{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2000:TPEOWQU2OLMMBC57ZXGHFUKUY2","short_pith_number":"pith:TPEOWQU2","schema_version":"1.0","canonical_sha256":"9bc8eb429a72d8c08bbfcdcc72d154c684ae0aaac6888b57164fa3f9a5bd02de","source":{"kind":"arxiv","id":"astro-ph/0005438","version":2},"attestation_state":"computed","paper":{"title":"Spherically Symmetric Simulation with Boltzmann Neutrino Transport of Core Collapse and Post-Bounce Evolution of a 15 Solar Mass Star","license":"","headline":"","cross_cats":["hep-ph"],"primary_cat":"astro-ph","authors_text":"Garching, Germany), H.-Th. Janka (MPA, M. Rampp","submitted_at":"2000-05-22T18:52:27Z","abstract_excerpt":"We present a spherically symmetric, Newtonian core-collapse simulation of a 15 solar mass star with a 1.28 solar mass iron core. The time-, energy-, and angle-dependent transport of electron neutrinos and antineutrinos was treated with a new code which iteratively solves the Boltzmann equation and the equations for neutrino number, energy and momentum to order O(v/c) in the velocity v of the stellar medium. The supernova shock expands to a maximum radius of 350 km instead of only about 240 km as in a comparable calculation with multi-group flux-limited diffusion (MGFLD) by Bruenn, Mezzacappa, "},"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":"astro-ph/0005438","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2000-05-22T18:52:27Z","cross_cats_sorted":["hep-ph"],"title_canon_sha256":"5076e8aede643ef2682e28c79fee163a8084b749d97a03f967d0a490aaf7a2f3","abstract_canon_sha256":"fccb5ab718564eb48e3b4aacc149eca1c8dab5bd1aa12f4ad50edaad42be2579"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:16:42.250855Z","signature_b64":"QQj5uV/QEseZVseeDlEpPCwBb80ApmWt3+nINEMPmtptG57Q8lvOR30pPSJA1O1IW7mctu1Iz2/5BAQEtY/VAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"9bc8eb429a72d8c08bbfcdcc72d154c684ae0aaac6888b57164fa3f9a5bd02de","last_reissued_at":"2026-07-04T16:16:42.250322Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:16:42.250322Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Spherically Symmetric Simulation with Boltzmann Neutrino Transport of Core Collapse and Post-Bounce Evolution of a 15 Solar Mass Star","license":"","headline":"","cross_cats":["hep-ph"],"primary_cat":"astro-ph","authors_text":"Garching, Germany), H.-Th. Janka (MPA, M. Rampp","submitted_at":"2000-05-22T18:52:27Z","abstract_excerpt":"We present a spherically symmetric, Newtonian core-collapse simulation of a 15 solar mass star with a 1.28 solar mass iron core. The time-, energy-, and angle-dependent transport of electron neutrinos and antineutrinos was treated with a new code which iteratively solves the Boltzmann equation and the equations for neutrino number, energy and momentum to order O(v/c) in the velocity v of the stellar medium. The supernova shock expands to a maximum radius of 350 km instead of only about 240 km as in a comparable calculation with multi-group flux-limited diffusion (MGFLD) by Bruenn, Mezzacappa, "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0005438","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/astro-ph/0005438/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":"astro-ph/0005438","created_at":"2026-07-04T16:16:42.250402+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0005438v2","created_at":"2026-07-04T16:16:42.250402+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0005438","created_at":"2026-07-04T16:16:42.250402+00:00"},{"alias_kind":"pith_short_12","alias_value":"TPEOWQU2OLMM","created_at":"2026-07-04T16:16:42.250402+00:00"},{"alias_kind":"pith_short_16","alias_value":"TPEOWQU2OLMMBC57","created_at":"2026-07-04T16:16:42.250402+00:00"},{"alias_kind":"pith_short_8","alias_value":"TPEOWQU2","created_at":"2026-07-04T16:16:42.250402+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.30756","citing_title":"Parameterizing the Standing Accretion Shock Instability for Inference with Galactic Supernova Neutrino Signals at IceCube","ref_index":73,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/TPEOWQU2OLMMBC57ZXGHFUKUY2","json":"https://pith.science/pith/TPEOWQU2OLMMBC57ZXGHFUKUY2.json","graph_json":"https://pith.science/api/pith-number/TPEOWQU2OLMMBC57ZXGHFUKUY2/graph.json","events_json":"https://pith.science/api/pith-number/TPEOWQU2OLMMBC57ZXGHFUKUY2/events.json","paper":"https://pith.science/paper/TPEOWQU2"},"agent_actions":{"view_html":"https://pith.science/pith/TPEOWQU2OLMMBC57ZXGHFUKUY2","download_json":"https://pith.science/pith/TPEOWQU2OLMMBC57ZXGHFUKUY2.json","view_paper":"https://pith.science/paper/TPEOWQU2","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0005438&json=true","fetch_graph":"https://pith.science/api/pith-number/TPEOWQU2OLMMBC57ZXGHFUKUY2/graph.json","fetch_events":"https://pith.science/api/pith-number/TPEOWQU2OLMMBC57ZXGHFUKUY2/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/TPEOWQU2OLMMBC57ZXGHFUKUY2/action/timestamp_anchor","attest_storage":"https://pith.science/pith/TPEOWQU2OLMMBC57ZXGHFUKUY2/action/storage_attestation","attest_author":"https://pith.science/pith/TPEOWQU2OLMMBC57ZXGHFUKUY2/action/author_attestation","sign_citation":"https://pith.science/pith/TPEOWQU2OLMMBC57ZXGHFUKUY2/action/citation_signature","submit_replication":"https://pith.science/pith/TPEOWQU2OLMMBC57ZXGHFUKUY2/action/replication_record"}},"created_at":"2026-07-04T16:16:42.250402+00:00","updated_at":"2026-07-04T16:16:42.250402+00:00"}