Energy and Mass Supply in the Decay Phase of Long-Duration Solar Flare Events

2002 ◽  
Vol 567 (1) ◽  
pp. L85-L87 ◽  
Author(s):  
Kiyoto Shibasaki
Keyword(s):  
Solar Flare ◽  
Decay Phase ◽  
Long Duration

scholarly journals On the Thermalisation of Flare-Time Energetic Electrons Observed at Radio and X-Ray Wavelengths

1980 ◽  
Vol 91 ◽  
pp. 223-226
Author(s):  
S. S. Degaonkar ◽  
H. S. Sawant ◽  
R. V. Bhonsle
Keyword(s):  
Solar Flare ◽  
Energetic Electrons ◽  
Gradual Rise ◽  
X Ray ◽  
Slow Decay ◽  
Microwave Burst ◽  
Long Duration ◽  
Microwave Bursts

An interesting microwave event at 2800 MHz was recorded at Ahmedabad on September 19, 1977 at 1026 UT at the same time as the H-Alpha solar flare of importance 3B. The microwave burst was of impulsive nature, with as many as twenty impulses in seventy minutes with a quasi-periodicity of 1 to 5 minutes. An X-ray burst recorded by GOES Satellite in 1-8A band showed at the same time a smooth soft X-ray profile with apparently no sign of hard X-ray bursts. This indicates that the acceleration of discrete electron streams which produced impulsive microwave bursts was not sufficient to produce the hard X-ray component but got thermalised to produce soft X-ray emission, with a gradual rise and a slow decay covering a long duration of more than 2 1/2 hours.

scholarly journals Observation of Reconnection Inflow of a Solar Flare

2001 ◽  
Vol 203 ◽  
pp. 344-346
Author(s):  
T. Yokoyama ◽  
K. Akita ◽  
T. Morimoto ◽  
K. Inoue ◽  
J. Newmark
Keyword(s):  
Mach Number ◽  
Solar Flare ◽  
Magnetic Reconnection ◽  
Reconnection Rate ◽  
X Ray ◽  
North East ◽  
The North ◽  
Upper Limit ◽  
Long Duration ◽  
East Limb

We find an important piece of evidence for magnetic reconnection inflow in a flare on March 18, 1999. The flare occurred on the north-east limb, displaying a nice cusp-shaped soft X-ray loop and a plasmoid ejection typical for the long-duration-events. As the plasmoid is ejected, magnetic reconnection occurs at the disconnecting point. A clear ingoing pattern toward the magnetic X-point is seen. The velocity of this apparent motion is about 5 km sec−1, which is an upper limit on reconnection inflow speed. Based on this observation, we derive the reconnection rate as MA = 0.001 − 0.03, where MA is a Alfvén Mach number of the inflow.

scholarly journals Eruption of a Twisted Filament and Associated Phenomena

1998 ◽  
Vol 167 ◽  
pp. 338-341
Author(s):  
Wahab Uddin ◽  
V.K. Verma
Keyword(s):  
Solar Flare ◽  
Geomagnetic Storms ◽  
Magnetic Energy ◽  
Radio Bursts ◽  
X Ray ◽  
Filament System ◽  
Long Duration ◽  
Major Flare ◽  
Ccd Observations ◽  
Microwave Bursts

AbstractIn this paper we present CCD observations between February 14–20, 1994 and analysis of the giant twisted filament evolved in the active region NOAA 7671. The dynamic eruption of the filament was accompanied by a major flare (3B/M4), CME, long duration type II, IV radio bursts, great microwave bursts, a long duration soft X-ray burst, SIDs, strong geomagnetic storms and a very energetic proton flare. We analysed and estimated the twist, length, volume, mass and energy associated with filament system between February 14 and 20, 1994. The present study shows that the magnetic energy required for the solar flare came from the filament system associated with the solar flare and associated phenomena.

scholarly journals The escape of trapped electrons in the decay phase of solar flare

2012 ◽  
Vol 8 (S294) ◽  
pp. 153-154
Author(s):  
Jing Huang
Keyword(s):  
Solar Flare ◽  
Solar Flares ◽  
Pitch Angle ◽  
Escape Rate ◽  
Decay Phase ◽  
Coulomb Collision ◽  
Energetic Electrons ◽  
Trapped Electrons ◽  
Flare Loops ◽  
Angle Scattering

AbstractFrom the observations of radio and HXR bursts, the escape rate of energetic electrons trapped in the flare loops is studied based on the trap-plus-precipitation model for the kinematics of energetic electrons in solar flares. Coulomb collision is regarded as the main pitch angle scattering of trapped electrons in the decay phase of the event on 2004 December 1. The escape rate of trapped electrons decreases firstly and then increases, which indicates the evolution of the plasma density in the flare loops during the decay phase.

Long Duration Solar Flare Events and Cosmic Ray Modulation (1969-1992)

1994 ◽  
Vol 144 ◽  
pp. 499-502
Author(s):  
A. Antalová ◽  
K. Kudela ◽  
D. Venkatesan ◽  
J. Rybák
Keyword(s):  
Solar Cycle ◽  
Solar Flare ◽  
Solar Flares ◽  
Cosmic Ray ◽  
Flare Activity ◽  
Cosmic Ray Intensity ◽  
Cosmic Ray Modulation ◽  
Long Duration ◽  
Flare Index ◽  
Galactic Cosmic Ray

AbstractWe present here the results of the correlation analysis between the galactic cosmic ray intensity decrease p (as observed on Calgary neutron monitor station) and the occurence of SXR long-lasting (LDE-type) solar flares, represented by the LDE-type flare index FI. It is shown, that for the solar cycle with the lower monthly values of FI (the 21-st solar cycle) the correlation coefficient is slighter (about 0.4) comparing to the cycles with the higher LDE-type flare activity (about 0.6, in the 20-th and the 22-nd cycles).

A Long-Duration Solar Flare with Mass Ejection and Global Consequences

1996 ◽  
Vol 470 ◽  
pp. 629 ◽  
Author(s):  
H. S. Hudson ◽  
L. W. Acton ◽  
S. L. Freeland
Keyword(s):  
Solar Flare ◽  
Long Duration ◽  
Mass Ejection

Cosmic ray anisotropies observed late in the decay phase of solar flare events

Solar Physics ◽  
1974 ◽  
Vol 38 (1) ◽  
pp. 227-256 ◽  
Author(s):  
F. R. Allum ◽  
R. A. R. Palmeira ◽  
K. G. McCracken ◽  
U. R. Rao ◽  
D. H. Fairfield ◽  
...  
Keyword(s):  
Solar Flare ◽  
Cosmic Ray ◽  
Decay Phase

The decay phase of solar flare events

Solar Physics ◽  
1971 ◽  
Vol 18 (1) ◽  
pp. 100-132 ◽  
Author(s):  
K. G. McCracken ◽  
U. R. Rao ◽  
R. P. Bukata ◽  
E. P. Keath
Keyword(s):  
Solar Flare ◽  
Decay Phase
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