Magnetopause Waves Controlling the Dynamics of Earth's Magnetosphere
Magnetopause Waves Controlling the Dynamics of Earth's Magnetosphere
Journal of Astronomy and Space Sciences. 2015. Mar, 32(1): 1-11
Copyright © 2015, The Korean Space Science Society
This is an Open Access article distributed under the terms of the Creative Commons Attribution Non-Commercial License ( which permits unrestricted non-commercial use, distribution, and reproduction in any medium, provided the original work is properly cited.
  • Received : February 24, 2015
  • Accepted : March 05, 2015
  • Published : March 15, 2015
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Kyoung-Joo, Hwang
Goddard Planetary Heliophysics Institute, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA

Earth’s magnetopause separating the fast and often turbulent magnetosheath and the relatively stagnant magnetosphere provides various forms of free energy that generate low-frequency surface waves. The source mechanism of this energy includes current-driven kinetic physical processes such as magnetic reconnection on the dayside magnetopause and flux transfer events drifting along the magnetopause, and velocity shear-driven (Kelvin-Helmholtz instability) or density/pressure gradient-driven (Rayleigh-Taylor instability) magnetohydro-dynamics (MHD) instabilities. The solar wind external perturbations (impulsive transient pressure pulses or quasi-periodic dynamic pressure variations) act as seed fluctuations for the magnetopause waves and trigger ULF pulsations inside the magnetosphere via global modes or mode conversion at the magnetopause. The magnetopause waves thus play an important role in the solar wind-magnetosphere coupling, which is the key to space weather. This paper presents recent findings regarding the generation of surface waves (e.g., Kelvin-Helmholtz waves) at the Earth’s magnetopause and analytic and observational studies accountable for the linking of the magnetopause waves and inner magnetospheric ULF pulsations, and the impacts of magnetopause waves on the dynamics of the magnetopause and on the inner magnetosphere.
The solar wind carrying the interplanetary magnetic field (IMF) outward through the Solar System features a variety of temporal variations in plasma and field parameters and/or multi-scale structures. The magnetopause is the outer boundary of the Earth’s magnetic shield, being an interface between the time-varying solar wind and the relatively stagnant magnetosphere. Solar wind mass, momentum, and energy are, however, transferred across the magnetopause via magnetopause dynamics such as magnetic reconnection (e.g., Russell & Elphic 1978 ), kinetic Alfvén waves or ion gyro-radius scale waves (e.g., Chaston et al. 2007 , Yao et al. 2011 ), or Kelvin-Helmholtz waves (e.g., Southwood 1968 ).
The importance of the magnetopause in the solar wind–magnetosphere coupling arises not only from its shape and location in response to interplanetary solar wind drivers, which, for example, leads to significant losses in the outer radiation belt electron fluxes to the magnetopause (e.g., Loto’aniu et al. 2010 , Turner et al. 2012 ), but also more importantly from physical processes occurring at the magnetopause. Physical processes occurring at the magnetopause include magnetopause waves/oscillations and magnetic reconnection, which both provide multiple channels by which solar wind enters the magnetosphere, and inner magnetospheric particle populations can be enhanced or lost. In particular, Ultra-Low-Frequency (ULF; 1 mHz ≤ f ≤ 10 Hz) waves inside the magnetosphere are thought to be generated by the Kelvin-Helmholtz waves excited along the magnetopause and contribute to radial transport, losses, and enhancements of the radiation belt electron fluxes (e.g., Elkington et al. 2002 , Loto’aniu et al. 2010 ). Dayside reconnection can drive outer and inner boundary motion and supply source populations to the radiation belts and ring current via storms and substorms. Flux transfer events (FTEs) generated by bursty or patchy reconnection drift along the magnetopause, exciting undulations of the magnetopause.
The dynamics of the magnetopause regulate magnetospheric responses to external interplanetary drivers (such as pressure pulses and quasi-periodic dynamic pressure perturbations) via frequency filtering of pristine solar wind or magnetosheath perturbations. In a steady state, the position of the magnetopause is determined by the balance between the total magnetosheath pressure, mostly contributed by the solar wind dynamic pressure, and the magnetospheric magnetic-field pressure (e.g., Aubry et al. 1971 , Glassmeier et al. 2008 ). Various approaches to model magnetopause perturbations around the stagnation point ( Smit 1968 , Freeman et al. 1995 , Børve et al. 2011 ) predicted damped harmonic oscillations for the magnetopause motion, having typical periods ranging from 2 to 12 min. This agrees well with in-situ observations of magnetopause fluctuations of periods of 3-5 to 10-15 min (e.g., Farrugia & Gratton 2011 ). The damping ratio and the transmissibility indicate that the magnetopause acts like a low-pass filter to suppress frequency modes that are much higher than the characteristic magnetopause and/or local field line resonance frequencies. Archer et al. (2013) demonstrated that impulsive and broadband magnetosheath pressure pulses are processed at the magnetopause into much smoother perturbations with longer periods (typically in the Pc5-6 range).
Recently, advanced multi-spacecraft, numerical simulations, and ground magnetometer/radar networks have enabled us to analyze the generation of magnetopause waves and their effects on the inner and outer magnetospheric dynamics. This paper reviews the role of the boundary waves in the dynamics of the magnetopause and the inner magnetosphere. In particular, Kelvin-Helmholtz waves and their nonlinear development into large-scale rolledup Kelvin-Helmholtz vortices have drawn increasing attention regarding their effects on solar wind entry across the magnetopause. This paper addresses theoretical and observational mechanisms responsible for the magnetopause waves triggering inner magnetospheric pulsations: cavity/waveguide/global modes (section 2); Kelvin-Helmholtz waves (section 3); and magnetic reconnection-driven processes (section 4). Conclusions follow in section 5.
