{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2005:HM6THACMI2LPPTADKNQDIT6VVM","short_pith_number":"pith:HM6THACM","schema_version":"1.0","canonical_sha256":"3b3d33804c4696f7cc035360344fd5ab370ef1756d701b7629d24c57906c550a","source":{"kind":"arxiv","id":"astro-ph/0510701","version":1},"attestation_state":"computed","paper":{"title":"Non-thermal high-energy emission from colliding winds of massive stars","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"(2) Iowa State University), A. Reimer (1), M. Pohl (2), O. Reimer (1) ((1) Stanford University","submitted_at":"2005-10-25T00:10:30Z","abstract_excerpt":"Colliding winds of massive star binary systems are considered as potential sites of non-thermal high-energy photon production. This is motivated merely by the detection of synchrotron radio emission from the expected colliding wind location. Here we investigate the properties of high-energy photon production in colliding winds of long-period WR+OB-systems. We found that in the dominating leptonic radiation process anisotropy and Klein-Nishina effects may yield spectral and variability signatures in the gamma-ray domain at or above the sensitivity of current or upcoming gamma-ray telescopes. An"},"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/0510701","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2005-10-25T00:10:30Z","cross_cats_sorted":[],"title_canon_sha256":"14179fdce349fe6e4c3f97226c7c2f7fa4cbd842106930817b81e397de024151","abstract_canon_sha256":"40267e861a518f47c8b57149e4ef628bc730d51139d350e6ed29c6b7dc1c9fc1"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:15:21.294985Z","signature_b64":"FMadn6g0EOxTNiR0XjBtWGg5LBGwsxDEWd+pHNgE9p30HFNcs0FQMnxJRIQrz4dEt7QiKmRkDBu9UFBe4nhiDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"3b3d33804c4696f7cc035360344fd5ab370ef1756d701b7629d24c57906c550a","last_reissued_at":"2026-07-04T17:15:21.294573Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:15:21.294573Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Non-thermal high-energy emission from colliding winds of massive stars","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"(2) Iowa State University), A. Reimer (1), M. Pohl (2), O. Reimer (1) ((1) Stanford University","submitted_at":"2005-10-25T00:10:30Z","abstract_excerpt":"Colliding winds of massive star binary systems are considered as potential sites of non-thermal high-energy photon production. This is motivated merely by the detection of synchrotron radio emission from the expected colliding wind location. Here we investigate the properties of high-energy photon production in colliding winds of long-period WR+OB-systems. We found that in the dominating leptonic radiation process anisotropy and Klein-Nishina effects may yield spectral and variability signatures in the gamma-ray domain at or above the sensitivity of current or upcoming gamma-ray telescopes. An"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0510701","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/0510701/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/0510701","created_at":"2026-07-04T17:15:21.294637+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0510701v1","created_at":"2026-07-04T17:15:21.294637+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0510701","created_at":"2026-07-04T17:15:21.294637+00:00"},{"alias_kind":"pith_short_12","alias_value":"HM6THACMI2LP","created_at":"2026-07-04T17:15:21.294637+00:00"},{"alias_kind":"pith_short_16","alias_value":"HM6THACMI2LPPTAD","created_at":"2026-07-04T17:15:21.294637+00:00"},{"alias_kind":"pith_short_8","alias_value":"HM6THACM","created_at":"2026-07-04T17:15:21.294637+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2606.21288","citing_title":"A broadband view of the thermal and non-thermal emission from the embedded massive star cluster RCW 38","ref_index":5,"is_internal_anchor":true},{"citing_arxiv_id":"2605.17636","citing_title":"Diffuse gamma-ray emission in the vicinity of open cluster Berkeley 87","ref_index":52,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/HM6THACMI2LPPTADKNQDIT6VVM","json":"https://pith.science/pith/HM6THACMI2LPPTADKNQDIT6VVM.json","graph_json":"https://pith.science/api/pith-number/HM6THACMI2LPPTADKNQDIT6VVM/graph.json","events_json":"https://pith.science/api/pith-number/HM6THACMI2LPPTADKNQDIT6VVM/events.json","paper":"https://pith.science/paper/HM6THACM"},"agent_actions":{"view_html":"https://pith.science/pith/HM6THACMI2LPPTADKNQDIT6VVM","download_json":"https://pith.science/pith/HM6THACMI2LPPTADKNQDIT6VVM.json","view_paper":"https://pith.science/paper/HM6THACM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0510701&json=true","fetch_graph":"https://pith.science/api/pith-number/HM6THACMI2LPPTADKNQDIT6VVM/graph.json","fetch_events":"https://pith.science/api/pith-number/HM6THACMI2LPPTADKNQDIT6VVM/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/HM6THACMI2LPPTADKNQDIT6VVM/action/timestamp_anchor","attest_storage":"https://pith.science/pith/HM6THACMI2LPPTADKNQDIT6VVM/action/storage_attestation","attest_author":"https://pith.science/pith/HM6THACMI2LPPTADKNQDIT6VVM/action/author_attestation","sign_citation":"https://pith.science/pith/HM6THACMI2LPPTADKNQDIT6VVM/action/citation_signature","submit_replication":"https://pith.science/pith/HM6THACMI2LPPTADKNQDIT6VVM/action/replication_record"}},"created_at":"2026-07-04T17:15:21.294637+00:00","updated_at":"2026-07-04T17:15:21.294637+00:00"}