一次极端紫外波事件中波动和非波动分量的正交观测及其解耦
Quadrature Observations of Wave and Non-Wave Components and Their Decoupling in an Extreme-Ultraviolet Wave Event
摘要：
我们报告了2011年1月27日极紫外（EUV）波事件的正交观测结果，由极紫外成像仪（EUVI）机载\emph{Solar Terrestrial Relations Observatory}（\emph{STEREO}）和大气成像组件（AIA）机载\emph{Solar Dynamics Observatory}（\emph{SDO}）。在极紫外波事件中揭示了两个分量。以$\sim$ 440 km s $^{-1}$的初始速度发射主锋。在较热的通道中出现显著的排放增强，而在较冷的通道中出现深度排放减少。当主锋遇到一个大的日冕环系统并减速时，一个次要的更微弱的锋从主锋发出，具有相对较高的$\sim$ 550 km s $^{-1}$的起始速度。之后，两个波前独立地传播，分离度增加。主锋最后停在磁分界线上，而次锋在它消失之前行进得更远。此外，当次级锋到达时，会触发日珥的横向振荡。我们认为这两个组成部分具有不同的性质。主锋属于非波型日冕物质抛射（CME）分量，可以用场线拉伸模型合理解释。这种多温度行为可能是由于CME锋面环的非线性绝热压缩所引起的相当大的加热所造成的。对于次级锋，它很可能是一个线性快模磁流体（MHD）波，通过典型的日冕温度的介质传播。X射线和无线电数据为我们提供了支持上述情况的补充证据。
英文摘要：
We report quadrature observations of an extreme-ultraviolet (EUV) wave event on 2011 January 27 obtained by the Extreme Ultraviolet Imager (EUVI) onboard \emph{Solar Terrestrial Relations Observatory} (\emph{STEREO}), and the Atmospheric Imaging Assembly (AIA) onboard the \emph{Solar Dynamics Observatory} (\emph{SDO}). Two components are revealed in the EUV wave event. A primary front is launched with an initial speed of $\sim$440 km s$^{-1}$. It appears significant emission enhancement in the hotter channel but deep emission reduction in the cooler channel. When the primary front encounters a large coronal loop system and slows down, a secondary much fainter front emanates from the primary front with a relatively higher starting speed of $\sim$550 km s$^{-1}$. Afterwards the two fronts propagate independently with increasing separation. The primary front finally stops at a magnetic separatrix, while the secondary front travels farther before it fades out. In addition, upon the arrival of the secondary front, transverse oscillations of a prominence are triggered. We suggest that the two components are of different natures. The primary front belongs to a non-wave coronal mass ejection (CME) component, which can be reasonably explained with the field-line stretching model. The multi-temperature behavior may be caused by considerable heating due to the nonlinear adiabatic compression on the CME frontal loop. For the secondary front, most probably it is a linear fast-mode magnetohydrodynamic (MHD) wave that propagates through a medium of the typical coronal temperature. X-ray and radio data provide us with complementary evidence in support of the above scenario.
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