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dc.contributor.authorCallingham, J. R.
dc.contributor.authorVedantham, H. K.
dc.contributor.authorShimwell, T. W.
dc.contributor.authorPope, B. J. S.
dc.contributor.authorDavis, I. E.
dc.contributor.authorBest, P. N.
dc.contributor.authorHardcastle, M. J.
dc.contributor.authorRottgering, H. J. A.
dc.contributor.authorSabater, J.
dc.contributor.authorTasse, C.
dc.contributor.authorWeeren, R. J. van
dc.contributor.authorWilliams, W. L.
dc.contributor.authorZarka, P.
dc.contributor.authorGasperin, F. de
dc.contributor.authorDrabent, A.
dc.date.accessioned2021-10-28T11:45:01Z
dc.date.available2021-10-28T11:45:01Z
dc.date.issued2021-10-11
dc.identifier.citationCallingham , J R , Vedantham , H K , Shimwell , T W , Pope , B J S , Davis , I E , Best , P N , Hardcastle , M J , Rottgering , H J A , Sabater , J , Tasse , C , Weeren , R J V , Williams , W L , Zarka , P , Gasperin , F D & Drabent , A 2021 , ' The population of M dwarfs observed at low radio frequencies ' , Nature Astronomy . https://doi.org/10.1038/s41550-021-01483-0
dc.identifier.issn2397-3366
dc.identifier.otherArXiv: http://arxiv.org/abs/2110.03713v1
dc.identifier.otherORCID: /0000-0001-7315-1596/work/102289358
dc.identifier.urihttp://hdl.handle.net/2299/25158
dc.description© 2021 Springer Nature Limited. This is the accepted manuscript version of an article which has been published in final form at https://doi.org/10.1038/s41550-021-01483-0
dc.description.abstractCoherent low-frequency (≲200 MHz) radio emission from stars encodes the conditions of the outer corona, mass-ejection events and space weather 1–5. Previous low-frequency searches for radio-emitting stellar systems have lacked the sensitivity to detect the general population, instead largely focusing on targeted studies of anomalously active stars 5–9. Here we present 19 detections of coherent radio emission associated with known M dwarfs from a blind flux-limited low-frequency survey. Our detections show that coherent radio emission is ubiquitous across the M dwarf main sequence, and that the radio luminosity is independent of known coronal and chromospheric activity indicators. While plasma emission can generate the low-frequency emission from the most chromospherically active stars of our sample 1,10, the origin of the radio emission from the most quiescent sources is yet to be ascertained. Large-scale analogues of the magnetospheric processes seen in gas giant planets 3,11,12 probably drive the radio emission associated with these quiescent stars. The slowest-rotating stars of this sample are candidate systems to search for star–planet interaction signatures.en
dc.format.extent1670070
dc.language.isoeng
dc.relation.ispartofNature Astronomy
dc.subjectastro-ph.SR
dc.subjectastro-ph.EP
dc.subjectastro-ph.HE
dc.subjectAstronomy and Astrophysics
dc.titleThe population of M dwarfs observed at low radio frequenciesen
dc.contributor.institutionSchool of Physics, Engineering & Computer Science
dc.contributor.institutionSPECS Deans Group
dc.contributor.institutionDepartment of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.date.embargoedUntil2022-03-11
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85116824387&partnerID=8YFLogxK
rioxxterms.versionofrecord10.1038/s41550-021-01483-0
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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