Forward Models of Solar Soft X-ray Emissions: What Can They Tell Us About Coronal Heating?

Details Forward Models of Solar Soft X-ray Emissions: What Can They Tell Us About Coronal Heating? Forward Models of Solar Soft X-ray Emissions: What Can They Tell Us About Coronal Heating?

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.1703l&link_type=abstract

American Astronomical Society, SPD meeting #37, #17.03; Bulletin of the American Astronomical Society, Vol. 38, p.245

Astronomy and Astrophysics

Astronomy

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Scientific paper

Forward modeling can yield a lot of insight about processes in the solar corona. For the purposes of constraining proposed coronal heating mechanisms, I have developed a forward modeling approach to predict active region coronal emissions, using magnetic field observations at the photosphere as input. First, I calculate a coronal magnetic field and a set of a few thousand magnetic field lines representing it. Next, I treat each field line as a steadily heated coronal loop, with the heating term approximated as a simple parameterized function based on magnetic field properties. Then I use a 1-D energy balance calculation with steady-state flows to solve for loop temperature and density profiles, using different heating parameterizations to simulate different proposed coronal heating mechanisms. After interpolating these thermodynamic variables to a 3-D grid, I then simulate the image expected from a coronal imaging instrument viewing the simulated active region. I compare the observed image to simulated images using different heating mechanisms to see which heating theories best match the observations.I have performed this forward modeling exercise for 10 active regions using four different heating parameterizations. I find significant differences in the predictive accuracy of the four mechanisms, with the best match from a volumetric heating rate that scales proportionally to average loop magnetic field strength and inversely proportional to field line loop length. However, none of the predicted emissions match well with the observed emissions. The mismatch implies that the corona is likely not heated in a steady-state fashion. I gratefully acknowledge funding support from the NASA GSRP program and the DOD solar MURI project at UC Berkeley for completion of this dissertation.

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