{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:V3ECWOL2SPTXIEX5PWGVFEPZ7J","short_pith_number":"pith:V3ECWOL2","schema_version":"1.0","canonical_sha256":"aec82b397a93e77412fd7d8d5291f9fa7b5a5dbfa3ae5cdf04943339c6bf6cd9","source":{"kind":"arxiv","id":"1901.03260","version":2},"attestation_state":"computed","paper":{"title":"Coherence constraints on physical parameters at bright radio sources and FRB emission mechanism","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["physics.plasm-ph"],"primary_cat":"astro-ph.HE","authors_text":"Maxim Lyutikov (Purdue University), Mohammad Rafat (The University of Sydney)","submitted_at":"2019-01-10T16:42:26Z","abstract_excerpt":"We discuss physical constrains that observations of high brightness temperature coherent radio emission, with brightness temperatures as high as $T_b \\sim 10^{35}$ K, impose on the plasma parameters at relativistically moving astrophysical sources. High brightness temperatures imply a minimal plasma energy density at the source. Additional important constraints come from the fact that resonantly emitting particles lose most of their energy to non-resonant inverse Compton and synchrotron processes.\n  We also interpret recent observations of high-to-low frequency drifting features in the spectra"},"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":"1901.03260","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2019-01-10T16:42:26Z","cross_cats_sorted":["physics.plasm-ph"],"title_canon_sha256":"cb910b75231bdbd4e6e52dcb6aa9d831194826bbf994c998bd534dfd72dfe00b","abstract_canon_sha256":"cfadbe04cf7251ddcc93a848a1b9ad653621535b26d4a990b1a77937ba8da2dd"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:44:24.599982Z","signature_b64":"mTz8GQfABk5fMhAWWYVojR1pgBLXztTH6ibEMVKx6beBX/Vg8jnNybbjwYmAxuZEDNg0bViIcN7DOEXS0eYxAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"aec82b397a93e77412fd7d8d5291f9fa7b5a5dbfa3ae5cdf04943339c6bf6cd9","last_reissued_at":"2026-07-05T00:44:24.599520Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:44:24.599520Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Coherence constraints on physical parameters at bright radio sources and FRB emission mechanism","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["physics.plasm-ph"],"primary_cat":"astro-ph.HE","authors_text":"Maxim Lyutikov (Purdue University), Mohammad Rafat (The University of Sydney)","submitted_at":"2019-01-10T16:42:26Z","abstract_excerpt":"We discuss physical constrains that observations of high brightness temperature coherent radio emission, with brightness temperatures as high as $T_b \\sim 10^{35}$ K, impose on the plasma parameters at relativistically moving astrophysical sources. High brightness temperatures imply a minimal plasma energy density at the source. Additional important constraints come from the fact that resonantly emitting particles lose most of their energy to non-resonant inverse Compton and synchrotron processes.\n  We also interpret recent observations of high-to-low frequency drifting features in the spectra"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1901.03260","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/1901.03260/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":"1901.03260","created_at":"2026-07-05T00:44:24.599578+00:00"},{"alias_kind":"arxiv_version","alias_value":"1901.03260v2","created_at":"2026-07-05T00:44:24.599578+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1901.03260","created_at":"2026-07-05T00:44:24.599578+00:00"},{"alias_kind":"pith_short_12","alias_value":"V3ECWOL2SPTX","created_at":"2026-07-05T00:44:24.599578+00:00"},{"alias_kind":"pith_short_16","alias_value":"V3ECWOL2SPTXIEX5","created_at":"2026-07-05T00:44:24.599578+00:00"},{"alias_kind":"pith_short_8","alias_value":"V3ECWOL2","created_at":"2026-07-05T00:44:24.599578+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"1907.01542","citing_title":"A fast radio burst localised to a massive galaxy","ref_index":26,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/V3ECWOL2SPTXIEX5PWGVFEPZ7J","json":"https://pith.science/pith/V3ECWOL2SPTXIEX5PWGVFEPZ7J.json","graph_json":"https://pith.science/api/pith-number/V3ECWOL2SPTXIEX5PWGVFEPZ7J/graph.json","events_json":"https://pith.science/api/pith-number/V3ECWOL2SPTXIEX5PWGVFEPZ7J/events.json","paper":"https://pith.science/paper/V3ECWOL2"},"agent_actions":{"view_html":"https://pith.science/pith/V3ECWOL2SPTXIEX5PWGVFEPZ7J","download_json":"https://pith.science/pith/V3ECWOL2SPTXIEX5PWGVFEPZ7J.json","view_paper":"https://pith.science/paper/V3ECWOL2","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1901.03260&json=true","fetch_graph":"https://pith.science/api/pith-number/V3ECWOL2SPTXIEX5PWGVFEPZ7J/graph.json","fetch_events":"https://pith.science/api/pith-number/V3ECWOL2SPTXIEX5PWGVFEPZ7J/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/V3ECWOL2SPTXIEX5PWGVFEPZ7J/action/timestamp_anchor","attest_storage":"https://pith.science/pith/V3ECWOL2SPTXIEX5PWGVFEPZ7J/action/storage_attestation","attest_author":"https://pith.science/pith/V3ECWOL2SPTXIEX5PWGVFEPZ7J/action/author_attestation","sign_citation":"https://pith.science/pith/V3ECWOL2SPTXIEX5PWGVFEPZ7J/action/citation_signature","submit_replication":"https://pith.science/pith/V3ECWOL2SPTXIEX5PWGVFEPZ7J/action/replication_record"}},"created_at":"2026-07-05T00:44:24.599578+00:00","updated_at":"2026-07-05T00:44:24.599578+00:00"}