{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2006:YHIMAUHCBL766X57EUPPJXIC6S","short_pith_number":"pith:YHIMAUHC","schema_version":"1.0","canonical_sha256":"c1d0c050e20affef5fbf251ef4dd02f4adeb01a03c765f685357b6f0ce3e649c","source":{"kind":"arxiv","id":"astro-ph/0603211","version":1},"attestation_state":"computed","paper":{"title":"Simulations of relativistic collisionless shocks: shock structure and particle acceleration","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Anatoly Spitkovsky (KIPAC, Stanford University)","submitted_at":"2006-03-09T00:14:34Z","abstract_excerpt":"We discuss 3D simulations of relativistic collisionless shocks in electron-positron pair plasmas using the particle-in-cell (PIC) method. The shock structure is mainly controlled by the shock's magnetization (\"sigma\" parameter). We demonstrate how the structure of the shock varies as a function of sigma for perpendicular shocks. At low magnetizations the shock is mediated mainly by the Weibel instability which generates transient magnetic fields that can exceed the initial field. At larger magnetizations the shock is dominated by magnetic reflections. We demonstrate where the transition occurs"},"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/0603211","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2006-03-09T00:14:34Z","cross_cats_sorted":[],"title_canon_sha256":"2c51384f25fff46e4e83067a02228c427c35b6777fe01c48ea8a2195d5b8b6fc","abstract_canon_sha256":"7891243ca14f9d7347bceb6ea046ea5294e7cf5abb6e9ce3fe334d1f08ed618c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:58:22.998336Z","signature_b64":"yvs8XCJB8xmaTa+/U0TtjrNndx8msoVkh+iEjBicDEmy0Xl9XuM+KH3RldNYTsZXS8WkhRwOmdFJGJQ0xpIOBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c1d0c050e20affef5fbf251ef4dd02f4adeb01a03c765f685357b6f0ce3e649c","last_reissued_at":"2026-07-04T16:58:22.997976Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:58:22.997976Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Simulations of relativistic collisionless shocks: shock structure and particle acceleration","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Anatoly Spitkovsky (KIPAC, Stanford University)","submitted_at":"2006-03-09T00:14:34Z","abstract_excerpt":"We discuss 3D simulations of relativistic collisionless shocks in electron-positron pair plasmas using the particle-in-cell (PIC) method. The shock structure is mainly controlled by the shock's magnetization (\"sigma\" parameter). We demonstrate how the structure of the shock varies as a function of sigma for perpendicular shocks. At low magnetizations the shock is mediated mainly by the Weibel instability which generates transient magnetic fields that can exceed the initial field. At larger magnetizations the shock is dominated by magnetic reflections. We demonstrate where the transition occurs"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0603211","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/0603211/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/0603211","created_at":"2026-07-04T16:58:22.998034+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0603211v1","created_at":"2026-07-04T16:58:22.998034+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0603211","created_at":"2026-07-04T16:58:22.998034+00:00"},{"alias_kind":"pith_short_12","alias_value":"YHIMAUHCBL76","created_at":"2026-07-04T16:58:22.998034+00:00"},{"alias_kind":"pith_short_16","alias_value":"YHIMAUHCBL766X57","created_at":"2026-07-04T16:58:22.998034+00:00"},{"alias_kind":"pith_short_8","alias_value":"YHIMAUHC","created_at":"2026-07-04T16:58:22.998034+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.12111","citing_title":"SN 1006: A Cosmic Laboratory for Investigating Shock Acceleration Physics","ref_index":274,"is_internal_anchor":true},{"citing_arxiv_id":"2605.03033","citing_title":"On The Nonthermal Power Laws In Magnetized Turbulent Plasmas","ref_index":259,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/YHIMAUHCBL766X57EUPPJXIC6S","json":"https://pith.science/pith/YHIMAUHCBL766X57EUPPJXIC6S.json","graph_json":"https://pith.science/api/pith-number/YHIMAUHCBL766X57EUPPJXIC6S/graph.json","events_json":"https://pith.science/api/pith-number/YHIMAUHCBL766X57EUPPJXIC6S/events.json","paper":"https://pith.science/paper/YHIMAUHC"},"agent_actions":{"view_html":"https://pith.science/pith/YHIMAUHCBL766X57EUPPJXIC6S","download_json":"https://pith.science/pith/YHIMAUHCBL766X57EUPPJXIC6S.json","view_paper":"https://pith.science/paper/YHIMAUHC","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0603211&json=true","fetch_graph":"https://pith.science/api/pith-number/YHIMAUHCBL766X57EUPPJXIC6S/graph.json","fetch_events":"https://pith.science/api/pith-number/YHIMAUHCBL766X57EUPPJXIC6S/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/YHIMAUHCBL766X57EUPPJXIC6S/action/timestamp_anchor","attest_storage":"https://pith.science/pith/YHIMAUHCBL766X57EUPPJXIC6S/action/storage_attestation","attest_author":"https://pith.science/pith/YHIMAUHCBL766X57EUPPJXIC6S/action/author_attestation","sign_citation":"https://pith.science/pith/YHIMAUHCBL766X57EUPPJXIC6S/action/citation_signature","submit_replication":"https://pith.science/pith/YHIMAUHCBL766X57EUPPJXIC6S/action/replication_record"}},"created_at":"2026-07-04T16:58:22.998034+00:00","updated_at":"2026-07-04T16:58:22.998034+00:00"}