Wave activity in the magnetosphere is often monochromatic and localized in latitude ( Walker et al. 1979 ). In particular, ULF waves are typically observed on the ground in the Pc3-5 frequency range (Pc3: 22–100 mHz; Pc4: 45–150 mHz; Pc5: 2–7 mHz) at mid to high latitudes. Early studies (e.g., Stix 1962 , Alfvén & Fälthammar 1963 ) reported that these wave modes have wavelengths comparable to the dimension of the magnetosphere cavity that is often bounded by the magnetopause and a turning point in the inner magnetosphere. Standing fast mode waves trapped between those magnetospheric boundaries are known as cavity modes or global modes (e.g., Kivelson & Southwood 1985 ). The boundaries are assumed to behave as perfect reflectors for waves, via strong gradients in physical quantities. Waves sustained in the magnetosphere cavity signify eigenfrequencies, which are determined by plasma conditions (e.g., the radial profile of the Alfvén speed) and the topology and the dimension of the cavity. Auroral HF-radar observations of discrete resonance frequencies at 1.3, 1.9, 2.3, 2.6, … mHz ( Walker et al. 1992 , Fenrich et al. 1995 ) are, however, too low to explain the wave cutoff location inside the magnetosphere. This has led to waveguide models where the energy of the fast mode waves that propagate azimuthally resonates radially between the magnetopause and a reflection region in the inner magnetosphere ( Harrold & Samson 1992 , Wright 1994 ).
The cavity/waveguide theory predicts that the mode traps energy of discrete-frequency fast waves between the outer and inner boundaries. The fast mode is thought to excite field line resonances (FLRs; standing shear Alfvén mode forming between perfectly reflecting ionospheres in the northern and southern hemispheres) at locations where the fast mode frequencies match the local Alfvén-wave frequency ( Southwood 1974 , Kivelson & Southwood 1985 ). When cavity modes excite FLRs, the Poynting flux should show an energy flow from the cavity mode into the FLR. Considering external sources that initially stimulate compressional modes, global modes behave like an intermediary that converts broadband solar-wind fluctuation energy to monochromatic, localized shear Alfvén waves ( Hartinger et al. 2012 ). Energy transport from the magnetopause to deep within the magnetosphere (often inside the plasmasphere) is also explained in the context of “quasi-cavity” modes where wave energy leaks through the imperfect boundaries ( Zhu & Kivelson 1989 , Lee & Kim 1999 ).
The inner-magnetosphere ULF pulsations are well correlated with enhancements, radial transport, or modulation in low-energy and relativistic (> MeV) radiation belt electron fluxes ( Elkington et al. 2002 , Loto’aniu et al. 2010 ). ULF waves resonantly exchange energy with the particles when ω - d = b , where ω is the wave frequency, ωd =and ωb are a particle’s drift and bounce frequencies, and m and N are azimuthal and bounce mode wave numbers ( Southward & Kivelson 1981 ). Poloidal ULF modes with azimuthal electric field oscillations are thought to more effectively resonate with an individual particle than toroidal modes, which are classical FLRs in the cavity theory and are characterized by azimuthal magnetic field and radial electric field fluctuations. Elkington et al. (2003) , on the other hand, suggested that bulk electron acceleration through a drift-resonant interaction is favored when more toroidal than poloidal power exists.
Direct observational support for the excitation of the waveguide modes and the coupling of fast mode waves to FLRs is, however, somewhat sparse ( Sarafopoulos 2005 ), although ground-based observations provide some statistical support for the cavity mode mechanism. While it was suggested that cavity modes may be an insignificant energy source for the FLR excitation ( Allan et al. 1997 ), Richard & Wright (1995) , using a 2-D MHD waveguide model, reproduced ULF pulsations detected by the DE 1 spacecraft, which traversed L shells ranging from L ≈ 13 to L ≈ 4. Waters et al. (2002) , using MHD simulations with comparisons to AMPTE/CCE data, proposed that the global mode is best identified by the bz fluctuations associated with the phase structure of resonance. Recently, multipoint observations have significantly enhanced our ability to identify the cavity mode: Conjugate observations of groundbased FLRs and the same-frequency fast modes detected by Cluster suggested that compressional waves launched at the magnetopause drive the FLRs ( Clausen & Yeoman 2009 ); Takahashi et al. (2010) later reported fast mode waves in the Pc4 band trapped in the dayside plasmasphere. While more cavity modes were observed inside the plasmasphere, Hartinger et al. (2013) analyzed 72 global mode events occurring outside the plasmasphere. They showed that these resonance modes peaked at frequency between 10 mHz and 20 mHz and were preferentially detected near the noon local time during high speed solar wind conditions.
