The Kelvin–Helmholtz instability under Parker-Spiral Interplanetary Magnetic Field conditions at the magnetospheric flanks

Adamson, E.; Nykyri, K.; Otto, A.

doi:10.1016/j.asr.2015.09.013

Cited by 17 publications

(23 citation statements)

References 59 publications

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“…For example, the best comparison with data and simulation in Nykyri, 2006-event was obtained when k-vector was tilted by 35 degrees from the initial shear flow plane. This result was later confirmed with 3-D simulations of the same event by Adamson et al (2016). Furthermore, the onset criteria is derived assuming infinitely thin boundary, and the real magnetopause has a finite thickness.…”

Section: Khi Under Different Imf Conditionssupporting

confidence: 58%

Kelvin–Helmholtz Instability: Lessons Learned and Ways Forward

Masson

Nykyri

2018

Space Sci Rev

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The Kelvin-Helmholtz instability (KHI) is a ubiquitous phenomenon across the Universe, observed from 500 m deep in the oceans on Earth to the Orion molecular cloud. Over the past two decades, several space missions have enabled a leap forward in our understanding of this phenomenon at the Earth's magnetopause. Key results obtained by these missions are first presented, with a special emphasis on Cluster and THEMIS. In particular, as an ideal instability, the KHI was not expected to produce mass transport. Simulations, later confirmed by spacecraft observations, indicate that plasma transport in Kelvin-Helmholtz (KH) vortices can arise during non-linear stage of its development via secondary process. In addition to plasma transport, spacecraft observations have revealed that KHI can also lead to significant ion heating due to enhanced ion-scale wave activity driven by the KHI. Finally, we describe what are the upcoming observational opportunities in 2018-2020, thanks to a unique constellation of multi-spacecraft missions including: MMS, Cluster, THEMIS, Van Allen Probes and Swarm.

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Section: Khi Under Different Imf Conditionssupporting

confidence: 58%

Kelvin–Helmholtz Instability: Lessons Learned and Ways Forward

Masson

Nykyri

2018

Space Sci Rev

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“…Adamson et al () and Nykyri et al () demonstrated using Cluster data and 2‐D and 3‐D MHD simulations that the k vector of the KHI does not need to be aligned with maximum velocity shear but that KH waves can propagate with an angle from the equatorial plane to minimize the tangential magnetic field tension to maximize the onset criteria. Cluster data during the KH event and 2‐D MHD simulations were consistent with the propagation angle of 35° (Nykyri et al, ), whereas the 3‐D investigation of the angle maximizing the onset criteria was 48° and corresponding angle observed in 3‐D MHD simulation was 41° (Adamson et al, ). To explore this statistically for the present set of KH events, equation was applied in order to determine the propagation angle with respect to the shear flow velocity that maximized the onset criteria for each event.…”

Section: Resultsmentioning

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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“…Even if this model is oversimplified, it yet gives some insights about the tilt angle of oblique modes observed in the 3‐D compressible simulations starting from 1‐D equilibria with ℓ ⋆ ≠0 (Adamson et al, ; Nakamura & Daughton, ). A moderate discrepancy between the predicted ϑ max and that observed in the simulations is related to the fact that the simplified model underestimates the role of the magnetic field inside the shear layer (

false| x false| ≲ ℓ_{⋆}

), where the mode amplitude is larger, while overestimates its importance in the two asymptotic region (| x |≫ ℓ ⋆ ).…”

Section: Large‐scale Dynamics Of Kh Vorticesmentioning

confidence: 99%

North‐South Asymmetric Kelvin‐Helmholtz Instability and Induced Reconnection at the Earth's Magnetospheric Flanks

et al. 2018

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We present a three-dimensional study of the plasma dynamics at the flank magnetopause of the Earth's magnetosphere during mainly northward interplanetary magnetic field periods. Two-fluid simulations show that the initial magnetic shear at the magnetopause and the field line bending caused by the dynamics itself (in a configuration taken as representative of the properties of the flank magnetopause) influence both the location where the Kelvin-Helmholtz (KH) instability and the induced magnetic reconnection take place and their nonlinear development. The KH vortices develop asymmetrically with respect to the Earth's equatorial plane where the local KH linear growth rate is maximal. Vortex-driven reconnection processes take place at different latitudes, ranging from the equatorial plane to midlatitude regions but only in the hemisphere that turns out to be the less KH unstable. These results suggest that KH-induced reconnection is not limited to specific regions around the vortices (inside, below, or above) but may be triggered over a broad and continuous range of locations in the vicinity of the vortices.

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The Kelvin–Helmholtz instability under Parker-Spiral Interplanetary Magnetic Field conditions at the magnetospheric flanks

Cited by 17 publications

References 59 publications

Kelvin–Helmholtz Instability: Lessons Learned and Ways Forward

Kelvin–Helmholtz Instability: Lessons Learned and Ways Forward

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

North‐South Asymmetric Kelvin‐Helmholtz Instability and Induced Reconnection at the Earth's Magnetospheric Flanks

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