Temporal variation of 2D multi-parameter fields of a post-flare loop system

New Astronomy ◽  
2003 ◽  
Vol 8 (5) ◽  
pp. 427-437 ◽  
Author(s):  
X.M. Gu ◽  
J.P. Dun ◽  
S.H. Zhong
Keyword(s):  
Temporal Variation ◽  
Loop System ◽  
Flare Loop

Kinematics of a System of Loop Prominences

1979 ◽  
Vol 44 ◽  
pp. 237-241 ◽  
Author(s):  
O. Engvold ◽  
E. Jensen ◽  
B.N. Andersen
Keyword(s):  
Loop System ◽  
Mass Motion ◽  
Flare Loop ◽  
Doppler Effects ◽  
Rare Phenomena ◽  
True Mass

A detailed description of the development of loops connected with flares has been given by Bruzek (1964). Data on true mass motion as inferred from Doppler-effects are sparse in the literature as flare loop prominences are rare phenomena (Kleczek 1965). Jefferies and Orrall (1965) reported high velocities near the top of a loop system. Gurtovenko et al. (1969) observed large Doppler velocities in the loop system of July 11th. 1966.

scholarly journals RE-FLARING OF A POST-FLARE LOOP SYSTEM DRIVEN BY FLUX ROPE EMERGENCE AND TWISTING

2010 ◽  
Vol 716 (1) ◽  
pp. L68-L73 ◽  
Author(s):  
X. Cheng ◽  
M. D. Ding ◽  
Y. Guo ◽  
J. Zhang ◽  
J. Jing ◽  
...  
Keyword(s):  
Flux Rope ◽  
Loop System ◽  
Flare Loop

The H?-cyclonic spectra of a flare loop system on 1981 April 27

Solar Physics ◽  
1983 ◽  
Vol 87 (1) ◽  
pp. 155-164 ◽  
Author(s):  
X. M. Gu ◽  
B. S. Li ◽  
Y. J. Ding ◽  
S. C. Li ◽  
Z. Li
Keyword(s):  
Loop System ◽  
Flare Loop

scholarly journals Two-dimensional multi-parameter fields of a limb flare loop system

2001 ◽  
Vol 380 (2) ◽  
pp. 704-713 ◽  
Author(s):  
X. M. Gu ◽  
J. P. Dun ◽  
S. H. Zhong
Keyword(s):  
Loop System ◽  
Two Dimensional ◽  
Flare Loop ◽  
Limb Flare

Interpretation of Magnetic Field Structures of AR 6659 in June 7-10, 1991

1994 ◽  
Vol 144 ◽  
pp. 201-205
Author(s):  
S. T. Wu ◽  
F. S. Weng ◽  
M. J. Hagyard ◽  
M. Machado ◽  
B. Schmieder
Keyword(s):  
Magnetic Field ◽  
Magnetic Energy ◽  
Loop System ◽  
Coronal Loops ◽  
Vector Magnetic Field ◽  
Flare Loop ◽  
Magnetic Field Data ◽  
Magnetic Structures ◽  
Free Model ◽  
System Configurations

AbstractWe examine the magnetic structures in AR 6659 by using the observatibn of vector magnetic fields obtained at Marshall Space Flight Center/National Aeronautics and Space Administration (MSFC/NASA). Using these vector magnetic field data as the input for the non-linear force-free model developed by Wuet al.(1990), the structure of coronal loops is revealed. The results obtained include: (i) loop system configurations and (ii) current distributions for AR 6659 during the period 1991 June 7-11. In addition, we also computed the total magnetic energy vs time of this region. It shows that there is indeed enough energy to propel the numerous, energetic flares that were observed in this region. It also revealed that the flare loop system corresponds to the two-ribbon flare on 1991 June 9.

scholarly journals Evolution of an eruptive flare loop system

2009 ◽  
Vol 498 (3) ◽  
pp. 901-907 ◽  
Author(s):  
P. Romano ◽  
F. Zuccarello ◽  
L. Fletcher ◽  
F. Rubio da Costa ◽  
H. M. Bain ◽  
...  
Keyword(s):  
Loop System ◽  
Flare Loop

Space and Time Distribution of Hard X-Ray Emission in a Loop at the Beginning of a Flare

1994 ◽  
Vol 144 ◽  
pp. 275-277
Author(s):  
M. Karlický ◽  
J. C. Hénoux
Keyword(s):  
Time Distribution ◽  
Electron Bombardment ◽  
Spatial Evolution ◽  
Superthermal Electrons ◽  
Flare Loop ◽  
X Ray ◽  
Superthermal Electron ◽  
Flare Loops ◽  
Chromospheric Evaporation ◽  
Temporal And Spatial

AbstractUsing a new ID hybrid model of the electron bombardment in flare loops, we study not only the evolution of densities, plasma velocities and temperatures in the loop, but also the temporal and spatial evolution of hard X-ray emission. In the present paper a continuous bombardment by electrons isotropically accelerated at the top of flare loop with a power-law injection distribution function is considered. The computations include the effects of the return-current that reduces significantly the depth of the chromospheric layer which is evaporated. The present modelling is made with superthermal electron parameters corresponding to the classical resistivity regime for an input energy flux of superthermal electrons of 109erg cm−2s−1. It was found that due to the electron bombardment the two chromospheric evaporation waves are generated at both feet of the loop and they propagate up to the top, where they collide and cause temporary density and hard X-ray enhancements.

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