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1·Why is the solar atmosphere hotter than the solar surface?

为什么是太阳大气比太阳表面更热？

2·Corona: the outer solar atmosphere, can be extended to a number of solar diameter, or even farther.

日冕：太阳大气的最外层，可以延伸到几个太阳直径，甚至更远。

3·The solar atmosphere above that consists of the photosphere, chromosphere, a transition region and the corona.

太阳大气则由光球层、色球层、过渡区和日冕组成。

4·Even in the umbra of sunspots, the strongest region in the solar atmosphere, the magnetic field strength is only about 2000 Gauss.

即使在磁场最强的黑子本影区，磁场强度通常也只有2000高斯左右。

5·The first section describes the spectral features of the dynamical processes in the solar atmosphere and the principles of their diagnostics.

第一节叙述太阳大气动力学过程的光谱特征及其诊断原理。

6·In a mission to learn more about the sun's inner workings, NASA is planning to launch a specially shielded spacecraft in 2018 that will plunge into the solar atmosphere.

为了一探太阳内部工作情况，NASA计划在2018年发射一个带有特殊防护的航空器，它将进入太阳的大气层。

7·Following what exactly happens during a reconnection event requires, first off, a general understanding of how invisible magnetic loops can trap hot gas in the solar atmosphere.

想了解磁力线重连事件中究竟发生了些什么事情，必须先对看不见的磁力环圈如何捕捉太阳大气里的热气有一些基本认识。

8·The ideal Magnetohydrodynamic equations (MHD), the governing equations of the solar atmosphere dynamical process, are taken to numerically simulate Coronal Mass Ejection (CME) phenomena.

采用理想磁流体力学方程组(MHD)作为太阳大气动力学过程的控制方程组，定性数值模拟日冕物质抛射(CME)现象。

9·Through the observational data which was transmitted back to the ground by space telescopes, we have seen many kinds of the three-dimensional structure of the active phenomena in solar atmosphere.

通过空间卫星传回的数据资料，我们可以看到太阳活动丰富多彩的三维结构。

10·Other planets in our solar system lack the oxygen atmosphere that helps explain why life exists on Earth.

我们太阳系的其他行星缺乏氧气大气层，这有助于解释为什么地球上存在生命。