Forward modeling of EUV and gyrosynchrotron emission from coronal plasmas with FoMo
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The 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.
Van 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 . DOI: 10.3389/fspas.2016.00004
Frontiers in Astronomy and Space Sciences
© 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.
Odysseus funding (FWO-Vlaanderen), IAPP7/08CHARM (Belspo), GOA-2015-014 (KULeuven), NAOJ Visiting Fellows Program. N Misa PhD student of the FWO-Vlaanderen.
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