Turbulence, complexity, and solar flares

被引：49

作者：

McAteer, R. T. James ^{[1
]}

Gallagher, Peter T. ^{[1
]}

Conlon, Paul A. ^{[1
]}

机构：

[1] Univ Dublin Trinity Coll, Sch Phys, Dublin 2, Ireland

来源：

ADVANCES IN SPACE RESEARCH | 2010年 / 45卷 / 09期

关键词：

Solar flares; Space weather; CORONAL MASS EJECTIONS; ACTIVE REGIONS; MAGNETIC-FIELD; SUNSPOT GROUPS; MAGNETOGRAMS; CLASSIFICATION; PREDICTION; ENERGY; PRODUCTIVITY; STATISTICS;

D O I：

10.1016/j.asr.2009.08.026

中图分类号：

V [航空、航天];

学科分类号：

08 ; 0825 ;

摘要：

The issue of predicting solar flares is one of the most fundamental in physics, addressing issues of plasma physics, high-energy physics, and modelling of complex systems. It also poses societal consequences, with our ever-increasing need for accurate space weather forecasts. Solar flares arise naturally as a competition between an input (flux emergence and rearrangement) in the photosphere and an output (electrical current build up and resistive dissipation) in the corona. Although initially localised, this redistribution affects neighbouring regions and an avalanche occurs resulting in large scale eruptions of plasma, particles, and magnetic field. As flares are powered from the stressed field rooted in the photosphere, a study of the photospheric magnetic complexity can be used to both predict activity and understand the physics of the magnetic field. The magnetic energy spectrum and multifractal spectrum are highlighted as two possible approaches to this. (C) 2009 COSPAR. Published by Elsevier Ltd. All rights reserved.

引用

页码：1067 / 1074

页数：8

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