Deformed neutron stars

Deformed neutron stars | 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PDF Research Article Deformed neutron stars Jonathan Quartuccio, Pedro Moraes, José Arbañil This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-4252499/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 solutions for non-spherically symmetric neutron stars. We begin by deriving the Tolman-Oppenheimer-Volkoff equations from a parameterized metric that takes into account the deformation of the star due to differences in equatorial and polar pressures, expressed in terms of a parameter $\mathcal{D}$, which is the ratio between polar and equatorial radius. The stellar structure is solved using the GM1 equation of state and the Tolman-Oppenheimer-Volkoff equations for deformed objects are numerically integrated using the fourth-order Runge-Kutta method for different values of the parameter $\mathcal{D}$. We show that larger values of $\mathcal{D}>1$, that describe prolate neutron stars, yield smaller values of mass and radius, while for smaller values of $\mathcal{D}<1$, describing oblate neutron stars, larger values for mass and radius are attained. From the confrontation of our model theoretical predictions with recent observational data on pulsars, it is possible to constrain the values of the parameter $\mathcal{D}$.\ \emph{Keywords}: general relativity; tov equation; neutron stars; deformation general relativity tov equation neutron stars deformation 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-4252499","acceptedTermsAndConditions":true,"allowDirectSubmit":true,"archivedVersions":[],"articleType":"Research Article","associatedPublications":[],"authors":[{"id":292939560,"identity":"7659cde2-93c6-45c9-b116-13eabee62e05","order_by":0,"name":"Jonathan Quartuccio","email":"data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAZAAAAAyAQMAAABI0h/eAAAABlBMVEX///8AAABVwtN+AAAACXBIWXMAAA7EAAAOxAGVKw4bAAAA60lEQVRIiWNgGAWjYBACxgZkXgKDDUis8QBRWnggWtLAYni1wAEPhDoMJvFqYW7vPcDwts0u314i+eGHBxXn7da2HwbaUmMTjdNhPecSGOe2JVv2SKQZSyScuZ287UwiUMuxtNwGXFpm5Bgw87YxG/BI5LAxJLbdTjY7ANTC2HCYkJZ6mJZzyWbnHxKl5TBMywE7sxuEbOk5Y3BwzrnjBjxnnoH8kpxgdgNoSwIevxi29xg+eFNWbcDenvzw448KO3uz8+kPH3yoscGtBShxgAdJIBGsMgGHchCQBxHIWuzxKB4Fo2AUjIIRCgAWpl6K9rj00wAAAABJRU5ErkJggg==","orcid":"","institution":"Universidade Cidade de São Paulo","correspondingAuthor":true,"prefix":"","firstName":"Jonathan","middleName":"","lastName":"Quartuccio","suffix":""},{"id":292939561,"identity":"8d972860-0061-4dd9-8fa1-79d1ffcb84ac","order_by":1,"name":"Pedro Moraes","email":"","orcid":"","institution":"Universidade Cidade de São Paulo","correspondingAuthor":false,"prefix":"","firstName":"Pedro","middleName":"","lastName":"Moraes","suffix":""},{"id":292939562,"identity":"1d628eec-af3f-46f3-93b4-dfbc2dd3c445","order_by":2,"name":"José Arbañil","email":"","orcid":"","institution":"Private University of the North","correspondingAuthor":false,"prefix":"","firstName":"José","middleName":"","lastName":"Arbañil","suffix":""}],"badges":[],"createdAt":"2024-04-11 12:42:11","currentVersionCode":1,"declarations":"","doi":"10.21203/rs.3.rs-4252499/v1","doiUrl":"https://doi.org/10.21203/rs.3.rs-4252499/v1","draftVersion":[],"editorialEvents":[],"editorialNote":"","failedWorkflow":false,"files":[{"id":56930281,"identity":"80762b52-7f5b-41b0-9e5e-81eb61c73d27","added_by":"auto","created_at":"2024-05-22 09:33:37","extension":"pdf","order_by":1,"title":"","display":"","copyAsset":false,"role":"manuscript-pdf","size":359153,"visible":true,"origin":"","legend":"","description":"","filename":"hfhzpvxzdrwjrtdwqmcxfwswcgbxydfn.pdf","url":"https://assets-eu.researchsquare.com/files/rs-4252499/v1_covered_26e04b28-c5b1-424c-9530-30d95bd67aad.pdf"}],"financialInterests":"No competing interests reported.","formattedTitle":"Deformed neutron stars","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":"general relativity, tov equation, neutron stars, deformation","lastPublishedDoi":"10.21203/rs.3.rs-4252499/v1","lastPublishedDoiUrl":"https://doi.org/10.21203/rs.3.rs-4252499/v1","license":{"name":"CC BY 4.0","url":"https://creativecommons.org/licenses/by/4.0/"},"manuscriptAbstract":"We present solutions for non-spherically symmetric neutron stars. We begin by deriving the Tolman-Oppenheimer-Volkoff equations from a parameterized metric that takes into account the deformation of the star due to differences in equatorial and polar pressures, expressed in terms of a parameter $\\mathcal{D}$, which is the ratio between polar and equatorial radius. The stellar structure is solved using the GM1 equation of state and the Tolman-Oppenheimer-Volkoff equations for deformed objects are numerically integrated using the fourth-order Runge-Kutta method for different values of the parameter $\\mathcal{D}$. We show that larger values of $\\mathcal{D}\u003e1$, that describe prolate neutron stars, yield smaller values of mass and radius, while for smaller values of $\\mathcal{D}\u003c1$, describing oblate neutron stars, larger values for mass and radius are attained. From the confrontation of our model theoretical predictions with recent observational data on pulsars, it is possible to constrain the values of the parameter $\\mathcal{D}$.\\\\\n\\emph{Keywords}: general relativity; tov equation; neutron stars; deformation","manuscriptTitle":"Deformed neutron stars","msid":"","msnumber":"","nonDraftVersions":[{"code":1,"date":"2024-04-19 19:22:50","doi":"10.21203/rs.3.rs-4252499/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":"88984fc3-495a-4c52-a77f-7a5bcc2e4ac2","owner":[],"postedDate":"April 19th, 2024","published":true,"recentEditorialEvents":[],"rejectedJournal":[],"revision":"","amendment":"","status":"posted","subjectAreas":[],"tags":[],"updatedAt":"2024-05-22T09:25:31+00:00","versionOfRecord":[],"versionCreatedAt":"2024-04-19 19:22:50","video":"","vorDoi":"","vorDoiUrl":"","workflowStages":[]},"version":"v1","identity":"rs-4252499","journalConfig":"researchsquare"},"__N_SSP":true},"page":"/article/[identity]/[[...version]]","query":{"redirect":"/article/rs-4252499","identity":"rs-4252499","version":["v1"]},"buildId":"8U1c8b4HqxoKbykW_rLl7","isFallback":false,"isExperimentalCompile":false,"dynamicIds":[84888],"gssp":true,"scriptLoader":[]}