References

ANGEO

Annales Geophysicae

ANGEO

Ann. Geophys.

1432-0576

Copernicus Publications

Göttingen, Germany

10.5194/angeo-31-1559-2013

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

Kilpua

E. K. J.

¹ Hietala

² Koskinen

H. E. J.

¹ ³ Fontaine

https://orcid.org/0000-0002-4348-2623

⁴ Turc

⁴

Department of Physics, P.O. Box 64, University of Helsinki, Finland

Space and Atmospheric Physics Group, The Blackett Laboratory, Imperial College, London SW7 2AZ, UK

Finnish Meteorological Institute, P.O. Box 503, Helsinki, Finland

Laboratoire de Physique des Plasmas, Ecole Polytechnique, Route de Saclay 91128 Palaiseau, France

10 09 2013

31 9 1559 1567

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 (Pdyn) 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 Pdyn 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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