Magnetic Fine Structures in the Solar Corona and Their Heating by Kinetic Alfven Waves  

作　　者：WU Dejin CHEN Ling 

机构地区：[1]Purple Mountain Observatory, CAS, Nanjing, 210008

出　　处：《Bulletin of the Chinese Academy of Sciences》2011年第3期215-219,共5页中国科学院院刊（英文版）

摘　　要：The Sun is our nearest star and the energy released by nuclear reactions near its centre is transported by photons inside the inner - 71% of the solar radius （ R⊙= 6.9 × 10^5km）, called the radiative zone. Outside this radiative zone, called the convective zone, photons are no longer able to transfer energy efficiently, so convective instabilities set in and vertical flows carry nearly all the excess heat to the solar surface. This visible surface, called the photosphere,

关 键 词：结构动力学 阿尔文波 太阳表面 取暖 日冕 能量效率 对流不稳定 辐射区 

分 类 号：P182.2[天文地球—天文学] TU311.3[建筑科学—结构工程]