Dual Nature of M Dwarf Star: Auroral Activity Meets Solar-like Bursts

Dual Nature of M Dwarf Star: Auroral Activity Meets Solar-like Bursts | 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 Article Dual Nature of M Dwarf Star: Auroral Activity Meets Solar-like Bursts Xiaofeng Wang, Qichun Liu, Jie Lin, Yuanming Wang, Joshua Pritchard, and 40 more This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-8716749/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 Our current understanding of astrophysical magnetic activity was historically grounded in observations within the solar system, where two separate magnetic activity regimes were first recognized. One is represented by auroral radio emission from magnetized planets, driven by electron cyclotron maser emission within large-scale, closed magnetospheres; the other is typified by the Sun, in which Type II/III radio bursts arise from coronal plasma emission along open magnetic field configurations. However, it remains unresolved whether these two distinct regimes, associated with divergent magnetic geometries, can operate on the same star, limited by both available diagnostic methods and coordinated multi-wavelength coverage. Here we report two sharply distinct forms of optical–radio association from the nearby M-dwarf binary G 9-38, uncovered through periodicity analysis combined with simultaneous radio, optical, and X-ray monitoring. One association arises from auroral activity, with both periodic radio pulses and optical brightening co-modulated on the stellar rotation period. The other association is characterised by the simultaneous occurrence of a fast-drifting, strongly polarized radio burst and an energetic optical flare, providing compelling evidence for a stellar analogue of a solar type III burst. Both forms of activity are localized to the same component, G 9-38A, implying that the auroral and flare-driven coherent radio emission mechanisms can coexist on an M dwarf. These results provide clear evidence that solar type III-like burst can operate within a strongly confined magnetosphere, bridging two traditionally separate regimes of magnetic activity from planets to the Sun. Physical sciences/Astronomy and planetary science/Astronomy and astrophysics/Stars Physical sciences/Astronomy and planetary science/Space physics/Magnetospheric physics Full Text Additional Declarations There is NO Competing Interest. 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-8716749","acceptedTermsAndConditions":true,"allowDirectSubmit":true,"archivedVersions":[],"articleType":"Article","associatedPublications":[],"authors":[{"id":593451332,"identity":"8db8313d-f5b5-4694-88a1-8f476945c18c","order_by":0,"name":"Xiaofeng Wang","email":"data:image/png;base64,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","orcid":"https://orcid.org/0000-0002-7334-2357","institution":"Physics Department and Tsinghua Center for Astrophysics, Tsinghua University, Beijing, 100084, China","correspondingAuthor":true,"prefix":"","firstName":"Xiaofeng","middleName":"","lastName":"Wang","suffix":""},{"id":593451333,"identity":"d3538e43-fe1f-4dde-af76-05d632a3eae6","order_by":1,"name":"Qichun Liu","email":"","orcid":"","institution":"Physics Department and Tsinghua Center for Astrophysics, Tsinghua University","correspondingAuthor":false,"prefix":"","firstName":"Qichun","middleName":"","lastName":"Liu","suffix":""},{"id":593451334,"identity":"f43aba67-91f9-4c2c-ad86-2785bb063b78","order_by":2,"name":"Jie Lin","email":"","orcid":"https://orcid.org/0000-0003-3965-6931","institution":"University of Science and Technology of China","correspondingAuthor":false,"prefix":"","firstName":"Jie","middleName":"","lastName":"Lin","suffix":""},{"id":593451335,"identity":"1cff1a57-7aa5-477a-ab6e-7ccea62c3a52","order_by":3,"name":"Yuanming Wang","email":"","orcid":"https://orcid.org/0000-0003-0203-1196","institution":"Swinburne University of Technology","correspondingAuthor":false,"prefix":"","firstName":"Yuanming","middleName":"","lastName":"Wang","suffix":""},{"id":593451336,"identity":"54226bb0-c08d-446a-b841-604281dd781f","order_by":4,"name":"Joshua Pritchard","email":"","orcid":"","institution":"Australia Telescope National Facility, CSIRO, Space and Astronomy, PO Box 76, Epping, NSW 1710, Australia","correspondingAuthor":false,"prefix":"","firstName":"Joshua","middleName":"","lastName":"Pritchard","suffix":""},{"id":593451337,"identity":"8ad30cb6-95bf-45c8-8aac-2d693a580f37","order_by":5,"name":"Yuzhe Song","email":"","orcid":"","institution":"Swinburne University of Technology","correspondingAuthor":false,"prefix":"","firstName":"Yuzhe","middleName":"","lastName":"Song","suffix":""},{"id":593451338,"identity":"4710d8fa-81ea-482f-a2c0-fdc96350d857","order_by":6,"name":"Andrew Zic","email":"","orcid":"https://orcid.org/0000-0002-9583-2947","institution":"CSIRO Space and Astronomy","correspondingAuthor":false,"prefix":"","firstName":"Andrew","middleName":"","lastName":"Zic","suffix":""},{"id":593451339,"identity":"57efff19-56b6-44c5-b619-e3ed7be995ba","order_by":7,"name":"David Kaplan","email":"","orcid":"https://orcid.org/0000-0001-6295-2881","institution":"University of Wisconsin-Milwaukee","correspondingAuthor":false,"prefix":"","firstName":"David","middleName":"","lastName":"Kaplan","suffix":""},{"id":593451340,"identity":"24434b50-93d2-42f6-90a3-7d51ef8bc3ba","order_by":8,"name":"Shengyu Yan","email":"","orcid":"","institution":"Physics Department and Tsinghua Center for Astrophysics, Tsinghua University","correspondingAuthor":false,"prefix":"","firstName":"Shengyu","middleName":"","lastName":"Yan","suffix":""},{"id":593451341,"identity":"b5df57e3-37a9-4fd0-b076-2f77f7b2de48","order_by":9,"name":"H.-W. 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One is represented by auroral radio emission from magnetized planets, driven by electron cyclotron maser emission within large-scale, closed magnetospheres; the other is typified by the Sun, in which Type II/III radio bursts arise from coronal plasma emission along open magnetic field configurations. However, it remains unresolved whether these two distinct regimes, associated with divergent magnetic geometries, can operate on the same star, limited by both available diagnostic methods and coordinated multi-wavelength coverage. Here we report two sharply distinct forms of optical–radio association from the nearby M-dwarf binary G 9-38, uncovered through periodicity analysis combined with simultaneous radio, optical, and X-ray monitoring. One association arises from auroral activity, with both periodic radio pulses and optical brightening co-modulated on the stellar rotation period. 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