A Model for Bright Knots in Solar Flare Loops
Spiros Patsourakos Submitted: 2004-06-28 07:32
EUV observations often indicate the presence of bright knots in flare
loops. The temperature of the knot plasma is of order 1MK, and the
knots themselves are usually localized somewhere near the loop tops.
We propose a model in which the formation of EUV knots is due to the
spatial structure of the non-flare active region heating. We present
the results of a series of 1D hydrodynamic, flare-loop simulations,
which include both an impulsive flare heating and a background, active
region heating. The simulations demonstrate that the formation of the
observed knots depends critically on the spatial distribution of the
background heating during the decay phase.
In particular, the heating must be localized
far from the loop apex and
have a magnitude comparable with the local
radiative losses of the cooling loop.
Our results, therefore,
provide strong constraints on both coronal heating and post-flare
Authors: S. Patsourakos, S. K. Antiochos, and J. A. Klimchuk
Publication Status: ApJ (in press)
Last Modified: 2004-06-28 07:32