scholarly journals Energetic Particle Abundances as Probes of an Interplanetary Shock Wave

2002 ◽  
Vol 575 (1) ◽  
pp. L37-L39 ◽  
Author(s):  
D. V. Reames ◽  
A. J. Tylka
Keyword(s):  
Shock Wave ◽  
Energetic Particle ◽  
Interplanetary Shock ◽  
Interplanetary Shock Wave

scholarly journals Nonthermal Processes in Large Solar Flares

1975 ◽  
Vol 68 ◽  
pp. 425-426
Author(s):  
H. S. Hudson ◽  
T. W. Jones ◽  
R. P. Lin
Keyword(s):  
Shock Wave ◽  
Solar Flares ◽  
Interplanetary Medium ◽  
Interplanetary Shock ◽  
Energy Output ◽  
Shock Acceleration ◽  
List Type ◽  
Lower Corona ◽  
X Ray ◽  
Interplanetary Shock Wave

SummaryIn many small solar flares the ∼10–100 keV electrons accelerated during the flash phase contain the bulk of the total flare energy output. In large flares, such as those in the period 1972, August 2–7, the flash phase electrons are present in substantially greater numbers. These electrons can explosively heat the chromosphere-lower corona and eject flare material. The ejected matter can produce a shock wave which will then accelerate nucleons and electrons to relativistic energies. We analyze energetic particle, radio, X-ray, gamma ray and interplanetary shock observations of the 1972 August flares to obtain quantitative estimates of the energy contained in each facet of these large flares. In general these observations are consistent with the above hypothesis. In particular: (1)From the X-ray emission (van Beek et al., 1973) the energy contained in >25 keV electrons is calculated to be 2 × 1032 erg for the 1972, August 4 event. Since the lower energy cutoff to the electron spectrum is known to be below 25 keV and possibly below 10 keV, the electrons contain enough energy to produce the following interplanetary shock wave, which has by far the bulk of the energy dissipated in the flare. Similar numbers are obtained for the large August 7 flare event.(2)From the γ-ray emission (Chupp et al., 1973) the energy in protons dumped at the same level of the atmosphere, assuming a thick target situation, is at least a factor of three smaller than the electrons. Moreover the γ-ray emission indicates that the bulk of the protons are accelerated at least several minutes after the electrons. Thus it is more likely that the electrons are responsible for the flare optical (Hα and white light) emissions which occur in the chromosphere.(3)Approximately 5% of the electrons and 99% of the protons escape into the interplanetary medium to be observed by spacecraft. This situation is consistent with the hypothesis of shock acceleration of the protons high in the solar corona.(4)The four most intense X-ray bursts observed during the period July 31–August 11 are the only bursts followed by an interplanetary shock wave and a new injection of energetic protons into the interplanetary medium.

Singly-ionized helium in the driver gas of an interplanetary shock wave

1980 ◽  
Vol 7 (3) ◽  
pp. 201-204 ◽  
Author(s):  
Rainer Schwenn ◽  
Helmut Rosenbauer ◽  
Karl-Heinz Mühlhäuser
Keyword(s):  
Shock Wave ◽  
Interplanetary Shock ◽  
Driver Gas ◽  
Interplanetary Shock Wave
Sign in / Sign up

Export Citation Format

Share Document