Fluid versus simulation model of solitons in solar wind: Application to Ulysses observations

doi:doi:10.1029/2007JA012557

Abstract

Cited By (2)

Abstract

JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 112, A12101, 13 PP., 2007
doi:10.1029/2007JA012557

Fluid versus simulation model of solitons in solar wind: Application to Ulysses observations

K. Baumgärtel

Astrophysikalisches Institut Potsdam, Potsdam, Germany

K. Sauer

Department of Physics, University of Alberta, Edmonton, Alberta, Canada

E. Mjølhus

Department of Mathematics and Statistics, University of Tromsø, Tromsø, Norway

E. Dubinin

Max Planck Institute for Solar System Research, Katlenburg-Lindau, Germany

This paper continues recent efforts based on Hall-MHD theory (Sauer et al., 2007) to explain a new class of magnetically compressive solitary structures in the interplanetary space, observed by the Ulysses magnetometer (Rees et al., 2006). The theoretical basis is extended by a kinetic approach via one-dimensional hybrid code simulations which reveal deficiencies of fluid theory in describing slow mode-type solitons in a collisionless finite β plasma. Kinetic solitary structures, resembling obliquely propagating Alfven wave pulses with quasi-circular or banana-type polarization are presented which may reproduce most of the observational features. This suggests that the soliton picture provides an adequate theoretical concept for the observed events.

Received 23 May 2007; accepted 8 September 2007; published 7 December 2007.

Citation: Baumgärtel, K., K. Sauer, E. Mjølhus, and E. Dubinin (2007), Fluid versus simulation model of solitons in solar wind: Application to Ulysses observations, J. Geophys. Res., 112, A12101, doi:10.1029/2007JA012557.

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