Alfvén Waves and Their Roles in the Dynamics of the Earth’s Magnetotail: A Review

Keiling, A.

doi:10.1007/s11214-008-9463-8

Cited by 151 publications

(131 citation statements)

References 202 publications

Supporting

Mentioning

128

Contrasting

Unclassified

Order By: Relevance

“…More references can be found in Keiling (2009). More recently, Hull et al (2010) performed a case study of the development of an acceleration region based on multi-point Cluster observations in the high altitude auroral zone, across the plasma sheet and into the polar cap.…”

Section: F Mottez: Parallel Electric Fieldsmentioning

confidence: 99%

Non-propagating electric and density structures formed through non-linear interaction of Alfvén waves

Mottez

2012

Ann. Geophys.

View full text Add to dashboard Cite

Abstract. In the auroral zone of the Earth, the electron acceleration by Alfvén waves is sometimes seen as a precursor of the non-propagating acceleration structures. In order to investigate how Alfvén waves could generate non-propagating electric fields, a series of simulations of counter-propagating waves in a homogeneous medium is presented. The waves propagate along the ambient magnetic field direction. It is shown that non-propagating electric fields are generated at the locus of the Alfvén waves crossing. These electric fields have a component orientated along the direction of the ambient magnetic field, and they generate a significant perturbation of the plasma density. The non-linear interaction of down and up-going Alfvén waves might be a cause of plasma density fluctuations (with gradients along the magnetic field) on a scale comparable to those of the Alfvén wavelengths. The present paper is mainly focused on the creation process of the non-propagating parallel electric field.

show abstract

Section: F Mottez: Parallel Electric Fieldsmentioning

confidence: 99%

Non-propagating electric and density structures formed through non-linear interaction of Alfvén waves

Mottez

2012

Ann. Geophys.

View full text Add to dashboard Cite

show abstract

“…The V Y component may appear, for example, due to the propagation of the MHD Alfvén waves (see e.g. Keiling et al 2009). These waves may be excited by different types of plasma instabilities (Angelopoulos et al 1989;Takada et al 2005Takada et al , 2006, including Kelvin-Helmholtz instability arising in PSBL due to propagation of accelerated field-aligned plasma flows with velocities larger than twice the Alfvén velocity (Burinskaya 2008;Grigorenko et al 2010a).…”

Section: Spatial and Temporal Characteristics Of Type-i Ion Beamsmentioning

confidence: 99%

Non-adiabatic Ion Acceleration in the Earth Magnetotail and Its Various Manifestations in the Plasma Sheet Boundary Layer

et al. 2011

View full text Add to dashboard Cite

Many physical phenomena in space involve energy dissipation which generally leads to charged particle acceleration, often up to very high energies. In the Earth magnetosphere energy accumulation and release occur in the magnetotail, namely in its Current Sheet (CS). The kinetic analysis of non-adiabatic ion trajectories in the CS region with finite but positive normal component of the magnetic field demonstrated that this region is essentially non-uniform in terms of scattering characteristics of ion orbits and contains spatially localized, well-separated sites of enhanced and reduced chaotization. The latter represent sources from which accelerated and energy-collimated ions are ejected into Plasma Sheet 134 E.E. Grigorenko et al.Boundary Layer (PSBL) and stream towards the Earth. Numerical simulations performed as part of a Large-Scale Kinetic Model have shown the multiplet ion structure of the PSBL is formed by a set of ion beams (beamlets) localized both in physical and velocity space. This structure of the PSBL is quite different from the one produced by CS acceleration near a magnetic reconnection region in which more energetic ion beams are generated with a broad range of parallel velocities. Multi-point Cluster observations in the magnetotail PSBL not only showed that non-adiabatic ion acceleration occurs on closed magnetic field lines with at least two CS sources operating simultaneously, but also allowed an estimation of their spatial and temporal characteristics. In this paper we discuss and compare the PSBL manifestations of both mechanisms of CS particle acceleration: one based on the peculiar properties of non-adiabatic ion trajectories which operates on closed magnetic field lines and the other representing the well-explored mechanism of particle acceleration during the course of magnetic reconnection. We show that these two mechanisms supplement each other and the first operates mostly during quiescent magnetotail periods.

show abstract

“…At present, the idea that downgoing waves may play a role during flares is considered more novel, although some progress in this field has been made by Emslie & Sturrock (1982), Melrose (1992), Wheatland & Melrose (1994), Liu et al (2006), Fletcher & Hudson (2008), Stasiewicz & Ekeberg (2008), Birn et al (2009), McClements & Fletcher (2009), Haerendel (2009, 2012, Bian et al (2010), Bian & Kontar (2011), Tsiklauri (2012 and Russell & Fletcher (2013). Downgoing waves are also thought to play an important role in Alfvénic auroras that is in some ways analogous (Stasiewicz et al 2000;Chaston et al 2002Chaston et al , 2007Semeter et al 2005;Keiling 2009;Watt & Rankin 2010).…”

Section: Introductionmentioning

confidence: 99%

Solar flares and focused energy transport by MHD waves

Russell

Stackhouse

2013

A&A

View full text Add to dashboard Cite

Context. Transport of flare energy from the corona to the chromosphere has traditionally been assigned to electron beams; however, interest has recently been renewed in magnetohydrodynamic (MHD) waves as a complementary or alternative mechanism. Aims. We determine whether, and under what conditions, MHD waves deliver spatially localised energy to the chromosphere, as required if MHD waves are to contribute to emission from flare ribbons and kernels. This paper also highlights several properties of MHD waves that are relevant to solar flares and demonstrates their application to the flare problem. Methods. Transport is investigated using a magnetic arcade model and 2.5D MHD simulations. Different wave polarisations are considered and the effect of fine structuring transverse to the magnetic field is also examined. Ray tracing provides additional insight into the evolution of waveguided fast waves. Results. Alfvén waves are very effective at delivering energy fluxes to small areas of chromosphere, localisation being enhanced by magnetic field convergence and phase mixing. Fast waves, in the absence of fine coronal structure, are more suited to powering emission from diffuse rather than compact sources; however, fast waves can be strongly localised by coronal waveguides, in which case focused energy is best transported to the chromosphere when waveguides are directly excited by the energy release. Conclusions. MHD waves pass an important test for inclusion in future flare models.

show abstract

Alfvén Waves and Their Roles in the Dynamics of the Earth’s Magnetotail: A Review

Cited by 151 publications

References 202 publications

Non-propagating electric and density structures formed through non-linear interaction of Alfvén waves

Non-propagating electric and density structures formed through non-linear interaction of Alfvén waves

Non-adiabatic Ion Acceleration in the Earth Magnetotail and Its Various Manifestations in the Plasma Sheet Boundary Layer

Solar flares and focused energy transport by MHD waves

Contact Info

Product

Resources

About