Exploring Type Iax supernovae observables and progenitors through one-dimensional radiation-hydrodynamics simulations of CO white dwarfs

Exploring Type Iax supernovae observables and progenitors through one-dimensional radiation-hydrodynamics simulations of CO white dwarfs | 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 Exploring Type Iax supernovae observables and progenitors through one-dimensional radiation-hydrodynamics simulations of CO white dwarfs Thomas Zhirui Yang, Dae-Sik Moon This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-5953446/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 Early-time radioactive signals from type Ia supernovae (SNeIa) can provide important constraints on the explosion mechanism and the progenitor system. We investigate whether shock ignition models of Chandresehkar-mass carbon oxygen white dwarf stars in the SD WD-He star scenario can account for observed population of the Type Iax supernovae (SN Iax) explosions. We compute 8 1D full-star radiation-hydrodynamic explosion models (using SNEC) from a WD model accreting pure helium from its helium star companion (using MESA), and compare their synthetic light curves as well as other profiles with that of well-observed real SNe Iax. In addition, we explore how the amount of nickel placed from the core of WD would shape these light curves. We find the 56 Ni shows a directly proportional relationship to peak luminosity, as peak luminosities of some models match to corresponding SNe Iax with calculated nickel masses. We find that synthetic lightcurves of our models predict early time light curves of observed SNe Iax fairly well, while more discrepancies arise after ~40 days after explosion. Which suggests that real SNe Iax has a more efficient γ-ray deposition in later times than models. This is also shown through color light curves, where model with M Ni =0.25M ⊙ has a decline rate of Δm 15 (B)=2.57 mag. Models also predict low-energy SNe better, such as with SN 2023mnc, SN 2019gsc, and SN 2019muj. The photospheric velocity of models reaches a peak kick velocity of ~167000 kms -1 for an E exp =1.63x10 52 erg explosion and then quickly decelerates to stationary at ~15 days. We find that velocity profile of the models shows similar deceleration rate as real SNe Iax and the power law after its been scaled by a factor of 0.1 to match SNe Iax explosion energies. Astrophysics and Cosmology hydrodynamics radiative transfer supernovae general white dwarf 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-5953446","acceptedTermsAndConditions":true,"allowDirectSubmit":true,"archivedVersions":[],"articleType":"Research Article","associatedPublications":[],"authors":[{"id":410713092,"identity":"2900d6de-81ad-4bb7-9c75-b050974cab6a","order_by":0,"name":"Thomas Zhirui Yang","email":"data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAZAAAAAyAQMAAABI0h/eAAAABlBMVEX///8AAABVwtN+AAAACXBIWXMAAA7EAAAOxAGVKw4bAAAArklEQVRIiWNgGAWjYHACxgcf2BgMQCwJotTzMDAwG84gVQubNA9JWuz5zxhI25QdNuZnYD54m4c4W84YGOecO2wm2cCWbE2cFsYeg+TctsM2Bgd4zKSJ08LMY3DYEqjF/gD/NyK1sPEYNjO2HTYzADKJ1HKGrZix51y6scRhNmPLOcRoYe8/vP3HjzJrw/725oc33hCjhYGBwwBCMxOnHGzPA+LVjoJRMApGwcgEAMdhKOUw8BwWAAAAAElFTkSuQmCC","orcid":"","institution":"Duke University","correspondingAuthor":true,"prefix":"","firstName":"Thomas","middleName":"Zhirui","lastName":"Yang","suffix":""},{"id":410713093,"identity":"dde52635-e43c-4935-bc85-86e972868056","order_by":1,"name":"Dae-Sik Moon","email":"","orcid":"","institution":"University of Toronto","correspondingAuthor":false,"prefix":"","firstName":"Dae-Sik","middleName":"","lastName":"Moon","suffix":""}],"badges":[],"createdAt":"2025-02-03 19:32:29","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-5953446/v1","doiUrl":"https://doi.org/10.21203/rs.3.rs-5953446/v1","draftVersion":[],"editorialEvents":[],"editorialNote":"","failedWorkflow":false,"files":[{"id":75469057,"identity":"ae07b907-71b3-4d7c-99fd-df497fd11ac4","added_by":"auto","created_at":"2025-02-05 