Ionized Gas and Fast Electrons in the Earth’s Neighborhood and Interplanetary Space

Gringauz, K. I.; Kurt, V. G.; Мороз, В. І.; Shklovskii, I. S.

doi:10.1007/978-1-4899-5959-1_7

Cited by 7 publications

(9 citation statements)

References 4 publications

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“…Later, Parker (1958) predicted the existence of the wind. Early experimental confirmation soon followed (Gringauz et al 1960;Gringauz 1961;Snyder and Neugebauer 1966), but the significance of those observations was not appreciated until later Wilcox 1964, 1966;Gringauz et al 1967). Measurements on Explorer 10 soon showed that the wind was continuous, filled the heliosphere, and, at least near solar minimum, existed in two states: fast, with velocities up to 800 km/s, and slow, with velocities more in the range of 200-350 km/s (Bonetti et al 1963;Bridge et al 1961;Scherb 1964).…”

Section: Introductionmentioning

confidence: 99%

Turbulence in the Solar Atmosphere and Solar Wind

Petrosyan

Balogh

Goldstein³

et al. 2010

Space Sci Rev

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The objective of this review article is to critically analyze turbulence and its role in the solar atmosphere and solar wind, as well as to provide a tutorial overview of topics worth clarification. Although turbulence is a ubiquitous phenomenon in the sun and its heliosphere, many open questions exist concerning the physical mechanisms of turbulence generation in solar environment. Also, the spatial and temporal evolution of the turbulence A. Petrosyan ( ) Space Research Institute of the Russian Academy Sciences,

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Section: Introductionmentioning

confidence: 99%

Turbulence in the Solar Atmosphere and Solar Wind

Petrosyan

Balogh

Goldstein³

et al. 2010

Space Sci Rev

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“…Pioneer 5 (Coleman, 1964), Explorer 10 (Heppner et al, 1963;Bonetti et al, 1963) and early Soviet probes (Gringauz et al, 1961;Shklovskii et al, 1960) provided the early measurements in the boundary regions but the exploratory nature of the experiments plus limited quantities of data prevented a clear understanding of the underlying physics of the solar wind-earth interaction. The first definitive studies which included mapping of the positions of the boundaries were carried out with data from the spacecraft Explorer 12 (Chaill and Amazeen, 1963;Freeman, 1964;Cahill and 'Patel, 1967) (magnetopause only) and IMP 1 (Ness et al, 1964;Bridge et al, 1965;Wolfe et al, 1966) (magnetopause and shock).…”

Section: Introductionmentioning

confidence: 99%

Average and unusual locations of the Earth's magnetopause and bow shock

Fairfield¹

1971

J. Geophys. Res.

835

526

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A best‐fit ellipse and hyperbola have been calculated to represent several hundred magnetopause and bow‐shock positions observed by six Imp spacecraft. Average geocentric distances to the magnetopause and bow shock near the ecliptic plane are 11.0 and 14.6 RE in the sunward direction, 15.1 and 22.8 RE in the dawn meridian, and 15.8 and 27.6 RE in the dusk meridian. The bow‐shock hyperbola is oriented in a direction consistent with that expected when the aberration of a radial solar wind is considered. Observed magnetopause crossings agree well with theoretical predictions in the noon meridian plane but fall outside the theoretical boundaries in the dawn‐dusk meridian planes. Imp 4 plasma data are used to demonstrate that the solar‐wind momentum flux is the prime factor controlling the orbit‐to‐orbit changes in the boundary positions. Data suggest that the interplanetary‐field orientation also affects the distance to the magnetopause boundary, more earthward crossings corresponding to southward fields. Six unusual bow‐shock locations up to 22 RE beyond the average position are found to be due to an enhanced standoff distance associated with a low Alfvén Mach number. The possibility that the solar wind may have become sub‐Alfvénic on July 31, 1967, is suggested.

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“…In the late fties, the satellites Luna-1 and Luna-2 discovered the solar wind [2], whose model was proposed by Parker [3] on the basis of his own and Biermann's…”

Section: Introductionmentioning

confidence: 99%

Surface Waves along the Martian Ionopause

Chmielewski¹,

Murawski²,

Kumar³

2013

Acta Phys. Pol. A

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We study the behaviour of surface waves propagating along the ionopause of the planet Mars and derive the onset criteria for unstable KelvinHelmholtz modes and negative energy waves at the Martian ionopause. Growth rate of unstable KelvinHelmholtz mode decreases with wavelength. The backward propagating waves became negative energy waves for the ionosheath velocity higher than critical velocity. It is found that short wavelength surface waves propagating along the Martian ionopause are less dispersive than long waves.

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Ionized Gas and Fast Electrons in the Earth’s Neighborhood and Interplanetary Space

Cited by 7 publications

References 4 publications

Turbulence in the Solar Atmosphere and Solar Wind

Turbulence in the Solar Atmosphere and Solar Wind

Average and unusual locations of the Earth's magnetopause and bow shock

Surface Waves along the Martian Ionopause

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