Kinetic Physics of the Solar Wind Plasma

Marsch, E.

doi:10.1007/978-3-642-75364-0_3

Cited by 190 publications

(100 citation statements)

References 221 publications

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“…All the parameters used as input for the dispersion relation solver are averaged values observed by STEREO from mirror-mode storm events observed in 2007 and 2008, except for the proton temperature anisotropy. Because STEREO has not yet provided temperature anisotropies (T ⊥ /T || ), we assume proton temperature anisotropies between 1 and 3 based on previous solar wind measurements at 1 AU [Winterhalter et al, 1994;Liu et al, 2006;Marsch et al, 1982;Marsch, 1991;Gary et al, 2002].…”

Section: Kinetic Dispersion Analysismentioning

confidence: 99%

Mirror‐mode storms inside stream interaction regions and in the ambient solar wind: A kinetic study

et al. 2013

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[1] Mirror-mode structures have been found in the solar wind at various heliocentric distances with different missions. Recently, STEREO has observed mirror-mode waves present as trains of holes and also as humps in the magnetic field magnitude. In some cases, mirror-mode trains last for very long periods of time and have been called "mirror-mode storms". We present case studies of mirror-mode storms observed in the solar wind using STEREO data in three different locations: in the downstream region of the forward shock of a stream interaction region, inside a stream interaction region far from the forward shock, and also in the ambient solar wind. To make a formal identification of the mirror mode, we determine wave characteristics using minimum variance analysis. Finally, we perform a kinetic dispersion analysis and discuss the possible origin of mirror-mode structures evaluating curves of growth for different regimes of proton temperature anisotropies in a plasma with a He component.

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Section: Kinetic Dispersion Analysismentioning

confidence: 99%

Mirror‐mode storms inside stream interaction regions and in the ambient solar wind: A kinetic study

et al. 2013

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“…In contrast, at higher flow speeds a third electron component, the "strahl," appears, and proton beams frequently arise [Feldman e! el., 1974; Marsch, 1991 We used the Ulysses high-resolution three-dimensional electron data set, utilizing parameters derived from biMaxwellian fits to both the core and halo velocity distributions. This data set includes the corrections for spacecraft potential developed and described by $cime et el.…”

Section: 559mentioning

confidence: 99%

Lower bound for electron core beta in the solar wind

Gary¹,

Newbury²,

Goldstein³

1998

J. Geophys. Res.

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“…The classical expression for proton conduction thus greatly overestimates the heat transport in the proton gas. On the other hand, it is often argued that the solar wind might be collisionally dominated in the inner corona, say inside 10 Rs [e.g., Marsch, 1991]. However, in a solar wind which basically reaches its final flow speeds at a few solar radii, the distance where the solar wind expansion time becomes large compared to the collision time moves much closer to the coronal base (to about 1.6 Rs in the models presented below).…”

Section: Description Of the Solar Wind Modelmentioning

confidence: 99%