Long-period geomagnetic pulsations caused by the solar wind negative pressure impulse on 22 March 1979 (CDAW-6)

Parkhomov, V. A.; Мишин, В. М.; Borovik, L. V.

doi:10.1007/s00585-998-0134-6

Cited by 15 publications

(4 citation statements)

References 14 publications

(31 reference statements)

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“…Narrow equatorial localization results in near zero occurrence rate at L > 8, where Arase reaches |MLAT| > 30° (Figures 7a–7e). The occurrence rate increase at dusk‐midnight sector probably corresponds to storm‐time pulsations (Anderson, 1993), while pre‐noon occurrence rate maximum may result from some external sources, for example, SW pressure pulse or interplanetary shock (Eriksson et al., 2006; Oliveira et al., 2020; Parkhomov et al., 1998; Zong, 2022). This conclusion is supported by the ϕ distribution that has a single maximum at the pre‐noon sector near ϕ = ϕ ⊥ (Figure 7h).…”

Section: Resultsmentioning

confidence: 99%

Polarization and Spatial Distribution Features of Pc4 and Pc5 Waves in the Magnetosphere

Rubtsov,

Nosé,

Matsuoka

et al. 2023

JGR Space Physics

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Ultra‐low frequency waves interact with different particle populations all over the magnetosphere. Some interaction mechanisms are associated with certain wave modes, but is it really so and what about waves interaction between each other? We present a statistical analysis of Pc4 and Pc5 waves in the magnetosphere of the Earth that were observed by Arase satellite from March 2017 to December 2020. These waves were classified by polarization into toroidal, poloidal, and compressional waves. Toroidal and poloidal waves are thought to be Alfvén waves that are eigenoscillations of Earth’s magnetic field lines. The former are believed to be generated by external sources, while the latter one — by internal sources. We compared spatial distribution features with well‐known case studies to reveal their nature for all three polarizations. A high inclination of Arase orbit supported a wave field‐aligned structure research. We found that toroidal waves are mostly odd harmonics and poloidal waves are both even and odd harmonics of Alfvén waves, while compressional waves were observed in a narrow equatorial region only. Different wave generation mechanisms that cause a clear difference in spatial distributions of toroidal, poloidal, and compressional waves could excite a specific wave polarization. Surprisingly, a statistics of wave polarization has a normal distribution without separate clusters. We suggest that polarization change and mode coupling processes make mixed polarization the most common type of polarization in the magnetosphere. This result raises the question of how the polarization change process affects wave‐particles interactions responsible for energy transport throughout the magnetosphere.

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Section: Resultsmentioning

confidence: 99%

Polarization and Spatial Distribution Features of Pc4 and Pc5 Waves in the Magnetosphere

Rubtsov,

Nosé,

Matsuoka

et al. 2023

JGR Space Physics

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“…The EEJ signature did not disappear abruptly, but faded away during the time it took for the dynamic pressure to weaken. The disappearance of the EEJ, however, was not smooth but overlaid with decaying wave activity (Parkhomov et al, 1998). This pulsation activity caused the most intense |dH/dt| by temporarily disrupting the EEJ.…”

Section: Prenoon Pulsation Event On 24 Nov 2001 At 07:32:20 Utmentioning

confidence: 94%

Drivers of rapid geomagnetic variations at high latitudes

Juusola

Viljanen

Dimmock

et al. 2022

Preprint

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Abstract. We have examined the most intense external (magnetospheric and ionospheric) and internal (induced) |dH/dt| (amplitude of the 10 s time derivative of the horizontal geomagnetic field) events observed by the high-latitude International Monitor for Auroral Geomagnetic Effects (IMAGE) magnetometers between 1994 and 2018. While the most intense external |dH/dt| events at adjacent stations typically occurred simultaneously, the most intense internal (and total) |dH/dt| events were more scattered in time, most likely due to the complexity of induction in the conducting ground. The most intense external |dH/dt| events occurred during geomagnetic storms, among which the Halloween storm in Oct 2003 featured prominently, and drove intense geomagnetically induced currents (GIC). Events in the prenoon local time sector were associated with sudden commencements (SC) and pulsations, and the most intense |dH/dt| values were driven by abrupt changes in the eastward electrojet due to solar wind dynamic pressure increase or decrease. Events in the premidnight and dawn local time sectors were associated with substorm activity, and the most intense |dH/dt| values were driven by abrupt changes in the westward electrojet, such as weakening and poleward retreat (premidnight) or undulation (dawn). Despite being associated with various event types and occurring at different local time sectors, there were common features among the drivers of most intense external |dH/dt| values: pre-existing intense ionospheric currents (SC events were an exception) that were abruptly modified by sudden changes in the magnetospheric magnetic field configuration. While proper description of the fast changes during SC events appears to require 1 s data, pulsations and substorms may be sufficiently described by 10 s |dH/dt|. 1 min data, however, significantly underestimates the |dH/dt| peaks. Our results contribute towards the ultimate goal of reliable forecasts of dH/dt and GIC.

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“…Two pulsation types, with frequencies of 2.3 and 4-6 mHz, were also registered in the event, accompanied by a sharp decrease in P d , considered in [8]. In this work it is assumed that the first pulsation type with a period independent of latitude is caused by magneto pause oscillations; the second pulsation type with a period dependent on latitude, by intramagnetospheric resonances.…”

Section: Psi Pulsations In the Nightside Magnetospherementioning

confidence: 99%

“…The dependence of dawn pulsation frequency on latitude makes it possible to assume (see [8]) that these pulsa tions are related to Alfvén resonance oscillations gener ated during the compression of the magnetosphere. The nature of such pulsations are traditionally based on the following physical pattern: periodic disturbances of the magnetospheric boundary, generated by the surface compression wave (or/and) Kelvin-Helmholtz insta bility, are attenuated when they propagate deep into the magnetosphere, but magnetic shell Alfvén oscillations are excited at the resonance shell where disturbance fre quency coincides with the field line oscillation eigenfre quency.…”

Section: Sources Of Hf and Lf Psi Pulsationsmentioning

confidence: 99%

Generation of different long-period geomagnetic pulsations during a sudden impulse

et al. 2015

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The space-time characteristics of geomagnetic pulsations during a sudden impulse on August 4, 2010 have been analyzed using ground based and satellite observations. It has been indicated that two types of geomagnetic pulsations with different spatial extensions, oscillation frequencies, and gen erations were observed at that time. It has been found that geomagnetic pulsations with identical oscillation frequencies (~4.5 mHz) at different latitudes were observed, with a maximal amplitude in the dusk sector. Oscillations with close frequencies were registered in the solar wind in the IMF Bz component. Higher frequency (7-10 mHz) pulsations dependent on latitude were registered on the dawn side. It is assumed that geomagnetic pulsations with frequencies of ~4.5 mHz were caused by oscillations penetrating from the interplanetary medium, and higher frequency pulsations were Alfvén resonance oscillations generated during the compression of the magnetosphere. An asymmetric oscillation amplitude distribution relative to noon was caused by the IMF orthospiral orientation in this event.

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Long-period geomagnetic pulsations caused by the solar wind negative pressure impulse on 22 March 1979 (CDAW-6)

Cited by 15 publications

References 14 publications

Polarization and Spatial Distribution Features of Pc4 and Pc5 Waves in the Magnetosphere

Polarization and Spatial Distribution Features of Pc4 and Pc5 Waves in the Magnetosphere

Drivers of rapid geomagnetic variations at high latitudes

Generation of different long-period geomagnetic pulsations during a sudden impulse

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