Spin orbit resonance cascade via core shell model. \Application to Mercury and Ganymede

Spin orbit resonance cascade via core shell model. \Application to Mercury and Ganymede | Research Square window.SnipcartSettings = { analytics: { enabled: false } }; (function() { var accessVector = localStorage.getItem('access_vector') || ''; window.dataLayer = window.dataLayer || []; if (accessVector) { window.dataLayer.push({ user: { profile: { profileInfo: { snid: accessVector } } } }); } })(); (function(w,d,s,l,i){w[l]=w[l]||[];w[l].push({'gtm.start':new Date().getTime(),event:'gtm.js'});var f=d.getElementsByTagName(s)[0],j=d.createElement(s),dl=l!='dataLayer'?'&l='+l:'';j.async=true;j.src='https://www.googletagmanager.com/gtm.js?id='+i+dl;f.parentNode.insertBefore(j,f);})(window,document,'script','dataLayer','GTM-K279D39R'); Browse Preprints In Review Journals COVID-19 Preprints AJE Video Bytes Research Tools Research Promotion AJE Professional Editing AJE Rubriq About Preprint Platform In Review Editorial Policies Our Team Advisory Board Help Center Sign In Submit a Preprint Cite Share Download PDF Research Article Spin orbit resonance cascade via core shell model. \Application to Mercury and Ganymede Gabriella Pinzari, Benedetto Scoppola, Matteo Veglianti This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-3953160/v1 This work is licensed under a CC BY 4.0 License Status: Published Journal Publication published 10 Sep, 2024 Read the published version in Celestial Mechanics and Dynamical Astronomy → Version 1 posted 11 You are reading this latest preprint version Abstract We discuss a model describing the spin orbit resonance cascade. We assume that the primary has a two-layer (core-shell) structure: it is composed by a thin solid crust and an inner and heavier solid core that are interacting due to the presence of a fluid interface. We assume two sources of dissipation: a viscous one, depending on the relative angular velocity between core and crust and a tidal one, smaller than the first, due to the viscoelastic structure of the core. We show how these two sources of dissipation are needful for the capture in spin-orbit resonance. The crust and the core fall in resonance with different time scales if the viscous coupling between them is big enough. Finally, the tidal dissipation of the viscoelastic core, decreasing the eccentricity, brings the system out of the resonance in a third very long time scale. This mechanism of entry and exit from resonance ends in the 1 : 1 stable state. tidal dissipation spin orbit resonance core shell model Full Text Additional Declarations No competing interests reported. Cite Share Download PDF Status: Published Journal Publication published 10 Sep, 2024 Read the published version in Celestial Mechanics and Dynamical Astronomy → Version 1 posted Editorial decision: Revision requested 20 Apr, 2024 Reviews received at journal 19 Apr, 2024 Reviewers agreed at journal 02 Apr, 2024 Reviews received at journal 27 Mar, 2024 Reviews received at journal 15 Mar, 2024 Reviewers agreed at journal 03 Mar, 2024 Reviewers agreed at journal 15 Feb, 2024 Reviewers invited by journal 14 Feb, 2024 Editor assigned by journal 13 Feb, 2024 Submission checks completed at journal 13 Feb, 2024 First submitted to journal 13 Feb, 2024 You are reading this latest preprint version Research Square lets you share your work early, gain feedback from the community, and start making changes to your manuscript prior to peer review in a journal. As a division of Research Square Company, we’re committed to making research communication faster, fairer, and more useful. 