Properties of magnetosheath mirror modes observed by Cluster and their response to changes in plasma parameters

Souček, J.; Lucek, E.; Dandouras, I.

doi:10.1029/2007ja012649

Cited by 145 publications

(287 citation statements)

References 47 publications

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“…The timescale of MMs in the solar wind at 0.72 AU is reported to vary from a few seconds up to 40 s (Zhang et al, 2009). Similar durations are also reported in the magnetosheath of the Earth (Soucek et al, 2008). We therefore expect the MMs to have similar durations in ICME-driven sheath regions.…”

Section: Mirror Mode (Mm) Identificationsupporting

confidence: 54%

“…Studies of planetary magnetosheaths have shown that peak-like MMs occur in mirror unstable plasma, whereas dip-like MMs are observed in both mirror stable and unstable plasma (e.g., Soucek et al, 2008;Califano et al, 2008;Génot et al, 2009a). Furthermore, in 2-D hybrid simulations, dip-like MMs were formed in low β plasma, whereas peak-like structures were generated in high β plasma (Shoji et al, 2012).…”

Section: M Ala-lahti Et Al: Mirror Mode Wave Occurrence In Icme-mentioning

confidence: 99%

“…ICMEdriven sheaths are of great interest for solar-terrestrial studies as they are strong drivers of geomagnetic activity (e.g., Tsurutani et al, 1988;Huttunen et al, 2002;Huttunen and Koskinen, 2004;Siscoe et al, 2007;Kilpua et al, 2017, see also Echer et al, 2011;Oliveira and Raeder, 2014;Lugaz et al, 2016), and their shocks have a key role in the acceleration of solar energetic particles (e.g., Reames, 1999;Manchester et al, 2005). Similarly to planetary magnetosheaths (e.g., Soucek et al, 2008;Osmane et al, 2015), MM waves may have large-scale effects on ICME sheaths.…”

Section: M Ala-lahti Et Al: Mirror Mode Wave Occurrence In Icme-mentioning

confidence: 99%

“…Previous studies have mostly utilized linear polarization and compression of MM waves when identifying these structures (e.g., Tátrallyay and Erdős, 2005;Soucek et al, 2008;Dimmock et al, 2015;Osmane et al, 2015). In practice, these studies have computed both the maximum variance direction of the magnetic field vector (B m ; Sonnerup and Cahill, 1967) and its direction with respect to the average magnetic field direction b 0 = [B 1 ,B 2 ,B 3 ]/|B 1 ,B 2 ,B 3 |, where the subscripts 1, 2 and 3 denote the components of the magnetic field vector, by applying the minimum variance analysis (MVA).…”

Section: Mirror Mode (Mm) Identificationmentioning

confidence: 99%

“…They are frequently observed in heliospheric plasma, in particular in different sheath structures. They are the most widely studied in the planetary magnetosheaths (e.g., Tsurutani et al, 1982;Hellinger et al, 2003;Soucek et al, 2008Soucek et al, , 2015Volwerk et al, 2008;Génot et al, 2009b;Herčík et al, 2013;Schmid et al, 2014;Volwerk et al, 2016), but also found in cometosheaths (e.g., Russell et al, 1991;Glassmeier et al, 1993;Tsurutani et al, 1999;Schmid et al, 2014), in the heliosheath (e.g., Liu et al, 2007;Génot, 2008;Tsurutani et al, 2011a) and ahead of the dipolarization front (Wang et al, 2016). MMs are also studied in the solar wind (e.g., Hellinger et al, 2006Hellinger et al, , 2017Bale et al, 2009;Russell et al, 2009), behind interplanetary shocks ) and in addition in interplanetary coronal mass ejections (ICMEs; Siu-Tapia et al, 2015).…”

Section: Introductionmentioning

confidence: 99%

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Statistical analysis of mirror mode waves in sheath regions driven by interplanetary coronal mass ejection

et al. 2018

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Abstract. We present a comprehensive statistical analysis of mirror mode waves and the properties of their plasma surroundings in sheath regions driven by interplanetary coronal mass ejection (ICME). We have constructed a semiautomated method to identify mirror modes from the magnetic field data. We analyze 91 ICME sheath regions from January 1997 to April 2015 using data from the Wind spacecraft. The results imply that similarly to planetary magnetosheaths, mirror modes are also common structures in ICME sheaths. However, they occur almost exclusively as dip-like structures and in mirror stable plasma. We observe mirror modes throughout the sheath, from the bow shock to the ICME leading edge, but their amplitudes are largest closest to the shock. We also find that the shock strength (measured by Alfvén Mach number) is the most important parameter in controlling the occurrence of mirror modes. Our findings suggest that in ICME sheaths the dominant source of free energy for mirror mode generation is the shock compression. We also suggest that mirror modes that are found deeper in the sheath are remnants from earlier times of the sheath evolution, generated also in the vicinity of the shock.

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Section: Mirror Mode (Mm) Identificationsupporting

confidence: 54%

Section: M Ala-lahti Et Al: Mirror Mode Wave Occurrence In Icme-mentioning

confidence: 99%

Section: M Ala-lahti Et Al: Mirror Mode Wave Occurrence In Icme-mentioning

confidence: 99%

Section: Mirror Mode (Mm) Identificationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Statistical analysis of mirror mode waves in sheath regions driven by interplanetary coronal mass ejection

et al. 2018

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Gyrokinetic particle simulation of nonlinear evolution of mirror instability

Porazik

2013

JGR Space Physics

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[1] A gyrokinetic simulation model for nonlinear studies of the mirror instability is described. The model is set in a uniform, periodic slab with anisotropic ions and cold electrons. Particle-in-cell simulations with a noise reducing ıf algorithm show agreement with the linear theory of the mirror instability. Results of nonlinear simulations near marginal stability are presented. Single-mode simulations show saturation due to trapping. Simulations with a spectrum of unstable modes show that the negative magnetic perturbations saturate at a lower amplitude and earlier than the positive magnetic perturbations, which results in the development of peaked saturated structures. The saturation amplitude of negative magnetic perturbations is in agreement with the trapped particle theory, while the saturation amplitude of the positive magnetic perturbations is determined by the local change in theˇ? (ratio of perpendicular plasma pressure to magnetic pressure) parameter.

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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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Properties of magnetosheath mirror modes observed by Cluster and their response to changes in plasma parameters

Cited by 145 publications

References 47 publications

Statistical analysis of mirror mode waves in sheath regions driven by interplanetary coronal mass ejection

Statistical analysis of mirror mode waves in sheath regions driven by interplanetary coronal mass ejection

Gyrokinetic particle simulation of nonlinear evolution of mirror instability

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

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