2:45 PM - 3:00 PM
[PEM19-11] Turbulent transport model in a three-dimensional structured solar wind
Keywords:solar wind , MHD, turbulence
Recently we have developed a solar wind MHD model for the inner heliosphere based on synoptic observations of the photospheric magnetic field (Shiota et al. 2014). The numerical results show reasonable agreement with in situ measurements of the solar wind at the orbits of Earth, Venus, and Mars. This MHD model is now used as part of the real-time space weather forecast system SUSANOO (http://st4a.stelab.nagoya-u.ac.jp/susanoo/).
We have extended our 3D MHD model to include the transport and dissipation of turbulence using the theoretical model developed by Zank et al. (2012). We solve a coupled model that describes the 3D inhomogeneous solar wind and the temporal and spatial evolution of three moments or variables that describe turbulent fluctuation intensities (the energy in forward and backward modes and the residual energy) and their corresponding correlation lengths. We find that the radial profiles for the three moments of the solar wind turbulence predicted by our model show good agreement with those of in situ measurements obtained from Ulysses and Helios observations. Based on the detailed analysis of the numerical results, we will discuss the connection between turbulence generation and global solar wind structure.