Forbush decreases in cosmic rays during intensegeomagnetic storms

Forbush decreases in cosmic rays during intensegeomagnetic storms | 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 Forbush decreases in cosmic rays during intensegeomagnetic storms Osman Ahmed, Badr Badruddin, Moncef Derouich This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-5320668/v1 This work is licensed under a CC BY 4.0 License Status: Posted Version 1 posted You are reading this latest preprint version Abstract We present the relationship between Forbush decreases (FDs) andassociated geomagnetic storms (GSs), along with their connections to interplanetary (IP) solar wind (SW) parameters, using both hourly and minute time bins.We have classified the data into groups and employed superposed epoch analysis(SEA) for each. A fast, turbulent high-field shock/sheath structure formed beforethe FD onset and passed through during CME-driven events. In contrast, CIR-driven events show delayed amplification and more perturbed dynamics. Thetime-lag between the onset of FDs and GSs were calculated and majority of the events show a time-lag of 1.5 to 4.5 hours, which is crucial for space weatherforecasting. Correlation analysis between FD amplitude and the peak values ofvarious IP SW parameters have been performed and FD amplitude is best repre-sented by the SW speed and three-parameter derivative of the perturbed IMF,merged with the IP electric field function [(σB/B)×B×v]. For CME-inducedevents, the correlation between FD amplitude and both Dst minimum and Dstamplitude shows that moderate and strong storms exhibit a better relationshipcompared to extreme CME-driven storms. We correlated the characteristics ofICME transient speed, transient period, and angular size with FD amplitudefrom the point of ejection to arrival at Earth’s orbit. Our findings indicate thattransit velocity has a stronger correlation with FD amplitude. Additionally, ICME events accompanied by a fast forward shock ahead of the compressionsheath region show a stronger correlation than those without a shock. The FDamplitude and cutoff rigidity as well as energy spectra were correlated for theselected events for various neutron monitor (NM) stations located with differentlatitudes and altitudes. The FD amplitude increases linearly with the decreaseof rigidity magnitude. Galactic cosmic ray intensity Geomagnetic Disturbances Forbush decrease Coronal Mass Ejections Interplanetary Solar wind Full Text Additional Declarations No competing interests reported. Cite Share Download PDF Status: Posted Version 1 posted 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-5320668","acceptedTermsAndConditions":true,"allowDirectSubmit":true,"archivedVersions":[],"articleType":"Research Article","associatedPublications":[],"authors":[{"id":372372502,"identity":"5d45a909-5a86-4f64-a0a1-cc9b3c9dc3b1","order_by":0,"name":"Osman Ahmed","email":"","orcid":"","institution":"King Abdulaziz University","correspondingAuthor":false,"prefix":"","firstName":"Osman","middleName":"","lastName":"Ahmed","suffix":""},{"id":372372503,"identity":"5f350632-9fd6-4c5f-b459-0a7970ab9e78","order_by":1,"name":"Badr Badruddin","email":"data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAZAAAAAyAQMAAABI0h/eAAAABlBMVEX///8AAABVwtN+AAAACXBIWXMAAA7EAAAOxAGVKw4bAAAA7klEQVRIiWNgGAWjYBACAzBiOADhfQBiNnZStDDOAGlhJkULMw+YJKDFnP3wtg+MO+4kzm8/nSZt82ubPB8zA+OHjzm4tVj2pBXPYDzzLHHDmdxt0rl9tw3bmBmYJWduw+OwAznGDIxthxM3MIC09NxmBGphY+bFp+X8G4iW+f1vt0lb9ty2J6zlBtSWhhtAWxh+3E4kqMVyxrNihsQzh4033Hi72bK34XZyGzNjM16/mPMnb2b4uOOw7Pz+3I03fvy5bTu/vfngh494tIBBYgODYwOIwdgGJhsIqIeosYew/hBWPApGwSgYBSMPAAARflcgQFhHyAAAAABJRU5ErkJggg==","orcid":"","institution":"King Abdulaziz University","correspondingAuthor":true,"prefix":"","firstName":"Badr","middleName":"","lastName":"Badruddin","suffix":""},{"id":372372504,"identity":"47afeb1d-1877-44a3-9cd0-8bf4ab06a192","order_by":2,"name":"Moncef