{"paper_id":"0686ca58-c55c-49ef-bc67-8bb2e68ecc98","body_text":"Constraints on maximum neutron star mass from proto-neutron star evolution | 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 Constraints on maximum neutron star mass from proto-neutron star evolution Deepak Kumar, Tuhin Malik, Hiranmaya Mishra, Constan\\c ca Provid\\^encia This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-6757777/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 A proto-neutron star (PNS) gets formed after a successful supernova when the stellar remnant decouples from the ejecta. In this study, we explore a relativistic framework for the finite-temperature $\\beta$-equilibrium limit of equation of state (EOS), constrained via a Bayesian inference methodology. The EOS is constrained by minimal approximations on a few nuclear saturation properties, low-density pure neutron matter constraints from chiral effective field theory, and a neutron star (NS) maximum mass greater than 2.0 $M_{\\odot}$. Two sets of EOS derived from the relativistic mean field model for nucleonic and hyperonic matter constrained by a Bayesian inference calculation at the zero temperature limit are used. The thermal adiabatic index ($\\Gamma_{\\rm Th}$) is calculated as a function of the baryonic density across several temperatures for both the sets. Our results suggest that the maximum NS mass is of the order of 2.15 $M_\\odot$ if hyperons are present. In addition, the present study suggests that an observation of NS with mass larger than $2.2\\ M_{\\odot}$ can indirectly indicates the absence of hyperons in its core. The deleptonization of hyperonic PNS reduces the stellar maximum mass rendering the PNS exceeding the zero temperature maximum stellar (baryonic) mass limit becomes metastable which is prone to collapse into a black hole while PNS below such a mass threshold evolves to a stable NS. Theoretical Astrophysics Neutron star evolution Equation of state 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-6757777\",\"acceptedTermsAndConditions\":true,\"allowDirectSubmit\":true,\"archivedVersions\":[],\"articleType\":\"Research Article\",\"associatedPublications\":[],\"authors\":[{\"id\":462397452,\"identity\":\"58454a70-477f-409f-9f77-bf8f2778181a\",\"order_by\":0,\"name\":\"Deepak Kumar\",\"email\":\"data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAZAAAAAyAQMAAABI0h/eAAAABlBMVEX///8AAABVwtN+AAAACXBIWXMAAA7EAAAOxAGVKw4bAAAA/UlEQVRIiWNgGAWjYDCCAxDCAMz5AKQgLAYJ4rQwziBZCzMPA1wLbsB3vPnYgx9nGIwNrh1+9tmmwCbPnIH34cMfDBZ5uLRInjmWbthzg8HM4Haa8ewcg7RiywZ2Y2MeBoliXFoMbuSYSfB8YLAxuJ1gzJxjcDhxwwE2NmmgXxIbcGm5//6b5B+wlvTPzBYQLew/f+DTcoOHTZoH7LAcY2YGqC0MPHi0SJ5JMzeWOSNhLHk7p5ixB+SXZjZmaR4D3Fr4jh9+9vDNMRvDvtvpmxl+/AGGGHsb48cfFXU4tQABGwNyxCUwMIMdjFs9VAsCJOBVOwpGwSgYBSMSAAC10FWV8ogoXAAAAABJRU5ErkJggg==\",\"orcid\":\"\",\"institution\":\"Institute of Physics, Sachivalaya Marg, Bhubaneswar 751005, India\",\"correspondingAuthor\":true,\"prefix\":\"\",\"firstName\":\"Deepak\",\"middleName\":\"\",\"lastName\":\"Kumar\",\"suffix\":\"\"},{\"id\":462397453,\"identity\":\"f2090182-6c3e-4410-9e76-8f80f59060f3\",\"order_by\":1,\"name\":\"Tuhin