Evolution of the Nova V906 Carinae progenitor

Evolution of the Nova V906 Carinae progenitor | 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 Evolution of the Nova V906 Carinae progenitor Chatief Kunjaya, Putra Mahasena, Aprilia Aprilia, Satrio Fatkhusalma, and 3 more This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-9228751/v1 This work is licensed under a CC BY 4.0 License Status: Under Review Version 1 posted 4 You are reading this latest preprint version Abstract V906 Carinae erupted as a nova in 2018 and subsequently classified as a moderately fast C-type nova.Observations indicate an orbital period of 1.641 hours, a white dwarf (WD) mass of approximately between 0.71 and 0.73 \((M_\odot)\) , and a donor mass near between 0.25 and 0.43 \((M_\odot)\) . We investigate the evolutionary history of the progenitor system using the MESA binary stellar evolution code in order to identify evolutionary tracks consistent with these observed parameters. Our simulations show that the most plausible post–common-envelope configuration consists of a 0.6 \((M_\odot)\) white dwarf and a 0.5 \((M_\odot)\) donor star. We find that variations in the initial binary parameters have little influence on the donor mass at the observed orbital period but significantly affect the final mass of the white dwarf.This lead to better estimation of the mass of donor star to 0.14 \((M_\odot)\) , while the white dwarf mass consistent with the observation when the system erupted as a nova at period 1.641 hours. Our simulation obtained also a more reasonable donor star temperature of about 3400 K. novae cataclysmic variables stars: individual: V906 Car binaries: close Full Text Additional Declarations No competing interests reported. Cite Share Download PDF Status: Under Review Version 1 posted Reviewers invited by journal 19 Apr, 2026 Editor assigned by journal 03 Apr, 2026 Submission checks completed at journal 02 Apr, 2026 First submitted to journal 25 Mar, 2026 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-9228751","acceptedTermsAndConditions":true,"allowDirectSubmit":false,"archivedVersions":[],"articleType":"Research Article","associatedPublications":[],"authors":[{"id":627176175,"identity":"7f7db6d2-c8d3-47d2-b71c-ddf5e3dc34ae","order_by":0,"name":"Chatief 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progenitor","fulltext":[],"fulltextSource":"","fullText":"","funders":[],"hasAdminPriorityOnWorkflow":false,"hasManuscriptDocX":false,"hasOptedInToPreprint":true,"hasPassedJournalQc":"","hasAnyPriority":false,"hideJournal":false,"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":"astrophysics-and-space-science","isNatureJournal":false,"hasQc":true,"allowDirectSubmit":false,"externalIdentity":"astr","sideBox":"Learn more about [Astrophysics and Space Science](https://www.springer.com/journal/10509)","snPcode":"10509","submissionUrl":"https://submission.nature.com/new-submission/10509/3","title":"Astrophysics and Space Science","twitterHandle":"","acdcEnabled":true,"dfaEnabled":true,"editorialSystem":"em","reportingPortfolio":"Springer Hybrid","inReviewEnabled":true,"inReviewRevisionsEnabled":false},"keywords":"novae, cataclysmic variables, stars: individual: V906 Car, binaries: close","lastPublishedDoi":"10.21203/rs.3.rs-9228751/v1","lastPublishedDoiUrl":"https://doi.org/10.21203/rs.3.rs-9228751/v1","license":{"name":"CC BY 4.0","url":"https://creativecommons.org/licenses/by/4.0/"},"manuscriptAbstract":"\u003cp\u003eV906 Carinae erupted as a nova in 2018 and subsequently classified as a moderately fast C-type nova.Observations indicate an orbital period of 