The ULF waves in the magnetosphere cavity can be excited by either internal or external sources. Internal sources include magnetospheric compressions that are internally driven associated with geomagnetic storms and substorms. External sources include magnetopause waves and quasi-periodic or impulsive variations in the solar wind. Early studies ( McHenry et al. 1990 , Mann et al. 1999 , 2002 ) suggested magnetopause waves such as Kelvin-Helmholtz waves that are generated along the velocity-shear layer between the fast magnetosheath flow and the relatively stagnant plasma sheet as the dominant excitation mechanism for fast mode energy. The coupling to magnetospheric ULF pulsations occurs at locations where the local field-line shell eigenfrequency equals the frequency of the driving Kelvin-Helmholtz waves. Although it was suggested that the role of Kelvin-Helmholtz waves in the ULF excitation is limited ( Takahashi et al. 1984 , Southwood 1968 ), recent multi-point measurements indicated that the Kelvin-Helmholtz instability powers waveguide modes: Mann et al. (2002) reported Cluster observations of quasi-periodic magnetopause motion and simultaneous ground observations of ULF FLRs; Rae et al. (2005) used coordinated Cluster and Polar observations to link Kelvin-Helmholtz waves and FLRs. Agapitov et al. (2009) provided details of a THEMIS event supporting a toroidal FLR mode generated by the Kelvin-Helmholtz instability on the magnetopause.
Fig. 1 shows another example of a classical FLR excited by Kelvin-Helmholtz waves ( Hwang et al. 2014 ). THEMIS-P2 traversing the dusk-side magnetopause observed surface waves identified by quasi-periodic fluctuations of the magnetic field and the plasma moments (density, flow vectors, and temperature) with a frequency of 1.9-2.0 mHz ( Figs. 1a and b ). The three inner THEMIS probes (P3-5) detected magnetic fluctuations peaked at a similar frequency of 1.8-1.9 mHz ( Fig. 1c ). These ULF pulsations are not directly correlated to the changes in solar wind dynamic pressure (not shown). The radial ( r ) and azimuthal ( φ ) components of the electric and magnetic field in the mean field-aligned coordinate system (upper panels of Fig. 1c ) show that Er exhibits stronger narrow-band wave power (with harmonics) than does Eφ . A 90° phase difference between Er nd Bφ indicates a toroidal mode, which is consistent with a classical FLR predicted from the waveguide theory.
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(a) THEMIS and Cluster configuration on May 25, 2009. (b) THEMIS-P2 observation of the magnetopause Kelvin-Helmholtz waves. (c) Simultaneous THEMIS-P5 observation of waveform and power spectra of electric and magnetic fields transformed to the mean field-aligned coordinate system in the inner magnetosphere. Er exhibits stronger narrow-band wave power (with harmonics) than does Eφ, and there is a 90° phase difference between Er and Bφ, indicating a toroidal-mode ULF structure. Corresponding low-energy plasma injection with density fluctuations is observed.
Since Dungey (1955) first proposed the importance of Kelvin-Helmholtz instability during northward IMF conditions, under which subsolar magnetic reconnection is suppressed, it has been suggested that Kelvin-Helmholtz waves provide a mechanism by which the solar wind enters into the magnetosphere. In particular, the nonlinear stage of Kelvin-Helmholtz instability, i.e., a rolled-up Kelvin-Helmholtz vortex, facilitates the solar wind transport via 1) diffusive transport through the turbulent decay of Kelvin-Helmholtz vortices or coalescence of neighboring vortices ( Matsumoto & Hoshino 2004 , 2006 , Cowee et al. 2009), 2) reconnection between stretched field lines due to the vortex motion ( Otto & Fairfield 2000 , Nykyri & Otto 2001 , Nakamura et al. 2011 ) and/or dual reconnection between the Kelvin-Helmholtz-stable lobe magnetic field and Kelvin-Helmholtz-induced engulfed magnetosheath field ( Takagi et al. 2006 ), or 3) kinetic Alfvén waves or ion gyro-radius scale waves via a mode conversion from Kelvin-Helmholtz waves ( Chaston et al. 2007 , Yao et al. 2011 ). Kelvin-Helmholtz waves thus are one of the candidate mechanisms for the formation of a broad and dense low-latitude boundary layer (LLBL) as a consequence of a mixture of solar wind and magnetospheric origin plasmas.
The Kelvin-Helmholtz instability condition for incompressible plasmas under the assumption that the velocity-shear interface layer has no thickness ( Chandrasekhar 1961 , Hasegawa 1975 ), however, shows no clear preference for northward over southward IMF:
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where v 1,2 , ρ 1,2 , and B 1,2 represent the flow velocity, plasma density, and magnetic field at sides 1 and 2 across the velocity shear interface and k represents the wave vector, which is typically anti-sunward. The velocity shear is typically subsonic at the dayside magnetopause, indicating a minor compressibility effect. The effect of the non-zero boundary thickness is also insignificant for the waves having wavelengths much larger than the boundary thickness. Thus, in general, Equation (1) is valid for Kelvin-Helmholtz waves in Earth’s dayside magnetopause environment. Equation (1) indicates that large velocity shear and/or plasma density, or a magnetic field perpendicular to k , lowers the instability threshold. Both northward and southward IMF provide the latter case where the magnetic field in the magnetospheric and magnetosheath sides are perpendicular to k for typically tailward-propagating Kelvin-Helmholtz waves along the flanks of the magnetosphere. Equation (1) also suggests that under southward IMF the Kelvin-Helmholtz mode can operate dominantly over or coexist with the tearing mode when the velocity shear is larger than or comparable to the local Alfvén velocity along k . Ma et al. (2014a , 2014b) used three-dimensional MHD and Hall MHD codes to show that magnetic reconnection and the Kelvin-Helmholtz mode can operate simultaneously on the magnetopause.
