Magnetosheath – Interplanetary medium reference frame: Application for a statistical study of mirror type waves in the terrestrial plasma environment

Веригин, М. И.; Tátrallyay, M.; Erdö́s, G.; Котова, Г. А.

doi:10.1016/j.asr.2005.03.042

Cited by 39 publications

(62 citation statements)

References 18 publications

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“…The reference solar wind conditions used are a dynamic pressure of 1 nPa and an IMF B Z = À1 nT, and data are averaged in 0.5 Â 0.5 R E bins for the distributions shown in Figures 7 to 9. For further details on the method, the reader is referred to Verigin et al [2006] and Génot et al [2009Génot et al [ , 2011. We here use this approach to order normalized magnetosheath flow speeds as a function of the angle between the Cluster position vector and the (lagged) IMF orientation.…”

Section: Statistical Study Of Magnetosheath Flowsmentioning

confidence: 99%

“…The representation shows the ion speed measured at Cluster normalized to the appropriately lagged ion speed measured at ACE for all available 5 min Cluster data averages (|V SHEATH |/|V SW |). The statistical data ordering is essentially based on the magnetosheath-interplanetary medium (MIPM) reference frame developed by Verigin et al [2006]. This consists of a spatial superposed analysis which orders spacecraft data from a given time and location relative to models of the magnetopause [Shue et al, 1997[Shue et al, , 1998] and bow shock positions [Verigin et al, 2006].…”

Section: Statistical Study Of Magnetosheath Flowsmentioning

confidence: 99%

“…Statistical distribution of the magnetosheath ion speed measured at Cluster normalized to the appropriately lagged ion speed measured at ACE for each 5 min data averages; a color palette of |V SHEATH |/|V SW | is given in the top right corner. The statistical data ordering is based on the magnetosheath-interplanetary medium (MIPM) reference frame developed by Verigin et al [2006], using models of the magnetopause [Shue et al, 1997[Shue et al, , 1998] and bow shock positions [Verigin et al, 2006] with appropriately lagged ACE data as inputs. Each data point is assigned an X and R (R = √(Y 2 + Z 2 )) position in the normalized reference frame.…”

Section: Statistical Study Of the Magnetopause Shapementioning

confidence: 99%

“…The statistical data ordering is essentially based on the magnetosheath-interplanetary medium (MIPM) reference frame developed by Verigin et al [2006]. This consists of a spatial superposed analysis which orders spacecraft data from a given time and location relative to models of the magnetopause [Shue et al, 1997[Shue et al, , 1998] and bow shock positions [Verigin et al, 2006]. Using appropriately lagged (using Cluster and ACE spacecraft positions and the measured solar wind velocity at ACE) ACE data as inputs to the models, a fractional position of Cluster in the magnetosheath, relative to the model boundaries (between 0 and 1), is obtained along the direction of the spacecraft position vector (see also Nĕmecek et al [2000Nĕmecek et al [ , 2003 for similar procedures).…”

Section: Statistical Study Of Magnetosheath Flowsmentioning

confidence: 99%

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Asymmetry of magnetosheath flows and magnetopause shape during low Alfvén Mach number solar wind

et al. 2013

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[1] Previous works have emphasized the significant influence of the solar wind Alfvén Mach number (M A ) on magnetospheric dynamics. Here we report statistical, observational results that pertain to changes in the magnetosheath flow distribution and magnetopause shape as a function of solar wind M A and interplanetary magnetic field (IMF) clock angle orientation. We use all Cluster 1 data in the magnetosheath during the period 2001-2010, using an appropriate spatial superposition procedure, to produce magnetosheath flow distributions as a function of location in the magnetosheath relative to the IMF and other parameters. The results demonstrate that enhanced flows in the magnetosheath are expected at locations quasi-perpendicular to the IMF direction in the plane perpendicular to the Sun-Earth line; in other words, for the special case of a northward IMF, enhanced flows are observed on the dawn and dusk flanks of the magnetosphere, while much lower flows are observed above the poles. The largest flows are adjacent to the magnetopause. Using appropriate magnetopause crossing lists (for both high and low M A ), we also investigate the changes in magnetopause shape as a function of solar wind M A and IMF orientation. Comparing observed magnetopause crossings with predicted positions from an axisymmetric semi-empirical model, we statistically show that the magnetopause is generally circular during high M A , while is it elongated (albeit with moderate statistical significance) along the direction of the IMF during low M A . These findings are consistent with enhanced magnetic forces that prevail in the magnetosheath during low M A . The component of the magnetic forces parallel to the magnetopause produces the enhanced flows along and adjacent to the magnetopause, while the component normal to the magnetopause exerts an asymmetric pressure on the magnetopause that deforms it into an elongated shape.

