A theoretical model analysis for non-thermal solar plasma fluctuations

A theoretical model analysis for non-thermal solar plasma fluctuations | 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 A theoretical model analysis for non-thermal solar plasma fluctuations Souvik Das, Atteya Ahmed, Pralay Kumar Karmakar This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-6843637/v1 This work is licensed under a CC BY 4.0 License Status: Under Review Version 1 posted 4 You are reading this latest preprint version Abstract Solar plasmas exhibit a broad spectrum of collective oscillatory modes essential to understanding helioseismic and dynamical phenomena. In this study, a linear fluctuation analysis is performed to explore the stability of non-thermal κ-modifiedviscoturbulent inhomogeneous solar plasmas. Fluid turbulence effects are incorporated using a modified Larson logabarotropic equation of state. The analysis yields a generalized linear cubic dispersion relation describing the self-gravitationally bounded solar interior plasma. We explore the influence of key physical parameters—including the non-thermality index, electron temperature, dynamic viscosity, and thermal conductivity—on the resulting dispersion signatures. The Routh–Hurwitz stability criterion is systematically applied to assess the plasma stability features. Both the helioseismic g-modes and p-modes are theoretically characterized. While the g-modes can induce large changes to the solar parameters, they cease to exhibit oscillatory behaviour beyond approximately 2.4 × 108 m from the solar core. In contrast, the p-modes propagate throughout the Sun. The excitation of the well-known five-minute oscillations is illustratively analysed and observationally validated. Our results indicate that electron non-thermality and thermal conductivity enhance mode propagation, whereas viscosity and electron temperature act as damping factors. The radially outward energy flux of the photospheric p-modes is estimated to lie in the range of 103 − 105 W m−2. These p-modes are shown to contribute substantially to chromospheric spicule formation via longitudinal-to-transverse mode conversion processes. The κ-modified wave characteristics reported here align well with prior results and are further supported by a broad range of solar observations, underscoring the robustness of our theoretical framework. Helioseismology Interior Instabilities Oscillations Full Text Additional Declarations No competing interests reported. Cite Share Download PDF Status: Under Review Version 1 posted Reviewers invited by journal 19 Aug, 2025 Editor assigned by journal 12 Jun, 2025 Submission checks completed at journal 12 Jun, 2025 First submitted to journal 07 Jun, 2025 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-6843637","acceptedTermsAndConditions":true,"allowDirectSubmit":false,"archivedVersions":[],"articleType":"Research Article","associatedPublications":[],"authors":[{"id":503245606,"identity":"ef972185-c946-4d8c-a78e-fae475695233","order_by":0,"name":"Souvik Das","email":"","orcid":"","institution":"Tezpur University","correspondingAuthor":false,"prefix":"","firstName":"Souvik","middleName":"","lastName":"Das","suffix":""},{"id":503245607,"identity":"4f578d1c-f21c-4350-9bf0-ea96190ea9f9","order_by":1,"name":"Atteya Ahmed","email":"","orcid":"","institution":"Alexandria University","correspondingAuthor":false,"prefix":"","firstName":"Atteya","middleName":"","lastName":"Ahmed","suffix":""},{"id":503245608,"identity":"81092f4a-4ea8-41d6-a6ac-ba3e6ee4df0e","order_by":2,"name":"Pralay Kumar Karmakar","email":"data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAZAAAAAyAQMAAABI0h/eAAAABlBMVEX///8AAABVwtN+AAAACXBIWXMAAA7EAAAOxAGVKw4bAAAAwklEQVRIiWNgGAWjYDACHjbGByh8YrQwGxyA8xKI08ImgayFMDDnOZZW/aGiLrGBvffZg48/GGTMCWmx7G07duPAGbbEBp7j5oYzgA6zbCCgxeA8e9uNg208iQ0SaWzSPEAtSD7DraXg4D+JxAb5Z2zSf4jScrbtGMPBBgOgLWxs0gzEaLHsOZYsceZYgnEbTxqbZE+aBGEt5jxphh8qaupk+9mPsUn8sLGxJ+wwGIMNQkkQUI+sZRSMglEwCkYBTgAAYQY5nIzq0LcAAAAASUVORK5CYII=","orcid":"","institution":"Tezpur University","correspondingAuthor":true,"prefix":"","firstName":"Pralay","middleName":"Kumar","lastName":"Karmakar","suffix":""}],"badges":[],"createdAt":"2025-06-07 15:23:18","currentVersionCode":1,"declarations":"","doi":"10.21203/rs.3.rs-6843637/v1","doiUrl":"https://doi.org/10.21203/rs.3.rs-6843637/v1","draftVersion":[],"editorialEvents":[],"editorialNote":"","failedWorkflow":false,"files":[{"id":90113585,"identity":"9bdcd0d4-86ae-4b07-988c-82d751210a48","added_by":"auto","created_at":"2025-08-28 15:41:25","extension":"pdf","order_by":1,"title":"","display":"","copyAsset":false,"role":"manuscript-pdf","size":3917731,"visible":true,"origin":"","legend":"","description":"","filename":"MS.pdf","url":"https://assets-eu.researchsquare.com/files/rs-6843637/v1_covered_de9526e0-6010-4fc4-896a-1b0b119c9cd5.pdf"}],"financialInterests":"No competing interests reported.","formattedTitle":"A theoretical model analysis for non-thermal solar plasma fluctuations","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":"Helioseismology, Interior, Instabilities, Oscillations","lastPublishedDoi":"10.21203/rs.3.rs-6843637/v1","lastPublishedDoiUrl":"https://doi.org/10.21203/rs.3.rs-6843637/v1","license":{"name":"CC BY 4.0","url":"https://creativecommons.org/licenses/by/4.0/"},"manuscriptAbstract":"Solar plasmas exhibit a broad spectrum of collective oscillatory modes essential to understanding helioseismic and dynamical phenomena. 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The excitation of the well-known five-minute oscillations is illustratively analysed and observationally validated. Our results indicate that electron non-thermality and thermal conductivity enhance mode propagation, whereas viscosity and electron temperature act as damping factors. The radially outward energy flux of the photospheric p-modes is estimated to lie in the range of 103 − 105 W m−2. These p-modes are shown to contribute substantially to chromospheric spicule formation via longitudinal-to-transverse mode conversion processes. 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