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Ceres is an ice-rich body with signs of cryovolcanic activity.\n  Aims. The aim of this paper is to determine the obliquity variations of Ceres and Vesta and to study their rotational stability.\n  Methods. The orbital and rotational motions have been integrated by symplectic integration. The rotational stability has b"},"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":"1808.10384","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.EP","submitted_at":"2018-08-30T16:26:52Z","cross_cats_sorted":[],"title_canon_sha256":"efe46e1810fd33035b9d24ea6b9bbb429118850b7ec843342391462136b889b2","abstract_canon_sha256":"97d60a47b4b93e88543e00047ef567f063cb8e7ea93f4bf55694123efe418454"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:51:14.292483Z","signature_b64":"QnRxFdx2ouaRP82XXSXA4iwZy5rsalpd7oeGrtWEBWpsVCkcMAl3QqNBJncqK79B57GtlAss4ey2C4gEoRbDCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ef08eefc60201b47513ab211a04c9b35760e49463d0a036db56469c2a967ea36","last_reissued_at":"2026-05-17T23:51:14.291992Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:51:14.291992Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Long-term orbital and rotational motions of Ceres and Vesta","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"J. Laskar, M. Gastineau, N. Rambaux, T. Vaillant","submitted_at":"2018-08-30T16:26:52Z","abstract_excerpt":"Context. The dwarf planet Ceres and the asteroid Vesta have been studied by the Dawn space mission. They are the two heaviest bodies of the main asteroid belt and have different characteristics. Notably, Vesta appears to be dry and inactive with two large basins at its south pole. Ceres is an ice-rich body with signs of cryovolcanic activity.\n  Aims. The aim of this paper is to determine the obliquity variations of Ceres and Vesta and to study their rotational stability.\n  Methods. The orbital and rotational motions have been integrated by symplectic integration. 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