VLF observations by the Akebono (EXOS-D) satellite.

Kimura, Ikuo; Hashimoto, K.; Nagano, I.; Okada, T.; Yamamoto, Masayuki; Yoshino, Takeo; Matsumoto, Hiroshi; Ejiri, Masaki; Hayashi, K.

doi:10.5636/jgg.42.459

Cited by 62 publications

(48 citation statements)

References 17 publications

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“…Thermal plasma densities were derived from the frequency of the upper-hybrid resonance waves measured by the Plasma Wave observation and Sounder experiments instrument of the Akebono satellite [Oya et al, 1990]. The data for whistler mode waves were obtained by the VLF instrument of the Akebono satellite [Kimura et al, 1990]. The relativistic electrons were obtained from GOES satellites at GEO and from the Radiation Monitor of the Akebono satellite [Takagi et al, 1993].…”

Section: Discussionmentioning

confidence: 99%

High‐speed solar wind with southward interplanetary magnetic field causes relativistic electron flux enhancement of the outer radiation belt via enhanced condition of whistler waves

Miyoshi

Kataoka

Kasahara

et al. 2013

Geophysical Research Letters

136

163

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Relativistic electron flux in the outer radiation belt tends to increase during the high‐speed solar wind stream (HSS) events. However, HSS events do not always cause large flux enhancement. To determine the HSS events that cause such enhancement and the mechanisms that are responsible for accelerating the electrons, we analyzed long‐term plasma data sets, for periods longer than one solar cycle. We demonstrate that during HSS events with the southward interplanetary magnetic field (IMF)‐dominant HSS (SBz‐HSS), relativistic electrons are accelerated by whistler mode waves; however, during HSS events with the northward IMF‐dominant HSS, this acceleration mechanism is not effective. The differences in the responses of the outer radiation belt flux variations are caused by the differences in the whistler mode wave–electron interactions associated with a series of substorms. During SBz‐HSS events, hot electron injections occur and the thermal plasma density decreases due to the shrinkage of the plasmapause, causing large flux enhancement of relativistic electrons through whistler mode wave excitation. These results explain why large flux enhancement of relativistic electrons tends to occur during SBz‐HSS events.

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Section: Discussionmentioning

confidence: 99%

High‐speed solar wind with southward interplanetary magnetic field causes relativistic electron flux enhancement of the outer radiation belt via enhanced condition of whistler waves

Miyoshi

Kataoka

Kasahara

et al. 2013

Geophysical Research Letters

136

163

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“…[15] Omega signals were detected by the VLF (very low frequency plasma wave detectors) instrument [Kimura et al, 1990] onboard the Akebono satellite. The Omega stations transmitted the common frequency 10.2kHz alternately with prescribed duration between 0.9 and 1.2sec at every 10sec.…”

Section: Instruments Onboard the Akebono Satellite And Observational mentioning

confidence: 99%

“…In this method, Omega signals of around 10kHz, which had been used for global navigation until 1997, were used. The Omega signals were transmitted from the stations distributed over the world and were continuously detected by the VLF instruments [Kimura et al, 1990] onboard Akebono in the plasmasphere. The wave normal directions and propagation delay times of the Omega signals along the satellite trajectory can be determined from the observed wave data, which can also be calculated by ray tracing.…”

Section: Introductionmentioning

confidence: 99%

Determination of plasmaspheric electron density profile by a stochastic approach

2003

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[1] The determination of plasmaspheric electron density profiles has been attempted using a stochastic approach, using Omega signals observed on the Akebono satellite. Since the wave normal directions and delay times of Omega signals can be theoretically calculated by ray tracing under an appropriate electron density model, the density profile can be estimated by fitting the calculated directions and times to the observed values. In the present paper, we introduce a flexible model and a novel algorithm in the fitting method, taking into account the stochastic factors of the density distribution and wave propagation. The stochastic representations of directions and times enable us to separately estimate the effects of the ionosphere and the plasmasphere. The validity of the proposed method is examined using observational data collected during the recovery phase of a magnetic storm. In another example, an estimation of the asymmetry of the plasmasphere is attempted.INDEX TERMS: 6984 Radio Science: Waves in plasma; 6969 Radio Science: Remote sensing; 2768 Magnetospheric Physics: Plasmasphere; 6982 Radio Science: Tomography and imaging; KEYWORDS: electron density profile, satellite observation, VLF wave Citation: Goto, Y., Y. Kasahara, and T. Sato, Determination of plasmaspheric electron density profile by a stochastic approach,

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“…By frequent passages above the aurora] zone, the Akebono has provided us with ample data of wave and particles around the region (Kimura et al, 1990).…”

Section: Introductionmentioning

confidence: 99%