Forward modeling of EUV and gyrosynchrotron emission from coronal plasmas with FoMo

Tom Van Doorsselaere, Patrick Antolin, Ding Yuan, Veronika Reznikova, Norbert Magyar

Research output: Contribution to journalArticlepeer-review

63 Citations (Scopus)


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.
Original languageEnglish
Article number4
Number of pages9
JournalFrontiers in Astronomy and Space Sciences
Publication statusPublished - 26 Feb 2016


  • Solar physics
  • Forward modelling
  • EUV emission
  • Gyrosynchrotron emission
  • Radio emission
  • Solar corona


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