Current Pinch Effect during Solar Flare Eruptions

Current Pinch Effect during Solar Flare Eruptions | 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 Current Pinch Effect during Solar Flare Eruptions Haili Li, Hongfei Liang, Xinping Zhou, Yu Liu This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-4311863/v1 This work is licensed under a CC BY 4.0 License Status: Published Journal Publication published 24 Apr, 2025 Read the published version in Solar Physics → Version 1 posted 7 You are reading this latest preprint version Abstract Based on the vector magnetograms obtained from the SDO/HMI, we calculate the line-of-sight current density distribution of the active region on 2017 September 6, using the integral form of Ampere's law. Comparing the distribution of the current density and the observed flare, we find that: Firstly, the changing trend of the total current density of the active region was consistent with the change of the X-ray flux of the X9.3 flare. Secondly, the distribution of the double-ribbon flare was co-spatial with a pair of conjugate current ribbons with opposite polarities, which were consistently located on both sides of the Line-of line. Additionally, these current ribbons exhibit significant and continuous changes during the flare eruption: During the early phase of the flare eruption, there was a substantial decrease in the area of the current ribbons, resulting in the emergence of a series of high-density small current islands. During the later phase, not only the area rapidly increases, but the flare kernel evolves into a the flare band with the full release of energy. We have discovered a strong spatial correspondence between the flare kernel and the current islands through positional comparisons. This process is consistent with the physical phenomenon of the current pinch effect. Therefore, we speculate that a current pinch effect may occur during the flare eruption, and the formation of the flare kernel is likely attributed to the current pinch effect. Solar activity Solar flare Solar magnetic fields Full Text Additional Declarations No competing interests reported. Cite Share Download PDF Status: Published Journal Publication published 24 Apr, 2025 Read the published version in Solar Physics → Version 1 posted Editorial decision: Revision requested 11 Jul, 2024 Reviews received at journal 10 Jul, 2024 Reviewers agreed at journal 12 May, 2024 Reviewers invited by journal 30 Apr, 2024 Submission checks completed at journal 30 Apr, 2024 Editor assigned by journal 30 Apr, 2024 First submitted to journal 23 Apr, 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-4311863","acceptedTermsAndConditions":true,"allowDirectSubmit":false,"archivedVersions":[],"articleType":"Research Article","associatedPublications":[],"authors":[{"id":298959308,"identity":"c977d9bf-d47d-48ad-9b63-935f3ec23fcb","order_by":0,"name":"Haili Li","email":"","orcid":"","institution":"Yunnan Normal University","correspondingAuthor":false,"prefix":"","firstName":"Haili","middleName":"","lastName":"Li","suffix":""},{"id":298959310,"identity":"c8c2d8e3-ad6d-4040-83f4-cf86d326c1fb","order_by":1,"name":"Hongfei Liang","email":"data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAZAAAAAyAQMAAABI0h/eAAAABlBMVEX///8AAABVwtN+AAAACXBIWXMAAA7EAAAOxAGVKw4bAAAAqElEQVRIiWNgGAWjYBACPgnGhw9I08ImwWxsQLIWMwkStUg3s1Xz7rCTY2A//IDh5w5itMgcZrvNeybZmIEnzYCx9wxRDss/dpu3jTmxgSGHgZmxjSgtyWzFvG31iQ38b0jQwszbdjixQYIEW5gl57YdN2aTeGZwsJcYLfwSyYwf3rZVy/HzJz988JMYLSDAxAOyDogPEKmBgYHxB9FKR8EoGAWjYEQCAHFoKWFcJRVIAAAAAElFTkSuQmCC","orcid":"","institution":"Yunnan Normal University","correspondingAuthor":true,"prefix":"","firstName":"Hongfei","middleName":"","lastName":"Liang","suffix":""},{"id":298959312,"identity":"e9c06a76-464b-4013-b189-731b88b4ce48","order_by":2,"name":"Xinping Zhou","email":"","orcid":"","institution":"Sichuan Normal University","correspondingAuthor":false,"prefix":"","firstName":"Xinping","middleName":"","lastName":"Zhou","suffix":""},{"id":298959315,"identity":"01eef6bf-0ec0-4e92-9622-bad55d90320d","order_by":3,"name":"Yu Liu","email":"","orcid":"","institution":"","correspondingAuthor":false,"prefix":"","firstName":"Yu","middleName":"","lastName":"Liu","suffix":""}],"badges":[],"createdAt":"2024-04-23 12:03:38","currentVersionCode":1,"declarations":"","doi":"10.21203/rs.3.rs-4311863/v1","doiUrl":"https://doi.org/10.21203/rs.3.rs-4311863/v1","draftVersion":[],"editorialEvents":[{"content":"https://doi.org/10.1007/s11207-025-02467-3","type":"published","date":"2025-04-24T15:57:19+00:00"}],"editorialNote":"","failedWorkflow":false,"files":[{"id":81569601,"identity":"86399a4a-9ede-422b-a383-e1b53382f891","added_by":"auto","created_at":"2025-04-28 16:07:50","extension":"pdf","order_by":1,"title":"","display":"","copyAsset":false,"role":"manuscript-pdf","size":986044,"visible":true,"origin":"","legend":"","description":"","filename":"ManuscriptTemplateforSolarPhysics.pdf","url":"https://assets-eu.researchsquare.com/files/rs-4311863/v1_covered_967b3f56-d195-4e06-9e4e-3709c1bdbfb1.pdf"}],"financialInterests":"No competing interests reported.","formattedTitle":"Current Pinch Effect during Solar Flare Eruptions","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 activity, Solar flare, Solar magnetic fields","lastPublishedDoi":"10.21203/rs.3.rs-4311863/v1","lastPublishedDoiUrl":"https://doi.org/10.21203/rs.3.rs-4311863/v1","license":{"name":"CC BY 4.0","url":"https://creativecommons.org/licenses/by/4.0/"},"manuscriptAbstract":"Based on the vector magnetograms obtained from the SDO/HMI, we calculate the line-of-sight current density distribution of the active region on 2017 September 6, using the integral form of Ampere's law. Comparing the distribution of the current density and the observed flare, we find that: Firstly, the changing trend of the total current density of the active region was consistent with the change of the X-ray flux of the X9.3 flare. Secondly, the distribution of the double-ribbon flare was co-spatial with a pair of conjugate current ribbons with opposite polarities, which were consistently located on both sides of the Line-of line. Additionally, these current ribbons exhibit significant and continuous changes during the flare eruption: During the early phase of the flare eruption, there was a substantial decrease in the area of the current ribbons, resulting in the emergence of a series of high-density small current islands. During the later phase, not only the area rapidly increases, but the flare kernel evolves into a the flare band with the full release of energy. 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