{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1997:4ZHZ4WKA3HF6D7GL3WZBZQJYSY","short_pith_number":"pith:4ZHZ4WKA","schema_version":"1.0","canonical_sha256":"e64f9e5940d9cbe1fccbddb21cc1389629575b30e24e69372d00493a3cdbd54f","source":{"kind":"arxiv","id":"hep-ph/9708303","version":1},"attestation_state":"computed","paper":{"title":"Primordial magnetic fields, anomalous isocurvature fluctuations and Big Bang nucleosynthesis","license":"","headline":"","cross_cats":["astro-ph"],"primary_cat":"hep-ph","authors_text":"Cambridge), M. E. Shaposhnikov (CERN), M. Giovannini (DAMTP","submitted_at":"1997-08-11T16:11:37Z","abstract_excerpt":"We show that the presence of primordial stochastic (hypercharge) magnetic fields before the electroweak (EW) phase transition induces isocurvature fluctuations (baryon number inhomogeneities). Depending on the details of the magnetic field spectrum and on the particle physics parameters (such as the strength of the EW phase transition and electron Yukawa couplings) these fluctuations may survive until the Big Bang nucleosynthesis (BBN). Their lenghtscale may exceed the neutron diffusion length at that time, while their magnitude can be so large that sizable antimatter domains are present. This"},"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":"hep-ph/9708303","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"hep-ph","submitted_at":"1997-08-11T16:11:37Z","cross_cats_sorted":["astro-ph"],"title_canon_sha256":"5ec86ceb7fd3e7746195df669783032eee42d447d394197a278b790c60e9a30a","abstract_canon_sha256":"089d001993ca2f4259f5f3bdbad14f631c5d3fabdd6390fa1bc58a1f6a645da1"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:17:48.296232Z","signature_b64":"ecP046sHzfifjZkd0bdewWtxSVM6rjXO1d5Zw9sqMmwFbRDC5QI52eAdjaiFFEwlTRsMYExC/TMu+14ApLYxBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"e64f9e5940d9cbe1fccbddb21cc1389629575b30e24e69372d00493a3cdbd54f","last_reissued_at":"2026-07-04T17:17:48.295759Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:17:48.295759Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Primordial magnetic fields, anomalous isocurvature fluctuations and Big Bang nucleosynthesis","license":"","headline":"","cross_cats":["astro-ph"],"primary_cat":"hep-ph","authors_text":"Cambridge), M. E. Shaposhnikov (CERN), M. Giovannini (DAMTP","submitted_at":"1997-08-11T16:11:37Z","abstract_excerpt":"We show that the presence of primordial stochastic (hypercharge) magnetic fields before the electroweak (EW) phase transition induces isocurvature fluctuations (baryon number inhomogeneities). Depending on the details of the magnetic field spectrum and on the particle physics parameters (such as the strength of the EW phase transition and electron Yukawa couplings) these fluctuations may survive until the Big Bang nucleosynthesis (BBN). Their lenghtscale may exceed the neutron diffusion length at that time, while their magnitude can be so large that sizable antimatter domains are present. This"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"hep-ph/9708303","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/hep-ph/9708303/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":"hep-ph/9708303","created_at":"2026-07-04T17:17:48.295868+00:00"},{"alias_kind":"arxiv_version","alias_value":"hep-ph/9708303v1","created_at":"2026-07-04T17:17:48.295868+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.hep-ph/9708303","created_at":"2026-07-04T17:17:48.295868+00:00"},{"alias_kind":"pith_short_12","alias_value":"4ZHZ4WKA3HF6","created_at":"2026-07-04T17:17:48.295868+00:00"},{"alias_kind":"pith_short_16","alias_value":"4ZHZ4WKA3HF6D7GL","created_at":"2026-07-04T17:17:48.295868+00:00"},{"alias_kind":"pith_short_8","alias_value":"4ZHZ4WKA","created_at":"2026-07-04T17:17:48.295868+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2509.23858","citing_title":"Revisiting constraints on magnetogenesis from baryon asymmetry","ref_index":37,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/4ZHZ4WKA3HF6D7GL3WZBZQJYSY","json":"https://pith.science/pith/4ZHZ4WKA3HF6D7GL3WZBZQJYSY.json","graph_json":"https://pith.science/api/pith-number/4ZHZ4WKA3HF6D7GL3WZBZQJYSY/graph.json","events_json":"https://pith.science/api/pith-number/4ZHZ4WKA3HF6D7GL3WZBZQJYSY/events.json","paper":"https://pith.science/paper/4ZHZ4WKA"},"agent_actions":{"view_html":"https://pith.science/pith/4ZHZ4WKA3HF6D7GL3WZBZQJYSY","download_json":"https://pith.science/pith/4ZHZ4WKA3HF6D7GL3WZBZQJYSY.json","view_paper":"https://pith.science/paper/4ZHZ4WKA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=hep-ph/9708303&json=true","fetch_graph":"https://pith.science/api/pith-number/4ZHZ4WKA3HF6D7GL3WZBZQJYSY/graph.json","fetch_events":"https://pith.science/api/pith-number/4ZHZ4WKA3HF6D7GL3WZBZQJYSY/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/4ZHZ4WKA3HF6D7GL3WZBZQJYSY/action/timestamp_anchor","attest_storage":"https://pith.science/pith/4ZHZ4WKA3HF6D7GL3WZBZQJYSY/action/storage_attestation","attest_author":"https://pith.science/pith/4ZHZ4WKA3HF6D7GL3WZBZQJYSY/action/author_attestation","sign_citation":"https://pith.science/pith/4ZHZ4WKA3HF6D7GL3WZBZQJYSY/action/citation_signature","submit_replication":"https://pith.science/pith/4ZHZ4WKA3HF6D7GL3WZBZQJYSY/action/replication_record"}},"created_at":"2026-07-04T17:17:48.295868+00:00","updated_at":"2026-07-04T17:17:48.295868+00:00"}