{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:CS6WFAFXJOC4UGRQZ5WAJMYLJ5","short_pith_number":"pith:CS6WFAFX","schema_version":"1.0","canonical_sha256":"14bd6280b74b85ca1a30cf6c04b30b4f40f6e15111834649c408fdc05ff79970","source":{"kind":"arxiv","id":"1812.01930","version":3},"attestation_state":"computed","paper":{"title":"Formation and Evolution of Primordial Black Hole Binaries in the Early Universe","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Christian Spethmann, Hardi Veerm\\\"ae, Martti Raidal, Ville Vaskonen","submitted_at":"2018-12-05T11:51:33Z","abstract_excerpt":"The abundance of primordial black holes (PBHs) in the mass range $0.1 - 10^3 M_\\odot$ can potentially be tested by gravitational wave observations due to the large merger rate of PBH binaries formed in the early universe. To put the estimates of the latter on a firmer footing, we first derive analytical PBH merger rate for general PBH mass functions while imposing a minimal initial comoving distance between the binary and the PBH nearest to it, in order to pick only initial configurations where the binary would not get disrupted. We then study the formation and evolution of PBH binaries before"},"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":"1812.01930","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2018-12-05T11:51:33Z","cross_cats_sorted":["astro-ph.HE","hep-ph"],"title_canon_sha256":"97c026e7ff28722195e3b1f54dc751bf1efbb9437081c31594243a7330fcd9ee","abstract_canon_sha256":"d5363f3499ab1033e252ccb5f6ea5b49e289c83924050be98a823009e8d465a7"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:52:30.009940Z","signature_b64":"LrZ48jESl94L5fGC9K1ViNxPazyzhR1DaoNwotqu7VKF59akVrt/wY/q9uJbebuHjNVOEUKDegqsboj3UVkoDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"14bd6280b74b85ca1a30cf6c04b30b4f40f6e15111834649c408fdc05ff79970","last_reissued_at":"2026-05-17T23:52:30.009351Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:52:30.009351Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Formation and Evolution of Primordial Black Hole Binaries in the Early Universe","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Christian Spethmann, Hardi Veerm\\\"ae, Martti Raidal, Ville Vaskonen","submitted_at":"2018-12-05T11:51:33Z","abstract_excerpt":"The abundance of primordial black holes (PBHs) in the mass range $0.1 - 10^3 M_\\odot$ can potentially be tested by gravitational wave observations due to the large merger rate of PBH binaries formed in the early universe. To put the estimates of the latter on a firmer footing, we first derive analytical PBH merger rate for general PBH mass functions while imposing a minimal initial comoving distance between the binary and the PBH nearest to it, in order to pick only initial configurations where the binary would not get disrupted. We then study the formation and evolution of PBH binaries before"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1812.01930","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":""},"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":"1812.01930","created_at":"2026-05-17T23:52:30.009437+00:00"},{"alias_kind":"arxiv_version","alias_value":"1812.01930v3","created_at":"2026-05-17T23:52:30.009437+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1812.01930","created_at":"2026-05-17T23:52:30.009437+00:00"},{"alias_kind":"pith_short_12","alias_value":"CS6WFAFXJOC4","created_at":"2026-05-18T12:32:19.392346+00:00"},{"alias_kind":"pith_short_16","alias_value":"CS6WFAFXJOC4UGRQ","created_at":"2026-05-18T12:32:19.392346+00:00"},{"alias_kind":"pith_short_8","alias_value":"CS6WFAFX","created_at":"2026-05-18T12:32:19.392346+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":12,"internal_anchor_count":7,"sample":[{"citing_arxiv_id":"2605.15749","citing_title":"Constraints on primordial black holes from the first part of LIGO-Virgo-KAGRA fourth observing run","ref_index":97,"is_internal_anchor":true},{"citing_arxiv_id":"2605.18097","citing_title":"Effects of formation channels and gravitational lensing on stochastic gravitational wave background","ref_index":70,"is_internal_anchor":true},{"citing_arxiv_id":"2508.09965","citing_title":"GW231123: A Possible Primordial Black Hole Origin","ref_index":86,"is_internal_anchor":true},{"citing_arxiv_id":"2510.11861","citing_title":"Impact of facility timing and coordination for next-generation gravitational-wave detectors","ref_index":42,"is_internal_anchor":true},{"citing_arxiv_id":"2303.15923","citing_title":"Science with the Einstein Telescope: a comparison of different designs","ref_index":270,"is_internal_anchor":true},{"citing_arxiv_id":"2006.02838","citing_title":"Primordial Black Holes as Dark Matter: Recent Developments","ref_index":228,"is_internal_anchor":true},{"citing_arxiv_id":"2601.19386","citing_title":"Constraints on Primordial Black Holes from Galactic Diffuse Synchrotron Emissions","ref_index":29,"is_internal_anchor":true},{"citing_arxiv_id":"2604.01684","citing_title":"Smoluchowski Coagulation Equation and the Evolution of Primordial Black Hole Clusters","ref_index":31,"is_internal_anchor":false},{"citing_arxiv_id":"2604.22731","citing_title":"Precision Analysis for $\\boldsymbol{H_0}$ Using Upcoming Multi-band Gravitational Wave Observations","ref_index":57,"is_internal_anchor":false},{"citing_arxiv_id":"2604.22462","citing_title":"Machine Learning for Multi-messenger Probes of New Physics and Cosmology: A Review and Perspective","ref_index":158,"is_internal_anchor":false},{"citing_arxiv_id":"2604.19316","citing_title":"Merger rate of initially clustered primordial black holes for the two-body channel","ref_index":17,"is_internal_anchor":false},{"citing_arxiv_id":"2604.14871","citing_title":"Microscopic primordial black holes as macroscopic dark matter from large extra dimensions","ref_index":56,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/CS6WFAFXJOC4UGRQZ5WAJMYLJ5","json":"https://pith.science/pith/CS6WFAFXJOC4UGRQZ5WAJMYLJ5.json","graph_json":"https://pith.science/api/pith-number/CS6WFAFXJOC4UGRQZ5WAJMYLJ5/graph.json","events_json":"https://pith.science/api/pith-number/CS6WFAFXJOC4UGRQZ5WAJMYLJ5/events.json","paper":"https://pith.science/paper/CS6WFAFX"},"agent_actions":{"view_html":"https://pith.science/pith/CS6WFAFXJOC4UGRQZ5WAJMYLJ5","download_json":"https://pith.science/pith/CS6WFAFXJOC4UGRQZ5WAJMYLJ5.json","view_paper":"https://pith.science/paper/CS6WFAFX","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1812.01930&json=true","fetch_graph":"https://pith.science/api/pith-number/CS6WFAFXJOC4UGRQZ5WAJMYLJ5/graph.json","fetch_events":"https://pith.science/api/pith-number/CS6WFAFXJOC4UGRQZ5WAJMYLJ5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/CS6WFAFXJOC4UGRQZ5WAJMYLJ5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/CS6WFAFXJOC4UGRQZ5WAJMYLJ5/action/storage_attestation","attest_author":"https://pith.science/pith/CS6WFAFXJOC4UGRQZ5WAJMYLJ5/action/author_attestation","sign_citation":"https://pith.science/pith/CS6WFAFXJOC4UGRQZ5WAJMYLJ5/action/citation_signature","submit_replication":"https://pith.science/pith/CS6WFAFXJOC4UGRQZ5WAJMYLJ5/action/replication_record"}},"created_at":"2026-05-17T23:52:30.009437+00:00","updated_at":"2026-05-17T23:52:30.009437+00:00"}