{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:JWX4MXOZ6DXNLOOUGKAAPNBJFT","short_pith_number":"pith:JWX4MXOZ","schema_version":"1.0","canonical_sha256":"4dafc65dd9f0eed5b9d4328007b4292ce8db4d73ccc8630302cba184db96d905","source":{"kind":"arxiv","id":"1207.7215","version":1},"attestation_state":"computed","paper":{"title":"Instabilities in the Ionization Zones Around the First Stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"A. O. Razoumov, E. I. Vorobyov, E. O. Vasiliev, Yu. A. Shchekinov","submitted_at":"2012-07-31T12:06:41Z","abstract_excerpt":"We consider the evolution of the ionization zone around Population III stars with $M_*\\sim 25-200 M_\\odot$ in protogalaxies with $M\\sim 10^7 M_\\odot$ at redshifts $z = 12$, assuming that the dark matter profile is a modified isothermal sphere. We study the conditions for the growth of instabilities in the ionization zones. The Rayleigh-Taylor and thermal instabilities develop efficiently in the ionization zones around 25-40 $M_\\odot$ stars, while this efficiency is lower for stars with $\\sim 120 M_\\odot$. For more massive stars ($\\sim 200 M_\\odot$), the flux of ionizing photons is strong enoug"},"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":"1207.7215","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2012-07-31T12:06:41Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"8980cafe886771f9ce98ab3456ebb384211f9c376dbf1464c7bfe466aaea762c","abstract_canon_sha256":"73ef7a705ff8bf78a4e5b7602ee5d97b4a5a69d0fd0d6bca5e7c7ca945245f49"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T03:49:46.488450Z","signature_b64":"T3YTpud7Oy4wEJ+Aqexhzv3IL3NjvXZO2KPbpnrpwJHstQFZzHs/2Vk8LPF/dq7+odBkkEtzXkn70ROEoCf/DA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"4dafc65dd9f0eed5b9d4328007b4292ce8db4d73ccc8630302cba184db96d905","last_reissued_at":"2026-05-18T03:49:46.487777Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T03:49:46.487777Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Instabilities in the Ionization Zones Around the First Stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"A. O. Razoumov, E. I. Vorobyov, E. O. Vasiliev, Yu. A. Shchekinov","submitted_at":"2012-07-31T12:06:41Z","abstract_excerpt":"We consider the evolution of the ionization zone around Population III stars with $M_*\\sim 25-200 M_\\odot$ in protogalaxies with $M\\sim 10^7 M_\\odot$ at redshifts $z = 12$, assuming that the dark matter profile is a modified isothermal sphere. We study the conditions for the growth of instabilities in the ionization zones. The Rayleigh-Taylor and thermal instabilities develop efficiently in the ionization zones around 25-40 $M_\\odot$ stars, while this efficiency is lower for stars with $\\sim 120 M_\\odot$. For more massive stars ($\\sim 200 M_\\odot$), the flux of ionizing photons is strong enoug"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1207.7215","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":"1207.7215","created_at":"2026-05-18T03:49:46.487896+00:00"},{"alias_kind":"arxiv_version","alias_value":"1207.7215v1","created_at":"2026-05-18T03:49:46.487896+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1207.7215","created_at":"2026-05-18T03:49:46.487896+00:00"},{"alias_kind":"pith_short_12","alias_value":"JWX4MXOZ6DXN","created_at":"2026-05-18T12:27:11.947152+00:00"},{"alias_kind":"pith_short_16","alias_value":"JWX4MXOZ6DXNLOOU","created_at":"2026-05-18T12:27:11.947152+00:00"},{"alias_kind":"pith_short_8","alias_value":"JWX4MXOZ","created_at":"2026-05-18T12:27:11.947152+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/JWX4MXOZ6DXNLOOUGKAAPNBJFT","json":"https://pith.science/pith/JWX4MXOZ6DXNLOOUGKAAPNBJFT.json","graph_json":"https://pith.science/api/pith-number/JWX4MXOZ6DXNLOOUGKAAPNBJFT/graph.json","events_json":"https://pith.science/api/pith-number/JWX4MXOZ6DXNLOOUGKAAPNBJFT/events.json","paper":"https://pith.science/paper/JWX4MXOZ"},"agent_actions":{"view_html":"https://pith.science/pith/JWX4MXOZ6DXNLOOUGKAAPNBJFT","download_json":"https://pith.science/pith/JWX4MXOZ6DXNLOOUGKAAPNBJFT.json","view_paper":"https://pith.science/paper/JWX4MXOZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1207.7215&json=true","fetch_graph":"https://pith.science/api/pith-number/JWX4MXOZ6DXNLOOUGKAAPNBJFT/graph.json","fetch_events":"https://pith.science/api/pith-number/JWX4MXOZ6DXNLOOUGKAAPNBJFT/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/JWX4MXOZ6DXNLOOUGKAAPNBJFT/action/timestamp_anchor","attest_storage":"https://pith.science/pith/JWX4MXOZ6DXNLOOUGKAAPNBJFT/action/storage_attestation","attest_author":"https://pith.science/pith/JWX4MXOZ6DXNLOOUGKAAPNBJFT/action/author_attestation","sign_citation":"https://pith.science/pith/JWX4MXOZ6DXNLOOUGKAAPNBJFT/action/citation_signature","submit_replication":"https://pith.science/pith/JWX4MXOZ6DXNLOOUGKAAPNBJFT/action/replication_record"}},"created_at":"2026-05-18T03:49:46.487896+00:00","updated_at":"2026-05-18T03:49:46.487896+00:00"}