He++  behavior on the an interplanetary shock wave 

2021 ◽  
Author(s):  
Olga Sapunova ◽  
Natalia Borodkova ◽  
Yuri Yermolaev ◽  
Georgii Zastenker
Keyword(s):  
Shock Wave ◽  
Relative Density ◽  
Solar Wind Plasma ◽  
Interplanetary Shock ◽  
High Time Resolution ◽  
Plasma Velocity ◽  
Short Term ◽  
Absolute Value ◽  
Interplanetary Shock Wave ◽  
Very High

<p>In our study we analyzing the fine structure of interplanetary shock wave fronts recorded by the BMSW experiment, installed onboard the SPEKTR-R satellite. The high time resolution of the spectrometer (0.031 s for the plasma flux magnitude and direction and 1.5 s for velocity, temperature, and density) makes it possible to study the internal structure of the IPs front.</p><p>BMSW experiment registered 55 IPs waves from 2011 to 2019. For 21 events (where the temperature was not very high), the parameters of twice-ionized helium (He++ or α-particles) - density (absolute value and relative to protons content in the solar wind plasma), velocity, temperature. It is shown that the speed of He++ is slightly less (for about 5%) than the speed of protons, the relative density of He++ rarely exceeds 10%, and the temperature of He++ is about 2 times higher than the temperature of protons.</p><p>On the IPs front, short-term and significant (up to 20%) jumps in the relative density of He++ were detected in several events. No dependence was found between Mms/proton beta and He++ density changing after IPs front. However, we detected that the lower Qbn parameter is, the more the relative density of He++ falls behind the IPs front.</p>

scholarly journals Magnetospheric response of two types in PSc geomagnetic pulsations to interaction with interplanetary shock waves

2018 ◽  
Vol 4 (3) ◽  
pp. 68-83
Author(s):  
Владимир Пархомов ◽  
Vladimir Parhomov ◽  
Наталия Бородкова ◽  
Natalia Borodkova ◽  
Александр Яхнин ◽  
...  
Keyword(s):  
Shock Wave ◽  
Shock Waves ◽  
Electric Field ◽  
Interplanetary Shock ◽  
Resonance Structure ◽  
Geomagnetic Pulsations ◽  
Short Term ◽  
The Earth ◽  
Interplanetary Shock Wave ◽  
Broadband Pulse

Using the June 22, 2015 event as an example, we present new data confirming the presence of a precursor of the sudden magnetic impulse caused by a powerful interplanetary shock wave (ISW). The precursor in the form of a train of oscillations (broadband pulse) with a falling frequency in the range 0.25÷11 Hz with a duration of ~20 s, which had a spectral resonance structure, was recorded globally by a network of induc-tion magnetometers at 18:33:27 UT. No significant phase delays of the signals were detected in four fre-quency bands at widely spaced observatories. It is sug-gested that the impulse can be excited in the Earth — ionosphere waveguide by a pulsed electric field which occurs in the ionosphere due to the short-term impact of ISW on the magnetosphere.

scholarly journals Magnetospheric response of two types in PSc geomagnetic pulsations to interaction with interplanetary shock waves

2018 ◽  
Vol 4 (3) ◽  
pp. 52-66
Author(s):  
Владимир Пархомов ◽  
Vladimir Parhomov ◽  
Наталия Бородкова ◽  
Natalia Borodkova ◽  
Александр Яхнин ◽  
...  
Keyword(s):  
Shock Wave ◽  
Shock Waves ◽  
Electric Field ◽  
Interplanetary Shock ◽  
Resonance Structure ◽  
Geomagnetic Pulsations ◽  
Short Term ◽  
The Earth ◽  
Interplanetary Shock Wave ◽  
Broadband Pulse

Using the June 22, 2015 event as an example, we present new data confirming the presence of a precursor of the sudden magnetic impulse caused by a powerful interplanetary shock wave (ISW). The precursor in the form of a train of oscillations (broadband pulse) with a falling frequency in the range 0.25÷11 Hz with a duration of ~20 s, which had a spectral resonance structure, was recorded globally by a network of induction magnetometers at 18:33:27 UT. No significant phase delays of the signals were detected in four frequency bands at widely spaced observatories. It is suggested that the impulse can be excited in the Earth – ionosphere waveguide by a pulsed electric field which occurs in the ionosphere due to the short-term impact of ISW on the magnetosphere.

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
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