Solar Wind Models

Both 1D and 2D solar wind models have been developed in this group. Our one dimensional solar wind models have been a great success. However, multi-dimensional solar wind models are needed because the corona and solar wind have structures. While the origin of the fast solar wind may seem straightforward, the source regions of slow solar wind are often complex. Our two-dimensional solar wind models has been successfully developed, it gives a complete picture of the global solar wind. The proposed research will study the 2D structure of the proton temperature anisotropy of the solar wind which has never been attempted before. Because the temperature anisotropy carries clues of any kinetic wave-particle interaction, the work in this area may offer important clues for our understanding of the difference between the heating mechanisms of the fast and slow wind. The initial work in this area is in good progress.

Contours of the proton temperature T_p, the electron temperature T_e, and the number density n for the solution of case A. The contour levels are equally spaced by 0.1 for log T_e and log T_p (K), and 0.5 for log$n$ (cm$^{-3}$), with 6 and 8 as one of the levels respectively.  

(A figure from a recent 2D solar wind model by Hu, Habbal, Chen and Li, submitted to JGR) This  model nicely describes the 2D structure of the solar wind at solar minimum. 

We also plan to study the 2D structure of the proton temperature anisotropy of the solar wind which has never been attempted before. Because the temperature anisotropy carries clues of any kinetic wave-particle interaction, the work in this area may offer important clues to our understanding what is the difference between the heating mechanisms of the fast and slow wind. The initial work in this area is in good progress.