Where do solar wind-controlled micropulsations originate?

Golikov, Y.Y.; Plyasova-Bakounina, T.A.; Troitskaya, V. A.; Chernikov, A. A.; Pustovalov, V. V.; Hedgecock, P. C.

doi:10.1016/0032-0633(80)90034-3

Cited by 9 publications

(6 citation statements)

References 11 publications

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“…Further, at high •N angles his study observes a constant ratio of occurrence of waves independent of period and •sN. Golikov et al (1980) muddied the waters by claiming the observations were in fact contradictory. Waves from the magnetosheath probably can couple to the magnetosphere and propagate to synchronous orbit from a variety of local times confusing the simple picture that appears to hold at lower L-values.…”

Section: Discussionmentioning

confidence: 82%

“…Southwood, 1968). In support of this mechanism is the observation that the amplitudes of Pc 3,4 pulsations in the magnetosphere are correlated with the velocity of the solar wind (Singer et al, 1977;Greenstadt et al, 1979a,b;Golikov et al, 1980;Wolfe et al, 1980). Chen and Hasegawa, 1974).…”

Section: Introductionmentioning

confidence: 95%

“…Chen and Hasegawa, 1974). In support of this mechanism is the observation that the amplitudes of Pc 3,4 pulsations in the magnetosphere are correlated with the velocity of the solar wind (Singer et al, 1977;Greenstadt et al, 1979a,b;Golikov et al, 1980;Wolfe et al, 1980). Despite the intense interest in these waves and the many correlations of their properties with that of the solar wind, there is no concensus on the source of these waves.…”

Section: Introductionmentioning

confidence: 99%

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The rate of occurrence of dayside Pc 3,4 pulsations: The L‐value dependence of the IMF cone angle effect

Russell¹,

Luhmann²,

Odera

et al. 1983

Geophysical Research Letters

138

101

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The normalized rate of occurrence of dayside Pc 3,4 pulsations from L=2.4 to 4.3 has a strong enhancement for low cone angles of the interplanetary magnetic field. When the angle of the IMF to the earth sun line, θBX, is 15° or less the occurrence rate is 7‐8 times the average rate at L=2.4 to 2.8 and 2.2 to 3.5 times the average rate at L=4 to 4.3. These waves disappear when the IMF is nearly at right angles to the sun‐earth‐line. This absence of pulsations occurs over the widest range of angles at lowest L‐values. These observations are consistent with a source originating in the waves upstream of the subsolar bow shock which are transported by convection to the magnetopause where they couple to oscillations of magnetospheric field lines. Since the index of refraction of the magnetospheric plasma decreases with decreasing radial distance, except at the plasmapause, inward propagating waves should be refracted away from the radial direction. Thus, to reach low L‐values the waves should couple near the stagnation point and propagate nearly radially inwards. Upstream waves should be convected to the stagnation point for only a limited range of θBX. However, to reach higher L‐values the coupling may be at later local times where cross streamline propagation can bring waves from a larger range of θBX. The streamline geometry and its connection to the foreshock region is illustrated for a variety of IMF orientations using a simple approximation to the magnetosheath flow field.

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Section: Discussionmentioning

confidence: 82%

Section: Introductionmentioning

confidence: 95%

Section: Introductionmentioning

confidence: 99%

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The rate of occurrence of dayside Pc 3,4 pulsations: The L‐value dependence of the IMF cone angle effect

Russell¹,

Luhmann²,

Odera

et al. 1983

Geophysical Research Letters

138

101

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“…The other possibility is the saturation of the Kelvin‐Helmholtz instability. Golikov et al [] have shown that unless:

{((), \frac{n_{i}}{n_{e}})}^{\frac{1}{2}} MathClass-rel< \frac{B_{e}}{B_{i}}

the instability is stabilized by the sausage mode. Here, the indices i and e notate the parameters inside and external to the layer of flow along the magnetopause in which the instability develops.…”

Section: Discussionmentioning

confidence: 99%

“…Here, the indices i and e notate the parameters inside and external to the layer of flow along the magnetopause in which the instability develops. The stabilization criteria of the Kelvin‐Helmholtz instability at the magnetopause should be recalculated in the conditions that are more realistic than those used by Golikov et al []. In general, the decrease in solar wind density should lead to the decrease of the magnetosheath density.…”

Section: Discussionmentioning

confidence: 99%

The analysis of electron fluxes at geosynchronous orbit employing a NARMAX approach

et al. 2013

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[1] The methodology based on the Error Reduction Ratio (ERR) determines the causal relationship between the input and output for a wide class of nonlinear systems. In the present study, ERR is used to identify the most important solar wind parameters, which control the fluxes of energetic electrons at geosynchronous orbit. The results show that for lower energies, the fluxes are indeed controlled by the solar wind velocity, as was assumed before. For the lowest energy range studied here (24.1 keV), the solar wind velocity of the current day is the most important control parameter for the current day's electron flux. As the energy increases, the solar wind velocity of the previous day becomes the most important factor. For the higher energy electrons (around 1 MeV), the solar wind velocity registered 2 days in the past is the most important controlling parameter. Such a dependence can, perhaps, be explained by either local acceleration processes due to the interaction with plasma waves or by radial diffusion if lower energy electrons possess higher mobility. However, in the case of even higher energies (2.0 MeV), the solar wind density replaces the velocity as the key control parameter. Such a dependence could be a result of solar wind density influence on the dynamics of various waves and pulsations that affect acceleration and loss of relativistic electrons. The study also shows that statistically the variations of daily high energy electron fluxes show little dependence on the daily averaged B z , daily time duration of the southward IMF, and daily integral R B s dt (where B s is the southward component of IMF).

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Role of Solar Wind Wave Events in the Generation of Geomagnetic Pulsations

Plyasova-Bakounina

1997

Acta Geod. Geoph. Hung

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Where do solar wind-controlled micropulsations originate?

Cited by 9 publications

References 11 publications

The rate of occurrence of dayside Pc 3,4 pulsations: The L‐value dependence of the IMF cone angle effect

The rate of occurrence of dayside Pc 3,4 pulsations: The L‐value dependence of the IMF cone angle effect

The analysis of electron fluxes at geosynchronous orbit employing a NARMAX approach

Role of Solar Wind Wave Events in the Generation of Geomagnetic Pulsations

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