Kelvin‐Helmholtz vortices observed by THEMIS at the duskside of the magnetopause under southward interplanetary magnetic field

Yan, Guoguo; Mozer, F. S.; Shen, Chao; Chen, Ti; Parks, G. K.; Cai, Chunlin; McFadden, J. P.

doi:10.1002/2014gl060589

Cited by 41 publications

(38 citation statements)

References 46 publications

(82 reference statements)

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“…The statistics of and show observations usually at low latitudes, and not only tailward but also sunward of the terminator (suggesting that at least sometimes they may develop very rapidly). Events have also been reported on the dusk flank during sourthward IMF conditions (Yan et al 2014), as previously predicted.…”

Section: Solar Wind Plasmasupporting

confidence: 82%

The Earth: Plasma Sources, Losses, and Transport Processes

et al. 2015

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This paper reviews the state of knowledge concerning the source of magnetospheric plasma at Earth. Source of plasma, its acceleration and transport throughout the system, its consequences on system dynamics, and its loss are all discussed. Both observational and modeling advances since the last time this subject was covered in detail (Hultqvist et al., Magnetospheric Plasma Sources and Losses, 1999) are addressed.

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Section: Solar Wind Plasmasupporting

confidence: 82%

The Earth: Plasma Sources, Losses, and Transport Processes

et al. 2015

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“…The occurrence of the K‐H instability is favorable under conditions of northward B z (Hasegawa et al, , ) or high solar wind speed (Rae et al, ), or both (Kavosi & Raeder, ). The instability nevertheless operates under every solar wind speed in the typically observed range, 200–600 km/s, and under virtually every IMF configuration (Farrugia et al, ; Hwang et al, ; Kavosi & Raeder, ; Yan et al, ), which could explain the persistence of the prenoon and postnoon enhanced broadband number flux for every ϕ IMF orientation in Figure . However, this explanation offers no obvious clues as to the apparent preferential generation of prenoon IAW power.…”

Section: Discussionmentioning

confidence: 90%

IMF Control of Alfvénic Energy Transport and Deposition at High Latitudes

et al. 2017

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We investigate the influence of the interplanetary magnetic field (IMF) clock angle ϕIMF on high‐latitude inertial Alfvén wave (IAW) activity in the magnetosphere‐ionosphere transition region using Fast Auroral SnapshoT (FAST) satellite observations. We find evidence that negative IMF Bz coincides with nightside IAW power generation and enhanced rates of IAW‐associated electron energy deposition, while positive IMF Bz coincides with enhanced dayside wave and electron energy deposition. Large ( ≳0.3em0.3em0.3em5 nT) negative IMF By coincides with enhanced postnoon IAW power, while large positive IMF By coincides with enhanced but relatively weaker prenoon IAW power. For each ϕIMF orientation we compare IAW Poynting flux and IAW‐associated electron energy flux distributions with previously published distributions of Alfvénic Poynting flux over ∼2–22 mHz, as well as corresponding wave‐driven electron energy deposition derived from Lyon‐Fedder‐Mobarry global MHD simulations. We also compare IAW Poynting flux distributions with distributions of broad and diffuse electron number flux, categorized using an adaptation of the Newell et al. (2009) precipitation scheme for FAST. Under negative IMF Bz in the vicinity of the cusp (9.5–14.5 magnetic local time), regions of intense dayside IAW power correspond to enhanced diffuse electron number flux but relatively weaker broadband electron precipitation. Differences between cusp region IAW activity and broadband precipitation illustrate the need for additional information, such as fields or pitch angle measurements, to identify the physical mechanisms associated with electron precipitation in the vicinity of the cusp.

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“…The KH waves have been frequently observed at the magnetopause of Earth's low-latitude boundary layer during northward (Eriksson et al, 2016;Fairfield et al, 2000;Hasegawa et al, 2004;Lin et al, 2014), PS (Moore, 2012;Moore et al, 2016;Nykyri et al, 2006), southward IMF (Hwang et al, 2011;Yan et al, 2014), and also at the boundary layers of other planets (Boardsen et al, 2010;Delamere & Bagenal, 2010;Ma et al, 2015;Masters et al, 2010;McComas & Bagenal, 2008;Pope et al, 2009;Ruhunusiri et al, 2016;Sundberg et al, 2012).…”

Section: 1002/2017ja024548mentioning

confidence: 99%

On the Dawn‐Dusk Asymmetry of the Kelvin‐Helmholtz Instability Between 2007 and 2013

et al. 2017

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Using data from Time History of Events and Macroscale Interactions during Substorms (THEMIS), a statistical study was performed to determine whether a dawn‐dusk asymmetry exists in the occurrence rates of the Kelvin‐Helmholtz instability during Parker‐Spiral (PS) and Ortho‐Parker‐Spiral (OPS) orientations of the interplanetary magnetic field (IMF). It is determined from the data that there is a strong preference toward the dawnside during PS orientation, and although a preference to the duskside during OPS is suggested, this requires further study for an unambiguous confirmation. The uncertainty in the OPS result is due to a low number of events, which satisfied our selection criteria. Because IMF is statistically in PS orientation, the Kelvin‐Helmholtz instability (KHI) preference for the dawn flank during this orientation may help explain the origin of the plasma sheet asymmetry of cold component ions because it has been shown that KHI can drive kinetic‐scale wave activity capable of ion heating.

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Kelvin‐Helmholtz vortices observed by THEMIS at the duskside of the magnetopause under southward interplanetary magnetic field

Cited by 41 publications

References 46 publications

The Earth: Plasma Sources, Losses, and Transport Processes

The Earth: Plasma Sources, Losses, and Transport Processes

IMF Control of Alfvénic Energy Transport and Deposition at High Latitudes

On the Dawn‐Dusk Asymmetry of the Kelvin‐Helmholtz Instability Between 2007 and 2013

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