACFEYF6DYOLGC2PIYAGQR3J/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/NJNACFEYF6DYOLGC2PIYAGQR3J/action/timestamp_anchor","attest_storage":"https://pith.science/pith/NJNACFEYF6DYOLGC2PIYAGQR3J/action/storage_attestation","attest_author":"https://pith.science/pith/NJNACFEYF6DYOLGC2PIYAGQR3J/action/author_attestation","sign_citation":"https://pith.science/pith/NJNACFEYF6DYOLGC2PIYAGQR3J/action/citation_signature","submit_replication":"https://pith.science/pith/NJNACFEYF6DYOLGC2PIYAGQR3J/action/replication_record"}},"created_at":"2026-05-18T01:37:10.741387+00:00","updated_at":"2026-05-18T01:37:10.741387+00:00"}