{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:V42MK5DVOOEXOLT3D7OFXUZJRV","short_pith_number":"pith:V42MK5DV","schema_version":"1.0","canonical_sha256":"af34c574757389772e7b1fdc5bd3298d4c9da1add4e04ccbe652f65a099a3c7a","source":{"kind":"arxiv","id":"2211.17065","version":4},"attestation_state":"computed","paper":{"title":"Microlensing effects of wormholes associated to blackhole spacetimes","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Ke Gao, Lei-Hua Liu, Mian Zhu","submitted_at":"2022-11-30T15:17:31Z","abstract_excerpt":"In this paper, we investigate the microlensing effects of wormholes associated to black hole spacetimes. Specifically, we work on three typical wormholes (WH): Schwarzschild WH, Kerr WH, and RN WH, as well as their blackhole correspondences. We evaluate the deflection angle upon the second order under weak field approximation using Gauss-Bonnet theorem. Then, we study their magnification with numerics.We find that a Kerr WH could lead to multi peaks in the magnification with certain parameters in the prograde case, while a Kerr BH predicts one peak. Therefore, the multi-peak feature of can be "},"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":"2211.17065","kind":"arxiv","version":4},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"gr-qc","submitted_at":"2022-11-30T15:17:31Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"81735794b5f1a3a955731b95578affbe7db7425d3220709b5c9874884b7eb517","abstract_canon_sha256":"5360b882190388452c2bf7d3b02aa5b96fb31b143009905dc871751b54723a07"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:18:51.775939Z","signature_b64":"6Oc1MKBroIhp9H02yjMXgxBkaca9+IiHSvwKY0uAZBl4xTuyUKY7My820AiHMza/HcLY6Synm3glZs7uMruSBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"af34c574757389772e7b1fdc5bd3298d4c9da1add4e04ccbe652f65a099a3c7a","last_reissued_at":"2026-07-05T06:18:51.775450Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:18:51.775450Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Microlensing effects of wormholes associated to blackhole spacetimes","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Ke Gao, Lei-Hua Liu, Mian Zhu","submitted_at":"2022-11-30T15:17:31Z","abstract_excerpt":"In this paper, we investigate the microlensing effects of wormholes associated to black hole spacetimes. Specifically, we work on three typical wormholes (WH): Schwarzschild WH, Kerr WH, and RN WH, as well as their blackhole correspondences. We evaluate the deflection angle upon the second order under weak field approximation using Gauss-Bonnet theorem. Then, we study their magnification with numerics.We find that a Kerr WH could lead to multi peaks in the magnification with certain parameters in the prograde case, while a Kerr BH predicts one peak. Therefore, the multi-peak feature of can be "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2211.17065","kind":"arxiv","version":4},"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/2211.17065/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":"2211.17065","created_at":"2026-07-05T06:18:51.775514+00:00"},{"alias_kind":"arxiv_version","alias_value":"2211.17065v4","created_at":"2026-07-05T06:18:51.775514+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2211.17065","created_at":"2026-07-05T06:18:51.775514+00:00"},{"alias_kind":"pith_short_12","alias_value":"V42MK5DVOOEX","created_at":"2026-07-05T06:18:51.775514+00:00"},{"alias_kind":"pith_short_16","alias_value":"V42MK5DVOOEXOLT3","created_at":"2026-07-05T06:18:51.775514+00:00"},{"alias_kind":"pith_short_8","alias_value":"V42MK5DV","created_at":"2026-07-05T06:18:51.775514+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.22181","citing_title":"Shadow dependent phenomenology framework for rotating black hole metric","ref_index":33,"is_internal_anchor":false},{"citing_arxiv_id":"2604.22181","citing_title":"Shadow dependent phenomenology framework for rotating black hole metric","ref_index":33,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/V42MK5DVOOEXOLT3D7OFXUZJRV","json":"https://pith.science/pith/V42MK5DVOOEXOLT3D7OFXUZJRV.json","graph_json":"https://pith.science/api/pith-number/V42MK5DVOOEXOLT3D7OFXUZJRV/graph.json","events_json":"https://pith.science/api/pith-number/V42MK5DVOOEXOLT3D7OFXUZJRV/events.json","paper":"https://pith.science/paper/V42MK5DV"},"agent_actions":{"view_html":"https://pith.science/pith/V42MK5DVOOEXOLT3D7OFXUZJRV","download_json":"https://pith.science/pith/V42MK5DVOOEXOLT3D7OFXUZJRV.json","view_paper":"https://pith.science/paper/V42MK5DV","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2211.17065&json=true","fetch_graph":"https://pith.science/api/pith-number/V42MK5DVOOEXOLT3D7OFXUZJRV/graph.json","fetch_events":"https://pith.science/api/pith-number/V42MK5DVOOEXOLT3D7OFXUZJRV/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/V42MK5DVOOEXOLT3D7OFXUZJRV/action/timestamp_anchor","attest_storage":"https://pith.science/pith/V42MK5DVOOEXOLT3D7OFXUZJRV/action/storage_attestation","attest_author":"https://pith.science/pith/V42MK5DVOOEXOLT3D7OFXUZJRV/action/author_attestation","sign_citation":"https://pith.science/pith/V42MK5DVOOEXOLT3D7OFXUZJRV/action/citation_signature","submit_replication":"https://pith.science/pith/V42MK5DVOOEXOLT3D7OFXUZJRV/action/replication_record"}},"created_at":"2026-07-05T06:18:51.775514+00:00","updated_at":"2026-07-05T06:18:51.775514+00:00"}