Nonlinearly developed Kelvin-Helmholtz waves under southward IMF were reported by Hwang et al. (2011) ( Fig. 2 ) and Yan et al. (2014) . Hwang et al. (2011) proposed that a spatially-irregular and temporally-intermittent evolution of Kelvin-Helmholtz waves leaves little chance to observe Kelvin-Helmholtz vortex structures under southward IMF. This idea is supported by global MHD simulations ( Collado-Vega et al. 2007 , Hwang et al. 2011 , Kuznetsova et al. 2008 ) demonstrating that under southward IMF Kelvin-Helmholtz vortices easily develop, but they quickly form as filamentary structures due to drifting flux ropes that originate at the subsolar magnetopause and disrupt previously formed vortices ( Fig. 3 ). In contrast, Kelvin-Helmholtz waves/vortices during northward IMF are relatively stationary and long-lasting.
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The first in-situ observation of highly-developed (formed as a vortical structure; see the bottom illustration) Kelvin-Helmholtz waves when the IMF is southward, i.e., oppositely aligned with the Earth’s magnetic field. The Cluster spacecraft detected both highly-developed Kelvin-Helmholtz vortices and lessdeveloped Kelvin-Helmholtz surface wave consecutively at the dawn-side (westward) flank of the night-side magnetospause during southward IMF conditions (Hwang et al. 2011): (a) the z-component of the magnetic field, (b) the electron energy spectrogram, (c) the electron pitch angle spectrogram, (d) the ion energy spectrogram, (e) plasma density, and (f) temperature. The repeated variations in these physical parameters indicate that the spacecraft passed by two different regions quasi-periodically. Kelvin-Helmholtz waves propagating along the magnetopause explain this periodicity well. The trajectory of the spacecraft, ‘C1’, relative to the Kelvin-Helmholtz wave structure is shown at the bottom of the figure. Seven sequential structures correspond to seven divisions separated by magenta vertical lines in the upper plot.
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MHD simulations of dayside dynamics (Kuznetsova et al. 2008). Under southward IMF, Kelvin-Helmholtz vortices are well developed along the magnetopause (A), but they quickly become unstable to fluctuations that originate from the subsolar magnetopause, such as flux transfer events (FTEs) drifting along the flank of the downtail magnetopause (B).
Recently, Hwang et al. (2012) reported the first in-situ observation of Kelvin-Helmholtz waves on the northern high-latitude magnetopause under strongly dawnward IMF conditions ( Fig. 4 ). Under radial (sunward or anti-sunward) IMF, expansion of the dayside magnetopause and enhanced magnetopause fluctuations caused by bow-shock origin phenomena are common features ( Dušik et al. 2010 , Omidi et al. 2009 , Suvorova et al. 2010 ). The magnetopause expansion causes the magnetopause to become unstable to Rayleigh-Taylor instability, and the Kelvin-Helmholtz instability combined with Rayleigh-Taylor instability drives the entire dayside magnetopause to become Kelvin-Helmholtz-unstable ( Farrugia et al. 1998 ). Gratton et al. (2012) and Farrugia et al. (2014) reported rolled-up Kelvin-Helmholtz vortices observed during a radial IMF. These studies indicate that Kelvin-Helmholtz waves are commonly observed over the entire surface of the dayside magnetopause for a wider range of IMF orientations than was previously thought, possibly providing a constant, although less efficient than reconnection, mechanism of solar wind transport into the magnetosphere.
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From Hwang et al. (2012). Illustrations of topologies of the magnetopause during (A) dawnward and (B) sunward IMF orientations for Cluster observations of Kelvin-Helmholtz waves on January 12, 2003. The IMF orientations are shown as red arrows and the regions of parallel or anti-parallel alignments between the IMF and Earth’s magnetospheric fields are marked by red shading. A slashed region indicates where Kelvin-Helmholtz waves preferentially occur on the surface of the magnetopause. The observed propagations of the Kelvin-Helmholtz waves are marked by green and blue (the low- and high-frequency modes, respectively, during westward IMF), and green (during radial IMF) arrows. Note that the magnetic configuration across the boundary layer near the northern duskward magnetopause during dawnward IMF is similar to that at the dayside flank magnetopause under northward IMF in that the magnetosheath and magnetospheric fields across the boundary layer are parallel, and both are perpendicular to the tailward propagation of the waves. This event suggests that Kelvin-Helmholtz waves can be generated and developed not only when the IMF is northward but also when the IMF is aligned with the dawn/duskward (A) and even sunward (B) directions.
Besides velocity-shear driven Kelvin-Helmholtz instability, other intrinsic instabilities operating at the magnetopause, such as current-driven instability, e.g., magnetic reconnection, can also provide seed perturbations for magnetopause motion. Magnetic reconnection on the dayside magnetopause controls the shape and location of the magnetopause, thereby modulating the properties of cavity/waveguide modes.