02:29:23","extension":"pdf","order_by":1,"title":"","display":"","copyAsset":false,"role":"manuscript-pdf","size":2699891,"visible":true,"origin":"","legend":"","description":"","filename":"ExploringTypeIaxsupernovaeobservablesandprogenitorsthroughonedimensionalradiationhydrodynamicssimulationsofCOwhitedwarfs.pdf","url":"https://assets-eu.researchsquare.com/files/rs-5953446/v1_covered_05048b90-1a4a-4364-9aac-4371fa8fe701.pdf"}],"financialInterests":"The authors declare no competing interests.","formattedTitle":"\u003cp\u003eExploring Type Iax supernovae observables and progenitors through one-dimensional radiation-hydrodynamics simulations of CO white dwarfs\u003c/p\u003e","fulltext":[],"fulltextSource":"","fullText":"","funders":[],"hasAdminPriorityOnWorkflow":false,"hasManuscriptDocX":false,"hasOptedInToPreprint":true,"hasPassedJournalQc":"","hasAnyPriority":true,"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":"hydrodynamics, radiative transfer, supernovae, general, white dwarf","lastPublishedDoi":"10.21203/rs.3.rs-5953446/v1","lastPublishedDoiUrl":"https://doi.org/10.21203/rs.3.rs-5953446/v1","license":{"name":"CC BY 4.0","url":"https://creativecommons.org/licenses/by/4.0/"},"manuscriptAbstract":"\u003cp\u003eEarly-time radioactive signals from type Ia supernovae (SNeIa) can provide important constraints on the explosion mechanism and the progenitor system. We investigate whether shock ignition models of Chandresehkar-mass carbon oxygen white dwarf stars in the SD WD-He star scenario can account for observed population of the Type Iax supernovae (SN Iax) explosions. We compute 8 1D full-star radiation-hydrodynamic explosion models (using SNEC) from a WD model accreting pure helium from its helium star companion (using MESA), and compare their synthetic light curves as well as other profiles with that of well-observed real SNe Iax. In addition, we explore how the amount of nickel placed from the core of WD would shape these light curves. We find the \u003csup\u003e56\u003c/sup\u003eNi shows a directly proportional relationship to peak luminosity, as peak luminosities of some models match to corresponding SNe Iax with calculated nickel masses. We find that synthetic lightcurves of our models predict early time light curves of observed SNe Iax fairly well, while more discrepancies arise after ~40 days after explosion. Which suggests that real SNe Iax has a more efficient γ-ray deposition in later times than models. This is also shown through color light curves, where model with M\u003csub\u003eNi\u003c/sub\u003e=0.25M\u003csub\u003e⊙ \u003c/sub\u003ehas a decline rate of Δm\u003csub\u003e15\u003c/sub\u003e(B)=2.57 mag. Models also predict low-energy SNe better, such as with SN 2023mnc, SN 2019gsc, and SN 2019muj. The photospheric velocity of models reaches a peak kick velocity of ~167000 kms\u003csup\u003e-1\u003c/sup\u003e for an E\u003csub\u003eexp\u003c/sub\u003e=1.63x10\u003csup\u003e52 \u003c/sup\u003eerg explosion and then quickly decelerates to stationary at ~15 days. We find that velocity profile of the models shows similar deceleration rate as real SNe Iax and the power law after its been scaled by a factor of 0.1 to match SNe Iax explosion energies.\u0026nbsp;\u003c/p\u003e","manuscriptTitle":"Exploring Type Iax supernovae observables and progenitors through one-dimensional radiation-hydrodynamics simulations of CO white dwarfs","msid":"","msnumber":"","nonDraftVersions":[{"code":1,"date":"2025-02-05 02:21:09","doi":"10.21203/rs.3.rs-5953446/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":"2ec00b70-ef57-4067-a79b-fe60b34885bf","owner":[],"postedDate":"February 5th, 2025","published":true,"recentEditorialEvents":[],"rejectedJournal":[],"revision":"","amendment":"","status":"posted","subjectAreas":[{"id":43789523,"name":"Astrophysics and Cosmology"}],"tags":[],"updatedAt":"2025-02-05T02:21:09+00:00","versionOfRecord":[],"versionCreatedAt":"2025-02-05 02:21:09","video":"","vorDoi":"","vorDoiUrl":"","workflowStages":[]},"version":"v1","identity":"rs-5953446","journalConfig":"researchsquare"},"__N_SSP":true},"page":"/article/[identity]/[[...version]]","query":{"redirect":"/article/rs-5953446","identity":"rs-5953446","version":["v1"]},"buildId":"8U1c8b4HqxoKbykW_rLl7","isFallback":false,"isExperimentalCompile":false,"dynamicIds":[84888],"gssp":true,"scriptLoader":[]}