{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:KHOMBGSBPEJKX4AS4BH4F5FSXD","short_pith_number":"pith:KHOMBGSB","schema_version":"1.0","canonical_sha256":"51dcc09a417912abf012e04fc2f4b2b8c9f1478a0f760a0993bb4b4285390d6a","source":{"kind":"arxiv","id":"2112.12335","version":3},"attestation_state":"computed","paper":{"title":"Primordial black hole formation from massless scalar isocurvature","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.CO","hep-th"],"primary_cat":"gr-qc","authors_text":"Chul-Moon Yoo, Hirotada Okawa, Misao Sasaki, Shin'ichi Hirano, Tomohiro Harada","submitted_at":"2021-12-23T03:12:24Z","abstract_excerpt":"We numerically study the primordial black hole (PBH) formation by an isocurvature perturbation of a massless scalar field on super Hubble scales in the radiation-dominated universe. As a first step we perform simulations of spherically symmetric configurations. For the initial condition, we employ the spatial gradient expansion and provide the general form of the growing mode solutions valid up through the second order in this expansion. The initial scalar field profile is assumed to be Gaussian with a characteristic comoving wavenumber $k$; $\\sim\\exp(-k^2R^2)$, where $R$ is the radial coordin"},"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":"2112.12335","kind":"arxiv","version":3},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"gr-qc","submitted_at":"2021-12-23T03:12:24Z","cross_cats_sorted":["astro-ph.CO","hep-th"],"title_canon_sha256":"bdd4be1627fa9f462b160b10477ba45972b6470293bf5ddb46762b11deb62d5b","abstract_canon_sha256":"7803d5605715b7e2c6f56a8ac69ebcc2bac4077808867b4ba135861a5c44a25a"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:33:28.128518Z","signature_b64":"Dn2WXCy0l2VIivGhBCARIpQ50UuosV0LsRw53UsTTAppbkPdikgy/WJev6e+qX7eKKVcHwlo5RvFMsV5sI1xCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"51dcc09a417912abf012e04fc2f4b2b8c9f1478a0f760a0993bb4b4285390d6a","last_reissued_at":"2026-07-05T04:33:28.128034Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:33:28.128034Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Primordial black hole formation from massless scalar isocurvature","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.CO","hep-th"],"primary_cat":"gr-qc","authors_text":"Chul-Moon Yoo, Hirotada Okawa, Misao Sasaki, Shin'ichi Hirano, Tomohiro Harada","submitted_at":"2021-12-23T03:12:24Z","abstract_excerpt":"We numerically study the primordial black hole (PBH) formation by an isocurvature perturbation of a massless scalar field on super Hubble scales in the radiation-dominated universe. As a first step we perform simulations of spherically symmetric configurations. For the initial condition, we employ the spatial gradient expansion and provide the general form of the growing mode solutions valid up through the second order in this expansion. The initial scalar field profile is assumed to be Gaussian with a characteristic comoving wavenumber $k$; $\\sim\\exp(-k^2R^2)$, where $R$ is the radial coordin"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2112.12335","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/2112.12335/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":"2112.12335","created_at":"2026-07-05T04:33:28.128093+00:00"},{"alias_kind":"arxiv_version","alias_value":"2112.12335v3","created_at":"2026-07-05T04:33:28.128093+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2112.12335","created_at":"2026-07-05T04:33:28.128093+00:00"},{"alias_kind":"pith_short_12","alias_value":"KHOMBGSBPEJK","created_at":"2026-07-05T04:33:28.128093+00:00"},{"alias_kind":"pith_short_16","alias_value":"KHOMBGSBPEJKX4AS","created_at":"2026-07-05T04:33:28.128093+00:00"},{"alias_kind":"pith_short_8","alias_value":"KHOMBGSB","created_at":"2026-07-05T04:33:28.128093+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.08738","citing_title":"The statistics of curvature-profile dispersion in primordial black hole formation","ref_index":16,"is_internal_anchor":true},{"citing_arxiv_id":"2606.26532","citing_title":"Primordial black hole formation in bulk-viscous cosmology","ref_index":12,"is_internal_anchor":false},{"citing_arxiv_id":"2512.22531","citing_title":"Cosmological long-wavelength solutions in non-adiabatic multi-fluid systems","ref_index":49,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/KHOMBGSBPEJKX4AS4BH4F5FSXD","json":"https://pith.science/pith/KHOMBGSBPEJKX4AS4BH4F5FSXD.json","graph_json":"https://pith.science/api/pith-number/KHOMBGSBPEJKX4AS4BH4F5FSXD/graph.json","events_json":"https://pith.science/api/pith-number/KHOMBGSBPEJKX4AS4BH4F5FSXD/events.json","paper":"https://pith.science/paper/KHOMBGSB"},"agent_actions":{"view_html":"https://pith.science/pith/KHOMBGSBPEJKX4AS4BH4F5FSXD","download_json":"https://pith.science/pith/KHOMBGSBPEJKX4AS4BH4F5FSXD.json","view_paper":"https://pith.science/paper/KHOMBGSB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2112.12335&json=true","fetch_graph":"https://pith.science/api/pith-number/KHOMBGSBPEJKX4AS4BH4F5FSXD/graph.json","fetch_events":"https://pith.science/api/pith-number/KHOMBGSBPEJKX4AS4BH4F5FSXD/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/KHOMBGSBPEJKX4AS4BH4F5FSXD/action/timestamp_anchor","attest_storage":"https://pith.science/pith/KHOMBGSBPEJKX4AS4BH4F5FSXD/action/storage_attestation","attest_author":"https://pith.science/pith/KHOMBGSBPEJKX4AS4BH4F5FSXD/action/author_attestation","sign_citation":"https://pith.science/pith/KHOMBGSBPEJKX4AS4BH4F5FSXD/action/citation_signature","submit_replication":"https://pith.science/pith/KHOMBGSBPEJKX4AS4BH4F5FSXD/action/replication_record"}},"created_at":"2026-07-05T04:33:28.128093+00:00","updated_at":"2026-07-05T04:33:28.128093+00:00"}