Non-steady bursty or intermittent reconnection, patchy reconnection, or sequential multiple X-line reconnection ( Phan et al. 2004 , Raeder 2006 , Hasegawa et al. 2010 ) can generate recurrent flux transfer events (FTEs) with an average separation time of a few to several minutes ( Wang et al. 2005 ). Russell & Elphic (1978) and Sckopke et al. (1983) noted that FTEs propagating along the downtail magnetopause produce magnetopause undulations similar to Kelvin-Helmholtz waves, possibly triggering the excitation of Kelvin-Helmholtz waves. Hasegawa et al. (2009) proposed that during northward IMF kinetic Alfvén waves that are excited through high-latitude reconnection and propagate toward lower latitudes cause perturbations in LLBL. These studies suggest a relationship between quasi-periodic reconnection at the subsolar (high-latitude) region under southward (northward) IMF and the quasi-periodic magnetopause perturbations. Such magnetopause perturbations, when their amplitudes are large, can launch compressional fast mode waves that traverse into the magnetosphere and excite inner magnetospheric ULF waves.
ULF waves themselves can regulate the dayside reconnection process. Prikryl et al. (1998) correlated the low-frequency (in Pc5 frequency range) oscillations with the IMF Bz component and convection patterns in the ionospheric footprints and suggested that ULF fluctuations in the solar wind modulate the rate of magnetic reconnection at the dayside magnetopause into pulses. Particle transit from the solar wind to the magnetosphere through magnetopause reconnection can facilitate ULF turbulence at the magnetopause ( Cornilleau-Wehrlin et al. 2008 ). Lee et al. (2014) reported that the fluxes of cold ions present at the magnetopause are modulated by the ULF oscillations of E × B drift. The importance of such cold and dense populations in the reconnection process is a topic of ongoing debate ( Cassak & Shay 2007 , Borovsky et al. 2008 , Drake et al. 2009 , Lee et al. 2013). Hwang et al. (2014) , using a THEMIS event, proposed that such cold ions of plasmaspheric plume or ionospheric outflow origin can play an important role in the competition between reconnection and Kelvin-Helmholtz instability during southward IMF, by reducing the reconnection rate but lowering the threshold of Kelvin-Helmholtz instability (Equation 1).
The Earth’s magnetopause provides diverse forms of free energy suitable for the growth of a variety of waves in association with kinetic-physics phenomena (such as magnetic reconnection in the dayside magnetopause and flux transfer events drifting along the downtail magnetopause) and velocity shear-driven or density/pressure gradient-driven MHD processes (e.g., Kelvin-Helmholtz or Rayleigh-Taylor instabilities). This paper reviewed those commonly observed magnetopause waves focusing on their generation mechanisms, links to the magnetospheric ULF pulsations, and effects on the outer (magnetopause) and inner magnetospheric system. The magnetopause waves play a significant role in the solar wind-magnetosphere coupling, while the magnetospheric ULF waves have a significant influence on mass, momentum, and energy transport within the magnetosphere. Pristine solar wind fluctuations and/or upstream bow shock phenomena that generate quasi-periodic or broadband impulsive perturbations downstream of the bow shock drive magnetopause motion and seed the magnetopause waves. The waves excite Aflvénic FLRs via coupling with magnetospheric modes that are well correlated with energization, transport, and losses of inner magnetospheric particles, for example, through the drift resonance. The magnetopause waves can, in turn, modulate the dynamics of the boundary layer, such as the development and evolution of Kelvin-Helmholtz waves/vortices and the efficiency of dayside reconnection.
Studies linking boundary waves occurring in the outer and inner regions suggest a need for further investigations to develop our understanding of how oscillations and wave energy generated at perturbed boundaries penetrate and evolve throughout the region between the boundaries and how they influence the magnetospheric responses to the external drivers. Coordinated multi-point analyses enabled by advanced multiple in-situ spacecraft and wide networks of ground-based measurements together with improved numerical models will address the coupling between surface waves and their effects on boundary-layer dynamics and Earth’s magnetosphere and ionosphere system, providing key information for space weather forecasts under a variety of interplanetary conditions and structures.
Agapitov O , Glassmeier K-H , Auster H , Constantinescu D , Angelopoulos V 2009 Surface waves and field line resonances: A THEMIS case study JGR 114 A00C27 -    DOI : 10.1029/2008JA013553
