Fine Distributions of Non-potential Magnetic Field Parameters in a Super-Active Region with Complex Structures and Strong Solar Flares

Fine Distributions of Non-potential Magnetic Field Parameters in a Super-Active Region with Complex Structures and Strong Solar Flares | 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 Fine Distributions of Non-potential Magnetic Field Parameters in a Super-Active Region with Complex Structures and Strong Solar Flares Suo Liu This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-4532367/v1 This work is licensed under a CC BY 4.0 License Status: Published Journal Publication published 07 Apr, 2025 Read the published version in Solar Physics → Version 1 posted 7 You are reading this latest preprint version Abstract The non-potential magnetic field parameters serve as vital indicators in solar active regions, profoundly intertwined with solar flares. In this study, extrapolation techniques are employed to reconstruct the three-dimensional magnetic field configuration from vector magnetic field on the photosphere of the active region NOAA 9077 with super strong X5.7 solar flare event (SOL2000-07-14T10:24), which observed by the Solar Magnetic Field Telescope (SMFT) at Huairou Solar Observing Station (HSOS). Then, various magnetic field parameters such as current density, shear angle, quasi-separatrix layers, twist, and field line helicity are calculated. With the aim to understand the relations between magnetic field properties and solar flares, the fine distributions of these non-potential magnetic field parameters are analysed, and their changes before and after solar flares are investigated with the greatest attention. Overall, helicity and free energy decrease after super flares, while free energy peaks ∼1.5 days before flare. The distributions of quasi-separatrix layers and twist have high degree of complexity before flare. Multi patterns of high current density regions probably suggest unstable magnetic structures prone to flaring, aligning with shear angle distributions. Relative field line helicity patterns differ from current density, but concentrate before flares and diverge afterward. Overall, current density patterns contrast relative field line helicity. Solar Magnetic Field Non-potential Parameters Solar Flare Full Text Additional Declarations No competing interests reported. Cite Share Download PDF Status: Published Journal Publication published 07 Apr, 2025 Read the published version in Solar Physics → Version 1 posted Editorial decision: Revision requested 25 Jun, 2024 Reviews received at journal 25 Jun, 2024 Reviewers agreed at journal 06 Jun, 2024 Reviewers invited by journal 06 Jun, 2024 Editor assigned by journal 05 Jun, 2024 Submission checks completed at journal 05 Jun, 2024 First submitted to journal 05 Jun, 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. Our growing team is made up of researchers and industry professionals working together to solve the most critical problems facing scientific publishing. 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-4532367","acceptedTermsAndConditions":true,"allowDirectSubmit":false,"archivedVersions":[],"articleType":"Research Article","associatedPublications":[],"authors":[{"id":315153924,"identity":"3c1aafd1-67a7-4237-aaef-1bc81444715d","order_by":0,"name":"Suo Liu","email":"data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAZAAAAAyAQMAAABI0h/eAAAABlBMVEX///8AAABVwtN+AAAACXBIWXMAAA7EAAAOxAGVKw4bAAAAp0lEQVRIiWNgGAWjYBACPmYg8YEkLWxALYwzSNMCxMw8pGlh5zH+bLvDTo6B/fDjDww1d4hxGI+ZdO6ZZGMGnjQzCYZjz4jTwpzbxpzYIMFgxsDYcJgoLcafLdvqgVrYP38gVouBNGPbYaAWHgMJIrWwlUn2th03ZuPJKZNIOEaEFn7+w5s//GyrluNnP775w4caIrQgrAMRCSRoGAWjYBSMglGABwAAotUqwrT1kXQAAAAASUVORK5CYII=","orcid":"","institution":"Chinese Academy of Science","correspondingAuthor":true,"prefix":"","firstName":"Suo","middleName":"","lastName":"Liu","suffix":""}],"badges":[],"createdAt":"2024-06-05 08:09:14","currentVersionCode":1,"declarations":"","doi":"10.21203/rs.3.rs-4532367/v1","doiUrl":"https://doi.org/10.21203/rs.3.rs-4532367/v1","draftVersion":[],"editorialEvents":[{"content":"https://doi.org/10.1007/s11207-025-02456-6","type":"published","date":"2025-04-07T16:05:26+00:00"}],"editorialNote":"","failedWorkflow":false,"files":[{"id":80558623,"identity":"5b18d38e-d955-4d91-b3d2-1e8a8644de16","added_by":"auto","created_at":"2025-04-14 