{"paper_id":"2e88b46d-554e-4903-9097-c61188949bb6","body_text":"Atypical radio pulsations from magnetar SGR 1935+2154 | 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 Atypical radio pulsations from magnetar SGR 1935+2154 Di Li, P. Wang, Jian Li, Long Ji, Xian Hou, Erbil Gügercinoğlu, and 30 more This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-3148075/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 Magnetars are neutron stars with extremely strong magnetic fields, frequently powering high-energy activity in X-rays 1 . Pulsed radio emission following some X-ray outbursts have been detected 2,3 , albeit its physical origin is unclear. It has long been speculated that the origin of magnetars’ radio signals is different from those from canonical pulsars, although convincing evidence is still lacking. Five months after magnetar SGR 1935+2154’s X-ray outburst and its associated Fast Radio Burst (FRB) 20200428 4,5 , a radio pulsar phase was discovered 6,7 . Here we report the discovery of X-ray spectral hardening associated with the emergence of periodic radio pulsations from SGR 1935+2154 and a detailed analysis of the properties of the radio pulses. The complex radio pulse morphology, which contains both narrow-band emission and frequency drifts, has not been seen before in other magnetars, but is similar to those of repeating FRBs – even though the luminosities are many orders of magnitude different. The observations suggest that radio emission originates from the outer magnetosphere of the magnetar, and the surface heating due to the bombardment of inward-going particles from the radio emission region is responsible for the observed X-ray spectral hardening. Physical sciences/Astronomy and planetary science/Astronomy and astrophysics/Compact astrophysical objects Physical sciences/Astronomy and planetary science/Astronomy and astrophysics/Transient astrophysical phenomena 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-3148075\",\"acceptedTermsAndConditions\":true,\"allowDirectSubmit\":true,\"archivedVersions\":[],\"articleType\":\"Article\",\"associatedPublications\":[],\"authors\":[{\"id\":226520119,\"identity\":\"c8ae2fed-48a4-450a-a9e0-b797c34f5737\",\"order_by\":0,\"name\":\"Di Li\",\"email\":\"data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAZAAAAAyAQMAAABI0h/eAAAABlBMVEX///8AAABVwtN+AAAACXBIWXMAAA7EAAAOxAGVKw4bAAAApklEQVRIiWNgGAWjYDCCw8wNBz6QqIWx4eAM0rQcYGxg5iFJB99xxsbDtjvs5BjYDz/+wFBzh7AWSaDDDueeSTZm4Ekzk2A49oywFgOwljbmxAYJBjMGIJtILZZt9UAt7J8/EK+Fse0wUAuPgQRRWkB+OdjbdtyYjSenTCLhGBFa+M4fPvzhZ1u1HD/78c0fPtQQoQUO2EBEAgkaRsEoGAWjYBTgAQAzoTmNtUm1PgAAAABJRU5ErkJggg==\",\"orcid\":\"https://orcid.org/0000-0003-3010-7661\",\"institution\":\"National Astronomical Observatories, Chinese Academy of Sciences;University of Chinese Academy of Sciences, Beijing 100049, China\",\"correspondingAuthor\":true,\"submittingAuthor\":false,\"prefix\":\"\",\"firstName\":\"Di\",\"middleName\":\"\",\"lastName\":\"Li\",\"suffix\":\"\"},{\"id\":226520120,\"identity\":\"bff4ec97-a7bf-4c4c-ab1b-1b5e89d5cd0c\",\"order_by\":1,\"name\":\"P. 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Niu\",\"email\":\"\",\"orcid\":\"\",\"institution\":\"National Astronomical Observatories, Chinese Academy of Sciences\",\"correspondingAuthor\":false,\"submittingAuthor\":false,\"prefix\":\"\",\"firstName\":\"J.R.\",\"middleName\":\"\",\"lastName\":\"Niu\",\"suffix\":\"\"},{\"id\":226520129,\"identity\":\"5d8cdbdc-d342-4b13-99ce-490c1e4ecd81\",\"order_by\":10,\"name\":\"Weiwei Zhu\",\"email\":\"\",\"orcid\":\"https://orcid.org/0000-0001-5105-4058\",\"institution\":\"Chinese Academy of Sciences\",\"correspondingAuthor\":false,\"submittingAuthor\":false,\"prefix\":\"\",\"firstName\":\"Weiwei\",\"middleName\":\"\",\"lastName\":\"Zhu\",\"suffix\":\"\"},{\"id\":226520130,\"identity\":\"aee45e93-fe56-421a-b996-61188a7f4176\",\"order_by\":11,\"name\":\"Bing Zhang\",\"email\":\"\",\"orcid\":\"https://orcid.org/0000-0002-9725-2524\",\"institution\":\"University of Nevada, Las Vegas\",\"correspondingAuthor\":false,\"submittingAuthor\":false,\"prefix\":\"\",\"firstName\":\"Bing\",\"middleName\":\"\",\"lastName\":\"Zhang\",\"suffix\":\"\"},{\"id\":226520131,\"identity\":\"716091c0-53db-4cfc-8f28-f54aa6fe2d45\",\"order_by\":12,\"name\":\"En-Wei