Alfvén H , Fälthammar CG 1963 Cosmical Electrodynamics Oxford Univ. Press New York
Allan W , Wright AN , McDiarmid DR 1997 Spacecraft transits across simulated field line resonance regions JGR 102 (14) 407 -    DOI : 10.1029/97JA01082
Archer MO , Horbury TS , Eastwood JP , Weygand JM , Yeoman TK 2013 Magnetospheric response to magnetosheath pressure pulses: A low-pass filter effect JGR 118 5454 - 5466    DOI : 10.1002/jgra.50519
Aubry MP , Kivelson MG , Russell CT 1971 Motion and structure of the magnetopause JGR 76 1673 - 1696    DOI : 10.1029/JA076i007p01673
Borovsky JE , Hesse M , Birn J , Kuznetsova MM 2008 What determines the reconnection rate at the dayside magnetosphere? JGR 113 A07210 -    DOI : 10.1029/2007JA012645
Børve S , Sato H , Pécseli HL , Trulsen JK 2011 Minute-scale period oscillations of the magnetosphere Annales Geophysicae 29 663 - 671    DOI : 10.5194/angeo-29-663-2011
Cassak PA , Shay MA 2007 Scaling of asymmetric magnetic reconnection: General theory and collisional simulations Physics of Plasmas 14 102114 -    DOI : 10.1063/1.2795630
Chandrasekhar S 1961 Hydrodynamic and Hydromagnetic Stability Oxford Univ. Press New York
Chaston CC , Wilber M , Mozer FS , Fujimoto F , Goldstein ML 2007 Mode Conversion and Anomalous Transport in Kelvin-Helmholtz Vortices and Kinetic Alfvén Waves at the Earth’s Magnetopause PhRvL 99 175004 -    DOI : 10.1103/PhysRevLett.99.175004
Clausen LBN , Yeoman TK 2009 Comprehensive survey of Pc4 and Pc5 band spectral content in Cluster magnetic field data Annales Geophysicae 27 3237 - 3248    DOI : 10.5194/angeo-27-3237-2009
Collado-Vega YM , Kessel RL , Shao X , Boller RA 2007 MHD flow visualization of magnetopause boundary region vortices observed during high-speed streams JGR 112 A06213 -    DOI : 10.1029/2006JA012104
Cornilleau-Wehrlin N , Grison B , Attié B , Belmont G , Rezeau L 2008 Latitude and local time dependence of ULF wave power at the magnetopause: A Cluster-Double Star study JGR 113 A07S09 -    DOI : 10.1029/2007JA012780
Cowee MM , Winske M , Gary SP 2010 Hybrid simulations of plasma transport by Kelvin-Helmholtz instability at the magnetopause: Density variations and magnetic shear JGR 115 A06214 -    DOI : 10.1029/2009JA015011
Drake JF , Swisdak M , Phan TD , Cassak PA , Shay MA 2009 Ion heating resulting from pickup in magnetic reconnection exhausts JGR 114 A05111 -    DOI : 10.1029/2008JA013701
Dungey JW 1955 Electrodynamics of the outer atmosphere The Physical Society of London Proceedings of the Ionosphere Conference
Dušík Š , Granko G , Šafránková J , Němeček Z , Jelínek K 2010 IMF cone angle control of the magnetopause location: Statistical study Geophysical Research Letters 37 L19103 -    DOI : 10.1029/2010GL044965
Elkington SR , Hudson MK , Wiltberger MJ , Lyon JG 2002 MHD/particle simulations of radiation belt dynamics Journal of Atmospheric and Solar-Terrestrial Physics 64 607 - 615    DOI : 10.1016/S1364-6826(02)00018-4
Elkington SR , Hudson MK , Chan AA 2003 Resonant acceleration and diffusion of outer zone electrons in an asymmetric geomagnetic field JGR 108 1116 -    DOI : 10.1029/2001JA009202
Farrugia CJ , Gratton FT , Bender L , Biermat HK , Erkaev NV 1998 Charts of joint Kelvin-Helmholtz and Rayleigh-Taylor instabilities at the dayside magnetopause for strongly northward interplanetary magnetic field JGR 103 6703 - 6727    DOI : 10.1029/97JA03248
Farrugia CJ , Gratton FT 2011 Aspects of magnetopause/magnetosphere response to interplanetary discontinuities, and features of magnetopause Kelvin-Helmholtz wave Journal of Atmospheric and Solar-Terrestrial Physics 73 40 - 51    DOI : 10.1016/j.jastp.2009.10.008
Farrugia CJ , Gratton FT , Gnavi G , Torbert RB , Wilson III LB 2014 A vortical dawn flank boundary layer for near-radial IMF: Wind observations on 24 October 2001 JGR 119 4572 - 4590    DOI : 10.1002/2013JA019578
Fenrich FR , Samson JC , Sofko G , Greenwald RA 1995 ULF high and low-m field line resonances observed with the Super Dual Auroral Radar Network JGR 100 21535 - 21547    DOI : 10.1029/95JA02024
Freeman MP , Freeman NC , Farrugia CJ 1995 A linear perturbation analysis of magnetopause motion in the Newton-Busemann limit Annales Geophysicae 13 907 - 918    DOI : 10.1007/s00585-995-0907-0
Glassmeier K , Auster H , Constantinescu D , Narita Y , Plaschke F 2008 Magnetospheric quasi-static response to the dynamic magnetosheath: A THEMIS case study Geophysical Research Letters 35 L17S01 -    DOI : 10.1029/2008GL033469
Gratton FT , Gnavi G , Farrugia CJ , Bilbao L , Torbert R 2012 Velocity shear instability and plasma billows at the Earth's magnetic boundary Journal of Physics: Conference Series 370 012003 -    DOI : 10.1088/1742-6596/370/1/012003
