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Comparative analyses of current three-dimensional numerical solar wind models

Science China Earth Sciences 2015年第6期58卷 839-858页

作者： Shi Tsan WU murray dryer Center for Space Plasma and Aeronomic Research the University of Alabama in Huntsville Space Weather Predictions Center National Weather Service National Oceanic and Atmospheric Administration

We present a comparative study of the most advanced three-dimensional time-dependent numerical simulation models of solar wind. These models can be classified into two categories：（I） theoretical, empirical and numerically based models and （Ⅱ） self-consistent multi-dimensional numerical magnetohydrodynamic （MHD） models. The models of Category I are used to sep- arately describe the solar wind solution in two plasma flows regions： transonic/trans-Alfvrnic and supersonic/super-Alfvenic, respectively. Models of Category II construct a complete, single, numerical solar wind solution through subsonic/sub-Alfvrnic region into supersonic/super-Alfvrnic region. The Wang-Sheeley-Arge （WSA）/ENLIL in CISM is the most successful space weather model that belongs to Category I, and the Block-Adaptive-Tree-Solarwind-Roe-Upwind-Scheme （BATS-R-US） code in SWMF （Space Weather Modeling Framework） and the solar-interplanetary conservative element solution element MHD （SIP-CESE MHD） model in SWIM （Space Weather Integrated Model） are the most commonly-used models that belong to Category II. We review the structures of their frameworks, the main results for solar wind background studies that are essential for solar transient event studies, and discuss the common features and differences between these two categories of solar wind models. Finally, we conclude that the transition of these two categories of models to operational use depends on the availability of computational resources at reasonable cost and point out that the models＇ prediction capabilities may be improved by employing finer computational grids, incorporating more observational data and by adding more physical constraints to the models.

关键词： space weather solar wind models comparative analyses

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Challenges of modeling solar disturbances' arrival times at the Earth

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Science China(Technological Sciences) 2008年第10期51卷 1580-1588页

作者： C. D. FRY Chin-Chun WU murray dryer Center for Space Plasma and Aeronomic Research The University of Alabama in Huntsville Huntsville AL 35899 USA Exploration Physics International Inc. Huntsville AL 35806 USA Center for Space Plasma and Aeronomic Research The University of Alabama in Huntsville Huntsville AL 35899 USA Space Weather Laboratory NASA/Goddard Space Flight Center Greenbelt MD 20771 USA Center for Space Plasma and Aeronomic Research The University of Alabama in Huntsville Huntsville AL 35899 USA Exploration Physics International Inc. Huntsville AL 35806 USA Space Weather Prediction Center National Oceanic and Atmospheric Administration (NOAA) Boulder Colorado USA

In recent years remarkable advances have been made in the development of phys-ics based models of various parts of the solar-terrestrial system (see JASTP special issues, October, November 2004; February 2007). In this paper, we focus our dis-cussions in a specific region of the Sun to the Earth’s environment (i.e. 1 AU). It is well-known that geomagnetic storms are caused by solar eruptions. The conse-quences of these storms include particle acceleration, solar wind impact on the Earth’s magnetosphere and ionosphere, UV-EUV radiation effects on the lower at-mosphere, etc. One of the main challenges is to predict the arrival time at 1 AU of the solar disturbance. The prospects look good for an accurate, real-time forecast scheme built on the acquisition of solar, heliosphere and the near-Earth data and large-scale models. However, the accuracy of these models still needs improve-ment. We will discuss the present status of the models and challenges to improve the simulation models.

关键词： space weather――magnetohydrodynamic (MHD) Modeling MHD Sun-Earth connection MHD Sun-Corona

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