Modeling the Radiative Signatures of Turbulent Heating in Coronal Loops

Details Modeling the Radiative Signatures of Turbulent Heating in Coronal Loops Modeling the Radiative Signatures of Turbulent Heating in Coronal Loops

Nov 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006apj...651.1219p&link_type=abstract

The Astrophysical Journal, Volume 651, Issue 2, pp. 1219-1228.

Astronomy and Astrophysics

Astronomy

19

Methods: Statistical, Magnetohydrodynamics: Mhd, Sun: Corona, Sun: Flares, Sun: Uv Radiation, Techniques: Spectroscopic, Turbulence

Scientific paper

The statistical properties of the radiative signature of a coronal loop subject to turbulent heating obtained from a three-dimensional (3D) magnetohydrodynamics (MHD) model are studied. The heating and cooling of a multistrand loop is modeled and synthetic spectra for Fe XII 195.12, Fe XV 284.163, and Fe XIX 1118.06 Å are calculated, covering a wide temperature range. The results show that the statistical properties of the thermal and radiative energies partially reflect those of the heating function in that power-law distributions are transmitted, but with very significant changes in the power-law indices. There is a strong dependence on the subloop geometry. Only high-temperature radiation (~107 K) preserves reasonably precise information on the heating function.

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