Harrold BG , Samson JC 1992 Standing ULF modes of the magnetosphere: A theory Geophysical Research Letters 19 1811 - 1814    DOI : 10.1029/92GL01802
Hartinger MD , Angelopoulos V , Moldwin MB , Takahashi K , Clausen LBN 2013 Statistical study of global modes outside the plasmasphere JGR 118 804 - 822    DOI : 10.1002/jgra.50140
Hartinger M , Angelopoulos V , Moldwin MB , Nishimura Y , Turner DL 2012 Observations of a Pc5 global (cavity/waveguide) mode outside the plasmasphere by THEMIS JGR 117 A06202 -    DOI : 10.1029/2011JA017266
Hasegawa A 1975 Plasma instabilities and non-linear effects Springer-Verlag New York
Hasegawa H , Retinò A , Vaivads A , Khotyaintsev Y , André M 2009 Kelvin-Helmholtz waves at the Earth’s magnetopause: Multiscale development and associated reconnection JGR 114 A12207 -    DOI : 10.1029/2009JA014042
Hasegawa H , Wang J , Dunlop MW , Pu ZY , Zhang QH 2010 Evidence for a flux transfer event generated by multiple X‐line reconnection at the magnetopause Geophysical Research Letters 37 L16101 -    DOI : 10.1029/2010GL044219
Hwang K-J , Kuznetsova MM , Sahraoui F , Goldstein ML , Lee E 2011 Kelvin‐Helmholtz waves under southward interplanetary magnetic field JGR 116 A08210 -    DOI : 10.1029/2011JA016596
Hwang K-J , Goldstein ML , Kuznetsova MM , Wang Y , Viñas AF 2012 The first in situ observation of Kelvin-Helmholtz waves at high-latitude magnetopause during strongly dawnward interplanetary magnetic field conditions JGR 117 A08233 -    DOI : 10.1029/2011JA017256
Hwang K-J , Sibeck DG , Goldsten ML , Nishimura Y , Donovan E The role of Kelvin-Helmholtz waves in the dynamics of the dayside magnetopause and the inner magnetosphere, in 2014 Eos Trans AGU Fall Meeting San Francisco, CA 15-19 Dec2014
Kivelson MG , Southwood DJ 1985 Resonant ULF waves: A new interpretation Geophysical Research Letters 12 49 - 52    DOI : 10.1029/GL012i001p00049
Kuznetsova M , Hesse M , Sibeck D , Rastaetter L , Toth G Non‐steady reconnection in global simulations of magnetosphere dynamics 2008 Eos Trans. AGU Fall Meeting San Francisco, CA 15-19 2008
Lee D-H , Kim H 1999 Compressional MHD waves in the magnetosphere: A new approach JGR 104 12379 - 12385    DOI : 10.1029/1999JA900053
Lee SH , Zhang H , Zong Q-G , Otto A , Sibeck DG 2014 Plasma and energetic particle behaviors during asymmetric magnetic reconnection at the magnetopause JGR 119 1658 - 1672    DOI : 10.1002/2013JA019168
Lee SH , Zhang H , Zong Q-G , Wang Y , Otto A Asymmetric ionospheric outflow observed at the dayside magnetopause 2014 Eos Trans. AGU Fall Meeting San Francisco, CA 15-19 Dec 2014
Loto’aniu TM , Singer HJ , Waters CL , Angelopoulos V , Mann IR 2010 Relativistic electron loss due to ultralow frequency waves and enhanced outward radial diffusion JGR 115 A12245 -    DOI : 10.1029/2010JA015755
Ma X , Otto A , Delamere PA 2014 Interaction of magnetic reconnection and Kelvin-Helmholtz modes for large magnetic shear: 1. Kelvin-Helmholtz trigger JGR 119 781 - 797    DOI : 10.1002/2013JA019224
Ma X , Otto A , Delamere PA 2014 Interaction of magnetic reconnection and Kelvin-Helmholtz modes for large magnetic shear: 2. Reconnection trigger JGR 119 808 - 820    DOI : 10.1002/2013JA019225
Mann IR , Wright AN , Mills KJ , Nakariakov VM 1999 Excitation of magnetospheric waveguide modes by magnetosheath flows JGR 104 333 - 353    DOI : 10.1029/1998JA900026
Mann IR , Coronkov I , Dunlop M , Donovan E , Yeoman DK 2002 Co-ordinated ground-based and Cluster observations of large amplitude global magnetospheric oscillations during a fast solar wind speed interval Annales Geophysicae 20 405 - 426    DOI : 10.5194/angeo-20-405-2002
Matsumoto Y , Hoshino M 2004 Onset of turbulence induced by a Kelvin-Helmholtz vortex Geophysical Research Letters 31 L02807 -    DOI : 10.1029/2003GL018195
Matsumoto Y , Hoshino M 2006 Turbulent mixing and transport of collisionless plasmas across a stratified velocity shear layer JGR 111 A05213 -    DOI : 10.1029/2004JA010988
McHenry MA , Clauer CR , Friis-Christense E , Newell T , Kelly JD 1990 Ground observations of magnetospheric boundary layer phenomena JGR 95 14995 - 15005    DOI : 10.1029/JA095iA09p14995
Nakamura TKM , Hasegawa H , Shinohara I , Fujimoto M 2011 Evolution of an MHD‐scale Kelvin--Helmholtz vortex accompanied by magnetic reconnection: Twodimensional particle simulations JGR 116 A03227 -    DOI : 10.1029/2010JA016046
Nykyri K , Otto A 2001 Plasma transport at the magnetospheric boundary due to reconnection in Kelvin-Helmholtz vortices JGR 28 3565 - 3568    DOI : 10.1029/2001GL013239
Omidi N , Sibeck DG , Blanco-Cano X 2009 Foreshock compressional boundary JGR 114 A08205 -    DOI : 10.1029/2008JA013950
