{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:UJYWGXLH2SHGZY7VKTDIJ2JW7T","short_pith_number":"pith:UJYWGXLH","schema_version":"1.0","canonical_sha256":"a271635d67d48e6ce3f554c684e936fce5879592858817e105850707e682ab7f","source":{"kind":"arxiv","id":"2012.03043","version":2},"attestation_state":"computed","paper":{"title":"Radiative turbulent flares in magnetically-dominated plasmas","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["physics.plasm-ph"],"primary_cat":"astro-ph.HE","authors_text":"A. M. Beloborodov, J. N\\\"attil\\\"a","submitted_at":"2020-12-05T14:52:15Z","abstract_excerpt":"We perform 2D and 3D kinetic simulations of reconnection-mediated turbulent flares in a magnetized electron-positron plasma, with weak and strong radiative cooling. Such flares can be generated around neutron stars and accreting black holes. We focus on the magnetically-dominated regime where tension of the background magnetic field lines exceeds the plasma rest mass by a factor $\\sigma_0 > 1$. In the simulations, turbulence is excited on a macroscopic scale $l_0$, and we observe that it develops by forming thin, dynamic current sheets on various scales. The deposited macroscopic energy dissip"},"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":"2012.03043","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2020-12-05T14:52:15Z","cross_cats_sorted":["physics.plasm-ph"],"title_canon_sha256":"5557f4ed97b430b73d534608fde205be4356cca58daf4f26d6841428a217c4e2","abstract_canon_sha256":"e09697d48760cdd9c716976e951432ea56fca6f890784763ecefb4d830c65546"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T03:31:55.457064Z","signature_b64":"D1dHMKMgwFh6hFxZpZvQGUQbKcxtYxuvK2Vc79x50PT/FbItJNa2p/a4O+NeOCC4z7i150VQsYGoGB3KHJk9DA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"a271635d67d48e6ce3f554c684e936fce5879592858817e105850707e682ab7f","last_reissued_at":"2026-07-05T03:31:55.456497Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T03:31:55.456497Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Radiative turbulent flares in magnetically-dominated plasmas","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["physics.plasm-ph"],"primary_cat":"astro-ph.HE","authors_text":"A. M. Beloborodov, J. N\\\"attil\\\"a","submitted_at":"2020-12-05T14:52:15Z","abstract_excerpt":"We perform 2D and 3D kinetic simulations of reconnection-mediated turbulent flares in a magnetized electron-positron plasma, with weak and strong radiative cooling. Such flares can be generated around neutron stars and accreting black holes. We focus on the magnetically-dominated regime where tension of the background magnetic field lines exceeds the plasma rest mass by a factor $\\sigma_0 > 1$. In the simulations, turbulence is excited on a macroscopic scale $l_0$, and we observe that it develops by forming thin, dynamic current sheets on various scales. The deposited macroscopic energy dissip"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2012.03043","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/2012.03043/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":"2012.03043","created_at":"2026-07-05T03:31:55.456577+00:00"},{"alias_kind":"arxiv_version","alias_value":"2012.03043v2","created_at":"2026-07-05T03:31:55.456577+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2012.03043","created_at":"2026-07-05T03:31:55.456577+00:00"},{"alias_kind":"pith_short_12","alias_value":"UJYWGXLH2SHG","created_at":"2026-07-05T03:31:55.456577+00:00"},{"alias_kind":"pith_short_16","alias_value":"UJYWGXLH2SHGZY7V","created_at":"2026-07-05T03:31:55.456577+00:00"},{"alias_kind":"pith_short_8","alias_value":"UJYWGXLH","created_at":"2026-07-05T03:31:55.456577+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2506.04212","citing_title":"Studying the mirror acceleration via kinetic simulations of relativistic plasma turbulence","ref_index":27,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/UJYWGXLH2SHGZY7VKTDIJ2JW7T","json":"https://pith.science/pith/UJYWGXLH2SHGZY7VKTDIJ2JW7T.json","graph_json":"https://pith.science/api/pith-number/UJYWGXLH2SHGZY7VKTDIJ2JW7T/graph.json","events_json":"https://pith.science/api/pith-number/UJYWGXLH2SHGZY7VKTDIJ2JW7T/events.json","paper":"https://pith.science/paper/UJYWGXLH"},"agent_actions":{"view_html":"https://pith.science/pith/UJYWGXLH2SHGZY7VKTDIJ2JW7T","download_json":"https://pith.science/pith/UJYWGXLH2SHGZY7VKTDIJ2JW7T.json","view_paper":"https://pith.science/paper/UJYWGXLH","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2012.03043&json=true","fetch_graph":"https://pith.science/api/pith-number/UJYWGXLH2SHGZY7VKTDIJ2JW7T/graph.json","fetch_events":"https://pith.science/api/pith-number/UJYWGXLH2SHGZY7VKTDIJ2JW7T/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/UJYWGXLH2SHGZY7VKTDIJ2JW7T/action/timestamp_anchor","attest_storage":"https://pith.science/pith/UJYWGXLH2SHGZY7VKTDIJ2JW7T/action/storage_attestation","attest_author":"https://pith.science/pith/UJYWGXLH2SHGZY7VKTDIJ2JW7T/action/author_attestation","sign_citation":"https://pith.science/pith/UJYWGXLH2SHGZY7VKTDIJ2JW7T/action/citation_signature","submit_replication":"https://pith.science/pith/UJYWGXLH2SHGZY7VKTDIJ2JW7T/action/replication_record"}},"created_at":"2026-07-05T03:31:55.456577+00:00","updated_at":"2026-07-05T03:31:55.456577+00:00"}