Mirror mode waves in Venus's magnetosheath: solar minimum vs. solar maximum

Volwerk, M.; Schmid, Daniel; Tsurutani, B. T.; Delva, M.; Plaschke, Ferdinand; Narita, Yasuhito; Zhang, Tielong; Glaßmeier, Karl‐Heinz

doi:10.5194/angeo-34-1099-2016

Cited by 39 publications

(74 citation statements)

References 39 publications

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“…Tsurutani, Dasgupta, et al () identified mirror mode structures and ion cyclotron waves within MDs. Proton temperature anisotropies with T ┴ / T || > 1 are necessary for the mirror instability to grow (Genot et al, ; Hasegawa, ; Hasegawa & Tsurutani, ; Hellinger, ; Hellinger et al, ; Pokhotelov et al, ; Price et al, ; Travnicek et al, ; Tsurutani, Lakhina, Verkhoglyadova, Echer, et al, ; Tsurutani, Smith, Anderson et al, ; Volwerk et al, , ). The same anisotropy is necessary for the proton temperature anisotropy instability to grow (Gary et al, ; Kennel & Petschek, ; Remya et al, ).…”

Section: Resultsmentioning

confidence: 99%

A Review of Alfvénic Turbulence in High‐Speed Solar Wind Streams: Hints From Cometary Plasma Turbulence

et al. 2018

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Solar wind turbulence within high‐speed streams is reviewed from the point of view of embedded single nonlinear Alfvén wave cycles, discontinuities, magnetic decreases (MDs), and shocks. For comparison and guidance, cometary plasma turbulence is also briefly reviewed. It is demonstrated that cometary nonlinear magnetosonic waves phase‐steepen, with a right‐hand circular polarized foreshortened front and an elongated, compressive trailing edge. The former part is a form of “wave breaking” and the latter that of “period doubling.” Interplanetary nonlinear Alfvén waves, which are arc polarized, have a ~180° foreshortened front and with an elongated trailing edge. Alfvén waves have polarizations different from those of cometary magnetosonic waves, indicating that helicity is a durable feature of plasma turbulence. Interplanetary Alfvén waves are noted to be spherical waves, suggesting the possibility of additional local generation. They kinetically dissipate, forming MDs, indicating that the solar wind is partially “compressive” and static. The ~2 MeV protons can nonresonantly interact with MDs leading to rapid cross‐field (~5.5% Bohm) diffusion. The possibility of local (~1 AU) generation of Alfvén waves may make it difficult to forecast High‐Intensity, Long‐Duration AE Activity and relativistic magnetospheric electrons with great accuracy. The future Solar Orbiter and Solar Probe Plus missions should be able to not only test these ideas but to also extend our knowledge of plasma turbulence evolution.

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Section: Resultsmentioning

confidence: 99%

A Review of Alfvénic Turbulence in High‐Speed Solar Wind Streams: Hints From Cometary Plasma Turbulence

et al. 2018

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“…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%

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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“…Apparently, the observations support the existence of mirror modes in different space plasma environments, like, terrestrial and other planetary magnetosheaths (ErdŐs & Balogh, ; Hasegawa & Tsurutani, ; Narita et al, ; Tsurutani et al, ; Volwerk et al, , ), cometary environments (Glassmeier et al, ; Russell et al, ; Tsurutani et al, ), the solar wind (Liu et al, ; Russell et al, ; Tsurutani et al, ) and the heliosheath (Tsurutani, Echer, et al, ), and even at sites of magnetic reconnection (Vörös, ). However, Tsurutani, Lakhina, et al () have shown that most of the traces reported in interplanetary space may actually be magnetic decreases of the ambient field, while mirror mode instabilities remain a major feature of planetary magnetosheaths and are only rarely seen in interplanetary space or at comets.…”

Section: Introductionmentioning

confidence: 63%

Stimulated Mirror Instability From the Interplay of Anisotropic Protons and Electrons, and their Suprathermal Populations

et al. 2018

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Mirror instability driven by the temperature anisotropy of protons can offer a plausible explanation for the mirror‐like fluctuations observed in planetary magnetosheaths. In the present paper we invoke a realistic kinetic approach which can reproduce nonthermal features of plasma particles reported by the observations, i.e., temperature anisotropies and suprathermal populations. Seeking accuracy, a numerical analysis is performed using an advanced code named DSHARK, recently proposed to resolve the linear dispersion and stability for an arbitrary propagation in bi‐Kappa distributed electron‐proton plasmas. The stimulating effect of the anisotropic bi‐Maxwellian electrons reported in Remya et al. (2013, https://doi.org/10.1002/jgra.50091) is markedly enhanced in the presence of suprathermal electrons described by the bi‐Kappa distribution functions. The influence of suprathermal protons is more temperate, but overall, present results demonstrate that these sources of free energy provide natural conditions for a stimulated mirror instability, more efficient than predicted before and capable to compete with other instabilities (e.g., the electromagnetic ion‐cyclotron instability) and mechanisms of relaxation.

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Mirror mode waves in Venus's magnetosheath: solar minimum vs. solar maximum

Cited by 39 publications

References 39 publications

A Review of Alfvénic Turbulence in High‐Speed Solar Wind Streams: Hints From Cometary Plasma Turbulence

A Review of Alfvénic Turbulence in High‐Speed Solar Wind Streams: Hints From Cometary Plasma Turbulence

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

Stimulated Mirror Instability From the Interplay of Anisotropic Protons and Electrons, and their Suprathermal Populations

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