Speaker
Description
The solar wind plasmas possess temperature anisotropies that cannot be described by the prediction of double-adiabatic theory. It is commonly accepted that the pervasive features of temperature anisotropy observed in the solar wind are thought to result from a combination of physical mechanisms including the expansion, turbulent heating, kinetic instabilities, and Coulomb collisions. In this study, we develop an expanding box model of velocity moment-based quasilinear kinetic analysis that includes the above-mentioned physical ingredients. By incorporating the local kinetic physics into the large scale expansion and/or Parker spiral magnetic field in the present model, we describe how the solar wind temperature anisotropy is formed and evolves in interplanetary space.