16:15:12","extension":"pdf","order_by":1,"title":"","display":"","copyAsset":false,"role":"manuscript-pdf","size":2145509,"visible":true,"origin":"","legend":"","description":"","filename":"manuscript.pdf","url":"https://assets-eu.researchsquare.com/files/rs-4532367/v1_covered_0fce9195-9cd8-475a-8ab8-64efd672b438.pdf"}],"financialInterests":"No competing interests reported.","formattedTitle":"Fine Distributions of Non-potential Magnetic Field Parameters in a Super-Active Region with Complex Structures and Strong Solar Flares","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 Magnetic Field, Non-potential Parameters, Solar Flare","lastPublishedDoi":"10.21203/rs.3.rs-4532367/v1","lastPublishedDoiUrl":"https://doi.org/10.21203/rs.3.rs-4532367/v1","license":{"name":"CC BY 4.0","url":"https://creativecommons.org/licenses/by/4.0/"},"manuscriptAbstract":"The non-potential magnetic field parameters serve as vital indicators in solar active regions, profoundly intertwined with solar flares. In this study, extrapolation techniques are employed to reconstruct the three-dimensional magnetic field configuration from vector magnetic field on the photosphere of the active region NOAA 9077 with super strong X5.7 solar flare event (SOL2000-07-14T10:24), which observed by the Solar Magnetic Field Telescope (SMFT) at Huairou Solar Observing Station (HSOS). Then, various magnetic field parameters such as current density, shear angle, quasi-separatrix layers, twist, and field line helicity are calculated. With the aim to understand the relations between magnetic field properties and solar flares, the fine distributions of these non-potential magnetic field parameters are analysed, and their changes before and after solar flares are investigated with the greatest attention. Overall, helicity and free energy decrease after super flares, while free energy peaks ∼1.5 days before flare. The distributions of quasi-separatrix layers and twist have high degree of complexity before flare. Multi patterns of high current density regions probably suggest unstable magnetic structures prone to flaring, aligning with shear angle distributions. Relative field line helicity patterns differ from current density, but concentrate before flares and diverge afterward. Overall, current density patterns contrast relative field line helicity.","manuscriptTitle":"Fine Distributions of Non-potential Magnetic Field Parameters in a Super-Active Region with Complex Structures and Strong Solar Flares","msid":"","msnumber":"","nonDraftVersions":[{"code":1,"date":"2024-06-19 02:22:52","doi":"10.21203/rs.3.rs-4532367/v1","editorialEvents":[{"type":"communityComments","content":0},{"type":"decision","content":"Revision requested","date":"2024-06-25T23:03:01+00:00","index":"","fulltext":""},{"type":"editorInvitedReview","content":"","date":"2024-06-25T17:24:15+00:00","index":"hide","fulltext":""},{"type":"reviewerAgreed","content":"322052632207142047465040547081815397344","date":"2024-06-06T14:19:51+00:00","index":"hide","fulltext":""},{"type":"reviewersInvited","content":"","date":"2024-06-06T05:10:13+00:00","index":"","fulltext":""},{"type":"editorAssigned","content":"","date":"2024-06-06T01:53:32+00:00","index":"","fulltext":""},{"type":"checksComplete","content":"","date":"2024-06-06T01:52:40+00:00","index":"","fulltext":""},{"type":"submitted","content":"Solar Physics","date":"2024-06-05T08:07:54+00:00","index":"","fulltext":""}],"status":"published","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}}],"origin":"","ownerIdentity":"9d22ff7e-59ce-46e3-97e6-bf8ed03ba82c","owner":[],"postedDate":"June 19th, 2024","published":true,"recentEditorialEvents":[],"rejectedJournal":[],"revision":"","amendment":"","status":"published-in-journal","subjectAreas":[],"tags":[],"updatedAt":"2025-04-14T16:09:41+00:00","versionOfRecord":{"articleIdentity":"rs-4532367","link":"https://doi.org/10.1007/s11207-025-02456-6","journal":{"identity":"solar-physics","isVorOnly":false,"title":"Solar Physics"},"publishedOn":"2025-04-07 16:05:26","publishedOnDateReadable":"April 7th, 2025"},"versionCreatedAt":"2024-06-19 02:22:52","video":"","vorDoi":"10.1007/s11207-025-02456-6","vorDoiUrl":"https://doi.org/10.1007/s11207-025-02456-6","workflowStages":[]},"version":"v1","identity":"rs-4532367","journalConfig":"researchsquare"},"__N_SSP":true},"page":"/article/[identity]/[[...version]]","query":{"redirect":"/article/rs-4532367","identity":"rs-4532367","version":["v1"]},"buildId":"_2-kVJe1T_tPrBINL-cwx","isFallback":false,"isExperimentalCompile":false,"dynamicIds":[84888],"gssp":true,"scriptLoader":[]}