Solar poloidal magnetic field generation rate from observations and mean-field dynamos

Solar poloidal magnetic field generation rate from observations and mean-field dynamos | 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 Solar poloidal magnetic field generation rate from observations and mean-field dynamos Valery Pipin This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-4448623/v1 This work is licensed under a CC BY 4.0 License Status: Published Journal Publication published 20 Aug, 2024 Read the published version in Solar Physics → Version 1 posted 7 You are reading this latest preprint version Abstract To estimate the hemispheric flux generation rate of the large-scaleradial magnetic field in the solar cycles 23 and 24 we use the photosphericobservations of the solar magnetic fields and results of the mean-fielddynamo models. Our analysis suggests that the hemispheric flux generationrate can be determined by the turbulent diffusion of the dynamo generatedmagnetic field at the solar equator. Observational data suggest thatspeed of magnetic field reconnection across equator, which representsthe effect of the latitudinal turbulent diffusion, can be insufficientto explain the magnitude of the hemispheric poloidal flux generationrate in the solar cycles 23 and 24. In addition, the results of dynamomodel show the powerful impact of the radial turbulent diffusion ofthe large-scale poloidal magnetic field on the hemispheric magneticflux generation rate and the global magnetic field distribution insidethe convection zone. Solar Cycle Dynamo Magnetic fields Full Text Additional Declarations No competing interests reported. Cite Share Download PDF Status: Published Journal Publication published 20 Aug, 2024 Read the published version in Solar Physics → Version 1 posted Editorial decision: Revision requested 19 Jun, 2024 Reviews received at journal 18 Jun, 2024 Reviewers agreed at journal 31 May, 2024 Reviewers invited by journal 30 May, 2024 Editor assigned by journal 21 May, 2024 Submission checks completed at journal 21 May, 2024 First submitted to journal 20 May, 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. We do this by developing innovative software and high quality services for the global research community. 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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-4448623","acceptedTermsAndConditions":true,"allowDirectSubmit":false,"archivedVersions":[],"articleType":"Research Article","associatedPublications":[],"authors":[{"id":309177193,"identity":"80346c8c-831a-4b65-8471-a82078afac07","order_by":0,"name":"Valery Pipin","email":"data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAZAAAAAyAQMAAABI0h/eAAAABlBMVEX///8AAABVwtN+AAAACXBIWXMAAA7EAAAOxAGVKw4bAAAAsklEQVRIie3QsQrCMBDG8a8E0qU16/kWAcFSfJkrgq6OTqUg9KkcIoVu7h0LgrNuDh1MdXGRxs3h/kO45UeSAyTpH1OIegaMH1QwUdaTeRVOAE0YCUJJFqftvh9KQpxebHRspkl+mG26ovY3qXjBuAYQ2yTLrqiSEkorBxdIdjwQ/UbA2r4IBxH/lzUVNZP2xLLbTpPMnE/3h9+YMa2im1sFPAzJe9DjwdPgg0iSJElfewKmSyvbBfFruQAAAABJRU5ErkJggg==","orcid":"","institution":"Institute of Solar-Terrestrial Physics","correspondingAuthor":true,"prefix":"","firstName":"Valery","middleName":"","lastName":"Pipin","suffix":""}],"badges":[],"createdAt":"2024-05-20 10:53:39","currentVersionCode":1,"declarations":"","doi":"10.21203/rs.3.rs-4448623/v1","doiUrl":"https://doi.org/10.21203/rs.3.rs-4448623/v1","draftVersion":[],"editorialEvents":[{"content":"https://doi.org/10.1007/s11207-024-02357-0","type":"published","date":"2024-08-20T15:57:42+00:00"}],"editorialNote":"","failedWorkflow":false,"files":[{"id":63998515,"identity":"d818b6f3-ec41-4d74-9d87-8afaa81b8c8c","added_by":"auto","created_at":"2024-09-04 18:17:37","extension":"pdf","order_by":1,"title":"","display":"","copyAsset":false,"role":"manuscript-pdf","size":2317595,"visible":true,"origin":"","legend":"","description":"","filename":"PipinVVSolarPhysics.pdf","url":"https://assets-eu.researchsquare.com/files/rs-4448623/v1_covered_52f4f2d1-770f-45ee-9ef3-ee05faa01084.pdf"}],"financialInterests":"No competing interests reported.","formattedTitle":"Solar poloidal magnetic field generation rate from observations and mean-field dynamos","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":"solar-physics","isNatureJournal":false,"hasQc":true,"allowDirectSubmit":false,"externalIdentity":"sola","sideBox":"Learn more about [Solar Physics](http://link.springer.com/journal/11207)","snPcode":"11207","submissionUrl":"https://submission.nature.com/new-submission/11207/3","title":"Solar Physics","twitterHandle":"","acdcEnabled":true,"dfaEnabled":true,"editorialSystem":"em","reportingPortfolio":"Springer Hybrid","inReviewEnabled":true,"inReviewRevisionsEnabled":false},"keywords":"Solar Cycle, Dynamo, Magnetic fields","lastPublishedDoi":"10.21203/rs.3.rs-4448623/v1","lastPublishedDoiUrl":"https://doi.org/10.21203/rs.3.rs-4448623/v1","license":{"name":"CC BY 4.0","url":"https://creativecommons.org/licenses/by/4.0/"},"manuscriptAbstract":"To estimate the hemispheric flux generation rate of the large-scaleradial magnetic field in the solar cycles 23 and 24 we use the photosphericobservations of the solar magnetic fields and results of the mean-fielddynamo models. 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