Statistical study of low-frequency magnetic field fluctuations near Venus during the solar cycle

2017 ◽  
Vol 122 (8) ◽  
pp. 8409-8418 ◽  
Author(s):  
S. D. Xiao ◽  
T. L. Zhang ◽  
G. Q. Wang
Keyword(s):  
Magnetic Field ◽  
Solar Cycle ◽  
Statistical Study ◽  
Low Frequency ◽  
Frequency Magnetic Field ◽  
Field Fluctuations

Wavelet analysis of low frequency magnetic field fluctuations in the Jupiter’s magnetotail

2021 ◽  
Author(s):  
Mariza Pereira de Souza Echer ◽  
Ezequiel Echer ◽  
Margarete Oliveira Domingues ◽  
Odim Mendes ◽  
Rodrigo Takeshi Seo ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Wavelet Analysis ◽  
Low Frequency ◽  
Frequency Magnetic Field ◽  
Field Fluctuations

Effect of Low-Frequency Magnetic Field Fluctuations on the Confinement of Plasma in the Uragan-3M Torsatron at Rare Collision Frequencies

2019 ◽  
Vol 64 (1) ◽  
pp. 47-55 ◽  
Author(s):  
V. K. Pashnev ◽  
E. L. Sorokovoy ◽  
A. A. Petrushenya ◽  
F. I. Ozherel’ev
Keyword(s):  
Magnetic Field ◽  
Low Frequency ◽  
Frequency Magnetic Field ◽  
Field Fluctuations

scholarly journals Low-frequency magnetic field fluctuations in Venus' solar wind interaction region: Venus Express observations

2010 ◽  
Vol 28 (4) ◽  
pp. 951-967 ◽  
Author(s):  
L. Guicking ◽  
K.-H. Glassmeier ◽  
H.-U. Auster ◽  
M. Delva ◽  
U. Motschmann ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Low Frequency ◽  
Interaction Region ◽  
Wave Intensity ◽  
Bow Shock ◽  
Solar Wind Interaction ◽  
Frequency Magnetic Field ◽  
Field Fluctuations ◽  
Wave Properties

Abstract. We investigate wave properties of low-frequency magnetic field fluctuations in Venus' solar wind interaction region based on the measurements made on board the Venus Express spacecraft. The orbit geometry is very suitable to investigate the fluctuations in Venus' low-altitude magnetosheath and mid-magnetotail and provides an opportunity for a comparative study of low-frequency waves at Venus and Mars. The spatial distributions of the wave properties, in particular in the dayside and nightside magnetosheath as well as in the tail and mantle region, are similar to observations at Mars. As both planets do not have a global magnetic field, the interaction process of the solar wind with both planets is similar and leads to similar instabilities and wave structures. We focus on the spatial distribution of the wave intensity of the fluctuating magnetic field and detect an enhancement of the intensity in the dayside magnetosheath and a strong decrease towards the terminator. For a detailed investigation of the intensity distribution we adopt an analytical streamline model to describe the plasma flow around Venus. This allows displaying the evolution of the intensity along different streamlines. It is assumed that the waves are generated in the vicinity of the bow shock and are convected downstream with the turbulent magnetosheath flow. However, neither the different Mach numbers upstream and downstream of the bow shock, nor the variation of the cross sectional area and the flow velocity along the streamlines play probably an important role in order to explain the observed concentration of wave intensity in the dayside magnetosheath and the decay towards the nightside magnetosheath. But, the concept of freely evolving or decaying turbulence is in good qualitative agreement with the observations, as we observe a power law decay of the intensity along the streamlines. The observations support the assumption of wave convection through the magnetosheath, but reveal at the same time that wave sources may not only exist at the bow shock, but also in the magnetosheath.

scholarly journals Low-frequency magnetic field fluctuations in Earth's plasma environment observed by THEMIS

2012 ◽  
Vol 30 (8) ◽  
pp. 1271-1283 ◽  
Author(s):  
L. Guicking ◽  
K.-H. Glassmeier ◽  
H.-U. Auster ◽  
Y. Narita ◽  
G. Kleindienst
Keyword(s):  
Magnetic Field ◽  
Low Frequency ◽  
Wave Generation ◽  
Wave Activity ◽  
Wave Intensity ◽  
Magnetic Wave ◽  
Plasma Environment ◽  
Frequency Magnetic Field ◽  
Field Fluctuations ◽  
Generation Mechanisms

Abstract. Low-frequency magnetic wave activity in Earth's plasma environment was determined based on a statistical analysis of THEMIS magnetic field data. We observe that the spatial distribution of low-frequency magnetic field fluctuations reveals highest values in the magnetosheath, but the observations differ qualitatively from observations at Venus presented in a previous study since significant wave activity at Earth is also observed in the nightside magnetosheath. Outside the magnetosheath the low-frequency wave activity level is generally very low. By means of an analytical streamline model for the magnetosheath plasma flow, we are able to investigate the spatial and temporal evolution of wave intensity along particular streamlines in order to characterise possible wave generation mechanisms. We observe a decay of wave intensity along the streamlines, but contrary to the situation at Venus, we obtain good qualitative agreement with the theoretical concept of freely evolving/decaying turbulence. Differences between the dawn region and the dusk region can be observed only further away from the magnetopause. We conclude that wave generation mechanisms may be primarily attributed to processes at or in the vicinity of the bow shock. The difference with the observations of the Venusian magnetosheath we interpret to be the result of the different types of solar wind interaction processes since the Earth possesses a global magnetic field while Venus does not, and therefore the observed magnetic wave activities may be caused by diverse magnetic field controlled characteristics of wave generation processes.

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