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Turbulence as a contributor to intermediate energy storage during solar flaresTurbulence is considered as a method for converting the energy observed as mass motions during the impulsive phase into thermal energy observed during the gradual phase of solar flares. The kinetic energy of the large-scale eddies driven by the upflowing material continuously cascades to smaller scale eddies until viscosity is able to convert it into thermal energy. The general properties of steady state, homogeneous, fluid turbulence is a nonmagnetic plasma and the properties of turbulent decay are reviewed. The time-dependent behavior of the velocities and energies observed by the X-Ray Polychromator (XRP) instrument on the SMM during the November 5, 1980 flare are compared with the properties of turbulence. This study indicates that turbulence may play a role in flare energies and may account for a fraction of the total amount of thermal energy observed during the gradual phase. The rate at which the observed flare velocities decrease is consistent with the decay of turbulent energy but may be too rapid to account for the entire time delay between the impulsive and gradual phases.
Document ID
19870044569
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Bornmann, P. L.
(Joint Institute for Laboratory Astrophysics; Colorado, University Boulder; National Solar Observatory, Sunspot, NM, United States)
Date Acquired
August 13, 2013
Publication Date
February 1, 1987
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 313
ISSN: 0004-637X
Subject Category
Solar Physics
Report/Patent Number
AFGL-TR-88-0081
AD-A193884
Accession Number
87A31843
Funding Number(s)
CONTRACT_GRANT: NGL-06-003-057
Distribution Limits
Public
Copyright
Other

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