An active current sheet in the solar wind

Schwartz, S. J.; Chaloner, C. P.; Christiansen, P. J.; Coates, A. J.; Hall, D. S.; Johnstone, A. D.; Gough, M. P.; Norris, Andrew J.; Rijnbeek, R. P.; Southwood, D. J.; Woolliscroft, L. J. C.

doi:10.1038/318269a0

Cited by 190 publications

(167 citation statements)

References 8 publications

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“…We also discuss minimum variance analysis of the upstream ULF wave field. SLAMS-like structures are distinguished from the magnetic signatures surrounding hot flow anomalies (HFA) (Schwartz, 1985(Schwartz, , 1991 by their plasma signatures, and so here we cannot definitely identify SLAMS. We do, however, find magnetic field structures with characteristics that are consistent with previous observations of SLAMS.…”

Section: Introductionmentioning

confidence: 80%

Cluster magnetic field observations at a quasi-parallel bow shock

et al. 2002

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Abstract. We present four-point Cluster magnetic field data from a quasi-parallel shock crossing which allows us to probe the three-dimensional structure of this type of shock for the first time. We find that steepened ULF waves typically have a scale larger than the spacecraft separation (∼400-1000 km), while SLAMS-like magnetic field enhancements have different signatures in |B| at the four spacecraft, suggesting that they have a smaller scale size. In the latter case, however, the angular variations of B are similar, consistent with the spacecraft making different trajectories through the same structure. The field enhancements have different orientations relative to a model bow shock normal, which might arise from different degrees of deceleration and deflection of the surrounding solar wind plasma. The observed rotation of the magnetic field rising from a direction approximately parallel to the model bow shock normal to a direction more perpendicular to the model normal across the field enhancement is consistent with previously published results. Successive magnetic field enhancements or ULF waves, and the leading and trailing edges of the same structure, are found to have different orientations.

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Section: Introductionmentioning

confidence: 80%

Cluster magnetic field observations at a quasi-parallel bow shock

et al. 2002

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“…HFAs are transient high-energy plasma populations that evolve along the interaction line of the shock and a tangential discontinuity (TD) plane embedded in the solar wind (Schwartz et al 1985, Thomsen et al 1986). Using the k-filtering analysis of the magnetic records of the multi-spacecraft Cluster mission it was shown by Tjulin et al (2008) that the magnetic variations inside the HFA cavity are strongly determined by wave phenomena.…”

Section: Nonlinear Study Of Solar Wind -Magnetosphere Dynamics (Pétermentioning

confidence: 99%

Hungarian national report on IAGA 2007–2010

Szarka¹,

Sátori²

2011

Acta Geodaetica et Geophysica Hungarica

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“…The structure edges are typically enhanced significantly over the ambient solar wind values, and plasma parameters and particle signatures provide evidence that these form fast mode-like shock interfaces with the solar wind (Schwartz et al, 1985;Fuselier et al, 1987;Paschmann et al, 1988;Thomsen et al, 1988). HFAs have magnetosheath manifestations and can impact the magnetopause and magnetosphere (Paschmann et al, 1988;Sibeck et al, 1999;Safránková et al, 2002;Eastwood et al, 2008).…”

Section: Introductionmentioning

confidence: 99%

“…Other well-studied foreshock plasma structures include hot flow anomalies (HFAs) that are characterized by large flow deviations, which at times have sunward-directed x GSE components, and interior particle temperatures greatly in excess of the ambient solar wind (Schwartz et al, 1985;Schwartz et al, 1988Schwartz et al, , 2000Woolliscroft et al, 1986;Thomsen et al, 1986;Thomsen et al, 1988;Thomsen et al, 1993;Paschmann et al, 1988;Lucek et al, 2004b). These appear to be the result of current sheets, specifically, tangential discontinuities (Thomsen et al, 1993), in the IMF interacting with Earth's bow shock.…”

Section: Introductionmentioning

confidence: 99%

“…Schwartz et al (1985) and Woolliscroft et al (1986), the former applied somewhat different selection criteria, which is reflected in their original term: hot diamagnetic cavities. Most notably, they considered cases where the magnetic field formed cavities centered on the IMF current sheet, which apparently were the result of the inferred plasma expansion.…”

Section: Introductionmentioning

confidence: 99%

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Foreshock density holes in the context of known upstream plasma structures

et al. 2008

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Abstract. We present case examples of foreshock density holes and results from a statistical survey, which provide additional characterizations of these recently-described structures. Specific effort is made to place these objects into context with well-studied foreshock phenomena, such as hot flow anomalies (HFAs) and large-amplitude magnetic pulsations (SLAMS). Density holes are observed during higherthan-average solar wind speeds (∼620 km s −1 ), have wellcorrelated density and magnetic field intensities, and anticorrelated density and temperature variations. Like HFAs, these structures occur over a wide range of foreshock geometries, suggesting that this is not a determining factor. They are embedded within IMF current sheets, but their crossstructure magnetic shears are considerably lower than for HFAs. When the Cluster spacecraft are widely separated, they are able to measure structure time development, with substantial changes occurring over 10s of seconds, confirming an earlier case study, and possibly indicating short lifetimes as well. We find that density holes can occur in the absence of strong upstream magnetic pulsations and/or density enhancements, which rules out a "wake effect" as the sole explanation for their formation. Most important is the observation that the observed solar wind motional electric fields tend to have components pointing away from the embedding IMF current sheets. Density holes have no connection with magnetic holes and foreshock cavities, and appear not to be early-stage or weakly-formed HFAs.

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An active current sheet in the solar wind

Cited by 190 publications

References 8 publications

Cluster magnetic field observations at a quasi-parallel bow shock

Cluster magnetic field observations at a quasi-parallel bow shock

Hungarian national report on IAGA 2007–2010

Foreshock density holes in the context of known upstream plasma structures

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