Concerning the generation of geomagnetic giant pulsations by drift-bounce resonance ring current instabilities

Glaßmeier, Karl‐Heinz; Buchert, Stephan; Motschmann, U.; Korth, A.; Pedersen, A.

doi:10.1007/s00585-999-0338-4

Cited by 70 publications

(129 citation statements)

References 30 publications

Supporting

Mentioning

125

Contrasting

Unclassified

Order By: Relevance

“…[41] Previous studies have reported satellite and groundbased observations of ULF waves associated with the unstable ring current protons [e.g., Hughes et al, 1978;Glassmeier et al, 1999;Wright et al, 2001]. They suggested that the drift-bounce resonance of these protons with nonMaxwellian distribution be responsible for the generation of the observed ULF waves.…”

Section: Comparison With Previous Studiesmentioning

confidence: 99%

“…However, the modulations of ring current ions, especially of O + , with ULF standing waves and the presumed acceleration process of these ions have been rarely reported. In contrast, the ring current ions (particular H + ) were always thought to be a free energy source in generating ULF waves in the magnetosphere [e.g., Hughes et al, 1978;Glassmeier et al, 1999;Wright et al, 2001].…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The role of ULF waves interacting with oxygen ions at the outer ring current during storm times

Yang

Zong

et al. 2011

J. Geophys. Res.

Self Cite

View full text Add to dashboard Cite

[1] The modulations of the outer ring current O + ion fluxes by ULF Pc5 waves are investigated by multisatellite observations during storm times. The O + ions have energies up to tens of keV. We concentrate on the process in terms of drift-bounce resonance of O + ions with ULF standing waves to understand whether the ring current O + ions could be accelerated/decelerated by ULF waves. Two case studies are performed, in which the Cluster satellites travel the outer ring current region in the morning sector with radial distances of about 5.5 R E . Distinct O + ion flux oscillations are observed associated with fundamental mode ULF standing waves. On 25 October 2002, both satellites SC1 and SC4 observe strong poloidal and toroidal standing waves at approximately the same region one by one with a time lag of 45 min. The O + ion flux oscillations at around 20 keV are dominantly coherent with the poloidal standing wave at 3.4 mHz with cross phases of near 90°with respect to the magnetic field waves. The O + phase space density spectra at 10 to 25 keV, measured by both satellites, deviate significantly from the typical power law distribution. We suggest that the O + ions at 10 to 25 keV are accelerated due to drift-bounce resonance with the poloidal standing wave. On 4 November 2002, satellite SC1 observes considerable poloidal and toroidal standing waves. The O + ion flux oscillation at around 7 keV is well correlated with both of the two wave modes at 3.7 mHz with cross phases of about 90°with respect to the magnetic field waves. The O + spectra at 4 to 8 keV deviates remarkably from the background power law distribution. When satellite SC4 closely encounters the same region 40 min later, the wave activities at 3.7 mHz are found to be rather weak and the O + spectra is close to the background power law distribution. We suggest that the spectra variation of SC1 results from the deceleration of O + ion at 4 to 8 keV via drift-bounce resonances during the strong wave activities. The observations made in this study reveal the effective role of ULF standing waves in accelerating/decelerating the ring current O + ions.Citation: Yang, B., Q.-G. Zong, S. Y. Fu, X. Li, A. Korth, H. S. Fu, C. Yue, and H. Reme (2011), The role of ULF waves interacting with oxygen ions at the outer ring current during storm times,

show abstract

Section: Comparison With Previous Studiesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The role of ULF waves interacting with oxygen ions at the outer ring current during storm times

Yang

Zong

et al. 2011

J. Geophys. Res.

Self Cite

View full text Add to dashboard Cite

show abstract

“…We still do not fully know what changes can be introduced into this picture by the azimuthal inhomogeneity of the magnetosphere and the associated field-aligned currents, the wide-band character and the possible narrow localization of oscillation sources, the interaction of waves with particles drifting in the magnetosphere, and the active role of the ionosphere. Work in this direction is underway, and this is testified by recently published papers addressing these issues (Salat and Tataronis, 1999;Klimushkin et al, 1995;Mann et al, 1997;Leonovich, 2000;Antonova et al, 2000;Vetoulis and Chen, 1996;Klimushkin, 2000;Glassmeier et al, 1999a;Leonovich and Mazur, 1996). However, the creation of a unified realistic model of MHD waves in the magnetosphere is a long way from now.…”

Section: On the Observation Of Toroidal And Poloidal Alfvén Waves In mentioning

confidence: 99%

Toroidal and poloidal Alfvén waves with arbitrary azimuthal wavenumbers in a finite pressure plasma in the Earth's magnetosphere

Klimushkin

Mager

Glaßmeier³

2004

Ann. Geophys.

