Alfvénic field line resonances in arbitrary magnetic field topology

Rankin, R.; Кабин, К.; Marchand, R.

doi:10.1016/j.asr.2005.09.034

Cited by 51 publications

(74 citation statements)

References 24 publications

(50 reference statements)

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“…We note that in the particular case of compressed dipole background field, we have explicit expressions for the fieldaligned coordinate system as functions of the usual spherical coordinates. This greatly simplifies our calculations and makes many numerical steps described in the previous papers (Rankin et al, 2005(Rankin et al, , 2006Kabin et al, 2007) unnecessary. The availability of analytical expressions for the gradients of the coordinates also allows us to minimize numerical errors.…”

Section: Eigenmode Equationsmentioning

confidence: 99%

“…We follow the approach of Rankin et al (2006) and write equations for the standing shear Alfvén wave as …”

Section: Eigenmode Equationsmentioning

confidence: 99%

“…For this system of equations, we need to solve a two-parameter eigenvalue problem for the period of the standing Alfvén wave and its polarization at one of the ionospheres. The polarization of the wave at any other point along the field line is then computed from the corresponding eigenfunctions, see Rankin et al (2006) for details. This approach to computing Alfvénic frequencies of the field lines and polarizations of the standing shear Alfvén waves is more self-consistent than the commonly used approach of Singer et al (1981), in which the polarizations of the waves have to be imposed explicitly.…”

Section: Eigenmode Equationsmentioning

confidence: 99%

“…The compressed dipole model includes interplanetary magnetic field (IMF), open, and closed field lines and somewhat realistically mimics the compression of the day-side magnetosphere and stretching of the magnetotail on the nightside. Next, we apply to this field a recently developed standing shear Alfvén wave model (Rankin et al, 2006) which allows us to compute self-consistently both the frequency and polarization of the standing shear Alfvén wave in the cold plasma approximation. This allows us to test, for the first time, some of the assumptions used by Elkington et al (2003).…”

Section: Introductionmentioning

confidence: 99%

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Polarization properties of standing shear Alfvén waves in non-axisymmetric background magnetic fields

et al. 2007

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Abstract. In this paper we present results concerning periods and polarizations of cold plasma ultra-low frequency (ULF) guided Alfvén waves in a non-axisymmetric geomagnetic field. The background geomagnetic field is approximated by a compressed dipole for which we propose a simple description in terms of Euler potentials. This study is motivated by the problem of outer-radiation belt electron acceleration by ULF waves, for which the polarization of the wave is of paramount importance. We consider an approximation appropriate to decoupled Alfvénic waves and find that the polarization of the waves can change significantly with local time. Therefore, the ULF wave's contribution to the MeV electron energization process can be localized in space.

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Section: Eigenmode Equationsmentioning

confidence: 99%

“…We follow the approach of Rankin et al (2006) and write equations for the standing shear Alfvén wave as …”

Section: Eigenmode Equationsmentioning

confidence: 99%

Section: Eigenmode Equationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Polarization properties of standing shear Alfvén waves in non-axisymmetric background magnetic fields

et al. 2007

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“…This coupling is due to the Alfven waves propagating practically along magnetic field lines, their frequency, for a fixed wavelength, is determined by the magnitude of the Alfven speed. Many-both theoretical (Inhester, 1987;Lee and Lysak, 1989;Leonovich and Mazur, 1989;Rankin et al, 2006), and experimental (Cheng et al, 1998;Rankin et al, 2005;Agapitov et al, 2009) (see also review by Pilipenko, 1990)-papers have scrutinised the Alfven resonance during magnetospheric phenomena.…”

Section: Introductionmentioning

confidence: 99%

Magnetosonic resonances in the magnetospheric plasma

Leonovich

Козлов

2013

Earth Planet Sp

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A problem of coupling between fast and slow magnetosonic waves in Earth's magnetosphere (magnetosonic resonance) is examined. Propagation both slow magnetosonic wave and Alfven wave can easily be canalized along the magnetic field line direction. The main difference between the two is that slow magnetosonic waves dissipate strongly due to their interaction with the background plasma ions, whose temperature is above the electron temperature. In Earth's magnetosphere, however, there is a region where the dissipation of slow magnetosonic waves can be weak-the inner plasmasphere. The slow magnetosonic waves generated there can be registered directly. In other regions, with strong dissipation of slow magnetosonic waves, their signature may be detected through their impact on the Alfven resonance at frequencies for which the resonant Alfven and slow magnetosonic waves exist simultaneously in the magnetosphere. Owing to their strong coupling with the background plasma ions, resonant slow magnetosonic waves can transfer the energy and impulse from the solar wind to the magnetospheric plasma ions via fast magnetosonic waves penetrating into the tail lobes. A problem of resonant conversion of fast magnetosonic waves into slow magnetosonic oscillations in a magnetosphere with dipole-like magnetic field is also examined.

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Field line resonances as a trigger and a tracer for substorm onset

et al. 2014

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In this paper, we show that periodic auroral arc structures are seen at the location of one particular auroral substorm onset for the 15 min preceding onset, suggesting that field line resonances should be considered a strong candidate for triggering substorm onset. Irrespective of whether this field line resonance is coincidentally or causally linked to this substorm onset, the characteristics of the field line resonance can be used to remote sense the characteristics of the geomagnetic field line that supports substorm onset. In this instance, the eigenfrequency of this resonance is around 12 mHz. Interestingly, however, there is no evidence of this field line resonance in a seven satellite major Time History of Events and Macroscale Interactions during Substorms (THEMIS)-GOES conjunction, ranging from geosynchronous orbit to~30 R E . However, using space-based cross-phase measurements of the local field line eigenfrequency at the inner THEMIS locations, we find that the local field line eigenfrequency is 6-10 mHz. Hence, we can reliably say that this 12 mHz Field Line Resonance (FLR) must lie inside of THEMIS locations. Our conclusion is that a high-m field line resonance can both represent a strong candidate for a trigger for substorm onset, as first proposed by Samson et al. (1992), and that its characteristics can provide invaluable information as to where substorm onset occurs in the magnetosphere.

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Alfvénic field line resonances in arbitrary magnetic field topology

Cited by 51 publications

References 24 publications

Polarization properties of standing shear Alfvén waves in non-axisymmetric background magnetic fields

Polarization properties of standing shear Alfvén waves in non-axisymmetric background magnetic fields

Magnetosonic resonances in the magnetospheric plasma

Field line resonances as a trigger and a tracer for substorm onset

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