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In the Petersen diagram these stars form three well separated sequences. The additional variability cannot correspond to other radial mode. This form of pulsation is still puzzling.\n  We find that amplitude of the additional variability is small, typically 2-4 per cent of the first overtone amplitude, which corresponds to "},"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":"1603.01042","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2016-03-03T10:12:36Z","cross_cats_sorted":[],"title_canon_sha256":"3f89caf0322d54c6867b1e08d2cbf117f1d6ec2cbeb116078328e213349e0490","abstract_canon_sha256":"9640856f7d91d86774a34de109e087447e99419fab269cccd27d2e760b2185c8"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:17:50.053736Z","signature_b64":"el/BAMYn/atF77le0w8yledVah7pSaRhks+dwBO+Vh6LLOcI+awKW4SDmwvbcWKQhKoUL7Mwtnj37zTU7hIfBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"240680b5a2b43b9ff7bcdd4fd434a93b9d8f9b9fabbb0554e83f28b59e254c0c","last_reissued_at":"2026-05-18T01:17:50.053068Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:17:50.053068Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Non-radial pulsation in first overtone Cepheids of the Small Magellanic Cloud","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"M. 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