Self Cite

124

View full text Add to dashboard Cite

Abstract. In this paper, in terms of an axisymmetric model of the magnetosphere, we formulate the criteria for which the Alfvén waves in the magnetosphere can be toroidally and poloidally polarized (the disturbed magnetic field vector oscillates azimuthally and radially, respectively). The obvious condition of equality of the wave frequency ω to the toroidal (poloidal) eigenfrequency T N ( P N ) is a necessary and sufficient one for the toroidal polarization of the mode and only a necessary one for the poloidal mode. In the latter case we must also add to it a significantly stronger condition, where m is the azimuthal wave number, and N is the longitudinal wave number. In cold plasma (the plasma to magnetic pressure ratio β = 0) the left-hand side of this inequality is too small for the routinely recorded (in the magnetosphere) second harmonic of radially polarized waves, therefore these waves must have nonrealistically large values of m. By studying several models of the magnetosphere differing by the level of disturbance, we found that the left-hand part of the poloidality criterion can be satisfied by taking into account finite plasma pressure for the observed values of m ∼ 50 − 100 (and in some cases, for even smaller values of the azimuthal wave numbers). When the poloidality condition is satisfied, the existence of two types of radially polarized Alfvén waves is possible. In magnetospheric regions, where the function P N is a monotonic one, the mode is poloidally polarized in a part of its region of localization. It propagates slowly across magnetic shells and changes its polarization from poloidal to toroidal. The other type of radially polarized waves can exist in those regions where this function reaches its extreme values (ring current, plasmapause). These waves are standing waves across magnetic shells, having a poloidal polarization throughout the region of its existence. Waves of this type are likely to be exemplified by giant pulsations. If the poloidality condition is not satisfied, then the mode is toroidally polarized throughout the region of its existence. Furthermore, itCorrespondence to: D. Yu. Klimushkin (klimush@iszf.irk.ru) has a resonance peak near the magnetic shell, the toroidal eigenfrequency of which equals the frequency of the wave.

show abstract

“…Ring current ions (mainly H ? ) with a positive gradient in velocity space (Gkioulidou et al 2014) are a potential source of ULF wave generation through drift-bounce resonance (e.g., Hughes et al 1978;Glassmeier et al 1999;. Low-energy ring current O ?…”

Section: Introductionmentioning

confidence: 99%

The interaction of ultra-low-frequency pc3-5 waves with charged particles in Earth’s magnetosphere

Zong

Rankin

Zhou

2017

Rev. Mod. Plasma Phys.

142

162

View full text Add to dashboard Cite

One of the most important issues in space physics is to identify the dominant processes that transfer energy from the solar wind to energetic particle populations in Earth's inner magnetosphere. Ultra-low-frequency (ULF) waves are an important consideration as they propagate electromagnetic energy over vast distances with little dissipation and interact with charged particles via drift resonance and drift-bounce resonance. ULF waves also take part in magnetosphereionosphere coupling and thus play an essential role in regulating energy flow throughout the entire system. This review summarizes recent advances in the characterization of ULF Pc3-5 waves in different regions of the magnetosphere, including ion and electron acceleration associated with these waves.

show abstract

Concerning the generation of geomagnetic giant pulsations by drift-bounce resonance ring current instabilities

Cited by 70 publications

References 30 publications

The role of ULF waves interacting with oxygen ions at the outer ring current during storm times

The role of ULF waves interacting with oxygen ions at the outer ring current during storm times

Toroidal and poloidal Alfvén waves with arbitrary azimuthal wavenumbers in a finite pressure plasma in the Earth's magnetosphere

The interaction of ultra-low-frequency pc3-5 waves with charged particles in Earth’s magnetosphere

Contact Info

Product

Resources

About