On the role of plasma parameters and the Kelvin-Helmholtz instability in a viscous interaction of solar wind streams

Korzhov, N. P.; Мишин, В. М.; Томозов, В. М.

doi:10.1016/0032-0633(84)90142-9

Cited by 51 publications

(13 citation statements)

References 25 publications

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“…Velocity shear in the solar wind is also of interest as a potential driver for MHD turbulence [ Coleman , 1968; Belcher and Davis , 1971; Roberts et al , 1992; Goldstein et al , 1999]. Driving of solar wind turbulence by Kelvin‐Helmholtz‐like instabilities in shear zones has been explored [ Korzhov et al , 1984; Roberts et al , 1992; Malara , 1999], as has the driving of solar wind turbulence by shearing low‐frequency Alfven waves [ Roberts et al , 1987, 1992; Grappin and Velli , 1996; Ghosh et al , 1998; Roberts and Ghosh , 1999] and by the reflection of outward‐traveling Alfven waves off shear structures [ Bavassano and Bruno , 1992; Klein et al , 1993]. A statistical study of the properties of solar wind fluctuations in the vicinity of corotating‐interaction‐region shear zones at 1 AU found no evidence for the production of turbulence [ Borovsky and Denton , 2010a].…”

Section: Introductionmentioning

confidence: 99%

“… Chen and Montgomery , 1987; Yoshizawa and Yokoi , 1996; Ishizawa and Hattori , 1998] but with complications owing to the anisotropy of the fluctuations, to the fluid memory provided by the field, and to the Alfvenic propagation of shear along the mean field. Attempts to calculate an eddy‐viscosity coefficient for the solar wind from observations of the velocity fluctuations have resulted in values that differ by 8 orders of magnitude [ Korzhov et al , 1984, 1985; Verma , 1996; Borovsky , 2006]. For the collisonless solar wind, Borovsky and Gary [2009, 2011] explored methods to calculate shear viscosities from Bohm diffusion and from Landau damping, which yield values below those of eddy‐viscosity estimates.…”

Section: Introductionmentioning

confidence: 99%

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The effect of sudden wind shear on the Earth's magnetosphere: Statistics of wind shear events and CCMC simulations of magnetotail disconnections

Borovsky

2012

J. Geophys. Res.

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[1] The solar wind is filled with strong current sheets and sudden velocity shears; often the two are co-located. Sudden velocity shears at 1 AU are statistically analyzed using ACE measurements from 1998 to 2008. The occurrence rates of passage and the orientations of the shear planes are examined. For shear layers with vector velocity changes |Dv| > 50 km/s, an average of $12 pass the Earth per day. In the fast wind, $60 sudden shear layers pass the Earth per day (about 2.5 per hour). To explore the effects of sudden wind shears on the Earth's magnetosphere, global magnetospheric MHD simulations with four different simulation codes are performed at the Community Coordinated Modeling Center (CCMC) with north-south and east-west wind shears. Windsock movement of the magnetotail is analyzed and comet-like disconnections of the magnetotail and magnetosheath are examined. Sudden changes in the cross-polar-cap potential and ionospheric Joule dissipation are seen as the shear layers pass the Earth. Other potential effects of sudden wind shear on the magnetosphere are discussed.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The effect of sudden wind shear on the Earth's magnetosphere: Statistics of wind shear events and CCMC simulations of magnetotail disconnections

Borovsky

2012

J. Geophys. Res.

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“…In the most recent coupled MHD solar corona-heliosphere models, the empirical velocity relationship parameters that impact the solar wind speed predictions are the divergence of coronal holes (through a coronal flux tube expansion factor) and the distance from the coronal hole boundary (or angular depth inside a coronal hole; Arge et al 2004; Lee et al 2009). Many theories have explored whether the KH instability could also occur in these regions (Korzhov et al 1984;Joarder et al 1997;Suess et al 2009). In general, the KH instability generated by shear flows across tangential discontinuities (Neugebauer et al 1986; Suess et al 1995) and other forms of shear-driven turbulence (Roberts et al 1992) could be responsible for Alfvénic fluctuations in the solar wind (Belcher & Davis 1971;Roberts et al 1987;Tsurutani et al 1994).…”