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Also discoverable on Platform About Our Team In Review Editorial Policies Advisory Board Help Center Resources Author Services Accessibility API Access RSS feed Manage Cookie Preferences © Research Square 2026 | ISSN 2693-5015 (online) Privacy Policy Terms of Service Do Not Sell My Personal Information {"props":{"pageProps":{"initialData":{"identity":"rs-3953160","acceptedTermsAndConditions":true,"allowDirectSubmit":false,"archivedVersions":[],"articleType":"Research Article","associatedPublications":[],"authors":[{"id":272817766,"identity":"495f9e6b-0b00-434b-a544-ad8ed10ebe79","order_by":0,"name":"Gabriella Pinzari","email":"","orcid":"","institution":"University of Padua","correspondingAuthor":false,"prefix":"","firstName":"Gabriella","middleName":"","lastName":"Pinzari","suffix":""},{"id":272817767,"identity":"82b8a338-46f3-41e8-bd28-7fd93d8ab7ad","order_by":1,"name":"Benedetto Scoppola","email":"","orcid":"","institution":"University of Rome Tor Vergata","correspondingAuthor":false,"prefix":"","firstName":"Benedetto","middleName":"","lastName":"Scoppola","suffix":""},{"id":272817768,"identity":"a0694004-f7c5-4f29-a771-35d107149828","order_by":2,"name":"Matteo Veglianti","email":"data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAZAAAAAyAQMAAABI0h/eAAAABlBMVEX///8AAABVwtN+AAAACXBIWXMAAA7EAAAOxAGVKw4bAAABD0lEQVRIiWNgGAWjYHACxgMJQJKNvQHCZQOTFQw8+PSAtEiw8RwAsuBazjDw4NMDUijBIJEAYUFsbmPAaY3B8fYLBx7U3Knjk3yd+PkDw+E8PunDRzf8YGOQscel5cyZggMJx55JsEnnbpY4wHC4mI0vLe1mDw9uh0nOyEk4kMB2GKRlA0hLYhsPj9kNHgk8Wua/AWr5B9QieXbzD5iWm38McGvhl2A/cCCxDahFgncb3JbbPAl4tPDkMBxI7Dss2caTu83ijEE6UAtb2m2ZAxI8oFDHBtjYjz98+OPbYX759rObb1RUWCfO72E+dvPtPxt7WNxiAh4DJA6CLYFLPRCwP8AjOQpGwSgYBaMACACdIlpfQc3EHgAAAABJRU5ErkJggg==","orcid":"","institution":"University of Rome Tor Vergata","correspondingAuthor":true,"prefix":"","firstName":"Matteo","middleName":"","lastName":"Veglianti","suffix":""}],"badges":[],"createdAt":"2024-02-13 09:19:17","currentVersionCode":1,"declarations":"","doi":"10.21203/rs.3.rs-3953160/v1","doiUrl":"https://doi.org/10.21203/rs.3.rs-3953160/v1","draftVersion":[],"editorialEvents":[{"content":"https://doi.org/10.1007/s10569-024-10207-1","type":"published","date":"2024-09-10T15:58:09+00:00"}],"editorialNote":"","failedWorkflow":false,"files":[{"id":64619518,"identity":"a8e4b072-f91a-49a5-b18b-fff6d8133556","added_by":"auto","created_at":"2024-09-16 16:15:33","extension":"pdf","order_by":1,"title":"","display":"","copyAsset":false,"role":"manuscript-pdf","size":442726,"visible":true,"origin":"","legend":"","description":"","filename":"Spinorbit.pdf","url":"https://assets-eu.researchsquare.com/files/rs-3953160/v1_covered_52843121-1002-413d-90b3-e92fe8d73c32.pdf"}],"financialInterests":"No competing interests reported.","formattedTitle":"Spin orbit resonance cascade via core shell model. \\\\Application to Mercury and Ganymede","fulltext":[],"fulltextSource":"","fullText":"","funders":[],"hasAdminPriorityOnWorkflow":false,"hasManuscriptDocX":false,"hasOptedInToPreprint":true,"hasPassedJournalQc":"","hasAnyPriority":false,"hideJournal":false,"highlight":"","institution":"","isAcceptedByJournal":true,"isAuthorSuppliedPdf":true,"isDeskRejected":"","isHiddenFromSearch":false,"isInQc":false,"isInWorkflow":false,"isPdf":true,"isPdfUpToDate":true,"isWithdrawnOrRetracted":false,"journal":{"display":true,"email":"[email protected]","identity":"celestial-mechanics-and-dynamical-astronomy","isNatureJournal":false,"hasQc":true,"allowDirectSubmit":false,"externalIdentity":"cele","sideBox":"Learn more about [Celestial Mechanics and Dynamical Astronomy](http://link.springer.com/journal/10569)","snPcode":"10569","submissionUrl":"https://submission.nature.com/new-submission/10569/3","title":"Celestial Mechanics and Dynamical Astronomy","twitterHandle":"","acdcEnabled":true,"dfaEnabled":true,"editorialSystem":"em","reportingPortfolio":"Springer Hybrid","inReviewEnabled":true,"inReviewRevisionsEnabled":false},"keywords":"tidal dissipation, spin orbit resonance, core shell model","lastPublishedDoi":"10.21203/rs.3.rs-3953160/v1","lastPublishedDoiUrl":"https://doi.org/10.21203/rs.3.rs-3953160/v1","license":{"name":"CC BY 4.0","url":"https://creativecommons.org/licenses/by/4.0/"},"manuscriptAbstract":"\u003cp\u003eWe discuss a model describing the spin orbit resonance cascade. 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