JpGU-AGU Joint Meeting 2017

Presentation information

[EJ] Oral

P (Space and Planetary Sciences) » P-EM Solar-Terrestrial Sciences, Space Electromagnetism & Space Environment

[P-EM20] [EJ] Heliosphere and Interplanetary Space

Wed. May 24, 2017 10:45 AM - 12:15 PM A02 (Tokyo Bay Makuhari Hall)

convener:Ken Tsubouchi(Tokyo Institute of Technology), Masaki N Nishino(Institute for Space-Earth Environmental Research, Nagoya University), Yasuhiro Nariyuki(Faculty of Human Development, University of Toyama), Chairperson:Ken Tsubouchi(Tokyo Institute of Technology), Chairperson:Fumiko Otsuka(Interdisciplinary Graduate School of Engineering Sciences Kyushu University)

11:00 AM - 11:15 AM

[PEM20-02] Turbulent transport MHD model in a structured three-dimensional solar wind

*Daikou Shiota1, Gary P. Zank2, Laxman Adhikari2, Peter Hunana2, Daniele Telloni3, Roberto Bruno4 (1.Institute for Space-Earth Environmental Research, Nagoya University, 2.Center for Space Plasma and Aeronomic Research (CSPAR), Department of Space Science, University of Alabama in Huntsville, 3.INAF - Astrophysical Observatory of Torino, 4.INAF-IAPS Istituto di Astrofisica e Planetologia Spaziali)

Keywords:solar wind, turbulence, MHD simulation

Turbulence in the solar wind can play essential roles in the heating of coronal and solar wind plasma and the acceleration of the solar wind and energetic particles. Turbulence sources are not well understood and thought to be partly enhanced by interaction with the large-scale inhomogeneity of the solar wind and the interplanetary magnetic field (IMF) and/or transported from the solar corona.
To investigate the interaction with background inhomogeneity and the turbulence sources, we have developed a new 3D MHD model that includes the transport and dissipation of turbulence using the theoretical model Zank et al. (2012). We solve for the temporal and spatial evolution of three moments or variables, the energy in the forward and backward fluctuating modes and the residual energy and their three corresponding correlation lengths. The transport model is coupled to our 3D model of the inhomogeneous solar wind. We present results of the coupled solar wind-turbulence model assuming a simple tilted dipole magnetic configuration that mimics solar minimum conditions, together with several comparative intermediate cases. By considering eight possible solar wind configurations, we show that the large-scale solar wind and IMF inhomogeneity and the strength of the turbulence sources significantly affect the distribution of turbulence in the heliosphere within 5 AU. We compare the predicted turbulence distribution results from a complete solar minimum model with in situ measurements made by the Helios and Ulysses spacecraft, finding that the synthetic profiles of the turbulence intensities show reasonable agreement with observations.
We will also discuss the capability of this model and a future direction of development of a more advanced model.