Section: Introductionmentioning

confidence: 99%

Plasmoid Releases in the Heliospheric Current Sheet and Associated Coronal Hole Boundary Layer Evolution

Foullon

Lavraud

Luhmann

et al. 2011

ApJ

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As the heliospheric current sheet (HCS) is corotating past STEREO-B, near-Earth spacecraft ACE, Wind and Cluster, and STEREO-A over more than three days between 2008 January 10 and 14, we observe various sections of (near-pressure-balanced) flux-rope-and magnetic-island-type plasmoids in the associated heliospheric plasma sheet (HPS). The plasmoids can qualify as slow interplanetary coronal mass ejections and are relatively low proton beta (<0.5) structures, with small length scales (an order of magnitude lower than typical magnetic cloud values) and low magnetic field strengths (2-8 nT). One of them, in particular, detected at STEREO-B, corresponds to the first reported evidence of a detached plasmoid in the HPS. The in situ signatures near Earth are associated with a long-decay X-ray flare and a slow small-scale streamer ejecta, observed remotely with white-light coronagraphs aboard STEREO-B and SOHO and tracked by triangulation. Before the arrival of the HPS, a coronal hole boundary layer (CHBL) is detected in situ. The multi-spacecraft observations indicate a CHBL stream corotating with the HCS but with a decreasing speed distribution suggestive of a localized or transient nature. While we may reasonably assume that an interaction between ejecta and CHBL provides the source of momentum for the slow ejecta's acceleration, the outstanding composition properties of the CHBL near Earth provide here circumstantial evidence that this interaction or possibly an earlier one, taking place during streamer swelling when the ejecta rises slowly, results in additional mixing processes.

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“…This applies also to the conclusions drawn in (Korzhov et al, 1984) about the instability of shear flows in the solar wind where the generation of oblique disturbances accounts for the spectrum of the waves observed there, and for the presence of a wide shear layer (Goldstein, 1995).…”

Section: Discussionmentioning

confidence: 68%

“…For that reason, it was of interest to us to prove our conclusions about the predominance of oblique disturbances using supersonic shear flows at the magnetospheric boundary (Mishin and Morozov, 1983) and in the solar wind (Korzhov et al, 1984).…”

Section: Role Of Oblique Disturbances In the Instability Of A Supersomentioning

confidence: 99%

On the predominance of oblique disturbances in the supersonic shear flow instability of the geomagnetic tail boundary

Мишин

2003

Nonlin. Processes Geophys.

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Abstract.A study is made of the influence of the longitudinal magnetic field and density inhomogeneity on the supersonic shear flow instability at the magnetospheric tail boundary. It is shown that the most unstable are slow oblique (3D) disturbances, with a phase velocity approaching at a sufficiently large angle (with respect to the flow direction) the magnetosonic velocity. Their growth rate and spectral width are much larger than those of the usually considered longitudinal (2D) supersonic disturbances. The magnetic field reduces the compressibility effect and, unlike the subsonic case, has a noticeable destabilizing effect on the excitation of oblique disturbances.

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On the role of plasma parameters and the Kelvin-Helmholtz instability in a viscous interaction of solar wind streams

Cited by 51 publications

References 25 publications

The effect of sudden wind shear on the Earth's magnetosphere: Statistics of wind shear events and CCMC simulations of magnetotail disconnections

The effect of sudden wind shear on the Earth's magnetosphere: Statistics of wind shear events and CCMC simulations of magnetotail disconnections

Plasmoid Releases in the Heliospheric Current Sheet and Associated Coronal Hole Boundary Layer Evolution

On the predominance of oblique disturbances in the supersonic shear flow instability of the geomagnetic tail boundary

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