Effect of Various Plasma Parameters on Whistler mode wave with Latitudinally varying Magnetic field and D.C. electric field in Jupiter’s Magnetosphere

Effect of Various Plasma Parameters on Whistler mode wave with Latitudinally varying Magnetic field and D.C. electric field in Jupiter’s Magnetosphere | 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 Effect of Various Plasma Parameters on Whistler mode wave with Latitudinally varying Magnetic field and D.C. electric field in Jupiter’s Magnetosphere R. S. Pandey, A. K. Dhaikar, R. K. Tyagi This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-8615598/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 investigate the linear growth, dispersion, and refractive index of whistler-mode electromagnetic waves in Jupiter’s magnetospheric plasma in the presence of a DC electric field and an empirically latitudinally varying magnetic-field model. Using a relativistic generalized distribution function (reducible to a bi-Maxwellian for j = 0 and a loss-cone type for j = 1) and a kinetic (Vlasov–Maxwell) formalism, the dispersion relation is derived and solved via the method of characteristics to obtain real frequencies, refractive indices, and dimensionless growth rates. Numerical calculations use Voyager-era parameters at R = 17 R J (after Bagenal, 1994) and the latitudinally varying magnetic field adopted in previous Jovian studies. For the loss-cone case (j = 1) growth rates are significantly larger than for the Maxwellian case (j = 0), accompanied by variations in refractive index profiles. Growth is generally enhanced by greater temperature anisotropy and higher thermal energy; it decreases with increasing relativistic factor (v/c). The parallel DC electric field modifies growth and refractive index profiles depending on magnetic geometry: under varying latitudinal angle conditions it can amplify whistler growth, while in other model runs its effect is reduced. These results quantify how plasma parameters and field geometry control whistler-mode instability, including refractive index variations, in Jupiter’s magnetosphere and provide a basis for comparative studies of planetary magnetospheres. Whistler mode wave Wave particle interaction Instability in Jupiter magnetosphere Effect of parallel DC electric field Loss cone distribution etc. 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-8615598","acceptedTermsAndConditions":true,"allowDirectSubmit":true,"archivedVersions":[],"articleType":"Research Article","associatedPublications":[],"authors":[{"id":580930339,"identity":"18e8ccb1-6ffc-4917-8959-a72934b8f9d6","order_by":0,"name":"R. S. 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Using a relativistic generalized distribution function (reducible to a bi-Maxwellian for j\u0026thinsp;=\u0026thinsp;0 and a loss-cone type for j\u0026thinsp;=\u0026thinsp;1) and a kinetic (Vlasov\u0026ndash;Maxwell) formalism, the dispersion relation is derived and solved via the method of characteristics to obtain real frequencies, refractive indices, and dimensionless growth rates. Numerical calculations use Voyager-era parameters at R\u0026thinsp;=\u0026thinsp;17 R\u003csub\u003eJ\u003c/sub\u003e (after Bagenal, 1994) and the latitudinally varying magnetic field adopted in previous Jovian studies. For the loss-cone case (j\u0026thinsp;=\u0026thinsp;1) growth rates are significantly larger than for the Maxwellian case (j\u0026thinsp;=\u0026thinsp;0), accompanied by variations in refractive index profiles. Growth is generally enhanced by greater temperature anisotropy and higher thermal energy; it decreases with increasing relativistic factor (v/c). The parallel DC electric field modifies growth and refractive index profiles depending on magnetic geometry: under varying latitudinal angle conditions it can amplify whistler growth, while in other model runs its effect is reduced. These results quantify how plasma parameters and field geometry control whistler-mode instability, including refractive index variations, in Jupiter\u0026rsquo;s magnetosphere and provide a basis for comparative studies of planetary magnetospheres.\u003c/p\u003e","manuscriptTitle":"Effect of Various Plasma Parameters on Whistler mode wave with Latitudinally varying Magnetic field and D.C. electric field in Jupiter’s Magnetosphere","msid":"","msnumber":"","nonDraftVersions":[{"code":1,"date":"2026-01-28 10:02:34","doi":"10.21203/rs.3.rs-8615598/v1","editorialEvents":[{"type":"communityComments","content":0}],"status":"published","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}}],"origin":"","ownerIdentity":"b5761098-ccc9-4931-a0d8-9ca3b6f2f330","owner":[],"postedDate":"January 28th, 2026","published":true,"recentEditorialEvents":[],"rejectedJournal":[],"revision":"","amendment":"","status":"posted","subjectAreas":[],"tags":[],"updatedAt":"2026-02-19T07:26:20+00:00","versionOfRecord":[],"versionCreatedAt":"2026-01-28 10:02:34","video":"","vorDoi":"","vorDoiUrl":"","workflowStages":[]},"version":"v1","identity":"rs-8615598","journalConfig":"researchsquare"},"__N_SSP":true},"page":"/article/[identity]/[[...version]]","query":{"redirect":"/article/rs-8615598","identity":"rs-8615598","version":["v1"]},"buildId":"XKTyCvWXoU3ODBz1xrDgd","isFallback":false,"isExperimentalCompile":false,"dynamicIds":[84888],"gssp":true,"scriptLoader":[]}