Malik\",\"email\":\"\",\"orcid\":\"\",\"institution\":\"FisUC, Department of Physics, University of Coimbra, PT 3004-516 Coimbra, Portugal\",\"correspondingAuthor\":false,\"prefix\":\"\",\"firstName\":\"Tuhin\",\"middleName\":\"\",\"lastName\":\"Malik\",\"suffix\":\"\"},{\"id\":462397454,\"identity\":\"c66c319a-2bbf-4c3e-a44c-aa349c5f2911\",\"order_by\":2,\"name\":\"Hiranmaya Mishra\",\"email\":\"\",\"orcid\":\"\",\"institution\":\"School of Physics, National Institute of Science Education and Research, An OCC of Homi Bhabha National Institute, Jatni - 752050, India\",\"correspondingAuthor\":false,\"prefix\":\"\",\"firstName\":\"Hiranmaya\",\"middleName\":\"\",\"lastName\":\"Mishra\",\"suffix\":\"\"},{\"id\":462397455,\"identity\":\"eb6cc876-c2cf-48ac-aeed-f704c8712f26\",\"order_by\":3,\"name\":\"Constan\\\\c ca Provid\\\\^encia\",\"email\":\"\",\"orcid\":\"\",\"institution\":\"FisUC, Department of Physics, University of Coimbra, PT 3004-516 Coimbra, Portugal\",\"correspondingAuthor\":false,\"prefix\":\"\",\"firstName\":\"Constan\\\\c\",\"middleName\":\"ca\",\"lastName\":\"Provid\\\\^encia\",\"suffix\":\"\"}],\"badges\":[],\"createdAt\":\"2025-05-27 09:24:23\",\"currentVersionCode\":1,\"declarations\":{\"humanSubjects\":false,\"vertebrateSubjects\":false,\"conflictsOfInterestStatement\":false,\"humanSubjectEthicalGuidelines\":false,\"humanSubjectConsent\":false,\"humanSubjectClinicalTrial\":false,\"humanSubjectCaseReport\":false,\"vertebrateSubjectEthicalGuidelines\":false},\"doi\":\"10.21203/rs.3.rs-6757777/v1\",\"doiUrl\":\"https://doi.org/10.21203/rs.3.rs-6757777/v1\",\"draftVersion\":[],\"editorialEvents\":[],\"editorialNote\":\"\",\"failedWorkflow\":false,\"files\":[{\"id\":83571565,\"identity\":\"22b1cc12-836a-4458-9764-754fb0ae82f3\",\"added_by\":\"auto\",\"created_at\":\"2025-05-28 17:07:35\",\"extension\":\"pdf\",\"order_by\":1,\"title\":\"\",\"display\":\"\",\"copyAsset\":false,\"role\":\"manuscript-pdf\",\"size\":1913160,\"visible\":true,\"origin\":\"\",\"legend\":\"\",\"description\":\"\",\"filename\":\"view.pdf\",\"url\":\"https://assets-eu.researchsquare.com/files/rs-6757777/v1_covered_31f5efe7-da24-4f9b-8d0b-4fac1e3d3fcc.pdf\"}],\"financialInterests\":\"The authors declare no competing interests.\",\"formattedTitle\":\"\\u003cp\\u003eConstraints on maximum neutron star mass from proto-neutron star evolution\\u003c/p\\u003e\",\"fulltext\":[],\"fulltextSource\":\"\",\"fullText\":\"\",\"funders\":[],\"hasAdminPriorityOnWorkflow\":false,\"hasManuscriptDocX\":false,\"hasOptedInToPreprint\":true,\"hasPassedJournalQc\":\"\",\"hasAnyPriority\":true,\"hideJournal\":true,\"highlight\":\"\",\"institution\":\"Institute of Physics, Sachivalaya Marg, Bhubaneswar 751005, India\",\"isAcceptedByJournal\":false,\"isAuthorSuppliedPdf\":true,\"isDeskRejected\":\"\",\"isHiddenFromSearch\":false,\"isInQc\":false,\"isInWorkflow\":false,\"isPdf\":true,\"isPdfUpToDate\":true,\"isWithdrawnOrRetracted\":false,\"journal\":{\"display\":true,\"email\":\"info@researchsquare.com\",\"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\":\"Neutron star evolution, Equation of