Liang\",\"email\":\"\",\"orcid\":\"\",\"institution\":\"Guangxi University\",\"correspondingAuthor\":false,\"submittingAuthor\":false,\"prefix\":\"\",\"firstName\":\"En-Wei\",\"middleName\":\"\",\"lastName\":\"Liang\",\"suffix\":\"\"},{\"id\":226520132,\"identity\":\"079dcc15-9837-4c68-9953-4807453a9533\",\"order_by\":13,\"name\":\"Li Zhang\",\"email\":\"\",\"orcid\":\"\",\"institution\":\"Yunnan University\",\"correspondingAuthor\":false,\"submittingAuthor\":false,\"prefix\":\"\",\"firstName\":\"Li\",\"middleName\":\"\",\"lastName\":\"Zhang\",\"suffix\":\"\"},{\"id\":226520133,\"identity\":\"8187faf6-b04d-4403-9511-285c7b115ba8\",\"order_by\":14,\"name\":\"Mingyu Ge\",\"email\":\"\",\"orcid\":\"\",\"institution\":\"Institute of High Energy Physics\",\"correspondingAuthor\":false,\"submittingAuthor\":false,\"prefix\":\"\",\"firstName\":\"Mingyu\",\"middleName\":\"\",\"lastName\":\"Ge\",\"suffix\":\"\"},{\"id\":226520134,\"identity\":\"72fb8b86-f188-4bdd-84f5-c38053e6549e\",\"order_by\":15,\"name\":\"Z.G. 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\\u003cb\\u003eNO\\u003c/b\\u003e Competing Interest.\",\"formattedTitle\":\"Atypical radio pulsations from magnetar SGR 1935+2154\",\"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\":\"info@researchsquare.com\",\"identity\":\"researchsquare\",\"isNatureJournal\":false,\"hasQc\":true,\"allowDirectSubmit\":true,\"externalIdentity\":\"\",\"sideBox\":\"\",\"snPcode\":\"\",\"submissionUrl\":\"/submission\",\"title\":\"Research 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Pulsed radio emission following some X-ray outbursts have been detected\\u003csup\\u003e2,3\\u003c/sup\\u003e, albeit its physical origin is unclear. It has long been speculated that the origin of magnetars’ radio signals is different from those from canonical pulsars, although convincing evidence is still lacking. Five months after magnetar SGR 1935+2154’s X-ray outburst and its associated Fast Radio Burst (FRB) 20200428\\u003csup\\u003e4,5\\u003c/sup\\u003e, a radio pulsar phase was discovered\\u003csup\\u003e6,7\\u003c/sup\\u003e. Here we report the discovery of X-ray spectral hardening associated with the emergence of periodic radio pulsations from SGR 1935+2154 and a detailed analysis of the properties of the radio pulses. The complex radio pulse morphology, which contains both narrow-band emission and frequency drifts, has not been seen before in other magnetars, but is similar to those of repeating FRBs – even though the luminosities are many orders of magnitude different. The observations suggest that radio emission originates from the outer magnetosphere of the magnetar, and the surface heating due to the bombardment of inward-going particles from the radio emission region is responsible for the observed X-ray spectral hardening.\\u003c/p\\u003e\",\"manuscriptTitle\":\"Atypical radio pulsations from magnetar SGR 1935+2154\",\"msid\":\"\",\"msnumber\":\"\",\"nonDraftVersions\":[{\"code\":1,\"date\":\"2023-08-16 04:47:59\",\"doi\":\"10.21203/rs.3.rs-3148075/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\":\"f0f1f223-5be9-401f-a18f-01b6ff2f99f0\",\"owner\":[],\"postedDate\":\"August 16th, 2023\",\"published\":true,\"recentEditorialEvents\":[],\"rejectedJournal\":[],\"revision\":\"\",\"amendment\":\"\",\"status\":\"posted\",\"subjectAreas\":[{\"id\":24054617,\"name\":\"Physical sciences/Astronomy and planetary science/Astronomy and astrophysics/Compact astrophysical objects\"},{\"id\":24054618,\"name\":\"Physical sciences/Astronomy and planetary science/Astronomy and astrophysics/Transient astrophysical phenomena\"}],\"tags\":[],\"updatedAt\":\"2025-09-12T12:16:43+00:00\",\"versionOfRecord\":[],\"versionCreatedAt\":\"2023-08-16 04:47:59\",\"video\":\"\",\"vorDoi\":\"\",\"vorDoiUrl\":\"\",\"workflowStages\":[]},\"version\":\"v1\",\"identity\":\"rs-3148075\",\"journalConfig\":\"researchsquare\"},\"__N_SSP\":true},\"page\":\"/article/[identity]/[[...version]]\",\"query\":{\"redirect\":\"/article/rs-3148075\",\"identity\":\"rs-3148075\",\"version\":[\"v1\"]},\"buildId\":\"ApUGefWb6u5IBVtyqm6d5\",\"isFallback\":false,\"isExperimentalCompile\":false,\"dynamicIds\":[84888],\"gssp\":true,\"scriptLoader\":[]}","source_license":"CC-BY-4.0","license_restricted":false}