Derouich","email":"","orcid":"","institution":"King Abdulaziz University","correspondingAuthor":false,"prefix":"","firstName":"Moncef","middleName":"","lastName":"Derouich","suffix":""}],"badges":[],"createdAt":"2024-10-23 17:08:18","currentVersionCode":1,"declarations":"","doi":"10.21203/rs.3.rs-5320668/v1","doiUrl":"https://doi.org/10.21203/rs.3.rs-5320668/v1","draftVersion":[],"editorialEvents":[],"editorialNote":"","failedWorkflow":false,"files":[{"id":69389207,"identity":"784f588e-e249-48fc-827b-c9ef37f5fd02","added_by":"auto","created_at":"2024-11-19 23:01:28","extension":"pdf","order_by":1,"title":"","display":"","copyAsset":false,"role":"manuscript-pdf","size":3006794,"visible":true,"origin":"","legend":"","description":"","filename":"Manuscriptsolarphysics.pdf","url":"https://assets-eu.researchsquare.com/files/rs-5320668/v1_covered_b9c2fec7-1fb8-4636-87c0-bc3fb5da5341.pdf"}],"financialInterests":"No competing interests reported.","formattedTitle":"Forbush decreases in cosmic rays during intensegeomagnetic storms","fulltext":[],"fulltextSource":"","fullText":"","funders":[],"hasAdminPriorityOnWorkflow":false,"hasManuscriptDocX":false,"hasOptedInToPreprint":true,"hasPassedJournalQc":"","hasAnyPriority":false,"hideJournal":true,"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":"researchsquare","isNatureJournal":false,"hasQc":true,"allowDirectSubmit":true,"externalIdentity":"","sideBox":"","snPcode":"","submissionUrl":"/submission","title":"Research Square","twitterHandle":"researchsquare","acdcEnabled":true,"dfaEnabled":false,"editorialSystem":"","reportingPortfolio":"","inReviewEnabled":false,"inReviewRevisionsEnabled":true},"keywords":"Galactic cosmic ray intensity, Geomagnetic Disturbances, Forbush decrease, Coronal Mass Ejections, Interplanetary, Solar wind","lastPublishedDoi":"10.21203/rs.3.rs-5320668/v1","lastPublishedDoiUrl":"https://doi.org/10.21203/rs.3.rs-5320668/v1","license":{"name":"CC BY 4.0","url":"https://creativecommons.org/licenses/by/4.0/"},"manuscriptAbstract":"We present the relationship between Forbush decreases (FDs) andassociated geomagnetic storms (GSs), along with their connections to interplanetary (IP) solar wind (SW) parameters, using both hourly and minute time bins.We have classified the data into groups and employed superposed epoch analysis(SEA) for each. A fast, turbulent high-field shock/sheath structure formed beforethe FD onset and passed through during CME-driven events. In contrast, CIR-driven events show delayed amplification and more perturbed dynamics. Thetime-lag between the onset of FDs and GSs were calculated and majority of the events show a time-lag of 1.5 to 4.5 hours, which is crucial for space weatherforecasting. Correlation analysis between FD amplitude and the peak values ofvarious IP SW parameters have been performed and FD amplitude is best repre-sented by the SW speed and three-parameter derivative of the perturbed IMF,merged with the IP electric field function [(σB/B)×B×v]. For CME-inducedevents, the correlation between FD amplitude and both Dst minimum and Dstamplitude shows that moderate and strong storms exhibit a better relationshipcompared to extreme CME-driven storms. We correlated the characteristics ofICME transient speed, transient period, and angular size with FD amplitudefrom the point of ejection to arrival at Earth’s orbit. Our findings indicate thattransit velocity has a stronger correlation with FD amplitude. Additionally, ICME events accompanied by a fast forward shock ahead of the compressionsheath region show a stronger correlation than those without a shock. The FDamplitude and cutoff rigidity as well as energy spectra were correlated for theselected events for various neutron monitor (NM) stations located with differentlatitudes and altitudes. 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