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The Inability of Steady Flow Models to Explain the EUV Coronal Loops View all abstracts by submitter

Spiros Patsourakos   Submitted: 2003-12-03 11:43

Recent observations from TRACE and EIT show that warm (1-1.5 MK) EUV coronal loops in active regions generally have enhanced densities, enhanced pressure scale heights, and flat filter ratio (temperature) profiles in comparison with the predictions of static equilibrium theory. It has been suggested that mass flows may explain these discrepancies. We investigate this conjecture using 1D hydrodynamic simulations of steady flows in coronal loops. The flows are driven by asymmetric heating that decreases exponentially along the loop from one footpoint to the other. We find that a sufficiently large heating asymmetry can produce density enhancements consistent with a sizable fraction of the observed loops, but that the pressure scale heights are smaller than the corresponding gravitational scale heights and that the filter ratio profiles are highly structured, in stark contrast with the observations. We conclude that most warm EUV loops cannot be explained by steady flows. It is thus likely that the heating in these loops is time dependent.

Authors: S. Patsourakos, J. A. Klimchuk & P. J. MacNeice
Projects: None

Publication Status: ApJ (in press)
Last Modified: 2003-12-03 11:43
Go to main E-Print page  Statistical Properties of Flaring and Sub-Flaring Activity in the Solar Atmosphere  On dissipative effects in solar prominences  Edit Entry  Delete Entry 

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