Unveiling U Gem Outbursts: Light Curve Analysis and Exploring Correlations of Outburst Mechanism

Unveiling U Gem Outbursts: Light Curve Analysis and Exploring Correlations of Outburst Mechanism | 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 Unveiling U Gem Outbursts: Light Curve Analysis and Exploring Correlations of Outburst Mechanism Md Talha Zobair, S.M. Fuad Hasan This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-6048492/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 As a nova-typed cataclysmic star, U Gem exhibits outbursts in brightness, and stars like this have left astronomers puzzled about the underlying mechanism. By analyzing the light curve of U Gem (a graph representing its changing magnitude over time that reveals the outburst cycle), the spectrums and the temperature variation of its white dwarf component, we gained a bit of understanding of these outbursts. Using professional data sites such as the American Association of Variable Star Observers (AAVSO) and the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope (HST), we gathered light curves to identify different phases of outbursts as well as collected the visible and ultraviolet spectrums. During the narrow and wide outbursts, it brightens about an average of 4.7 mags, and 5.6667 mags, respectively, in Vis. band, the radial velocity increased 314.486 ± 11.2 km/s throughout different phases, and the WD cools from a temperature of ~41,500 K, 15 days after the peak of the outburst, to ~36,250 K, 56 days after the peak of the outburst. By studying periods of outbursts, we have linked them to material activities in U Gem. To follow the variations in radial velocity during outburst phases, the Balmer spectral lines were also investigated. Correlating these phases with variations in radial velocity, derived from spectral line shifts, and white dwarf temperature changes during quiescence provides crucial insights into the system's behavior and helps to understand the dynamics of the accretion disk and the evolution of cataclysmic variable stars. This, I hope, will make it easier for others who may wish to study further about cataclysmic variable stars and the intricate dynamics of peculiar stars like this one to do so. Cataclysmic Variable Stars Nova Dwarf Outburst Light Curves Spectroscopicy Radial Velocity White Dwarf 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-6048492","acceptedTermsAndConditions":true,"allowDirectSubmit":true,"archivedVersions":[],"articleType":"Research Article","associatedPublications":[],"authors":[{"id":423003236,"identity":"c9de1075-25e1-4ae2-86f8-2014f6a36e55","order_by":0,"name":"Md Talha Zobair","email":"data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAZAAAAAyAQMAAABI0h/eAAAABlBMVEX///8AAABVwtN+AAAACXBIWXMAAA7EAAAOxAGVKw4bAAABEklEQVRIiWNgGAWjYFAC5jYwZcDA2MCQwPNfDsQ58ACPBh4GRiQtH2SYjcFaEojTwsDAOMOGObEBxMOnxZ79YNuDHwx1cubsh9s+8+Swpc8PO/wQaIudnG4DDlt4EtsNexjYjC17Eptn85zhyd14O80AqCXZ2OwALocltknwMPAkbjiQ2MzM2yORu3F2AkjLgcRtuLTwP2yT/MMgkbjh/EOgln8G6Yaz0z/g1yKR2CbNw2CQuOFGYjPjDJ6EBHnpHAK23HjYJi1jkGBsOeNhM8MHngOGG6RzCg4kGOD2C3t/8jHJNxXAEONPfwyMygPy8rPTN3/4UGEnh0sLBBggsw+gixAE8g2kqB4Fo2AUjIKRAAB86l2KLgxipwAAAABJRU5ErkJggg==","orcid":"","institution":"Ideal School and College","correspondingAuthor":true,"prefix":"","firstName":"Md","middleName":"Talha","lastName":"Zobair","suffix":""},{"id":423003237,"identity":"17e1b09e-359d-437a-8121-6a0de1966b80","order_by":1,"name":"S.M. 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By analyzing the light curve of U Gem (a graph representing its changing magnitude over time that reveals the outburst cycle), the spectrums and the temperature variation of its white dwarf component, we gained a bit of understanding of these outbursts. Using professional data sites such as the American Association of Variable Star Observers (AAVSO) and the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope (HST), we gathered light curves to identify different phases of outbursts as well as collected the visible and ultraviolet spectrums. During the narrow and wide outbursts, it brightens about an average of 4.7 mags, and 5.6667 mags, respectively, in Vis. band, the radial velocity increased 314.486 ± 11.2 km/s throughout different phases, and the WD cools from a temperature of ~41,500 K, 15 days after the peak of the outburst, to ~36,250 K, 56 days after the peak of the outburst. By studying periods of outbursts, we have linked them to material activities in U Gem. To follow the variations in radial velocity during outburst phases, the Balmer spectral lines were also investigated. Correlating these phases with variations in radial velocity, derived from spectral line shifts, and white dwarf temperature changes during quiescence provides crucial insights into the system's behavior and helps to understand the dynamics of the accretion disk and the evolution of cataclysmic variable stars. This, I hope, will make it easier for others who may wish to study further about cataclysmic variable stars and the intricate dynamics of peculiar stars like this one to do so.","manuscriptTitle":"Unveiling U Gem Outbursts: Light Curve Analysis and Exploring Correlations of Outburst Mechanism","msid":"","msnumber":"","nonDraftVersions":[{"code":1,"date":"2025-03-04 03:19:38","doi":"10.21203/rs.3.rs-6048492/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":"4c5d0533-6aba-4103-9207-cdadffe68b0f","owner":[],"postedDate":"March 4th, 2025","published":true,"recentEditorialEvents":[],"rejectedJournal":[],"revision":"","amendment":"","status":"posted","subjectAreas":[],"tags":[],"updatedAt":"2025-03-04T03:19:38+00:00","versionOfRecord":[],"versionCreatedAt":"2025-03-04 03:19:38","video":"","vorDoi":"","vorDoiUrl":"","workflowStages":[]},"version":"v1","identity":"rs-6048492","journalConfig":"researchsquare"},"__N_SSP":true},"page":"/article/[identity]/[[...version]]","query":{"redirect":"/article/rs-6048492","identity":"rs-6048492","version":["v1"]},"buildId":"8U1c8b4HqxoKbykW_rLl7","isFallback":false,"isExperimentalCompile":false,"dynamicIds":[84888],"gssp":true,"scriptLoader":[]}