Using synthetic emission images to constrain heating parameters

L. L. Lundquist*, G. H. Fisher, J. M. McTiernan, Stephane Régnier

*Corresponding author for this work

Research output: Contribution to journalConference articlepeer-review

12 Citations (Scopus)


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.

Original languageEnglish
Pages (from-to)306-311
Number of pages6
JournalEuropean Space Agency, (Special Publication) ESA SP
Issue number575
Publication statusPublished - 1 Dec 2004
EventSOHO 15 Workshop: Coronal Heating - , United Kingdom
Duration: 6 Sept 20049 Sept 2004


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