太阳色球层-日冕中扰动的传播(Ⅱ)

首先讨论了磁流波传播的线性特征，然后构造了球坐标中-自治的非等温，非均匀等离子体初态，应用二维时变可压缩磁流体动力学模拟，数值研究了色球层底部压力脉冲所引起扰动的全球传播过程，结果表明，在极区，压力脉冲导致的扰动传播可以区分成两类不同模式的波动，快磁声波与慢磁声波，而在赤道附近，传播扰动是快模磁声波，在源区附近还存在一非传播的扰动，模拟结果的特征有助于解释SOHO/EIT观测到的波动事件。

PROPAGATION OF DISTURBANCES IN THE SOLAR CHROMOSPHERE-CORONA (Ⅱ)

In the first part of this article, the linear properties of MHD wave propagation is discussed. Then, in order to simulate the global characteristics of wave propagation in the solar chromosphere-corona, by employing a 2-dimensional time-dependent compressible MHD simulation subject to a self-consistent non-isothermal, non-uniform initial state, we study numerically the global propagation process of the disturbances initiated by a pressure pulse implemented at the bottom of chromosphere. Numerical results indicate that, in polar region, propagating disturbances can be distinguished into two modes, i.e. fast and slow magneto-acoustic waves. Whereas in the vicinity of solar equator, propagating disturbance is regarded as fast mode wave, and a standing disturbance is found to be located near the source region. These results may help explaining the wave events observed by SOHO/EIT.