Plasma transport at the magnetospheric boundary due to reconnection in Kelvin‐Helmholtz vortices

By K. Nykyri, A. Otto. 2001

315 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/1940f2ebff865b99137914d18784bb1bec9010c5

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Citations in the corpus

Role of solar wind turbulence in the coupling of the solar wind to the Earth's magnetosphere (2003, background): “…interaction between the solar wind and the magnetosphere is often thought to be owed to instabilities on the boundary of the magnetosphere [Eviatar and Wolf, 1968; Haerendel, 1978], particularly Kelvin-Helmholtz type instabilities driven by the solar wind flow [Mishin, 1981; Nykyri and Otto, 2001].”
Single-spacecraft detection of rolled-up Kelvin-Helmholtz vortices at the flank magnetopause (2006, result): “On the other hand, recent studies by Øieroset et al. [2005] and Li et al.”
Cluster observations of reconnection due to the Kelvin-Helmholtz instability at the dawnside magnetospheric flank (2006, methodology): “We note that the KH dynamics for this magnetic field configuration is different from the dynamics of KH evolution with initially strongly parallel magnetic fields ( Nykyri and Otto, 2001).”
Solar wind driving of magnetospheric ULF waves: Pulsations driven by velocity shear at the magnetopause (2008, methodology): “The structure of the simulation boundary layer is very similar to the diagram of Model B presented by Sckopke et al. [1981]. Sckopke et al.”
Altered solar wind-magnetosphere interaction at low Mach numbers: Coronal mass ejections (2008, background): “By contrast, Lavraud et al. [2007] and Rosenqvist et al. [2007] recently found magnetosheath flows that exceeded the solar wind flow speed by up to 60%, with peaks at ~1040 and ~750 km/s, respectively.”
Solar wind interaction with Jupiter's magnetosphere (2009, background): “[19] There are three different types of magnetic reconnection that can be caused by KH modes: (1) compression of a preexisting current layer (even for Alfven Mach number > 1) [Nakamura et al., 2006; Nykyri et al., 2006], (2) reconnection in self‐generated current layers within the KH vortex structur”
MAGNETIC KELVIN–HELMHOLTZ INSTABILITY AT THE SUN (2011, unknown): “…(panel (c) in Figure 3), which entrain magnetic fields of opposing direction (Nykyri & Otto 2004), allowing reconnection to occur as a secondary process and thus, for the magnetopause, allowing solar wind plasma to gain access to the magnetosphere (Nykyri & Otto 2001; Hasegawa et al. 2004).”