The form and energy of the shock waves from the solar flares of August 2, 4, and 7, 1972

1978 ◽  
Vol 83 (A3) ◽  
pp. 1035 ◽  
Author(s):  
G. N. Zastenker ◽  
V. V. Temny ◽  
C. D'Uston ◽  
J. M. Bosqued
Keyword(s):  
Shock Waves ◽  
Solar Flares

On Proton and Electron Acceleration by Shock Waves during Large Solar Flares

1978 ◽  
Vol 3 (3) ◽  
pp. 236-238
Author(s):  
V. M. Gubchenko ◽  
V. V. Zaitsev
Keyword(s):  
Shock Waves ◽  
Total Energy ◽  
Satisfactory Agreement ◽  
Solar Flares ◽  
Interplanetary Medium ◽  
Thermal Processes ◽  
Proton Acceleration ◽  
X Ray ◽  
Target Model ◽  
Γ Ray

Lin and Hudson (1976) have recently analysed non-thermal processes in proton flares, using observations of a series of major events in August 1972. They concluded that the 10–100 keV electrons accelerated during the flash phase account for the bulk of the total energy of a large proton flare (about 1032 – 1033 ergs); that most protons are accelerated later than the 10 — 100 keV electrons; and that most energetic protons escape to the interplanetary medium. Their conclusions with regard to proton acceleration are supported firstly by the delay of the maximum of γ-ray emission by 3-5 minutes after the maximum of X-ray emission, and secondly by the satisfactory agreement between the 7-ray spectrum and the thin-target model of emission. The energetic protons contain a very small fraction of the total flare energy (of the order of 10-5).

Formation of fast magnetosonic shock waves during a two-current-loop collision in solar flares

Solar Physics ◽  
1994 ◽  
Vol 151 (1) ◽  
pp. 137-145 ◽  
Author(s):  
Shinji Koide ◽  
Jun-Ichi Sakai
Keyword(s):  
Shock Waves ◽  
Solar Flares ◽  
Current Loop

scholarly journals Radio Data and Computer Simulations for Shock Waves Generated by Solar Flares

1980 ◽  
Vol 91 ◽  
pp. 251-255
Author(s):  
Alan Maxwell ◽  
Murray Dryer
Keyword(s):  
Shock Waves ◽  
Solar Corona ◽  
Computer Simulations ◽  
Solar Flares ◽  
Solar Radio ◽  
Radio Bursts ◽  
Type Ii ◽  
Fast Mode ◽  
Solar Radio Bursts ◽  
Radio Data

Solar radio bursts of spectral type II provide a prime diagnostic for the passage of shock waves, generated by solar flares, through the solar corona. In this investigation we have compared radio data on the shocks with computer simulations for the propagation of fast-mode MHD shocks through the solar corona. The radio data were recorded at the Harvard Radio Astronomy Station, Fort Davis, Texas. The computer simulations were carried out at NOAA, Boulder, Colorado.

scholarly journals Shock Waves and Plasma Ejection: Corpuscular and Interplanetary Evidence

1974 ◽  
Vol 57 ◽  
pp. 361-363
Author(s):  
A. J. Hundhausen
Keyword(s):  
Shock Waves ◽  
Solar Flares ◽  
Interplanetary Space ◽  
Space Exploration ◽  
Cosmic Ray ◽  
Geomagnetic Disturbances ◽  
The Past ◽  
Solar Material

The ejection of rapidly-moving solar material into interplanetary space in association with solar flares has been discussed since 1859, when geomagnetic disturbances and auroral displays followed shortly after the first observation of a flare by Carrington and Hodgson. Until the advent of in situ interplanetary observations in the early 1960's, such discussions were based upon the indirect information regarding interplanetary space that could be inferred from geomagnetic or cosmic ray data. The past decade of space exploration has provided a great deal of direct information regarding the interplanetary effects of solar flares and some quantitative implications regarding the nature of transient coronal disturbances.

scholarly journals Solar flares and coronal shock waves

2001 ◽  
Vol 106 (A11) ◽  
pp. 25291-25300 ◽  
Author(s):  
Bojan Vršnak
Keyword(s):  
Shock Waves ◽  
Solar Flares ◽  
Coronal Shock

scholarly journals Type II Solar Radio Bursts in the Decimeter Band

1974 ◽  
Vol 57 ◽  
pp. 343-343
Author(s):  
Alan Maxwell
Keyword(s):  
Shock Waves ◽  
Solar Flares ◽  
Radio Bursts ◽  
Type Ii ◽  
Solar Radio Bursts ◽  
Lower Corona ◽  
Previous Discussion ◽  
Radio Equipment ◽  
Interplanetary Plasma ◽  
Radio Band

(Solar Phys.) The progress of shock waves generated by solar flares through the corona is delineated in the radio band by radio bursts of spectral type II. Previous discussion of these bursts has been mainly concerned with their characteristics at frequencies below 200 MHz. This paper discusses the characteristics of the bursts in the range 2000–200 MHz, and the information that may then be deduced about the propagation of shock waves through the lower corona. Particular attention is paid to the type II burst emitted by the flare of 1972 August 7, 1500 UT. The shock from this flare was subsequently tracked (by radio equipment on the IMP-6 satellite) through the interplanetary plasma right to the Earth.

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