Extended MHD modeling of the steady solar corona and the solar wind

被引：71

作者：

Gombosi, Tamas I. ^{[1
]}

van der Holst, Bart ^{[1
]}

Manchester, Ward B. ^{[1
]}

Sokolov, Igor V. ^{[1
]}

机构：

[1] Univ Michigan, Ctr Space Environm Modeling, 2455 Hayward, Ann Arbor, MI 48109 USA

来源：

LIVING REVIEWS IN SOLAR PHYSICS | 2018年 / 15卷

基金：

美国国家科学基金会; 欧盟地平线“2020”;

关键词：

Sun; Solar wind; MHD; Global simulations; Space weather; INTERPLANETARY MAGNETIC-FIELD; COROTATING STREAM FRONTS; WHITE-LIGHT BRIGHTNESS; AMPLITUDE ALFVEN WAVES; MASS EJECTIONS; 3-DIMENSIONAL MODEL; TRANSITION REGION; LOW-FREQUENCY; MAGNETOHYDRODYNAMIC SIMULATIONS; TURBULENCE-DRIVEN;

D O I：

10.1007/s41116-018-0014-4

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The history and present state of large-scale magnetohydrodynamic modeling of the solar corona and the solar wind with steady or quasi-steady coronal physics is reviewed. We put the evolution of ideas leading to the recognition of the existence of an expanding solar atmosphere into historical context. The development and main features of the first generation of global corona and solar wind models are described in detail. This historical perspective is also applied to the present suite of global corona and solar wind models. We discuss the evolution of new ideas and their implementation into numerical simulation codes. We point out the scientific and computational challenges facing these models and discuss the ways various groups tried to overcome these challenges. Next, we discuss the latest, state-of-the art models and point to the expected next steps in modeling the corona and the interplanetary medium.

引用

页数：57

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