1.641 hours, a white dwarf (WD) mass of approximately between 0.71 and 0.73 \u003cspan class=\"InlineEquation\"\u003e\u003cspan class=\"mathinline\"\u003e\\((M_\\odot)\\)\u003c/span\u003e\u003c/span\u003e, and a donor mass near between 0.25 and 0.43 \u003cspan class=\"InlineEquation\"\u003e\u003cspan class=\"mathinline\"\u003e\\((M_\\odot)\\)\u003c/span\u003e\u003c/span\u003e. We investigate the evolutionary history of the progenitor system using the MESA binary stellar evolution code in order to identify evolutionary tracks consistent with these observed parameters. Our simulations show that the most plausible post\u0026ndash;common-envelope configuration consists of a 0.6 \u003cspan class=\"InlineEquation\"\u003e\u003cspan class=\"mathinline\"\u003e\\((M_\\odot)\\)\u003c/span\u003e\u003c/span\u003e white dwarf and a 0.5 \u003cspan class=\"InlineEquation\"\u003e\u003cspan class=\"mathinline\"\u003e\\((M_\\odot)\\)\u003c/span\u003e\u003c/span\u003e donor star. We find that variations in the initial binary parameters have little influence on the donor mass at the observed orbital period but significantly affect the final mass of the white dwarf.This lead to better estimation of the mass of donor star to 0.14 \u003cspan class=\"InlineEquation\"\u003e\u003cspan class=\"mathinline\"\u003e\\((M_\\odot)\\)\u003c/span\u003e\u003c/span\u003e, while the white dwarf mass consistent with the observation when the system erupted as a nova at period 1.641 hours. Our simulation obtained also a more reasonable donor star temperature of about 3400 K.\u003c/p\u003e","manuscriptTitle":"Evolution of the Nova V906 Carinae progenitor","msid":"","msnumber":"","nonDraftVersions":[{"code":1,"date":"2026-04-27 08:38:23","doi":"10.21203/rs.3.rs-9228751/v1","editorialEvents":[{"type":"communityComments","content":0},{"type":"reviewersInvited","content":"","date":"2026-04-19T14:39:11+00:00","index":"","fulltext":""},{"type":"editorAssigned","content":"","date":"2026-04-03T17:24:42+00:00","index":"","fulltext":""},{"type":"checksComplete","content":"","date":"2026-04-02T15:14:59+00:00","index":"","fulltext":""},{"type":"submitted","content":"Astrophysics and Space Science","date":"2026-03-26T03:34:04+00:00","index":"","fulltext":""}],"status":"published","journal":{"display":true,"email":"[email protected]","identity":"astrophysics-and-space-science","isNatureJournal":false,"hasQc":true,"allowDirectSubmit":false,"externalIdentity":"astr","sideBox":"Learn more about [Astrophysics and Space Science](https://www.springer.com/journal/10509)","snPcode":"10509","submissionUrl":"https://submission.nature.com/new-submission/10509/3","title":"Astrophysics and Space Science","twitterHandle":"","acdcEnabled":true,"dfaEnabled":true,"editorialSystem":"em","reportingPortfolio":"Springer Hybrid","inReviewEnabled":true,"inReviewRevisionsEnabled":false}}],"origin":"","ownerIdentity":"e040a576-b496-453c-a09b-6e15312436d4","owner":[],"postedDate":"April 27th, 2026","published":true,"recentEditorialEvents":[],"rejectedJournal":[],"revision":"","amendment":"","status":"under-review","subjectAreas":[],"tags":[],"updatedAt":"2026-04-27T08:38:23+00:00","versionOfRecord":[],"versionCreatedAt":"2026-04-27 08:38:23","video":"","vorDoi":"","vorDoiUrl":"","workflowStages":[]},"version":"v1","identity":"rs-9228751","journalConfig":"researchsquare"},"__N_SSP":true},"page":"/article/[identity]/[[...version]]","query":{"redirect":"/article/rs-9228751","identity":"rs-9228751","version":["v1"]},"buildId":"XKTyCvWXoU3ODBz1xrDgd","isFallback":false,"isExperimentalCompile":false,"dynamicIds":[84888],"gssp":true,"scriptLoader":[]}