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Section: Statistical Study Of Magnetosheath Flowsmentioning

confidence: 99%

Section: Statistical Study Of Magnetosheath Flowsmentioning

confidence: 99%

Section: Statistical Study Of the Magnetopause Shapementioning

confidence: 99%

Section: Statistical Study Of Magnetosheath Flowsmentioning

confidence: 99%

See 2 more Smart Citations

Asymmetry of magnetosheath flows and magnetopause shape during low Alfvén Mach number solar wind

et al. 2013

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“…The time intervals of the Cluster observations in the magnetosheath are chosen for the mission phase with the smallest spacecraft separation (100 km) from February to June 2002, from which 84 magnetosheath traversals are investigated. It is convenient to introduce the solar wind coordinate system (Narita et al, 2006;Verigin et al, 2006). Its basis vectors are spanned as…”

Section: Statistical Studymentioning

confidence: 99%

Propagation pattern of low frequency waves in the terrestrial magnetosheath

Narita¹,

Glaßmeier²

2006

Ann. Geophys.

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Abstract. Propagation pattern (distribution of phase velocities) is determined in three dimensions in the terrestrial magnetosheath on a statistical basis using Cluster spacecraft observations. It is found that the anti-sunward propagation dominates and that the propagation direction is toward the magnetosheath flank at smaller zenith angles, while it is toward the magnetopause at larger angles. This pattern is axially symmetric regardless of the interplanetary magnetic field direction and agrees qualitatively with the density gradient directions in a hydromagnetic flow model of the magnetosheath, suggesting that the wave refraction mechanism is more significant than the wave drift effect.

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A statistical study of magnetic field fluctuations in the dayside magnetosheath and their dependence on upstream solar wind conditions

2014

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The magnetosheath functions as a natural interface connecting the interplanetary and magnetospheric plasma. Since the magnetosheath houses the shocked solar wind, it is populated with abundant magnetic field turbulence which are generated both locally and externally. Although the steady state magnetosheath is to date relatively well understood, the same cannot be said of transient magnetic perturbations due to their kinetic nature and often complex and numerous generation mechanisms. The current manuscript presents a statistical study of magnetic field fluctuations in the dayside magnetosheath as a function of upstream solar wind conditions. We concentrate on the ambient higher‐frequency fluctuations in the range of 0.1 Hz → 2 Hz. We show evidence that the dawn (quasi‐parallel) flank is visibly prone to higher‐amplitude magnetic perturbations compared to the dusk (quasi‐perpendicular) region. Our statistical data also suggest that the magnitude of turbulence can be visibly enhanced close to the magnetopause during periods of southward interplanetary magnetic field orientations. Faster (> 400 km s−1) solar wind velocities also appear to drive higher‐amplitude perturbations compared to slower speeds. The spatial distribution also suggests some dependence on the magnetic pileup region at the subsolar magnetopause.

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Magnetosheath – Interplanetary medium reference frame: Application for a statistical study of mirror type waves in the terrestrial plasma environment

Cited by 39 publications

References 18 publications

Asymmetry of magnetosheath flows and magnetopause shape during low Alfvén Mach number solar wind

Asymmetry of magnetosheath flows and magnetopause shape during low Alfvén Mach number solar wind

Propagation pattern of low frequency waves in the terrestrial magnetosheath

A statistical study of magnetic field fluctuations in the dayside magnetosheath and their dependence on upstream solar wind conditions

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