Three-Dimensional Solar Wind Structures Obtained with MHD Simulation Model Using Observation-Based Time-Varying Inner Boundary Map

Details Three-Dimensional Solar Wind Structures Obtained with MHD Simulation Model Using Observation-Based Time-Varying Inner Boundary Map Three-Dimensional Solar Wind Structures Obtained with MHD Simulation Model Using Observation-Based Time-Varying Inner Boundary Map

Oct 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aspc..444..111h&link_type=abstract

5th international conference of numerical modeling of space plasma flows (astronum 2010). Proceedings of a 5th international con

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We report our recent efforts to reproduce numerically three-dimensional time-dependent structures of the solar wind in the heliosphere responding to the time-varying boundary data on the inner boundary sphere at the heliocentric distance of 50 radii. The computation region is extended up to 10050 solar radii (approximately 47AU). A boundary model we recently developed is used to include the time-varying observation-based data map in the inner heliosphere including the radial component of the magnetic field. One merit of using the time-varying boundary conditions in the MHD simulation is that we will be able to determine better the MHD variables of the solar wind at the time and position of interest, especially in the distant regions from the Sun. The boundary data used here were derived from the IPS (interplanetary scintillation) at Nagoya University of Japan that can yield the solar wind speed at both high and low heliographic latitudes, and the solar-surface magnetic field data, such as those by SOHO/MDI and WSO. In this article, we will show the comparisons of our simulation results with the in-situ measurements made by space probes, such as the nearby-Earth measurement dataset (OMNIweb data), Ulysses, and Voyager 1 and 2 (COHOweb database), in 1991.

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