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- W2524498983 endingPage "88" @default.
- W2524498983 startingPage "88" @default.
- W2524498983 abstract "In collisionless plasmas such as the solar wind, the coupling between plasma constituents and the embedded magnetic field occurs on various temporal and spatial scales, and is primarily responsible for the transfer of energy between waves and particles. Recently, it was shown that the transfer of energy between solar wind plasma particles and waves is governed by a new and unique relationship: the ratio between the magnetosonic energy and the plasma frequency is constant, Ems/ωpl ∼ ℏ*. This paper examines the variability and substantial departure of this ratio from ℏ* observed at ∼1 au, which is caused by a dispersion of fast magnetosonic (FMS) waves. In contrast to the efficiently transferred energy in the fast solar wind, the lower efficiency of the slow solar wind can be caused by this dispersion, whose relation and characteristics are derived and studied. In summary, we show that (i) the ratio Ems/ωpl transitions continuously from the slow to the fast solar wind, tending toward the constant ℏ*; (ii) the transition is more efficient for larger thermal, Alfvén, or FMS speeds; (iii) the fast solar wind is almost dispersionless, characterized by quasi-constant values of the FMS speed, while the slow wind is subject to dispersion that is less effective for larger wind or magnetosonic speeds; and (iv) the constant ℏ* is estimated with the best known precision, ℏ* ≈ (1.160 ± 0.083) × 10−22 Js." @default.
- W2524498983 created "2016-10-07" @default.
- W2524498983 creator A5010313183 @default.
- W2524498983 creator A5080379161 @default.
- W2524498983 date "2016-09-26" @default.
- W2524498983 modified "2023-10-17" @default.
- W2524498983 title "PLASMA-FIELD COUPLING AT SMALL LENGTH SCALES IN SOLAR WIND NEAR 1 au" @default.
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- W2524498983 doi "https://doi.org/10.3847/0004-637x/829/2/88" @default.
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