state\",\"lastPublishedDoi\":\"10.21203/rs.3.rs-6757777/v1\",\"lastPublishedDoiUrl\":\"https://doi.org/10.21203/rs.3.rs-6757777/v1\",\"license\":{\"name\":\"CC BY 4.0\",\"url\":\"https://creativecommons.org/licenses/by/4.0/\"},\"manuscriptAbstract\":\"\\u003cp\\u003eA proto-neutron star (PNS) gets formed after a successful supernova when the stellar remnant decouples from the ejecta. In this study, we explore a relativistic framework for the finite-temperature $\\\\beta$-equilibrium limit of equation of state (EOS), constrained via a Bayesian inference methodology. The EOS is constrained by minimal approximations on a few nuclear saturation properties, low-density pure neutron matter constraints from chiral effective field theory, and a neutron star (NS) maximum mass greater than 2.0 $M_{\\\\odot}$. Two sets of EOS derived from the relativistic mean field model for nucleonic and hyperonic matter constrained by a Bayesian inference calculation at the zero temperature limit are used. The thermal adiabatic index ($\\\\Gamma_{\\\\rm Th}$) is calculated as a function of the baryonic density across several temperatures for both the sets. Our results suggest that the maximum NS mass is of the order of 2.15 $M_\\\\odot$ if hyperons are present. In addition, the present study suggests that an observation of NS with mass larger than $2.2\\\\ M_{\\\\odot}$ can indirectly indicates the absence of hyperons in its core. The deleptonization of hyperonic PNS reduces the stellar maximum mass rendering the PNS exceeding the zero temperature maximum stellar (baryonic) mass limit becomes metastable which is prone to collapse into a black hole while PNS below such a mass threshold evolves to a stable NS.\\u003c/p\\u003e\",\"manuscriptTitle\":\"Constraints on maximum neutron star mass from proto-neutron star evolution\",\"msid\":\"\",\"msnumber\":\"\",\"nonDraftVersions\":[{\"code\":1,\"date\":\"2025-05-28 16:59:23\",\"doi\":\"10.21203/rs.3.rs-6757777/v1\",\"editorialEvents\":[{\"type\":\"communityComments\",\"content\":0}],\"status\":\"published\",\"journal\":{\"display\":true,\"email\":\"info@researchsquare.com\",\"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\":\"b4d8d00b-e600-4158-af38-eea9e0550c96\",\"owner\":[],\"postedDate\":\"May 28th, 2025\",\"published\":true,\"recentEditorialEvents\":[],\"rejectedJournal\":[],\"revision\":\"\",\"amendment\":\"\",\"status\":\"posted\",\"subjectAreas\":[{\"id\":49187375,\"name\":\"Theoretical Astrophysics\"}],\"tags\":[],\"updatedAt\":\"2025-05-28T16:59:23+00:00\",\"versionOfRecord\":[],\"versionCreatedAt\":\"2025-05-28 16:59:23\",\"video\":\"\",\"vorDoi\":\"\",\"vorDoiUrl\":\"\",\"workflowStages\":[]},\"version\":\"v1\",\"identity\":\"rs-6757777\",\"journalConfig\":\"researchsquare\"},\"__N_SSP\":true},\"page\":\"/article/[identity]/[[...version]]\",\"query\":{\"redirect\":\"/article/rs-6757777\",\"identity\":\"rs-6757777\",\"version\":[\"v1\"]},\"buildId\":\"8U1c8b4HqxoKbykW_rLl7\",\"isFallback\":false,\"isExperimentalCompile\":false,\"dynamicIds\":[84888],\"gssp\":true,\"scriptLoader\":[]}","source_license":"CC-BY-4.0","license_restricted":false}