Implications of comprehensive nuclear and astrophysics data on the equations of state of neutron star matter

Implications of comprehensive nuclear and astrophysics data on the equations of state of neutron star matter | 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 Implications of comprehensive nuclear and astrophysics data on the equations of state of neutron star matter Sk Md Adil Imam, Tuhin Malik, Constança Providência, B. K. Agrawal This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-4232175/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 The equations of state (EoSs) governing neutron star (NS) matter obtained for both non-relativistic and relativistic mean-field models are systematically confronted with a diverse set of terrestrial data and astrophysical observations within the Bayesian framework. The terrestrial data, spans from bulk properties of finite nuclei to the heavy-ion collisions, constrain the symmetric nuclear matter EoS and the symmetry energy up to twice the saturation density ( ρ 0 = 0.16 fm −3 ). The astrophysical observations encompass the NS radius, the tidal deformability, and the lower bound on maximum mass. Three distinct posterior distributions of EoSs are generated by gradually updating the priors with different constraints: (i) only the maximum NS mass, (ii) incorporating additional terrestrial data, (iii) combining both the terrestrial data and astrophysical observations. These EoS distributions are then compared using the Kullback-Liebler divergence which highlights the significant constraints imposed on the EoSs by the currently available lower bound of NS maximum mass and terrestrial data. The remaining astrophysical observations marginally refine the EoS within the density range ∼ 2-3 ρ 0 . It is observed that the relativistic mean field model yields stiffer EoS around the saturation density, but predict smaller values of the speed of sound and proton fraction in the interior of massive stars. Nuclear Physics Theoretical Astrophysics Full Text Additional Declarations The authors declare no competing interests. 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-4232175","acceptedTermsAndConditions":true,"allowDirectSubmit":true,"archivedVersions":[],"articleType":"Research Article","associatedPublications":[],"authors":[{"id":288488082,"identity":"15b77685-d6ab-4704-be81-d06de766bf13","order_by":0,"name":"Sk Md Adil Imam","email":"data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAZAAAAAyAQMAAABI0h/eAAAABlBMVEX///8AAABVwtN+AAAACXBIWXMAAA7EAAAOxAGVKw4bAAAA7UlEQVRIiWNgGAWjYDACHgYGCQY2CRk2EOcDELOxE6mFB6SFcQZICzNxWkAUAwMzhCSgQ77ndOKNH2UWPHxih59utvm1TZ6PmYHxw8cc3FoMzvZutuw5B3SYdJrZ7dy+24ZtzAzMkjO34dHCz7tNgrcNpCUBqKXnNiNQCxszLx4t8v282yT/grWkf7tt2XPbnqAWhrO926QhtuSY3Wb4cTuRoBaDM2c3W8uA/ZJTdrO34XZyGzNjM16/yPfkbrz5pqxOTn52+rYbP/7ctp3f3nzww0d8DkMBjG1gsoFY9SDwhxTFo2AUjIJRMFIAADoeSobxsBYnAAAAAElFTkSuQmCC","orcid":"https://orcid.org/0000-0003-3308-2615","institution":"Saha Institute of Nuclear Physics, Homi Bhabha National Institute","correspondingAuthor":true,"prefix":"","firstName":"Sk","middleName":"Md Adil","lastName":"I","suffix":"Md"},{"id":288488083,"identity":"be6be68f-27aa-4209-be7a-0552a73dc5ee","order_by":1,"name":"Tuhin Malik","email":"","orcid":"https://orcid.org/0000-0003-2633-5821","institution":"CFisUC, Department of Physics, University of Coimbra","correspondingAuthor":false,"prefix":"","firstName":"Tuhin","middleName":"","lastName":"Malik","suffix":""},{"id":288488084,"identity":"207dabd2-1535-4aa1-b82e-39da4091a9b7","order_by":2,"name":"Constança Providência","email":"","orcid":"https://orcid.org/0000-0001-6464-8023","institution":"CFisUC, Department of Physics, University of Coimbra","correspondingAuthor":false,"prefix":"","firstName":"Constança","middleName":"","lastName":"Providência","suffix":""},{"id":288488085,"identity":"3ee51918-2259-4e49-a7bc-d4b9fb0afaca","order_by":3,"name":"B. 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The terrestrial data, spans \u0026nbsp;from bulk properties of finite nuclei to the heavy-ion collisions, constrain the symmetric nuclear matter EoS and the symmetry energy up to twice the saturation density (\u003cem\u003eρ\u003c/em\u003e\u003csub\u003e0\u003c/sub\u003e= 0.16 fm\u003csup\u003e−3\u003c/sup\u003e). The astrophysical observations encompass the NS radius, the tidal deformability, and the lower bound on maximum mass. Three distinct posterior distributions of EoSs are generated by gradually updating the priors with different constraints: (i) only the maximum NS mass, (ii) incorporating additional terrestrial data, (iii) combining both the terrestrial data and astrophysical observations. These EoS distributions are then compared using the Kullback-Liebler divergence which highlights the significant constraints imposed on the EoSs by the currently available lower bound of NS maximum mass and terrestrial data. The remaining astrophysical observations marginally refine the EoS within the density range ∼ 2-3\u003cem\u003eρ\u003c/em\u003e\u003csub\u003e0\u003c/sub\u003e. It is observed that the relativistic mean field model yields stiffer EoS around the saturation density, but predict smaller values of the speed of sound and proton fraction in the interior of massive stars.\u003c/p\u003e","manuscriptTitle":"Implications of comprehensive nuclear and astrophysics data on the equations of state of neutron star matter","msid":"","msnumber":"","nonDraftVersions":[{"code":1,"date":"2024-04-08 04:01:45","doi":"10.21203/rs.3.rs-4232175/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":"c49c43de-3bfa-4289-ade5-2b51a3d0b499","owner":[],"postedDate":"April 8th, 2024","published":true,"recentEditorialEvents":[],"rejectedJournal":[],"revision":"","amendment":"","status":"posted","subjectAreas":[{"id":30371779,"name":"Nuclear Physics"},{"id":30371780,"name":"Theoretical Astrophysics"}],"tags":[],"updatedAt":"2024-04-08T04:01:45+00:00","versionOfRecord":[],"versionCreatedAt":"2024-04-08 04:01:45","video":"","vorDoi":"","vorDoiUrl":"","workflowStages":[]},"version":"v1","identity":"rs-4232175","journalConfig":"researchsquare"},"__N_SSP":true},"page":"/article/[identity]/[[...version]]","query":{"redirect":"/article/rs-4232175","identity":"rs-4232175","version":["v1"]},"buildId":"qtupq5eGEP_6zYnWcrvyt","isFallback":false,"isExperimentalCompile":false,"dynamicIds":[84888],"gssp":true,"scriptLoader":[]}