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dc.contributor.authorLlama, Joe
dc.contributor.authorJardine, Moira M.
dc.contributor.authorWood, Kenneth
dc.contributor.authorHallinan, Gregg
dc.contributor.authorMorin, Julien
dc.identifier.citationLlama , J , Jardine , M M , Wood , K , Hallinan , G & Morin , J 2018 , ' Simulating radio emission from low-mass stars ' , Astrophysical Journal , vol. 854 , no. 1 , 7 .
dc.identifier.otherPURE: 252394815
dc.identifier.otherPURE UUID: a4de99fd-e14a-4c26-ba04-e9f1c51af78c
dc.identifier.otherWOS: 000424362100001
dc.identifier.otherScopus: 85042457208
dc.identifier.otherWOS: 000424362100001
dc.identifier.otherORCID: /0000-0002-1466-5236/work/57821855
dc.descriptionM.M.J. acknowledges support from STFC grant ST/M001296/1.en
dc.description.abstractUnderstanding the origins of stellar radio emission can provide invaluable insight into the strength and geometry of stellar magnetic fields and the resultant space weather environment experienced by exoplanets. Here, we present the first model capable of predicting radio emission through the electron cyclotron maser instability using observed stellar magnetic maps of low-mass stars. We determine the structure of the coronal magnetic field and plasma using spectropolarimetric observations of the surface magnetic fields and the X-ray emission measure. We then model the emission of photons from the locations within the corona that satisfy the conditions for electron cyclotron maser emission. Our model predicts the frequency and intensity of radio photons from within the stellar corona. We have benchmarked our model against the low-mass star V374 Peg. This star has both radio observations from the Very Large Array and a nearly simultaneous magnetic map. Using our model we are able to fit the radio observations of V374 Peg, providing additional evidence that the radio emission observed from low-mass stars may originate from the electron cyclotron maser instability. Our model can now be extended to all stars with observed magnetic maps to predict the expected frequency and variability of stellar radio emission in an effort to understand and guide future radio observations of low-mass stars.
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2018. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at:
dc.subjectStars: activityen
dc.subjectStars: individual (V374 Peg)en
dc.subjectStars: low-massen
dc.subjectStars: magnetic fielden
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleSimulating radio emission from low-mass starsen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.description.statusPeer revieweden

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