ULF waves at Mercury: Earth, the giants, and their little brother compared

Glaßmeier, Karl‐Heinz; Klimushkin, D. Yu.; Othmer, Carsten; Mager, P. N.

doi:10.1016/j.asr.2003.04.047

Cited by 53 publications

(49 citation statements)

References 28 publications

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“…If the ratio ω/ω ci is finite, the resonant excitation of Alfvén waves via coupling to FMS waves is possible even for the special case m=0 (e.g. Leonovich et al, 1983;Timofeev, 1992;Glassmeier et al, 2003). This is due to the fact that at finite gyrofrequencies and assuming a vanishing electric field along the background magnetic field, the MHD wave dispersion relation becomes (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…Alfvén resonances, also called field line resonances, are one of the key physical processes in the magnetosphere of the Earth (Tamao, 1965;Hasegawa and Chen, 1974;Southwood, 1974) and other planets (Khurana, 1993; Correspondence to: D. Klimushkin (klimush@iszf.irk.ru) Glassmeier et al, 1999Glassmeier et al, , 2004Othmer et al, 1999). Treatment of this phenomenon in a one-dimensional inhomogeneous model of the magnetosphere, using a one-fluid MHD plasma model, is as follows.…”

Section: Introductionmentioning

confidence: 99%

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Axisymmetric Alfvén resonances in a multi-component plasma at finite ion gyrofrequency

Klimushkin

Mager

Glaßmeier³

2006

Ann. Geophys.

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Abstract. This paper deals with the spatial structure of zero azimuthal wave number ULF oscillations in a 1-D inhomogeneous multi-component plasma when a finite ion gyrofrequency is taken into account. Such oscillations may occur in the terrestrial magnetosphere as Pc1-3 waves or in the magnetosphere of the planet Mercury. The wave field was found to have a sharp peak on some magnetic surfaces, an analogy of the Alfvén (field line) resonance in one-fluid MHD theory. The resonance can only take place for waves with frequencies in the intervals ω<ω ch or 0 <ω<ω cp , where ω ch and ω cp are heavy and light ions gyrofrequencies, and 0 is a kind of hybrid frequency. Contrary to ordinary Alfvén resonance, the wave resonance under consideration takes place even at the zero azimuthal wave number. The radial component of the wave electric field has a pole-type singularity, while the azimuthal component is finite but has a branching point singularity on the resonance surface. The later singularity can disappear at some frequencies. In the region adjacent to the resonant surface the mode is standing across the magnetic shells.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Axisymmetric Alfvén resonances in a multi-component plasma at finite ion gyrofrequency

Klimushkin

Mager

Glaßmeier³

2006

Ann. Geophys.

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“…For Mercury, where the magnetic field is relatively weak, the wavelength of field-aligned modes can be comparable to the size of the magnetosphere. Therefore, IIH waves oscillate globally along the magnetic field lines for Mercury, similar to the field line resonance on Earth (Othmer et al 1999;Glassmeier et al 2003Glassmeier et al , 2004Klimushkin et al 2006;Kim et al 2008Kim et al , 2011aKim et al , 2013Kim et al , 2015a. On the other hand, on Earth, the magnetic field strength is larger and the wavelength is shorter, which typically localizes mode converted waves between the Buchsbaum cutoff locations, which occur at around 10 degrees latitude.…”

Section: Introductionmentioning

confidence: 99%

Localization of Ultra-Low Frequency Waves in Multi-Ion Plasmas of the Planetary Magnetosphere

Kim¹,

Lee²

2015

Journal of Astronomy and Space Sciences

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“…They have been observed in every planetary magnetosphere (Glassmeier et al, 2004) including Mercury (Russell, 1989. In the case of Earth, ULF waves are standing MHD waves in the magnetospheric system with the north and south ionosphere being the boundaries where the oscillations exhibit a mode (Kivelson, 1995;Glassmeier et al, 2004).…”

Section: Introductionmentioning

confidence: 99%

“…In the case of Earth, ULF waves are standing MHD waves in the magnetospheric system with the north and south ionosphere being the boundaries where the oscillations exhibit a mode (Kivelson, 1995;Glassmeier et al, 2004). The magnetosphere of Mercury, on the other hand, has no significant ionosphere, and it is a rather stiff magnetosphere, and it can start to ring under the influence of solar wind dynamic pressure variations (Glassmeier et al, 2004).…”

Section: Introductionmentioning

confidence: 99%

Wavelet analysis of ULF waves in the mercury's magnetosphere

Echer¹

2010

Rev. Bras. Geof.

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ABSTRACT. Ultra-low-frequency (ULF) waves have been observed in the Mercury's magnetosphere. In this work, Mariner-10 and MESSENGER high resolution magnetic field data are studied with wavelet analysis. Two ULF wave intervals have been selected: 29 March 1974 (Mariner-10) and 14 January 2008 (MESSENGER).Non-stationary oscillations, with strong amplitude and narrow bandwidth have been found. The Mariner-10 ULF wave interval showed periods of ∼1.5-3.0 s, and the MESSENGER ULF wave interval had periods of ∼0.5-1.0 s. These periods of ULF waves are slightly longer than the proton gyroperiods (∼0.8 and ∼0.5 s, respectively).Therefore, these waves are most likely kinetic, not magnetohydrodynamic waves.

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ULF waves at Mercury: Earth, the giants, and their little brother compared

Cited by 53 publications

References 28 publications

Axisymmetric Alfvén resonances in a multi-component plasma at finite ion gyrofrequency

Axisymmetric Alfvén resonances in a multi-component plasma at finite ion gyrofrequency

Localization of Ultra-Low Frequency Waves in Multi-Ion Plasmas of the Planetary Magnetosphere

Wavelet analysis of ULF waves in the mercury's magnetosphere

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