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As the two binaries are definite proper motion members of omega Centauri, we estimated their physical parameters, obtaining M_1=1.13\\pm0.03M_\\odot, R_1=0.98\\pm0.01R_\\odot and M_2=0.33\\pm0.01M_\\odot, R_2=0.92\\pm0.01R_\\odot for V211; M_1=1.30\\pm0.05M_\\odot, R_1=1.03\\pm0.01R_\\odot and M_2=0.58\\pm0.02M_\\odot, R_2=0.78\\pm0.01R_\\odot for NV358. On the color-magnitude diagram of omega C"},"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":"1303.0602","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/3.0/","primary_cat":"astro-ph.SR","submitted_at":"2013-03-04T04:58:24Z","cross_cats_sorted":[],"title_canon_sha256":"989482541c50c8408d6c54d7979cb6005ed8c5ac8dd02ec6d1844334140638f5","abstract_canon_sha256":"55238dcd6ec4405a479ed9c67fad341ac27b2b2d9ed5c204b206502ed7b40f41"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:51:17.587398Z","signature_b64":"+BhH5bhykr/1rmj7nxrFJH97gEdGvxPkR3TIWCTJhew6GrEIdz+BE6N64YZXfYTrAbeJtIlm5aZoRjsL9qyuCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b3922b7cedec90fb9782b314d3e40a3ba17339705238b27a06cbdcb7af1bdeae","last_reissued_at":"2026-05-18T01:51:17.586908Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:51:17.586908Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Two particular EA-type binaries in the globular cluster omega Centauri","license":"http://creativecommons.org/licenses/by/3.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Kai Li, Shengbang Qian","submitted_at":"2013-03-04T04:58:24Z","abstract_excerpt":"We analyzed the B and V light curves of two EA-type binaries V211 and NV358 using the WD code for the first time. Our analysis shows that V211 is a typical Algol-type binary and NV358 is a well detached binary system. As the two binaries are definite proper motion members of omega Centauri, we estimated their physical parameters, obtaining M_1=1.13\\pm0.03M_\\odot, R_1=0.98\\pm0.01R_\\odot and M_2=0.33\\pm0.01M_\\odot, R_2=0.92\\pm0.01R_\\odot for V211; M_1=1.30\\pm0.05M_\\odot, R_1=1.03\\pm0.01R_\\odot and M_2=0.58\\pm0.02M_\\odot, R_2=0.78\\pm0.01R_\\odot for NV358. 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