Direct Measurements of Solar-Wind Fluctuations Between 0.0048 and 13.3 HZ

Unti, T.; Neugebauer, M.; Goldstein, B. E.

doi:10.1086/151987

Cited by 65 publications

(37 citation statements)

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“…The values of the slopes and the frequencies of point intersections of these lines (breakpoint 1 and breakpoint 2 in the figure) are shown in figure 2b, together with the slope of the Kolmogorov spectrum −5/3 (dashed line). A similar spectrum with flattening around ion scales was first observed in [13,14,16,17,42]. Safrnakova et al [37] have shown that the breakpoint locations are controlled by the gyro-frequency.…”

Section: Introductionsupporting

confidence: 69%

“…We discuss these results in §3. High-resolution plasma data were earlier accomplished up to 13.3 Hz by SW flux measurements in the OGO-5 experiment [17], up to approximately 5 Hz by electron density measurements in ISEE-1 and ISEE-2 experiments [13,14] and up to 2.5 Hz by electron density measurements on the CLUSTER experiment [16]. However, these authors did not note the steepening of the spectra.…”

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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Section: Introductionsupporting

confidence: 69%

Section: Introductionmentioning

confidence: 99%

Dynamic properties of small-scale solar wind plasma fluctuations

Рязанцева

Budaev

Zelenyǐ

et al. 2015

Phil. Trans. R. Soc. A.

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“…In Figure 1 some synthetic density data calculated from published density power spectra are shown [Unti et al, 1973;Neugebauer, 1975Neugebauer, , 1976Celniker et al, 1983Celniker et al, , 1987. To make these curves, which essentially means reconstructing a time series statistically similar to the original data from which the power spectra were calculated, we have calculated a Fourier series for a much longer time period than shown (100 times longer), in which each amplitude is proportional to the square root of the power spectrum, integrated over the increment in frequency appropriate to a harmonic coefficient of the longer time period, and we have given the Fourier amplitude a random phase between 0 and 2•z and then done an inverse transform.…”

Section: Density Fluctuations the Wkb Approximation And Mode Evolutionmentioning

confidence: 99%

Langmuir waves in a fluctuating solar wind

Kellogg¹,

Goetz²,

Monson³

et al. 1999

J. Geophys. Res.

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“…It is possible that the irregularity spectrum extends below '" 6 km (i.e. beyond 10 Hz) since all observed IPS spectra (and the spectra of Unti et al 1973) show no signs of tapering off at high frequencies. The spectra all meet the noise before any such effect is observed.…”

Section: Discussionmentioning

confidence: 99%

Interplanetary Scintillation Power Spectra

Milne¹

1976

Aust. J. Phys.

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Aust. J. Phys., 1976,29,201-9 Power spectrum measurements of interplanetary scintillation at 408 MHz show that an inverse power law spectrum provides the best description for all scintillating radio sources. The inverse power law index is reasonably constant at ~ 2·4 for solar elongation angles 8 > 10°, and this agrees well with spacecraft observations. For 8 < 10° the index apparently decreases with decreasing 8, and this appears to be consistent with recent strong scattering theory. A Bessel analysis attempted in order to detect Fresnel structure proved unsuccessful because of noise on the power spectra.

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Direct Measurements of Solar-Wind Fluctuations Between 0.0048 and 13.3 HZ

Cited by 65 publications

References 0 publications

Dynamic properties of small-scale solar wind plasma fluctuations

Dynamic properties of small-scale solar wind plasma fluctuations

Langmuir waves in a fluctuating solar wind

Interplanetary Scintillation Power Spectra

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