The Plasma Wave Instrument on Board the AMPTE IRM Satellite

Häusler, B.; Anderson, R. R.; Gurnett, D. A.; Koons, H. C.; Holzworth, R. H.; Bauer, O. H.; Treumann, R. A.; Gnaiger, K.; Odem, D. L.; Harbridge, W. B.; Eberl, Frank

doi:10.1109/tgrs.1985.289526

Cited by 39 publications

(9 citation statements)

References 12 publications

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“…The electron density is obtained from the upper hybrid noise band measured using the plasma wave instrument [ Häusler et al , 1985]. We normally measured the upper hybrid frequency as the midpoint of the upper hybrid noise band.…”

Section: Methodsmentioning

confidence: 99%

“…There is a greater difference in the equilibrium pressure profiles (Figure 4f), though the equilibrium beta values are fairly similar except for a slight shift in L (Figure 4g). Unfortunately, the IRM plasma wave instrument [ Häusler et al , 1985] did not give reliable data except when the spacecraft was at L = 9.2–10.1 ( L range of solid curve in Figure 4e). For both the mapped dipole and MHD equilibrium models, we used a n e ∝ L −4.5 fit (plasmatrough L dependence given by Carpenter and Anderson 's [1992] electron density model).…”

Section: Wave Eventsmentioning

confidence: 99%

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Radial localization of magnetospheric guided poloidal Pc 4‐5 waves

2003

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[1] The toroidal Alfvén wave, with magnetic field oscillations in the azimuthal direction, exhibits a singularity in the vicinity of the toroidal resonant frequency (field line resonance), so it is not surprising that this wave often exhibits varying frequency as a function of L shell. It is less clear why the poloidal Alfvén wave, with magnetic field oscillations in the radial direction, often exhibits a relatively constant frequency over a range of L shells. So far, the most promising proposal to explain this phenomenon is the theory of Vetoulis and Chen [1994, 1996], who showed that an energetically trapped global poloidal mode can exist in a region where the poloidal Alfvén frequency is lower than the toroidal frequency and where it exhibits a dip (minimum) with respect to L. While this theory is mathematically plausible, it has never been shown that poloidal Alfvén waves actually occur in association with such a dip in poloidal frequency. Here we examine poloidal wave events observed by the AMPTE/IRM spacecraft and calculate the theoretical poloidal frequency as a function of L using the equilibrium parameters obtained from the spacecraft observations. We find that the poloidal Alfvén wave does occur in association with such a dip (or at least a flattening) in poloidal frequency. While Vetoulis and Chen hypothesized that such a dip would occur because of a sharp gradient in plasma pressure, we find that the dip in poloidal frequency may result from the L dependence of the equilibrium density or magnetic field. The observed frequencies are in rough agreement with the theoretical frequencies, though in some cases we must assume that the observed oscillations result from a high harmonic (third or fourth harmonic structure along the magnetic field). We also apply the same analysis to compressional wave events (with oscillations in the direction of the equilibrium magnetic field). Such oscillations may be on the poloidal wave branch or the mirror mode branch. Here also, the observed fluctuations occur in the region of a dip in poloidal frequency. In one case the observed frequency is consistent with the theoretical poloidal frequency, whereas in another case it is not.

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Section: Methodsmentioning

confidence: 99%

Section: Wave Eventsmentioning

confidence: 99%

Radial localization of magnetospheric guided poloidal Pc 4‐5 waves

2003

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“…The data presented in this paper are from the plasma wave experiment aboard the IRM. For a complete description of this instrument, see Hiiusler et al [1985]. The electric antenna is an extendible beryllium-copper dipole element with a tip-to-tip length of 47.42 m. The nominal diameter of the element is 5 mm.…”

Section: Introductionmentioning

confidence: 99%

A comparison of the plasma wave spectra for the eight AMPTE chemical releases

Koons¹,

Anderson²

1988

J. Geophys. Res.

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The Active Magnetospheric Particle Tracer Explorers (AMPTE) IRM spacecraft performed a series of eight chemical releases in essentially comparable pairs. There were two lithium releases in the solar wind, two lithium and two barium releases in the near‐Earth magnetotail, and two barium releases to simulate artificial comets, one in the solar wind and the other in the magnetosheath. A variety of plasma waves were observed in conjunction with each of the releases. Although there were unique features associated with some of the individual releases, the comparable releases generally produced similar wave emissions. This paper discusses the similarities and differences among the releases.

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“…DataInterpretation LaBelle et al[1999] presented statistical results of magnetospheric banded emissions observed by the plasma wave instrument[Hausler et al, 1985] during the 2-year lifetime of the Active Magnetospheric Particle and Tracer Explorers/Ion Release Module (AMPTE/IRM) as a complement to an earlier thorough statistical analysis of the occurrence rate and spectral power of these emissions byRoeder and Koons [1989]. An illustration from LaBelle et al[ 1999], showing a sample of these emissions including a spectral slice that reveals well-defined peak frequencies, was shown here as Figure 1.…”

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confidence: 99%

An interpretation of banded magnetospheric radio emissions

Benson¹,

Osherovich²,

Fainberg³

et al. 2001

J. Geophys. Res.

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Abstract. Recently published Active Magnetospheric Particle Tracer Explorers/Ion Release Module (AMPTE/IRM) banded magnetospheric emissions, commonly referred to as "(n + 1/2)fee" emissions, where fee is the electron gyrofrequency, are analyzed by treating them as analogous to sounder-stimulated ionospheric emissions. We show that both individual spectra of magnetospheric banded emissions and a statistically derived spectra observed over the 2-year lifetime of the mission can be interpreted in a self-consistent manner. The analysis, which predicts all spectral peaks within 4% of the observed peaks, interprets the higher-frequency emissions as due to low group velocity Bernsteinmode waves and interprets the lower-frequency emissions as eigenmodes of cylindrical-electromagnetic plasma oscillations. The demarcation between these two classes of emissions is the electron plasma frequency fpe where an emission is often observed. This fpe emission is not necessarily the strongest. None of the observed banded emissions were attributed to the upper hybrid frequency. We present Alouette 2 and ISIS 1 plasma resonance data and model electron temperature (Te) values to support the argument that the frequency spectrum of ionospheric sounder-stimulated emissions is not strongly temperature dependent and thus that the interpretation of these emissions in the ionosphere is relevant to other plasmas (such as the magnetosphere) where N e and T e can be quite different but where the ratio fpe/fee is identical. The N e values deduced from the spectral interpretation do not agree with the values determined from the AMPTEB_RM three-dimensional plasma instrument. The latter, which represent a lower •ound, are found to be higher than the former by a factor of 3.2 -3.5. All values were less than 1 cm-, a domain known for measurement difficulties. One possible explanation is that the wave and plasma techniques respond to different components of a non-Maxwellian magnetospheric electron distribution.

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The Plasma Wave Instrument on Board the AMPTE IRM Satellite

Cited by 39 publications

References 12 publications

Radial localization of magnetospheric guided poloidal Pc 4‐5 waves

Radial localization of magnetospheric guided poloidal Pc 4‐5 waves

A comparison of the plasma wave spectra for the eight AMPTE chemical releases

An interpretation of banded magnetospheric radio emissions

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