{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2002:ORXBJPDDWP5BRDOJW636RYXSIR","short_pith_number":"pith:ORXBJPDD","schema_version":"1.0","canonical_sha256":"746e14bc63b3fa188dc9b7b7e8e2f2446310d2593769f7d820298e769215eed1","source":{"kind":"arxiv","id":"astro-ph/0210634","version":1},"attestation_state":"computed","paper":{"title":"Stability of Standing Accretion Shocks, With an Eye Toward Core Collapse Supernovae","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Anthony Mezzacappa, Christine DeMarino, John M. Blondin","submitted_at":"2002-10-29T18:33:40Z","abstract_excerpt":"We examine the stability of standing, spherical accretion shocks. Accretion shocks arise in core collapse supernovae (the focus of this paper), star formation, and accreting white dwarfs and neutron stars. We present a simple analytic model and use time-dependent hydrodynamics simulations to show that this solution is stable to radial perturbations. In two dimensions we show that small perturbations to a spherical shock front can lead to rapid growth of turbulence behind the shock, driven by the injection of vorticity from the now non-spherical shock. We discuss the ramifications this instabil"},"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/0210634","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2002-10-29T18:33:40Z","cross_cats_sorted":[],"title_canon_sha256":"3fe19613451d405c9229a6ef6c9e287361ea8ccb30225cb8793a20c45c67deaf","abstract_canon_sha256":"1a90ec813d16d0f305d1254a4c70ac3a430db8b128daa0b2cc741a9fe5f90dc0"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:31:03.501709Z","signature_b64":"nrzGlOsOxT6LaMj0loOq0+uS7DIrcW6guiRbLlYr6BP8eGzZnYGaGzVwPMofyJIrsgtO/QzXRfXFs1v0np7rDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"746e14bc63b3fa188dc9b7b7e8e2f2446310d2593769f7d820298e769215eed1","last_reissued_at":"2026-07-04T16:31:03.501358Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:31:03.501358Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Stability of Standing Accretion Shocks, With an Eye Toward Core Collapse Supernovae","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Anthony Mezzacappa, Christine DeMarino, John M. Blondin","submitted_at":"2002-10-29T18:33:40Z","abstract_excerpt":"We examine the stability of standing, spherical accretion shocks. Accretion shocks arise in core collapse supernovae (the focus of this paper), star formation, and accreting white dwarfs and neutron stars. We present a simple analytic model and use time-dependent hydrodynamics simulations to show that this solution is stable to radial perturbations. In two dimensions we show that small perturbations to a spherical shock front can lead to rapid growth of turbulence behind the shock, driven by the injection of vorticity from the now non-spherical shock. We discuss the ramifications this instabil"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0210634","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/astro-ph/0210634/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/0210634","created_at":"2026-07-04T16:31:03.501416+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0210634v1","created_at":"2026-07-04T16:31:03.501416+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0210634","created_at":"2026-07-04T16:31:03.501416+00:00"},{"alias_kind":"pith_short_12","alias_value":"ORXBJPDDWP5B","created_at":"2026-07-04T16:31:03.501416+00:00"},{"alias_kind":"pith_short_16","alias_value":"ORXBJPDDWP5BRDOJ","created_at":"2026-07-04T16:31:03.501416+00:00"},{"alias_kind":"pith_short_8","alias_value":"ORXBJPDD","created_at":"2026-07-04T16:31:03.501416+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":3,"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":45,"is_internal_anchor":true},{"citing_arxiv_id":"2605.28944","citing_title":"Impact of the equation of state on core collapse supernovae I: the low-$T/|W|$ instability","ref_index":59,"is_internal_anchor":true},{"citing_arxiv_id":"2605.18972","citing_title":"Flavor Conversion Enhances or Suppresses Supernova Explodability Independent of the Progenitor Mass","ref_index":16,"is_internal_anchor":true},{"citing_arxiv_id":"2605.04896","citing_title":"Parameter Estimation Horizon of Core-Collapse Supernovae with Current and Next-Generation Gravitational-Wave Detectors","ref_index":39,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ORXBJPDDWP5BRDOJW636RYXSIR","json":"https://pith.science/pith/ORXBJPDDWP5BRDOJW636RYXSIR.json","graph_json":"https://pith.science/api/pith-number/ORXBJPDDWP5BRDOJW636RYXSIR/graph.json","events_json":"https://pith.science/api/pith-number/ORXBJPDDWP5BRDOJW636RYXSIR/events.json","paper":"https://pith.science/paper/ORXBJPDD"},"agent_actions":{"view_html":"https://pith.science/pith/ORXBJPDDWP5BRDOJW636RYXSIR","download_json":"https://pith.science/pith/ORXBJPDDWP5BRDOJW636RYXSIR.json","view_paper":"https://pith.science/paper/ORXBJPDD","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0210634&json=true","fetch_graph":"https://pith.science/api/pith-number/ORXBJPDDWP5BRDOJW636RYXSIR/graph.json","fetch_events":"https://pith.science/api/pith-number/ORXBJPDDWP5BRDOJW636RYXSIR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ORXBJPDDWP5BRDOJW636RYXSIR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ORXBJPDDWP5BRDOJW636RYXSIR/action/storage_attestation","attest_author":"https://pith.science/pith/ORXBJPDDWP5BRDOJW636RYXSIR/action/author_attestation","sign_citation":"https://pith.science/pith/ORXBJPDDWP5BRDOJW636RYXSIR/action/citation_signature","submit_replication":"https://pith.science/pith/ORXBJPDDWP5BRDOJW636RYXSIR/action/replication_record"}},"created_at":"2026-07-04T16:31:03.501416+00:00","updated_at":"2026-07-04T16:31:03.501416+00:00"}