{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:XWFGYAUKHQ3UKVAORNLUWL2UN7","short_pith_number":"pith:XWFGYAUK","schema_version":"1.0","canonical_sha256":"bd8a6c028a3c3745540e8b574b2f546fdb1d677e9d2f343671f5e20f4261cc6f","source":{"kind":"arxiv","id":"1711.03804","version":1},"attestation_state":"computed","paper":{"title":"Evolution of hydromagnetic turbulence from the electroweak phase transition","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.CO","authors_text":"Alberto Roper Pol, Alexander G. Tevzadze, Axel Brandenburg, Sayan Mandal, Tanmay Vachaspati, Tina Kahniashvili","submitted_at":"2017-11-10T13:16:10Z","abstract_excerpt":"We present new simulations of decaying hydromagnetic turbulence for a relativistic equation of state relevant to the early universe. We compare helical and nonhelical cases either with kinetically or magnetically dominated initial fields. Both kinetic and magnetic initial helicities lead to maximally helical magnetic fields after some time, but with different temporal decay laws. Both are relevant to the early universe, although no mechanisms have yet been identified that produce magnetic helicity with strengths comparable to the big bang nucleosynthesis limit at scales comparable to the Hubbl"},"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":"1711.03804","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2017-11-10T13:16:10Z","cross_cats_sorted":["astro-ph.EP"],"title_canon_sha256":"9bde0ae2200348b8c5998a64c74d680823c9650680e58c1bf6c4fec64d571517","abstract_canon_sha256":"067d83c28e3c87abcd8164c963e6b7fa8667dbef9738cc0d36a12e235f6d68f2"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:27:09.080831Z","signature_b64":"0m8KGZtm/i/P9zBhh5nRdrTM7vXpZlRbjR2y1SN+97mTsSZxVBttACtL4YGR1kWZ+iC33sCuRq4mr5Z0H5UhCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"bd8a6c028a3c3745540e8b574b2f546fdb1d677e9d2f343671f5e20f4261cc6f","last_reissued_at":"2026-05-18T00:27:09.080242Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:27:09.080242Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Evolution of hydromagnetic turbulence from the electroweak phase transition","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.CO","authors_text":"Alberto Roper Pol, Alexander G. Tevzadze, Axel Brandenburg, Sayan Mandal, Tanmay Vachaspati, Tina Kahniashvili","submitted_at":"2017-11-10T13:16:10Z","abstract_excerpt":"We present new simulations of decaying hydromagnetic turbulence for a relativistic equation of state relevant to the early universe. We compare helical and nonhelical cases either with kinetically or magnetically dominated initial fields. Both kinetic and magnetic initial helicities lead to maximally helical magnetic fields after some time, but with different temporal decay laws. Both are relevant to the early universe, although no mechanisms have yet been identified that produce magnetic helicity with strengths comparable to the big bang nucleosynthesis limit at scales comparable to the Hubbl"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1711.03804","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":"1711.03804","created_at":"2026-05-18T00:27:09.080329+00:00"},{"alias_kind":"arxiv_version","alias_value":"1711.03804v1","created_at":"2026-05-18T00:27:09.080329+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1711.03804","created_at":"2026-05-18T00:27:09.080329+00:00"},{"alias_kind":"pith_short_12","alias_value":"XWFGYAUKHQ3U","created_at":"2026-05-18T12:31:56.362134+00:00"},{"alias_kind":"pith_short_16","alias_value":"XWFGYAUKHQ3UKVAO","created_at":"2026-05-18T12:31:56.362134+00:00"},{"alias_kind":"pith_short_8","alias_value":"XWFGYAUK","created_at":"2026-05-18T12:31:56.362134+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"2505.08011","citing_title":"Primordial black holes and magnetic fields in conformal neutrino mass models","ref_index":24,"is_internal_anchor":true},{"citing_arxiv_id":"2605.21092","citing_title":"Audible Axion Magnetogenesis: Linking Intergalactic Magnetic Fields and Gravitational Waves","ref_index":107,"is_internal_anchor":true},{"citing_arxiv_id":"2509.23858","citing_title":"Revisiting constraints on magnetogenesis from baryon asymmetry","ref_index":61,"is_internal_anchor":true},{"citing_arxiv_id":"2604.20768","citing_title":"Primordial Magnetogenesis and Gravitational Waves from ALP-assisted Phase Transition","ref_index":51,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/XWFGYAUKHQ3UKVAORNLUWL2UN7","json":"https://pith.science/pith/XWFGYAUKHQ3UKVAORNLUWL2UN7.json","graph_json":"https://pith.science/api/pith-number/XWFGYAUKHQ3UKVAORNLUWL2UN7/graph.json","events_json":"https://pith.science/api/pith-number/XWFGYAUKHQ3UKVAORNLUWL2UN7/events.json","paper":"https://pith.science/paper/XWFGYAUK"},"agent_actions":{"view_html":"https://pith.science/pith/XWFGYAUKHQ3UKVAORNLUWL2UN7","download_json":"https://pith.science/pith/XWFGYAUKHQ3UKVAORNLUWL2UN7.json","view_paper":"https://pith.science/paper/XWFGYAUK","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1711.03804&json=true","fetch_graph":"https://pith.science/api/pith-number/XWFGYAUKHQ3UKVAORNLUWL2UN7/graph.json","fetch_events":"https://pith.science/api/pith-number/XWFGYAUKHQ3UKVAORNLUWL2UN7/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XWFGYAUKHQ3UKVAORNLUWL2UN7/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XWFGYAUKHQ3UKVAORNLUWL2UN7/action/storage_attestation","attest_author":"https://pith.science/pith/XWFGYAUKHQ3UKVAORNLUWL2UN7/action/author_attestation","sign_citation":"https://pith.science/pith/XWFGYAUKHQ3UKVAORNLUWL2UN7/action/citation_signature","submit_replication":"https://pith.science/pith/XWFGYAUKHQ3UKVAORNLUWL2UN7/action/replication_record"}},"created_at":"2026-05-18T00:27:09.080329+00:00","updated_at":"2026-05-18T00:27:09.080329+00:00"}