We have developed a steady-state energy balance model of the solar corona, which calculates coronal magnetic field structure and thermodynamics from a photospheric magnetogram. Our method involves a solution of energy and momentum equations along individual coronal loops, allowing for flows, gravity, non-uniform heating, and cross-sectional area variations. The model yields predicted plasma emissivities which are interpolated to a 3-D grid and used to create synthetic X-ray and EUV emission images. Such images can be generated using different heating approximations and compared with observed coronal images from past and future satellite missions to get observational constraints on coronal heating mechanisms.
|Number of pages||6|
|Journal||European Space Agency, (Special Publication) ESA SP|
|Publication status||Published - 1 Dec 2004|
|Event||SOHO 15 Workshop: Coronal Heating - , United Kingdom|
Duration: 6 Sep 2004 → 9 Sep 2004