Multi-lane type II radio bursts: Insights into shock propagation inthe corona

Multi-lane type II radio bursts: Insights into shock propagation inthe corona | 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 Multi-lane type II radio bursts: Insights into shock propagation inthe corona Nadiya K, Divya Paliwal, Anshu Kumari This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-9006547/v1 This work is licensed under a CC BY 4.0 License Status: Under Revision Version 1 posted 7 You are reading this latest preprint version Abstract Type II solar radio bursts are considered as the signatures of the coronal shocks. These bursts are generated from plasma waves excited by magnetohydrodynamic (MHD) shocks, and then converted into radio waves at the local plasma frequency and/or its harmonics. Hence, these bursts often have fundamental-harmonic (FH) and band-splitting (SB) structures, which provide insights into shock generation and propagation in the corona, hence, in turn, the corresponding coronal conditions. In the present study, we analysed an unusual multi-lane type II burst observed with ground-based solar radio spectrographs on May 29, 2024, between 14:24 and 14:43 UT. The start and end frequencies of the type II burst were 450 MHz and 25 MHz, respectively. By combining spectral information with radio imaging data, we found that radio waves were escaping from the corona via emissions from distinct shock regions. In addition, along with the traditional FH and SB, there were multi-lane structures in the type II bursts. Our analysis suggests complex, inhomogeneous shock dynamics near the leading edge (LE) of the coronal mass ejection (CME). This indicates that the plasma material compresses more strongly in these forefront regions. This was confirmed by radio imaging observations, which showed that the higher-frequency emission occurred at a higher altitude than the lower-frequency emission. Our results suggest that the shock geometry and plasma inhomogeneity play an important role in the generation of type II bursts, leading to traditional fundamental-harmonic split-band (FH-SB) pairs with additional splitting in the type II bands. Radio radiation Coronal mass ejections Flares Corona Activity Full Text Additional Declarations No competing interests reported. Cite Share Download PDF Status: Under Revision Version 1 posted Editorial decision: Revision requested 30 Apr, 2026 Reviews received at journal 30 Apr, 2026 Reviewers agreed at journal 05 Mar, 2026 Reviewers invited by journal 04 Mar, 2026 Editor assigned by journal 02 Mar, 2026 Submission checks completed at journal 02 Mar, 2026 First submitted to journal 02 Mar, 2026 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-9006547","acceptedTermsAndConditions":true,"allowDirectSubmit":false,"archivedVersions":[],"articleType":"Research Article","associatedPublications":[],"authors":[{"id":601019635,"identity":"faeaff3b-5daa-40f2-a6b9-90d2acee4dde","order_by":0,"name":"Nadiya K","email":"","orcid":"","institution":"Mahatma Gandhi University","correspondingAuthor":false,"prefix":"","firstName":"Nadiya","middleName":"","lastName":"K","suffix":""},{"id":601019636,"identity":"afb30a50-2886-44d0-a7d6-09dbbfc76e2a","order_by":1,"name":"Divya Paliwal","email":"","orcid":"","institution":"Physical Research Laboratory","correspondingAuthor":false,"prefix":"","firstName":"Divya","middleName":"","lastName":"Paliwal","suffix":""},{"id":601019637,"identity":"661e7732-816d-47ed-91d3-3130e9678198","order_by":2,"name":"Anshu Kumari","email":"data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAZAAAAAyAQMAAABI0h/eAAAABlBMVEX///8AAABVwtN+AAAACXBIWXMAAA7EAAAOxAGVKw4bAAAAvUlEQVRIiWNgGAWjYHACNgaGCgYGPghHglgtZ8AkKVoY2+BaiAD8s9ufPeaddyefjYH34cMfDBZ5BLVI3Dljbsy77ZllGwO7sTEPg0QxYWtu5LBJ8247bMDGwMYmDTQisYGQDvkb6c+keeeAtbD//EGMFoMbCWbSvA0QWxh4iNFieCPHTHLOsWcGbMxszNI8BkRokQM6TOJNzR0DfvY2xo8/KuoIa4GCAwwMzGB3EqkeomUUjIJRMApGAS4AAMNPMCeJe+JYAAAAAElFTkSuQmCC","orcid":"","institution":"Physical Research Laboratory","correspondingAuthor":true,"prefix":"","firstName":"Anshu","middleName":"","lastName":"Kumari","suffix":""}],"badges":[],"createdAt":"2026-03-02 06:53:40","currentVersionCode":1,"declarations":"","doi":"10.21203/rs.3.rs-9006547/v1","doiUrl":"https://doi.org/10.21203/rs.3.rs-9006547/v1","draftVersion":[],"editorialEvents":[],"editorialNote":"","failedWorkflow":false,"files":[{"id":104404748,"identity":"8eaf7101-c7bc-4d56-8a83-8aef9492a4a0","added_by":"auto","created_at":"2026-03-11 12:21:00","extension":"pdf","order_by":1,"title":"","display":"","copyAsset":false,"role":"manuscript-pdf","size":4174291,"visible":true,"origin":"","legend":"","description":"","filename":"May292024.pdf","url":"https://assets-eu.researchsquare.com/files/rs-9006547/v1_covered_efb7f7da-ad26-4af3-8c30-f7556b244600.pdf"}],"financialInterests":"No competing interests reported.","formattedTitle":"Multi-lane type II radio bursts: Insights into shock propagation inthe corona","fulltext":[],"fulltextSource":"","fullText":"","funders":[],"hasAdminPriorityOnWorkflow":false,"hasManuscriptDocX":false,"hasOptedInToPreprint":true,"hasPassedJournalQc":"","hasAnyPriority":false,"hideJournal":false,"highlight":"","institution":"","isAcceptedByJournal":false,"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":"Radio radiation, Coronal mass ejections, Flares, Corona, Activity","lastPublishedDoi":"10.21203/rs.3.rs-9006547/v1","lastPublishedDoiUrl":"https://doi.org/10.21203/rs.3.rs-9006547/v1","license":{"name":"CC BY 4.0","url":"https://creativecommons.org/licenses/by/4.0/"},"manuscriptAbstract":"Type II solar radio bursts are considered as the signatures of the coronal shocks. 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Our analysis suggests complex, inhomogeneous shock dynamics near the leading edge (LE) of the coronal mass ejection (CME). This indicates that the plasma material compresses more strongly in these forefront regions. This was confirmed by radio imaging observations, which showed that the higher-frequency emission occurred at a higher altitude than the lower-frequency emission. 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