{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:BXHI6R5Z4ETQ2O2BABXUAMCFQB","short_pith_number":"pith:BXHI6R5Z","schema_version":"1.0","canonical_sha256":"0dce8f47b9e1270d3b41006f403045807e30762ce0098b618a194cd8d9458f00","source":{"kind":"arxiv","id":"1301.6429","version":1},"attestation_state":"computed","paper":{"title":"An Asteroid Belt Interpretation for the Timing Variations of the Millisecond Pulsar B1937+21","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"A. Jessner, B. W. Stappers, G. Desvignes, G. H. Janssen, G. Theureau, I. Cognard, J. M. Cordes, K. Lazaridis, M. B. Purver, M. Kramer, R. M. Shannon, T. J. W. Lazio, T. S. Metcalfe","submitted_at":"2013-01-28T02:35:31Z","abstract_excerpt":"Pulsar timing observations have revealed companions to neutron stars that include other neutron stars, white dwarfs, main-sequence stars, and planets. We demonstrate that the correlated and apparently stochastic residual times of arrival from the millisecond pulsar B1937+21 are consistent with the signature of an asteroid belt having a total mass less than approximately 0.05 Earth masses. Unlike the solar system's asteroid belt, the best fit pulsar asteroid belt extends over a wide range of radii, consistent with the absence of any shepherding companions. We suggest that any pulsar that has un"},"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":"1301.6429","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2013-01-28T02:35:31Z","cross_cats_sorted":["astro-ph.EP"],"title_canon_sha256":"27124cce239b74c989bc440cf5cc85f8c4c05b91a16aa22793cfb6cb1dc15df2","abstract_canon_sha256":"a8cf4a84a7a04440e016a6c1660d765e2924ae4a96d04360a48064c21d44688b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:51:58.068199Z","signature_b64":"v45Z+WxS5x5rmQc2H3UQdFZ31+mbjIDXiSp1Aq+NwRCduNmRPEOVyZdL5lpgvjzh/0REy2E5cIGVZuJG0QG2Dg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"0dce8f47b9e1270d3b41006f403045807e30762ce0098b618a194cd8d9458f00","last_reissued_at":"2026-05-18T01:51:58.067698Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:51:58.067698Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"An Asteroid Belt Interpretation for the Timing Variations of the Millisecond Pulsar B1937+21","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"A. Jessner, B. W. Stappers, G. Desvignes, G. H. Janssen, G. Theureau, I. Cognard, J. M. Cordes, K. Lazaridis, M. B. Purver, M. Kramer, R. M. Shannon, T. J. W. Lazio, T. S. Metcalfe","submitted_at":"2013-01-28T02:35:31Z","abstract_excerpt":"Pulsar timing observations have revealed companions to neutron stars that include other neutron stars, white dwarfs, main-sequence stars, and planets. We demonstrate that the correlated and apparently stochastic residual times of arrival from the millisecond pulsar B1937+21 are consistent with the signature of an asteroid belt having a total mass less than approximately 0.05 Earth masses. Unlike the solar system's asteroid belt, the best fit pulsar asteroid belt extends over a wide range of radii, consistent with the absence of any shepherding companions. We suggest that any pulsar that has un"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1301.6429","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":""},"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":"1301.6429","created_at":"2026-05-18T01:51:58.067785+00:00"},{"alias_kind":"arxiv_version","alias_value":"1301.6429v1","created_at":"2026-05-18T01:51:58.067785+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1301.6429","created_at":"2026-05-18T01:51:58.067785+00:00"},{"alias_kind":"pith_short_12","alias_value":"BXHI6R5Z4ETQ","created_at":"2026-05-18T12:27:40.988391+00:00"},{"alias_kind":"pith_short_16","alias_value":"BXHI6R5Z4ETQ2O2B","created_at":"2026-05-18T12:27:40.988391+00:00"},{"alias_kind":"pith_short_8","alias_value":"BXHI6R5Z","created_at":"2026-05-18T12:27:40.988391+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2606.28571","citing_title":"The NANOGrav 15 yr Data Set: Customized Chromatic Noise Models","ref_index":3,"is_internal_anchor":true},{"citing_arxiv_id":"2606.28554","citing_title":"The NANOGrav 15 yr Data Set: Impacts of Customized Chromatic Noise Models on Gravitational Wave Analyses","ref_index":14,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/BXHI6R5Z4ETQ2O2BABXUAMCFQB","json":"https://pith.science/pith/BXHI6R5Z4ETQ2O2BABXUAMCFQB.json","graph_json":"https://pith.science/api/pith-number/BXHI6R5Z4ETQ2O2BABXUAMCFQB/graph.json","events_json":"https://pith.science/api/pith-number/BXHI6R5Z4ETQ2O2BABXUAMCFQB/events.json","paper":"https://pith.science/paper/BXHI6R5Z"},"agent_actions":{"view_html":"https://pith.science/pith/BXHI6R5Z4ETQ2O2BABXUAMCFQB","download_json":"https://pith.science/pith/BXHI6R5Z4ETQ2O2BABXUAMCFQB.json","view_paper":"https://pith.science/paper/BXHI6R5Z","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1301.6429&json=true","fetch_graph":"https://pith.science/api/pith-number/BXHI6R5Z4ETQ2O2BABXUAMCFQB/graph.json","fetch_events":"https://pith.science/api/pith-number/BXHI6R5Z4ETQ2O2BABXUAMCFQB/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/BXHI6R5Z4ETQ2O2BABXUAMCFQB/action/timestamp_anchor","attest_storage":"https://pith.science/pith/BXHI6R5Z4ETQ2O2BABXUAMCFQB/action/storage_attestation","attest_author":"https://pith.science/pith/BXHI6R5Z4ETQ2O2BABXUAMCFQB/action/author_attestation","sign_citation":"https://pith.science/pith/BXHI6R5Z4ETQ2O2BABXUAMCFQB/action/citation_signature","submit_replication":"https://pith.science/pith/BXHI6R5Z4ETQ2O2BABXUAMCFQB/action/replication_record"}},"created_at":"2026-05-18T01:51:58.067785+00:00","updated_at":"2026-05-18T01:51:58.067785+00:00"}