{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:MRDFH3TBDWFXAJT4FSJJZ3FIEU","short_pith_number":"pith:MRDFH3TB","schema_version":"1.0","canonical_sha256":"644653ee611d8b70267c2c929ceca82504d8ca4553baab02c3737077750cee5d","source":{"kind":"arxiv","id":"0903.2944","version":1},"attestation_state":"computed","paper":{"title":"Radio emission and nonlinear diffusive shock acceleration of cosmic rays in the supernova SN 1993J","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Vincent Tatischeff","submitted_at":"2009-03-17T11:29:37Z","abstract_excerpt":"The extensive observations of the supernova SN 1993J at radio wavelengths make this object a unique target for the study of particle acceleration in a supernova shock. To describe the radio synchrotron emission we use a model that couples a semianalytic description of nonlinear diffusive shock acceleration with self-similar solutions for the hydrodynamics of the supernova expansion. The synchrotron emission, which is assumed to be produced by relativistic electrons propagating in the postshock plasma, is worked out from radiative transfer calculations that include the process of synchrotron se"},"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":"0903.2944","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2009-03-17T11:29:37Z","cross_cats_sorted":[],"title_canon_sha256":"5357fd3344b7c362c0fd9ebce7a7c8168ec550fac50d38c6ce9362a11c7a8f9d","abstract_canon_sha256":"dd508845027781f6acb70ba5ada14f754e98a0a646a041518f9738c7f308cca8"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:14:27.813332Z","signature_b64":"63GzKDJ5Vf95I6+49JxNdo3YJdRekuyFFaB1UQplJrkCTSpEGGVdfMogzH5f+5NzlBitKJkM/flxSH9tALEwBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"644653ee611d8b70267c2c929ceca82504d8ca4553baab02c3737077750cee5d","last_reissued_at":"2026-05-18T02:14:27.812784Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:14:27.812784Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Radio emission and nonlinear diffusive shock acceleration of cosmic rays in the supernova SN 1993J","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Vincent Tatischeff","submitted_at":"2009-03-17T11:29:37Z","abstract_excerpt":"The extensive observations of the supernova SN 1993J at radio wavelengths make this object a unique target for the study of particle acceleration in a supernova shock. To describe the radio synchrotron emission we use a model that couples a semianalytic description of nonlinear diffusive shock acceleration with self-similar solutions for the hydrodynamics of the supernova expansion. The synchrotron emission, which is assumed to be produced by relativistic electrons propagating in the postshock plasma, is worked out from radiative transfer calculations that include the process of synchrotron se"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0903.2944","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":"0903.2944","created_at":"2026-05-18T02:14:27.812875+00:00"},{"alias_kind":"arxiv_version","alias_value":"0903.2944v1","created_at":"2026-05-18T02:14:27.812875+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0903.2944","created_at":"2026-05-18T02:14:27.812875+00:00"},{"alias_kind":"pith_short_12","alias_value":"MRDFH3TBDWFX","created_at":"2026-05-18T12:26:00.592388+00:00"},{"alias_kind":"pith_short_16","alias_value":"MRDFH3TBDWFXAJT4","created_at":"2026-05-18T12:26:00.592388+00:00"},{"alias_kind":"pith_short_8","alias_value":"MRDFH3TB","created_at":"2026-05-18T12:26:00.592388+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"1908.02171","citing_title":"Numerical Simulations of Cosmic-Ray Acceleration at Core-Collapse Supernovae","ref_index":1,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MRDFH3TBDWFXAJT4FSJJZ3FIEU","json":"https://pith.science/pith/MRDFH3TBDWFXAJT4FSJJZ3FIEU.json","graph_json":"https://pith.science/api/pith-number/MRDFH3TBDWFXAJT4FSJJZ3FIEU/graph.json","events_json":"https://pith.science/api/pith-number/MRDFH3TBDWFXAJT4FSJJZ3FIEU/events.json","paper":"https://pith.science/paper/MRDFH3TB"},"agent_actions":{"view_html":"https://pith.science/pith/MRDFH3TBDWFXAJT4FSJJZ3FIEU","download_json":"https://pith.science/pith/MRDFH3TBDWFXAJT4FSJJZ3FIEU.json","view_paper":"https://pith.science/paper/MRDFH3TB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0903.2944&json=true","fetch_graph":"https://pith.science/api/pith-number/MRDFH3TBDWFXAJT4FSJJZ3FIEU/graph.json","fetch_events":"https://pith.science/api/pith-number/MRDFH3TBDWFXAJT4FSJJZ3FIEU/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MRDFH3TBDWFXAJT4FSJJZ3FIEU/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MRDFH3TBDWFXAJT4FSJJZ3FIEU/action/storage_attestation","attest_author":"https://pith.science/pith/MRDFH3TBDWFXAJT4FSJJZ3FIEU/action/author_attestation","sign_citation":"https://pith.science/pith/MRDFH3TBDWFXAJT4FSJJZ3FIEU/action/citation_signature","submit_replication":"https://pith.science/pith/MRDFH3TBDWFXAJT4FSJJZ3FIEU/action/replication_record"}},"created_at":"2026-05-18T02:14:27.812875+00:00","updated_at":"2026-05-18T02:14:27.812875+00:00"}