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In the solar wind, long-wavelength compressive slow-mode fluctuations lead to changes in $\\beta_{\\parallel \\mathrm p}\\equiv 8\\pi n_{\\mathrm p}k_{\\mathrm B}T_{\\parallel \\mathrm p}/B^2$ and in $R_{\\mathrm p}\\equiv T_{\\perp \\mathrm p}/T_{\\parallel \\mathrm p}$, where $T_{\\perp \\mathrm p}$ and $T_{\\parallel \\mathrm p}$ are the perpendicular and parallel temperatures of the protons, $B$ is the magnetic field strength, and $n_{\\mathrm p}$ is the proton density. 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