Distribution of alpha temperature anisotropy in the slow and fast solar wind: WIND observations and Vlasov theory

Context. Alpha particles in the solar wind frequently show temperature anisotropies, which can be constrained by various kinetic instabilities. However, the detailed constraint mechanism remains unclear, especially in different types of solar wind.Aims. Using data obtained by the Wind spacecraft between 2005 and 2015, we investigate the distribution of alpha temperature anisotropy and the correlation with background plasma parameters in the slow and fast solar wind.Methods. We present a comparison between observations of the alpha temperature anisotropy by the Wind spacecraft and theoretical results obtained with the linear Vlasov theory.Results. The results show that the distribution of the alpha temperature anisotropy depends not only on the parallel temperature ratio of alpha to proton T-a?/T-p? and the proton temperature anisotropy T-p?/T-p?, but also on the drift velocity of alpha to proton v(a)/v(A) and the solar wind velocity v(sw). In particular, there are clearly different constraining mechanisms on the distribution of alpha temperature anisotropy in the slow and fast solar wind.Conclusions. The alpha temperature anisotropy instability together with different types of free energy can be effective for regulating the alpha temperature anisotropy in the slow and fast solar wind.

Automated summary

Using data from the Wind spacecraft between 2005 and 2015, the distribution of alpha temperature anisotropy and its correlation with background plasma parameters in the slow and fast solar wind were investigated. The results show that the distribution of alpha temperature anisotropy depends on the parallel temperature ratio of alpha to proton, the proton temperature anisotropy, the drift velocity of alpha to proton, and the solar wind velocity. The constraining mechanisms on the distribution of alpha temperature anisotropy are different in the slow and fast solar wind.