Fast Solar Wind Monitor (BMSW): Description and First Results

Šafránková, Jana; Němeček, Zdenek; Přech, Lubomír; Zastenker, G. N.; Cermak, I.; Chesalin, L. S.; Komárek, Arnošt; Vaverka, Jakub; Beránek, M.; Pavlu, Jiri; Gavrilova, E. A.; Karimov, B. T.; Leibov, A. V.

doi:10.1007/s11214-013-9979-4

Cited by 74 publications

(41 citation statements)

References 11 publications

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“…Our study is based on data of the BMSW (fast solar wind monitor) instrument (Zastenker et al, 2013;Šafránková et al, 2013b) on board the Spektr-R spacecraft. Though Spektr-R was designed for astrophysical purposes, its orbit (apogee ∼ 52 R E , perigee ∼ 0.1 R E , duration ∼ 8 days) is convenient for monitoring the SW and MSH parameters.…”

Section: Observationsmentioning

confidence: 99%

Plasma fluctuations at the flanks of the Earth's magnetosheath at ion kinetic scales

2016

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Abstract. We present a statistical study of the magnetosheath plasma fluctuation spectra at a high-frequency range (with frequencies from 0.01 to 10 Hz). Variations of ion flux value and its direction are considered. The direction of ion flux is characterized by a polar angle -the deviation of the ion flux vector from the Sun-Earth line. We consider 290 Fourier's spectra that can be described by two power laws with a break, i.e., a change of slope. The ion flux fluctuation spectra are shown to have breaks at higher frequencies compared to the polar angle spectra. We compare the frequency of the break with the gyrostructure frequency for a number of cases. We show the polar angle break frequency to usually be smaller than the gyrostructure frequency. The dependencies of spectrum parameters such as the slopes and the break frequency on plasma parameters are also considered.

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Section: Observationsmentioning

confidence: 99%

Plasma fluctuations at the flanks of the Earth's magnetosheath at ion kinetic scales

2016

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“…The first results provided by this instrument are published in [23,[34][35][36][37][38]. Such multiscale structure of SW is described in numerous papers (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…The mixing of frequencies was excluded, because the amplifiers of the BMSW Faraday cups were equipped with Bessel's filters at the Nyquist frequency [34]. The laboratory tests and analysis of in-flight calibration intervals have shown that the noise of BMSW amplifiers can spoil the ion flux frequency spectra above 8-10 Hz [27,34] when the level of the ion flux fluctuations is very low, thus the reasonable estimate for the upper boundary of the range of SW ion flux variations is about 10 Hz. The spectra of some other SW plasma parameters (density, velocity and temperature) can be obtained by measurements carried in the 'adaptive mode' [34].…”

Section: Introductionmentioning

confidence: 99%

“…The laboratory tests and analysis of in-flight calibration intervals have shown that the noise of BMSW amplifiers can spoil the ion flux frequency spectra above 8-10 Hz [27,34] when the level of the ion flux fluctuations is very low, thus the reasonable estimate for the upper boundary of the range of SW ion flux variations is about 10 Hz. The spectra of some other SW plasma parameters (density, velocity and temperature) can be obtained by measurements carried in the 'adaptive mode' [34]. The presence of the break qualitatively corresponds to the prediction of fractal model (see [40]).…”

Section: Introductionmentioning

confidence: 99%

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Dynamic properties of small-scale solar wind plasma fluctuations

Рязанцева

Budaev

Zelenyǐ

et al. 2015

Phil. Trans. R. Soc. A.

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The paper presents the latest results of the studies of small-scale fluctuations in a turbulent flow of solar wind (SW) using measurements with extremely high temporal resolution (up to 0.03 s) of the bright monitor of SW (BMSW) plasma spectrometer operating on astrophysical SPECTR-R spacecraft at distances up to 350 000 km from the Earth. The spectra of SW ion flux fluctuations in the range of scales between 0.03 and 100 s are systematically analysed. The difference of slopes in low- and high-frequency parts of spectra and the frequency of the break point between these two characteristic slopes was analysed for different conditions in the SW. The statistical properties of the SW ion flux fluctuations were thoroughly analysed on scales less than 10 s. A high level of intermittency is demonstrated. The extended self-similarity of SW ion flux turbulent flow is constantly observed. The approximation of non-Gaussian probability distribution function of ion flux fluctuations by the Tsallis statistics shows the non-extensive character of SW fluctuations. Statistical characteristics of ion flux fluctuations are compared with the predictions of a log-Poisson model. The log-Poisson parametrization of the structure function scaling has shown that well-defined filament-like plasma structures are, as a rule, observed in the turbulent SW flows.

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“…For standard operation, the ratios 0.3 and 0.5 are used, and these FCs provide three points of the distribution function with a full time resolution of 31 ms. To achieve this time resolution, the feed-back loops should keep the preselected ratios of FC currents even under abrupt changes of solar wind parameters. The full description of the basic principles of the BMSW instrument, its operation modes and demonstration of its capability to provide a comprehensive set of data can be found in Šafránková et al [9].…”

Section: A Short Bmsw Descriptionmentioning

confidence: 99%