?Heated layer? effect in interaction of an interplanetary shock wave with a geomagnetic tail

1993 ◽  
Vol 64 (5) ◽  
pp. 444-448
Author(s):  
P. E. Aleksandrov
Keyword(s):  
Shock Wave ◽  
Interplanetary Shock ◽  
Heated Layer ◽  
Geomagnetic Tail ◽  
Layer Effect ◽  
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

scholarly journals Review of pulse impacts on the magnetospheric oscillations

2015 ◽  
Vol 1 (4) ◽  
pp. 72-81
Author(s):  
Анатолий Гульельми ◽  
Anatol Guglielmi ◽  
Александр Потапов ◽  
Alexander Potapov ◽  
Борис Довбня ◽  
...  
Keyword(s):  
Practical Importance ◽  
Low Frequency ◽  
Oscillatory System ◽  
Interplanetary Shock ◽  
Space Physics ◽  
Near Earth Space ◽  
Oscillatory Systems ◽  
Impulse Action ◽  
Geomagnetic Tail ◽  
Interplanetary Shock Wave

Response of magnetospheric oscillatory systems in the ultra-low-frequency (ULF) range on electromagnetic, mechanical, thermal, and chemical impulse action are overviewed and selectively analyzed. Impulses can occur both inside the magnetosphere (e.g. explosion in the geomagnetic tail, impulsive injection of energetic particles) and outside (e.g. solar flare, interplanetary shock wave, thunderstorm discharge, earthquake, volcanic eruption etc.). We suggest systematics of impulses which is based on geophysics and space physics data and is closely related to the theory of ULF oscillations. The systematics is of cognitive and practical importance, and it allows us to interpret a rich variety of responses of the magnetosphere to impulses of the terrestrial and space origins. The classification principle is selected according to which an impulse type is determined from two criteria such as impulse origin location and character of impulse action on one or another oscillatory system of the magnetosphere. The primary conditions for completeness and validity of division are fulfilled because all possible terms of putting impulses to classes, types and forms are specified, and the terms do not overlap. The classification and introduced nomenclature are helpful because they make possible to systematize common properties and specific features of types and forms of impulses. This is especially important with regard to reaction of the Earth’s plasma sheaths to impulses generated during an earthquake preparation as well as under experimental study of dynamic processes in the near-Earth space. The examples of response of ULF oscillations to impulsive actions are shown. The particular focus is given to review of studies which still are not mentioned in reviews and monographies.

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