{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:UXL7FNGIQM7BWWEOKAGZSPMUIZ","short_pith_number":"pith:UXL7FNGI","schema_version":"1.0","canonical_sha256":"a5d7f2b4c8833e1b588e500d993d9446698e940c2e6232461e78ec95794491aa","source":{"kind":"arxiv","id":"2507.02423","version":1},"attestation_state":"computed","paper":{"title":"MeV cosmic-ray electrons modify the TeV pair-beam plasma instability","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["physics.plasm-ph"],"primary_cat":"astro-ph.HE","authors_text":"Christopher M. Hirata, Heyang Long, Mahmoud Alawashra, Martin Pohl, Yuanyuan Yang","submitted_at":"2025-07-03T08:31:50Z","abstract_excerpt":"Relativistic pair beams created in the intergalactic medium (IGM) by TeV gamma rays from blazars are expected to produce a detectable GeV-scale electromagnetic cascade, but the cascade component is absent in the spectra of many hard-spectrum TeV-emitting blazars. One common explanation is that weak intergalactic magnetic fields deflect the electron-positron pairs away from our line of sight. An alternative possibility is that electrostatic beam-plasma instabilities drain the energy of these pairs before a cascade can develop. Recent studies have shown that beam scattering by oblique electrosta"},"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":"2507.02423","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2025-07-03T08:31:50Z","cross_cats_sorted":["physics.plasm-ph"],"title_canon_sha256":"ac9ac40270e092a91869752c4c6539aeec32020d768d37c2f6c80dc4c51b8ff6","abstract_canon_sha256":"e7f0cbdfcc242fb3011a6248befc94e87a4312aa52ede7a4141e3a89d0bed1a7"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T12:07:09.250207Z","signature_b64":"ZK6ok55bNkfdt84jYvMXq1BD3SJocpQRl9raPSJQ1h6UoAoJfEyMMhrk2DxP4bBLcpvpU6b6IaoBjuUbAKvpDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"a5d7f2b4c8833e1b588e500d993d9446698e940c2e6232461e78ec95794491aa","last_reissued_at":"2026-07-05T12:07:09.249751Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T12:07:09.249751Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"MeV cosmic-ray electrons modify the TeV pair-beam plasma instability","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["physics.plasm-ph"],"primary_cat":"astro-ph.HE","authors_text":"Christopher M. Hirata, Heyang Long, Mahmoud Alawashra, Martin Pohl, Yuanyuan Yang","submitted_at":"2025-07-03T08:31:50Z","abstract_excerpt":"Relativistic pair beams created in the intergalactic medium (IGM) by TeV gamma rays from blazars are expected to produce a detectable GeV-scale electromagnetic cascade, but the cascade component is absent in the spectra of many hard-spectrum TeV-emitting blazars. One common explanation is that weak intergalactic magnetic fields deflect the electron-positron pairs away from our line of sight. An alternative possibility is that electrostatic beam-plasma instabilities drain the energy of these pairs before a cascade can develop. Recent studies have shown that beam scattering by oblique electrosta"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2507.02423","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/2507.02423/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":"2507.02423","created_at":"2026-07-05T12:07:09.249806+00:00"},{"alias_kind":"arxiv_version","alias_value":"2507.02423v1","created_at":"2026-07-05T12:07:09.249806+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2507.02423","created_at":"2026-07-05T12:07:09.249806+00:00"},{"alias_kind":"pith_short_12","alias_value":"UXL7FNGIQM7B","created_at":"2026-07-05T12:07:09.249806+00:00"},{"alias_kind":"pith_short_16","alias_value":"UXL7FNGIQM7BWWEO","created_at":"2026-07-05T12:07:09.249806+00:00"},{"alias_kind":"pith_short_8","alias_value":"UXL7FNGI","created_at":"2026-07-05T12:07:09.249806+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2510.08025","citing_title":"On the contribution of galaxies to the magnetic field in cosmic voids","ref_index":22,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/UXL7FNGIQM7BWWEOKAGZSPMUIZ","json":"https://pith.science/pith/UXL7FNGIQM7BWWEOKAGZSPMUIZ.json","graph_json":"https://pith.science/api/pith-number/UXL7FNGIQM7BWWEOKAGZSPMUIZ/graph.json","events_json":"https://pith.science/api/pith-number/UXL7FNGIQM7BWWEOKAGZSPMUIZ/events.json","paper":"https://pith.science/paper/UXL7FNGI"},"agent_actions":{"view_html":"https://pith.science/pith/UXL7FNGIQM7BWWEOKAGZSPMUIZ","download_json":"https://pith.science/pith/UXL7FNGIQM7BWWEOKAGZSPMUIZ.json","view_paper":"https://pith.science/paper/UXL7FNGI","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2507.02423&json=true","fetch_graph":"https://pith.science/api/pith-number/UXL7FNGIQM7BWWEOKAGZSPMUIZ/graph.json","fetch_events":"https://pith.science/api/pith-number/UXL7FNGIQM7BWWEOKAGZSPMUIZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/UXL7FNGIQM7BWWEOKAGZSPMUIZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/UXL7FNGIQM7BWWEOKAGZSPMUIZ/action/storage_attestation","attest_author":"https://pith.science/pith/UXL7FNGIQM7BWWEOKAGZSPMUIZ/action/author_attestation","sign_citation":"https://pith.science/pith/UXL7FNGIQM7BWWEOKAGZSPMUIZ/action/citation_signature","submit_replication":"https://pith.science/pith/UXL7FNGIQM7BWWEOKAGZSPMUIZ/action/replication_record"}},"created_at":"2026-07-05T12:07:09.249806+00:00","updated_at":"2026-07-05T12:07:09.249806+00:00"}