Observations of spectral lines of metal, helium and hydrogen in solar flares and prominences show that their profiles contain narrow emission component which corresponds to the very strong magnetic fields (10 3 - 10 4 G) and very low temperatures, approximately an order of magnitude lower than that outside the regions of strong fields (see. eg. Lozitsky V.G. Advances in Space Research, 2015, 55, 958; Lozitsky V.G. et al., Kinematics and Physics of Celestial Bodies., Suppl., 2000, No 3, 449). Because of the limited spectral resolution of observations, the exact value of the lower limit of temperature and the turbulent velocity remains unknown. And what says about this the theory?
please have a look at
Magnetohydrodynamics — Historical Evolution and Trends
S. Molokov, R. Moreau and H. K. Moffatt, Eds.
(Berlin: Springer 2007) pp. 85–115 [E-print: astro-ph/0507686]
for more details
Dear Dr. Nihal Ercan,
thank you very much !
Sincerely,
Vsevolod Lozitsky
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