{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:PN5ETRAYET4SRNIVDRFBOF7NYY","short_pith_number":"pith:PN5ETRAY","schema_version":"1.0","canonical_sha256":"7b7a49c41824f928b5151c4a1717edc60715a624c902659609c94b2a598a15df","source":{"kind":"arxiv","id":"0910.3684","version":1},"attestation_state":"computed","paper":{"title":"Space and velocity distributions of Galactic isolated old Neutron stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.GA","authors_text":"E. O. Ofek","submitted_at":"2009-10-19T20:15:02Z","abstract_excerpt":"I present the results of Monte-Carlo orbital simulations of Galactic Neutron Stars (NSs). The simulations take into account the up-to-date observed NS space and velocity distributions at birth, and account for their formation rate. I simulate two populations of NSs. Objects in the first population were born in the Galactic disk at a constant rate, in the past 12 Gyr. Those in the second population were formed simultaneously 12 Gyr ago in the Galactic bulge. I assume that the NSs born in the Galactic disk comprise 40% of the total NS population. Since the initial velocity distribution of NSs is"},"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":"0910.3684","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2009-10-19T20:15:02Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"6c5a38160e1f9c50b3a27f9da81519621d7e0bd7ec98eb3b06b76b49c3215f76","abstract_canon_sha256":"6272786022500be2ece3003a8ba4d0d79a23ef18c7ed37582c0e624fbcfdc366"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:37:33.572929Z","signature_b64":"6twu3Kc/tgyd8x+SGUQ97G5peQ3Pj3KoEWvDwfN+hp20QgdZCQ0qll17dW0fZjlH3qfSy4AZ2uE4z3Ey2/l+Dw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7b7a49c41824f928b5151c4a1717edc60715a624c902659609c94b2a598a15df","last_reissued_at":"2026-05-18T04:37:33.572207Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:37:33.572207Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Space and velocity distributions of Galactic isolated old Neutron stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.GA","authors_text":"E. O. Ofek","submitted_at":"2009-10-19T20:15:02Z","abstract_excerpt":"I present the results of Monte-Carlo orbital simulations of Galactic Neutron Stars (NSs). The simulations take into account the up-to-date observed NS space and velocity distributions at birth, and account for their formation rate. I simulate two populations of NSs. Objects in the first population were born in the Galactic disk at a constant rate, in the past 12 Gyr. Those in the second population were formed simultaneously 12 Gyr ago in the Galactic bulge. I assume that the NSs born in the Galactic disk comprise 40% of the total NS population. Since the initial velocity distribution of NSs is"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0910.3684","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":"0910.3684","created_at":"2026-05-18T04:37:33.572329+00:00"},{"alias_kind":"arxiv_version","alias_value":"0910.3684v1","created_at":"2026-05-18T04:37:33.572329+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0910.3684","created_at":"2026-05-18T04:37:33.572329+00:00"},{"alias_kind":"pith_short_12","alias_value":"PN5ETRAYET4S","created_at":"2026-05-18T12:26:01.383474+00:00"},{"alias_kind":"pith_short_16","alias_value":"PN5ETRAYET4SRNIV","created_at":"2026-05-18T12:26:01.383474+00:00"},{"alias_kind":"pith_short_8","alias_value":"PN5ETRAY","created_at":"2026-05-18T12:26:01.383474+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.21652","citing_title":"Constraining dark matter self-interaction from kinetic heating in neutron stars","ref_index":110,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/PN5ETRAYET4SRNIVDRFBOF7NYY","json":"https://pith.science/pith/PN5ETRAYET4SRNIVDRFBOF7NYY.json","graph_json":"https://pith.science/api/pith-number/PN5ETRAYET4SRNIVDRFBOF7NYY/graph.json","events_json":"https://pith.science/api/pith-number/PN5ETRAYET4SRNIVDRFBOF7NYY/events.json","paper":"https://pith.science/paper/PN5ETRAY"},"agent_actions":{"view_html":"https://pith.science/pith/PN5ETRAYET4SRNIVDRFBOF7NYY","download_json":"https://pith.science/pith/PN5ETRAYET4SRNIVDRFBOF7NYY.json","view_paper":"https://pith.science/paper/PN5ETRAY","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0910.3684&json=true","fetch_graph":"https://pith.science/api/pith-number/PN5ETRAYET4SRNIVDRFBOF7NYY/graph.json","fetch_events":"https://pith.science/api/pith-number/PN5ETRAYET4SRNIVDRFBOF7NYY/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PN5ETRAYET4SRNIVDRFBOF7NYY/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PN5ETRAYET4SRNIVDRFBOF7NYY/action/storage_attestation","attest_author":"https://pith.science/pith/PN5ETRAYET4SRNIVDRFBOF7NYY/action/author_attestation","sign_citation":"https://pith.science/pith/PN5ETRAYET4SRNIVDRFBOF7NYY/action/citation_signature","submit_replication":"https://pith.science/pith/PN5ETRAYET4SRNIVDRFBOF7NYY/action/replication_record"}},"created_at":"2026-05-18T04:37:33.572329+00:00","updated_at":"2026-05-18T04:37:33.572329+00:00"}