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Бархатов, Н. А.; Belliustin, N. S.; Bougeret, J. L.; Sakharov, S. Yu.; Tokarev, Yu. V.

doi:10.1023/a:1014828310176

Cited by 8 publications

(4 citation statements)

References 3 publications

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“…Disturbed SW (ICME, CIR) features variations in IMF direction, which leads to an increase in the IMF component tangential to BS. Under such conditions, the magnetic field strengthens behind BS, which can cause turbulence to weaken [Barkhatov et al, 2001]. The relationship between turbulence characteristics and the magnetic field strength we have demonstrated in this work can be produced by this effect.…”

Section: Discussionmentioning

confidence: 63%

“…Geoeffectiveness of large-scale phenomena such as interplanetary coronal mass ejections (ICMEs), compression regions in front of them (sheaths), as well as coroting interaction regions (CIRs) has been repeatedly demonstrated by experimental statistical studies . A number of studies have pointed out the special role of sheaths and CIRs in the response of the magnetosphere and ionosphere Barkhatov et al, 2019Barkhatov et al, , 2001. Solar wind (SW) plasma and the interplanetary magnetic field (IMF) do not, however, directly affect the magnetospherethey first pass through the bow (near-Earth) shock wave (BS) and the transition region behind it, the magnetosheath (MSH).…”

Section: Introductionmentioning

confidence: 99%

“…Peculiarities of the development of turbulence behind BS have been observed for a long time, in particular in experiments on radio translucence of the disturbed subsolar MSH region [Barkhatov et al, 2001]. Fullscale satellite studies became possible later with the advent of a sufficient number of spacecraft in this region.…”

Section: Introductionmentioning

confidence: 99%

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Turbulence development behind the bow shock during disturbed and undisturbed solar wind

Rakhmanova,

Khokhlachev,

Riazantseva

et al. 2024

Solar-Terrestrial Physics

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Magnetosheath is a transition layer between the solar wind and the magnetosphere and may contribute to the geoeffectiveness of various large-scale interplanetary phenomena. In this paper, we examine the dynamics of the turbulent fluctuation spectra behind the bow shock during undisturbed solar wind and when interplanetary coronal mass ejections and corotation interaction regions interact with the magnetosphere. The study is based on statistical analysis of the turbulence features inside the magnetosheath at different distances from the bow shock. We demonstrate that the turbulence features change when plasma crosses the bow shock for the solar wind of all types and they usually recover when plasma moves away from the bow shock. However, peculiarities in the turbulence development occur during interplanetary coronal mass ejections. Moreover, during disturbed solar wind there are relations between the turbulence features at the sub-ion scales and background plasma parameters such as plasma parameter β, the angle θBN between the interplanetary magnetic field and the local bow shock normal, solar wind bulk velocity, and the distance to the magnetosheath boundaries.

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Section: Discussionmentioning

confidence: 63%

Section: Introductionmentioning

confidence: 99%

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Turbulence development behind the bow shock during disturbed and undisturbed solar wind

Rakhmanova,

Khokhlachev,

Riazantseva

et al. 2024

Solar-Terrestrial Physics

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show abstract

“…From a comparison of model estimates of the IPP inhomogeneity parameters between the "Sura"-WIND experiments data and the data of direct measurements of the SW speed and density onboard the WIND SC it is found that the spatial spectrum of plasma-density fluctuations in the transition region has a plateau in the vicinity of scales of the order of 1000 km [129]. Dependence of the scintillation index of the observed scattered signal, which characterizes the average level of turbulence in the transition region, on the orientation and magnitude of the interplanetary magnetic field is revealed [130].…”

Section: Small-scale Turbulence Of the Interplanetary Plasmamentioning

confidence: 99%