Linking computational models to follow the evolution of heated coronal plasma

Jack Reid*, Peter Cargill, Craig David Johnston, Alan William Hood

*Corresponding author for this work

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A ‘proof of principle’ is presented, whereby the Ohmic and viscous heating determined by a three-dimensional (3D) MHD model of a coronal avalanche are used as the coronal heating input for a series of field-aligned, one-dimensional (1D) hydrodynamic models. Three-dimensional coronal MHD models require large computational resources. For current numerical parameters, it is difficult to model both the magnetic field evolution and the energy transport along field lines for coronal temperatures much hotter than 1MK⁠, because of severe constraints on the time step from parallel thermal conduction. Using the 3D MHD heating derived from a simulation and evaluated on a single field line, the 1D models give coronal temperatures of 1MK and densities 1014--1015m−3 for a coronal loop length of 80Mm⁠. While the temperatures and densities vary smoothly along the field lines, the heating function leads to strong asymmetries in the plasma flows. The magnitudes of the velocities in the 1D model are comparable with those seen in 3D reconnection jets in our earlier work. Advantages and drawbacks of this approach for coronal modelling are discussed.
Original languageEnglish
Pages (from-to)4141-4150
Number of pages10
JournalMonthly Notices of the Royal Astronomical Society
Issue number3
Early online date4 May 2021
Publication statusPublished - Aug 2021


  • Sun: corona
  • Sun: magnetic fields
  • Magnetohydrodynamics (MHD)
  • Methods: numerical


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