The Foreshock

Eastwood, J. P.; Lucek, E.; Mazelle, C.; Meziane, K.; Narita, Yasuhito; Pickett, J. S.; Treumann, R. A.

doi:10.1007/s11214-005-3824-3

Cited by 275 publications

(327 citation statements)

References 119 publications

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“…Thus, it is expected that turbulent characteristics of the ICME sheath and embedded ULF fluctuations are also modified when the sheath interacts with the bow shock. The interaction begins already in the foreshock region, where a large variety of different plasma waves exist (e.g., Eastwood et al, 2005). It is also possible that part of the ULF fluctuations that eventually hit the magnetopause are generated by local sources in the foreshock and bow shock downstream regions (see e.g., Gutysnka et al, 2012;Hartinger et al, 2012, and references therein).…”

Section: Discussionmentioning

confidence: 99%

Magnetic field and dynamic pressure ULF fluctuations in coronal-mass-ejection-driven sheath regions

et al. 2013

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Compressed sheath regions form ahead of interplanetary coronal mass ejections (ICMEs) that are sufficiently faster than the preceding solar wind. The turbulent sheath regions are important drivers of magnetospheric activity, but due to their complex internal structure, relatively little is known on the distribution of the magnetic field and plasma variations in them. In this paper we investigate ultra low frequency (ULF) fluctuations in the interplanetary magnetic field (IMF) and in dynamic pressure (P_dyn) using a superposed epoch analysis of 41 sheath regions observed during solar cycle 23. We find strongest fluctuation power near the shock and in the vicinity of the ICME leading edge. The IMF and P_dyn ULF power have different profiles within the sheath; the former is enhanced in the leading part of the sheath, while the latter is increased in the trailing part of the sheath. We also find that the ICME properties affect the level and distribution of the ULF power in sheath regions. For example, sheath regions associated with strong or fast ICMEs, or those that are crossed at intermediate distances from the center, have strongest ULF power and large variation in the power throughout the sheath region. The weaker or slower ICMEs, or those that are crossed centrally, have in general considerably weaker ULF power with relatively smooth profiles. The strong and abrupt decrease of the IMF ULF power at the ICME leading edge could be used to distinguish the ICME from the preceding sheath plasma

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Section: Discussionmentioning

confidence: 99%

Magnetic field and dynamic pressure ULF fluctuations in coronal-mass-ejection-driven sheath regions

et al. 2013

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“…Ion foreshock intervals can be identified on the basis of correlated 30 s period density and magnetic field strength fluctuations and suprathermal (>1 keV) ion fluxes (Fairfield et al, 1990;Eastwood et al, 2006). Based on these considerations, the observations shown in Fig.…”

Section: Comparison With Observationsmentioning

confidence: 98%

On the edge of the foreshock: model-data comparisons

et al. 2008

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Abstract. We present the results of a global hybrid code simulation for the solar wind-interaction with the Earth's magnetosphere during an interval of steady radial IMF. The model predicts a foreshock marked by innumerable localized, correlated, and large amplitude, density and magnetic field strength variations, depressed velocities, and enhanced temperatures. The foreshock is bounded by a broad (∼0.8 R E ) region of enhanced densities, temperatures, and magnetic field strengths that extends far (∼8.6 R E ) upstream from the bow shock. Flow perturbations within the boundary are directed perpendicular to the boundary, towards the unperturbed solar wind and away from the foreshock. Cluster observations of the ion foreshock and pristine solar wind confirm the predictions of the model. The observations suggest that foreshock cavities, crater-like density and magnetic field strength structures whose cores are filled with suprathermal particles, can be interpreted in terms of transient encounters with the foreshock boundary.

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“…3. Here we briefly summarise some of the main features; many more specific reviews have been published (e.g., Tsurutani and Stone 1985;Fuselier 1994Fuselier , 1995Le and Russell 1994;Burgess 1995;Burgess et al 2005;Eastwood et al 2005b). In Fig.…”

Section: Planetary Bow Shock Structurementioning

confidence: 99%

What Controls the Structure and Dynamics of Earth’s Magnetosphere?

et al. 2014

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Unlike most cosmic plasma structures, planetary magnetospheres can be extensively studied in situ. In particular, studies of the Earth's magnetosphere over the past few decades have resulted in a relatively good experimental understanding of both its basic structural properties and its response to changes in the impinging solar wind. In this article we provide a broad overview, designed for researchers unfamiliar with magnetospheric physics, of the main processes and parameters that control the structure and dynamics of planetary magnetospheres, especially the Earth's. In particular, we concentrate on the structure and dynamics of three important regions: the bow shock, the magnetopause and the magnetotail. In the final part of this review we describe the current status of global magnetospheric modelling, which is crucial to placing in situ observations in the proper context and providing a better understanding of magnetospheric structure and dynamics under all possible input conditions. Although the parameter regime experienced in the solar system is limited, the plasma physics that is learned by studying planetary magnetospheres can, in principle, be translated to more general studies of cosmic plasma structures. Conversely, studies of cosmic plasma under a wide range of conditions should be used to understand Earth's

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The Foreshock

Cited by 275 publications

References 119 publications

Magnetic field and dynamic pressure ULF fluctuations in coronal-mass-ejection-driven sheath regions

Magnetic field and dynamic pressure ULF fluctuations in coronal-mass-ejection-driven sheath regions

On the edge of the foreshock: model-data comparisons

What Controls the Structure and Dynamics of Earth’s Magnetosphere?

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