Open AccessAbout the nature of long‐term microflare energy release in solar active regions
Author(s) -
Bogod Vladimir M.,
Mercier Claude,
Yasnov Leonid V.
Publication year - 2001
Publication title -
journal of geophysical research: space physics
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 1.67
H-Index - 298
eISSN - 2156-2202
pISSN - 0148-0227
DOI - 10.1029/2000ja004013
Subject(s) - physics , microburst , flux (metallurgy) , coronal mass ejection , astrophysics , instability , magnetic reconnection , noise (video) , corona (planetary geology) , electron , plasma , geophysics , computational physics , astronomy , solar wind , meteorology , mechanics , wind speed , materials science , wind shear , quantum mechanics , artificial intelligence , astrobiology , computer science , venus , metallurgy , image (mathematics)
In this paper we compare the long‐term impulsive microflares (microbursts (MB) in the range 1000 MHz) using RATAN‐600 observations and impulsive noise storm (NS) emission on frequencies 233 and 164 MHz using Nancay radioheliograph data. It is shown that these processes result from destruction of current sheets at the top of a coronal loop as a result of the development of plasma instability sequences. The coincidence in time between the generation of microbursts and coronal mass ejections is of special interest. The impulses of NS radio emission at meter waves arise after the appearance of the MB at decimeter waves. The temporal parameters of the processes are determined. It is shown that the MB duration is determined by the spreading time of the magnetic flux in the reconnection region along the current sheet. The flux of energy in the form of fast electrons is equal to 9.2 × 10 4 ergs cm −2 s −1 .