Otto A , Fairfield DH 2000 Kelvin-Helmholtz instability at the magnetotail boundary: MHD simulation and comparison with Geotail observations JGR 105 21175 - 21190    DOI : 10.1029/1999JA000312
Phan TD , Dunlop MW , Paschmann G , Klecker B , Bosqued JM 2004 Cluster observations of continuous reconnection at the magnetopause under steady interplanetary magnetic field conditions Annales Geophysicae 22 2355 - 2367    DOI : 10.5194/angeo-22-2355-2004
Prikryl P , Greenwald RA , Sofko GJ , Villain JP , Ziesolleck CWS 1998 Solar-wind-driven pulsed magnetic reconnection at the dayside magnetopause, Pc5 compressional oscillations, and field line resonances JGR 103 17307 - 17322    DOI : 10.1029/97JA03595
Rae IJ , Donovan EF , Mann IR , Fenrich FR , Watt CEJ 2005 Evolution and characteristics of global Pc5 ULF waves during a high solar wind speed interval JGR 110 A12211 -    DOI : 10.1029/2005JA011007
Raeder J 2006 Flux Transfer Events: 1. generation mechanism for strong southward IMF Annales Geophysicae 24 381 - 392    DOI : 10.5194/angeo-24-381-2006
Rickard GJ , Wright AN 1995 ULF pulsations in a magnetospheric waveguide: Comparison of real and simulated satellite data JGR 100 3531 - 3537    DOI : 10.1029/94JA02935
Russell CT , Elphic RC 1978 Initial ISEE magnetometer results: magnetopause observations SSRv 22 681 - 715    DOI : 10.1007/BF00212619
Sarafopoulos DV 2005 A case study testing the cavity mode model of the magnetosphere Annales Geophysicae 23 1867 - 1880    DOI : 10.5194/angeo-23-1867-2005
Sckopke N , Paschmann G , Bame SJ , Gosling JT , Russell CT 1983 Evolution of ion distributions across the nearly perpendicular bow shock: Specularly and non-specularly reflected ions JGR 88 6121 - 6136    DOI : 10.1029/JA088iA08p06121
Smit GR 1968 Oscillatory motion of the nose region of the magnetopause JGR 73 4990 - 4993    DOI : 10.1029/JA073i015p04990
Southwood DJ 1968 hydromagnetic stability of the magnetospheric boundary P&SS 16 587 - 605    DOI : 10.1016/0032-0633(68)90100-1
Southwood DJ 1974 Some features of field line resonances in the magnetosphere P&SS 17 483 - 491    DOI : 10.1016/0032-0633(74)90078-6
Southwood DJ , Kivelson MG 1981 Charged particle behavior in lowfrequency geomagnetic pulsations. I Transverse waves JGR 86 5643 - 5655    DOI : 10.1029/JA086iA07p05643
Stix TH 1962 The Theory of Plasma Waves McGraw-Hill New York
Suvorova AV , Shue J-H , Dmitrievm AV , Sibeck DG , McFadden JP 2010 Magnetopause expansions for quasi‐radial interplanetary magnetic field: THEMIS and Geotail observations JGR 115 A10216 -    DOI : 10.1029/2010JA015404
Takagi K , Hashimoto C , Hasegawa H , Fujimoto F 2006 Helmholtz instability in a magnetotail flank-like geometry: Three-dimensional MHD simulations JGR 111 A08202 -    DOI : 10.1029/2006JA011631
Takahashi K , McPherron RL , Hughes WJ 1984 Multispacecraft observations of the harmonic structure of Pc3-4 magnetic pulsations JGR 89 6758 -    DOI : 10.1029/JA089iA08p06758
Takahashi K , Bonnell J , Classmeier K-H , Angelopoulos V , Singer HJ 2010 Multipoint observation of fast mode waves trapped in the dayside plasmasphere JGR 115 A12247 -    DOI : 10.1029/2010JA015956
Turner DL , Shprits Y , Hartinger M , Angelopoulos V 2012 Explaining sudden losses of outer radiation belt electrons during geomagnetic storms Nature Physics 8 208 - 212    DOI : 10.1038/nphys2185
Walker ADM , Greenwald RA , Stuart WF , Green CA 1979 Stare aurora1 radar observations of PC 5 geomagnetic pulsations JGR 84 3373 - 3388    DOI : 10.1029/JA084iA07p03373
Walker ADM , Ruohoniemi JM , Baker KD , Greenwald RA , Samson JC 1992 Spatial and temporal behavior of ULF pulsations observed by the Goose Bay HF radar JGR 97 12187 - 12202    DOI : 10.1029/92JA00329
Wang Y , Elphic RC , Lavraud B , Taylor MGG , Birn J Initial results of high-latitude magnetopause and low-latitude flank flux transfer events from 3 years of Cluster observations JGR 110 A11221 -    DOI : 10.1029/2005JA011150
Waters CL , Takahashi K , Lee D-H , Anderson BJ 2002 Detection of ultralow-frequency cavity modes using spacecraft data JGR 107 1284 -    DOI : 10.1029/2001JA000224
Wright AN 1994 Dispersion and wave coupling in inhomogeneous MHD waveguides JGR 99 159 - 167    DOI : 10.1029/93JA02206
Yan GQ , Mozer FS , Shen C , Chen T , Parks GK 2014 Kelvin-Helmholtz vortices observed by THEMIS at the duskside of the magnetopause under southward interplanetary magnetic field Geophysical Research Letters 41 4427 - 4434    DOI : 10.1002/2014GL060589
Yao Y , Chaston CC , Glassmeier K-H , Angelopoulos V 2011 Electromagnetic waves on ion gyro‐radii scales across the magnetopause Geophysical Research Letters 38 L09102 -    DOI : 10.1029/2011GL047328
Zhu X , Kivelson MG 1989 Global mode ULF pulsations in a magnetosphere with a nonmonotonic Alfven velocity profile JGR 94 1479 - 1485    DOI : 10.1029/JA094iA02p01479