Kick bimodality of neutron stars and mode dependence of their parameters

Kick bimodality of neutron stars and mode dependence of their parameters | 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 Kick bimodality of neutron stars and mode dependence of their parameters Anton Lazarev, Sergei Popov This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-9495641/v1 This work is licensed under a CC BY 4.0 License Status: Under Review Version 1 posted 5 You are reading this latest preprint version Abstract Analysis of observational data and theoretical modeling favour a bimodal distribution of the natal velocity kick of neutron stars. For \((\sim200)\) normal isolated radio pulsars with well-determined spin and kinematic parameters, we determine if they belong to the low- or high-velocity mode of the distribution. Our results demonstrate that about 45% belong to the low-velocity mode. We then analyze the differences in the properties of the two sets of pulsars. For some parameters (characteristic ages, distances, and radio luminosities), we see a clear difference between the two modes. However, for these quantities, it can be easily attributed to selection bias. For those parameters that are not a subject of strong selection, such as pulse width, we do not observe any difference. Interestingly, we detect a significant difference in the magnetic field distribution between the two modes. Lower field pulsars ( \((B\lesssim 10^{12})\) G) are overabundant among objects from the low-velocity mode in comparison to the high-velocity one. Among pulsars with low field ( \((\lesssim 10^{11})\) G), we identify only one object from the high-velocity mode of the kick distribution. The origin of this discrepancy is not clear. neutron stars pulsars Full Text Additional Declarations No competing interests reported. Cite Share Download PDF Status: Under Review Version 1 posted Reviewers agreed at journal 28 Apr, 2026 Reviewers invited by journal 27 Apr, 2026 Editor assigned by journal 27 Apr, 2026 Submission checks completed at journal 23 Apr, 2026 First submitted to journal 22 Apr, 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. 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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-9495641","acceptedTermsAndConditions":true,"allowDirectSubmit":false,"archivedVersions":[],"articleType":"Research Article","associatedPublications":[],"authors":[{"id":630956366,"identity":"5c85768c-cffd-41f6-92ee-7e1ef29af238","order_by":0,"name":"Anton Lazarev","email":"data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAZAAAAAyAQMAAABI0h/eAAAABlBMVEX///8AAABVwtN+AAAACXBIWXMAAA7EAAAOxAGVKw4bAAAA+0lEQVRIiWNgGAWjYPACZgY+KEsORBx4QEA1mGCDco3BWhJI0ZLYACLxaeGf3X/wcQGDNQMb+/GHnysqDqfPDzv8EGiLnZxuA3YtEncOMxvPYEhnYONJSJY8c+Zw7sbbaQZALcnGZgdwWHMjmU2ah+Ew0GEJByQb29JyN85OAGk5kLgNhxZ5uBb+h80/G/+lpRvOTv+AV4sBXItEMptkY4NNgrx0Dn5bDG8kGxvzGKTzsEk8Y7NsOGZjuEE6p+BAggFuv8jdSHz4mKfCWo6fP/3xzYYaCXn52embP3yosJPD6X2I8xh4EOwDEBESgHwDKapHwSgYBaNgJAAAh29Wtbsh2IsAAAAASUVORK5CYII=","orcid":"","institution":"Lomonosov Moscow State University","correspondingAuthor":true,"prefix":"","firstName":"Anton","middleName":"","lastName":"Lazarev","suffix":""},{"id":630956367,"identity":"e326e082-c1e4-4b6f-8059-7532792866b2","order_by":1,"name":"Sergei Popov","email":"","orcid":"","institution":"Lomonosov Moscow State University","correspondingAuthor":false,"prefix":"","firstName":"Sergei","middleName":"","lastName":"Popov","suffix":""}],"badges":[],"createdAt":"2026-04-22 11:27:14","currentVersionCode":1,"declarations":"","doi":"10.21203/rs.3.rs-9495641/v1","doiUrl":"https://doi.org/10.21203/rs.3.rs-9495641/v1","draftVersion":[],"editorialEvents":[],"editorialNote":"","failedWorkflow":false,"files":[{"id":108804923,"identity":"70a76619-4250-43ff-9a30-699414807db7","added_by":"auto","created_at":"2026-05-08 15:24:15","extension":"pdf","order_by":1,"title":"","display":"","copyAsset":false,"role":"manuscript-pdf","size":3315515,"visible":true,"origin":"","legend":"","description":"","filename":"Kickbimodalityofneutronstarsandmodedependanceoftheirparameters.pdf","url":"https://assets-eu.researchsquare.com/files/rs-9495641/v1_covered_5aedc01b-6c58-4b24-b28d-f479ae26c9af.pdf"}],"financialInterests":"No competing interests reported.","formattedTitle":"Kick bimodality of neutron stars and mode dependence of their parameters","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":"neutron stars, pulsars","lastPublishedDoi":"10.21203/rs.3.rs-9495641/v1","lastPublishedDoiUrl":"https://doi.org/10.21203/rs.3.rs-9495641/v1","license":{"name":"CC BY 4.0","url":"https://creativecommons.org/licenses/by/4.0/"},"manuscriptAbstract":"\u003cp\u003eAnalysis of observational data and theoretical modeling favour a bimodal distribution of the natal velocity kick of neutron stars. For \u003cspan class=\"InlineEquation\"\u003e\u003cspan class=\"mathinline\"\u003e\\((\\sim200)\\)\u003c/span\u003e\u003c/span\u003e normal isolated radio pulsars with well-determined spin and kinematic parameters, we determine if they belong to the low- or high-velocity mode of the distribution. Our results demonstrate that about 45% belong to the low-velocity mode. We then analyze the differences in the properties of the two sets of pulsars. For some parameters (characteristic ages, distances, and radio luminosities), we see a clear difference between the two modes. However, for these quantities, it can be easily attributed to selection bias. For those parameters that are not a subject of strong selection, such as pulse width, we do not observe any difference. Interestingly, we detect a significant difference in the magnetic field distribution between the two modes. Lower field pulsars (\u003cspan class=\"InlineEquation\"\u003e\u003cspan class=\"mathinline\"\u003e\\((B\\lesssim 10^{12})\\)\u003c/span\u003e\u003c/span\u003e G) are overabundant among objects from the low-velocity mode in comparison to the high-velocity one. Among pulsars with low field (\u003cspan class=\"InlineEquation\"\u003e\u003cspan class=\"mathinline\"\u003e\\((\\lesssim 10^{11})\\)\u003c/span\u003e\u003c/span\u003e G), we identify only one object from the high-velocity mode of the kick distribution. 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