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Wohlmuth, R.; Plettemeier, Dirk; Edenhofer, P.; Bird, M. K.; Ефимов, А. И.; Andreev, V. E.; Samoznaev, L. N.; Чашей, И. В.

doi:10.1023/a:1011845221808

Cited by 29 publications

(18 citation statements)

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“…F o rt h es o l a rw i n d ,α ∼ 11/3 agrees with that of Kolmogorov derived for fluid turbulence (Spangler & Sakurai, 1995;Spangler et al , 2002;Spangler , 2002;Tu & Marsch , 1994;Wohlmuth et al , 2001;Woo et al , 1995). The inner scale l i (which is also known as the dissipative scale) increases linearly with heliocentric distance as l i =(…”

Section: Electron Density Fluctuationssupporting

confidence: 82%

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Monte Carlo Simulations in Solar Radio Astronomy

Thejappa¹,

MacDowall²

2011

Applications of Monte Carlo Method in Science and Engineering

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Section: Electron Density Fluctuationssupporting

confidence: 82%

“…In this study, we assume that l i ∼ 100 km, and for the outer scale l 0 , we use the empirical formula derived by Wohlmuth et al (2001) using the Galileo data between 7 to 80 R ⊙ l 0 = 19r 0.82 .…”

Section: Electron Density Fluctuationsmentioning

confidence: 99%

Monte Carlo Simulations in Solar Radio Astronomy

Thejappa¹,

MacDowall²

2011

Applications of Monte Carlo Method in Science and Engineering

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“…A result that is more supportive of an outer scale in the range that I have proposed is that of Wohlmuth et al (2001). Wohlmuth et al (2001) analyzed downlink frequency fluctuations of the Ulysses spacecraft transmitter during solar occultations in 1991 and 1995.…”

Section: Observational Resultsmentioning

confidence: 82%

“…They identified a peak in the frequency fluctuation power spectrum that is related to the outer scale of the turbulence. The data of Wohlmuth et al (2001) indicate that the outer scale increases with heliocentric distance and has a value of 2.7-3.5 R at a heliocentric distance of 20 R .…”

Section: Observational Resultsmentioning

confidence: 92%

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The Amplitude of Magnetohydrodynamic Turbulence in the Inner Solar Wind

Spangler

2002

ApJ

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Recent radio wave interplanetary scintillation observations have improved our knowledge of the level of turbulent fluctuations of plasma density in the inner solar wind at heliocentric distances of 16-26 R and less accurately outside this range. This information relates to fluctuations in the inertial subrange of the turbulence. Of particular concern in this paper is the heliocentric distance dependence of the power-law normalization parameter C 2 N . This measurement of C 2 N , when combined with independent measurements of the mean plasma density in the inner solar wind, indicates that the dimensionless amplitude of the turbulence n =n n is low, of the order of 6%-15%, where n is the standard deviation of the density fluctuations and n n is the mean value. The deduced value for depends on an assumed value for the outer scale of the turbulence, l o . I adopt a fiducial value of l o ¼ 1 R . A comparison is made with independent estimates of , from both radio remote sensing in the same part of space and in situ measurements at greater distances. Satisfactory agreement occurs. I discuss the possibility that this dimensionless density amplitude might be a proxy for the corresponding amplitude of the magnetic field fluctuations. This is a controversial assertion. However, if it is the case, the measurements suggest that the turbulence in the inner solar wind is weak, in the sense of being dynamically and thermodynamically important.

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Monte Carlo Simulation of Scattering of Solar Radio Emissions

Thejappa

MacDowall

Astrophysics and Space Science Proceedings

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Cited by 29 publications

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Monte Carlo Simulations in Solar Radio Astronomy

Monte Carlo Simulations in Solar Radio Astronomy

The Amplitude of Magnetohydrodynamic Turbulence in the Inner Solar Wind

Monte Carlo Simulation of Scattering of Solar Radio Emissions

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