日冕

Aureola is a diminutive of aurea, ie aurea corona.

Aureola是一个小型的黄花，黄花即日冕。

Besides wrecking havoc, CMEs also produce dazzling displays known as the aurora borealis or australis, the northern and southern lights.

除了破坏严重，日冕物质抛射产生耀眼的显示器也被称为北极光或芦苇，北部和南部的灯。

A "time-dependent relaxation" method is proposed to accurately implement given photospheric footpoint displacements and force-free conditions. The method is applied to analyzing the energy buildup of coronal magnetic fields, and the numerical results confirm the Aly conjecture (the magnetic energy of the force-free field is bounded above by the fully-open field energy), and extends it from fully-open to partially-open force-free fields.

提出计算无力磁场的"时变松弛"方法，能精确实现光球足点位移和无力条件；采用该方法分析日冕磁场的剪切储能，验证了Aly猜想（无力场磁能以全开放场磁能为上限），并将该猜想由全开放无力场推广至部分开放无力场。

The corona we see during an eclipse is an overlap of the continuous,largely polarized, K-corona, the basically unpolarized F-corona, and in the inner corona an overlay of emission lines.

在日蚀期间我们所见到的日冕是连续的重叠，K-corona极化程度很大，F-corona基本上不极化，在日冕内部覆盖一组射线。

Mainly in the corona being, but often associated with chromospheric connected to the lower density than the surrounding corona, large 103-104 times, the temperature of about 70K.

主要存在于日冕之中，但下部常与色球相连，密度比周围的日冕大103—104倍，温度约70K。

In the frame of constructing hydrodynamical model, some basic assumptions and equations were described in detail. Besides, there are three distinguish improvements above the former work: a new formula of chromosphere radiative loss was deduced out, which can roughly reproduce the results calculated by detailed non-LTE theory; a new physical process, i.e.

在构造耀斑动力学模型理论框架中，我们详细交待了基本假设和基本方程组，以及方程中各项的选取情况；针对现有耀斑动力学模型色球研究的不足，文中导得了新的色球辐射损失经验公式，它基本能够再生现有详细非局部热动平衡计算结果，较以前的处理方法有很大程度上的改善；引入了以前在耀斑环研究中从未被考虑过的日冕软x辐射加热色球的能量过程，推得了日冕软x辐射色球沉积的自恰公式。

We now know that the corona we see has three main parts: emission from hot coronal gases, absorption from the solar photospheric spectrum reflected from dust particles in interplanetary space relatively near the Sun, and a continuum from scattering of photospheric light off coronal electrons .

我们现在知道现在所观测到的日冕主要有三个部分：发出的射线来自日冕温度较高的区域，来自太阳光球层光谱的吸收线是源于太阳附近空间的尘埃粒子的反射。

Using magnetohydrodynamic model, this project studies the dynamic structure of the solar wind, the magnetic energy buildup in the corona by photospheric shear, and coronal flux rope catastrophic phenomena.

本项目采用磁流体力学模型，研究太阳风动力学结构、日冕磁场的剪切储能及日冕磁绳的灾变现象。

The answer applies not only to the solar corona but also to the coronas of thousands of other stars that are observed with the Chandra X-ray Observatory and other X-ray telescopes.

这个答案不仅可以应用于解释太阳的日冕而且也可以上千其他被钱德拉X射线望远镜和其他X射线望远镜观测过的恒星表面的日冕。

The low corona can also be monitored to some extent from mountain-top coronagraphs, such as the K-coronameter of the High Altitude Observatory onMauna Loa, Hawaii, but even that instrument occults the lowest corona, and its images are relatively noisy and show little detail.

较小的日冕也能被高海拔检测站检测到，例如夏威夷的高海拔天文台K-coronameter，但对于极低日冕，其图像分辨率较低。

As she looked at Warrington's manly face, and dark, melancholy eyes, she had settled in her mind that he must have been the victim of an unhappy attachment.

每逢看到沃林顿那刚毅的脸，那乌黑、忧郁的眼睛，她便会相信，他一定作过不幸的爱情的受害者。

Maybe they'll disappear into a pothole.

也许他们将在壶穴里消失