{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2008:XIHOMUKKAB64UAZGSZBLRECTKC","short_pith_number":"pith:XIHOMUKK","schema_version":"1.0","canonical_sha256":"ba0ee6514a007dca03269642b890535099c2e9f423370c539543efb8d6d1f755","source":{"kind":"arxiv","id":"0807.0659","version":2},"attestation_state":"computed","paper":{"title":"Role of dense matter in collective supernova neutrino transformations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ph"],"primary_cat":"astro-ph","authors_text":"A. Esteban-Pretel, A. Mirizzi, G.G. Raffelt, G. Sigl, P.D. Serpico, R. Tomas, S. Pastor","submitted_at":"2008-07-07T14:22:48Z","abstract_excerpt":"For neutrinos streaming from a supernova (SN) core, dense matter suppresses self-induced flavor transformations if the electron density n_e significantly exceeds the neutrino density n_nu in the conversion region. If n_e is comparable to n_nu one finds multi-angle decoherence, whereas the standard self-induced transformation behavior requires that in the transformation region n_nu is safely above n_e. This condition need not be satisfied in the early phase after supernova core bounce. Our new multi-angle effect is a subtle consequence of neutrinos traveling on different trajectories when strea"},"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":"0807.0659","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph","submitted_at":"2008-07-07T14:22:48Z","cross_cats_sorted":["hep-ph"],"title_canon_sha256":"9721124ffb04f91ae5ea5dbcb86aab76826ad65e542037e178568afa9a8c91ba","abstract_canon_sha256":"267c94a14f6f7a466b3e78a54e9c7047cc67319f3c38f93d8899ba57f1fa6baa"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:30:20.803582Z","signature_b64":"PQtyvWI7gJLIjOoNnlmegqO9ZAgSuwoguO4XIPRxtIRSPkJP3FdwT48taA+aM6X/sZdkkpIigvaZvuw0bzASBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ba0ee6514a007dca03269642b890535099c2e9f423370c539543efb8d6d1f755","last_reissued_at":"2026-07-04T15:30:20.803180Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:30:20.803180Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Role of dense matter in collective supernova neutrino transformations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ph"],"primary_cat":"astro-ph","authors_text":"A. Esteban-Pretel, A. Mirizzi, G.G. Raffelt, G. Sigl, P.D. Serpico, R. Tomas, S. Pastor","submitted_at":"2008-07-07T14:22:48Z","abstract_excerpt":"For neutrinos streaming from a supernova (SN) core, dense matter suppresses self-induced flavor transformations if the electron density n_e significantly exceeds the neutrino density n_nu in the conversion region. If n_e is comparable to n_nu one finds multi-angle decoherence, whereas the standard self-induced transformation behavior requires that in the transformation region n_nu is safely above n_e. This condition need not be satisfied in the early phase after supernova core bounce. Our new multi-angle effect is a subtle consequence of neutrinos traveling on different trajectories when strea"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0807.0659","kind":"arxiv","version":2},"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/0807.0659/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":"0807.0659","created_at":"2026-07-04T15:30:20.803236+00:00"},{"alias_kind":"arxiv_version","alias_value":"0807.0659v2","created_at":"2026-07-04T15:30:20.803236+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0807.0659","created_at":"2026-07-04T15:30:20.803236+00:00"},{"alias_kind":"pith_short_12","alias_value":"XIHOMUKKAB64","created_at":"2026-07-04T15:30:20.803236+00:00"},{"alias_kind":"pith_short_16","alias_value":"XIHOMUKKAB64UAZG","created_at":"2026-07-04T15:30:20.803236+00:00"},{"alias_kind":"pith_short_8","alias_value":"XIHOMUKK","created_at":"2026-07-04T15:30:20.803236+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"1908.10594","citing_title":"Neutrino halo effect on collective neutrino oscillation in iron core-collapse supernova model of a 9.6 $M_{\\odot}$ star","ref_index":21,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/XIHOMUKKAB64UAZGSZBLRECTKC","json":"https://pith.science/pith/XIHOMUKKAB64UAZGSZBLRECTKC.json","graph_json":"https://pith.science/api/pith-number/XIHOMUKKAB64UAZGSZBLRECTKC/graph.json","events_json":"https://pith.science/api/pith-number/XIHOMUKKAB64UAZGSZBLRECTKC/events.json","paper":"https://pith.science/paper/XIHOMUKK"},"agent_actions":{"view_html":"https://pith.science/pith/XIHOMUKKAB64UAZGSZBLRECTKC","download_json":"https://pith.science/pith/XIHOMUKKAB64UAZGSZBLRECTKC.json","view_paper":"https://pith.science/paper/XIHOMUKK","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0807.0659&json=true","fetch_graph":"https://pith.science/api/pith-number/XIHOMUKKAB64UAZGSZBLRECTKC/graph.json","fetch_events":"https://pith.science/api/pith-number/XIHOMUKKAB64UAZGSZBLRECTKC/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XIHOMUKKAB64UAZGSZBLRECTKC/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XIHOMUKKAB64UAZGSZBLRECTKC/action/storage_attestation","attest_author":"https://pith.science/pith/XIHOMUKKAB64UAZGSZBLRECTKC/action/author_attestation","sign_citation":"https://pith.science/pith/XIHOMUKKAB64UAZGSZBLRECTKC/action/citation_signature","submit_replication":"https://pith.science/pith/XIHOMUKKAB64UAZGSZBLRECTKC/action/replication_record"}},"created_at":"2026-07-04T15:30:20.803236+00:00","updated_at":"2026-07-04T15:30:20.803236+00:00"}