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dc.contributor.authorVan Doorsselaere, Tom
dc.contributor.authorAntolin, Patrick
dc.contributor.authorYuan, Ding
dc.contributor.authorReznikova, Veronika
dc.contributor.authorMagyar, Norbert
dc.date.accessioned2017-02-13T15:30:12Z
dc.date.available2017-02-13T15:30:12Z
dc.date.issued2016-02-26
dc.identifier.citationVan Doorsselaere , T , Antolin , P , Yuan , D , Reznikova , V & Magyar , N 2016 , ' Forward modeling of EUV and gyrosynchrotron emission from coronal plasmas with FoMo ' , Frontiers in Astronomy and Space Sciences , vol. 3 , 4 . https://doi.org/10.3389/fspas.2016.00004en
dc.identifier.issn2296-987X
dc.identifier.otherPURE: 248969272
dc.identifier.otherPURE UUID: e207b478-89ab-4429-ae7f-4dc56c14d814
dc.identifier.otherBibCode: 2016FrASS...3....4V
dc.identifier.otherScopus: 85079120085
dc.identifier.urihttps://hdl.handle.net/10023/10275
dc.descriptionOdysseus funding (FWO-Vlaanderen), IAPP7/08CHARM (Belspo), GOA-2015-014 (KULeuven), NAOJ Visiting Fellows Program. N Misa PhD student of the FWO-Vlaanderen.en
dc.description.abstractThe FOMO code was developed to calculate the EUV and UV emission from optically thin coronal plasmas. The input data for FOMO consists of the plasma density, temperature and velocity on a 3D grid. This is translated to emissivity on the 3D grid, using CHIANTI data. Then, the emissivity is integrated along the line-of-sight (LOS) to calculate the emergent spectral line for synthetic spectrometer observations. The code also generates the emission channels for synthetic AIA imaging observations. Moreover, the code has been extended to model also the gyrosynchrotron emission from plasmas with a population of non-thermal particles. In this case, also optically thick plasmas may be modeled. The radio spectrum is calculated over a large wavelength range, allowing for the comparison with data from a wide range of radio telescopes.
dc.format.extent9
dc.language.isoeng
dc.relation.ispartofFrontiers in Astronomy and Space Sciencesen
dc.rights© 2016 Van Doorsselaere, Antolin, Yuan, Reznikova and Magyar. This is an open-access article distributed under the terms of the Creative Commons Attribution License (CC BY). The use, distribution or reproduction in other forums is permitted, provided the original author(s) or licensor are credited and that the original publication in this journal is cited, in accordance with accepted academic practice. No use, distribution or reproduction is permitted which does not comply with these terms.en
dc.subjectSolar physicsen
dc.subjectForward modellingen
dc.subjectEUV emissionen
dc.subjectGyrosynchrotron emissionen
dc.subjectRadio emissionen
dc.subjectSolar coronaen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleForward modeling of EUV and gyrosynchrotron emission from coronal plasmas with FoMoen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.3389/fspas.2016.00004
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2016FrASS...3....4Ven


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