太阳大气

多层太阳大气模式中Alfvén波的传播

Propagation of Alfven waves in multi-layer solar atmosphere model

太阳大气中磁重联的MHD数值模拟

MHD Numerical Simulations of Magnetic Reconnection in Solar Atmosphere

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。

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

粗略的估算表明宁静太阳大气温度极小区的温度在一个太阳周的变幅为30K～50K。

Rough estimation yields a temperature variation of about 30 ~ 50 K of TMR in the quiet sun atmosphere .

本文用多方过程方程式封闭一维带引力场的流体力学方程组，用不同的γ值计算了不同类型的扰动在HSRA太阳大气模型中向上传播和演化。

We computed the upward propagation and evolution of different kinds of perturbations in the solar atmosphere , using HSRA as the unperturbed model . The dynamical equation used is an one dimensional compressible flow equation under gravitational acceleration at the solar surface .

太阳大气中双拱结构的平衡与非平衡

Equilibrium and nonequilibrium of two-arch structures in the solar atmosphere

在重力分层的太阳大气中磁流浮现的数值解

Numerical Solution of Magnetic Flux Emergence in Gravity - Stratified Solar Atmosphere

Ⅲ型爆发及其在太阳大气行星际等离子体中的传播

Type Iff Burst and Its Propagation in Solar Atmospheric and Interplanetary Plasma

太阳大气磁精细结构的射电探讨

The Radio Approach of Magnetic Fine Structures in Solar Atmosphere

太阳大气中矢量磁场信息的推导

A derivation of the information of vector magnetic fields in solar atmosphere

太阳大气中磁场的扭转储能

On the energy storage in the solar atmosphere by twisting magnetic field

太阳大气中自发重联的数值模拟（Ⅰ）

Numerical simulation for magnetic spontaneous reconnection in solar atmosphere (ⅰ)

太阳大气中环状结构的形状

The Configuration of the Loop-like Structure of Solar Atmosphere

我国近年来太阳大气和行星际动力学研究的进展

Recent progress of research on dynamics of solar atmosphere and interplanetary medium in China

太阳大气中非线性波的数字计算

Numerical computations of non-linear waves in solar atmosphere

太阳大气动力学的数值研究

Numerical studies of the solar atmospheric dynamics

太阳大气铍丰度的衰减

Beryllium Depletion in the Solar Atmosphere

太阳大气锂丰度的衰减

Lithium Depletion in the Solar Atmospere

太阳大气和太阳活动

Solar atmosphere and solar activities

太阳大气中自发磁重联的数值模拟（Ⅱ）重力、热传导下二维三分量的计算结果

Numerical simulation of spontaneous magnetic reconnection in solar atmosphere (ⅱ) 2.5d results with gravity and heat conduction

传统上，光谱观测是太阳大气物理参数诊断的主要方法。

Traditionally the primary means to measure the parameters of the solar atmosphere is via spectroscopic observations .

我们利用这个微弱的特性，来测量太阳大气中的黄金成份。

And we use this weak feature to measure the composition of gold in the atmosphere of the sun .

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。

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

这些谱线分别在色球层、光球最深层和光球上层形成，因此用它们可以探测太阳大气中很大范围的磁场。

Therefore , they can be used to probe the magnetic fields in a large range of height in the solar atmosphere .

有关特解的具体形式及对太阳大气的应用将在本系列的下几篇论文中另作讨论。

The concrete forms of the solutions and their application to the solar atmosphere is relegated to the subsequent papers of this series .

其余部分则以声波即机械振动的形式散逸，它们加热了太阳大气的中间一层，即色球层。

The rest escapes as sound waves , mechanical vibrations that heat the chromosphere , the middle layer of the sun 's atmosphere .

从1974年起，基特峰天文台几乎每月定期对太阳大气的K线及其他一些谱线进行观测记录。

Calcium K line as well as some other solar spectral lines have been measured regularly nearly every month since 1974 at Kitt Peak .

无论在光球与它上面的太阳大气之间，或是在光球层与它下面的太阳本体之间，都没有明显的突变。

There is no sharp break between the photosphere and the outer atmosphere of the sun on one side and the solar interior on the other .

如果飞机释放的距离近到能够感受到太阳大气的话，它会在1秒之内灰飞烟灭。

If the plane were released close enough to the Sun to feel its atmosphere at all , it would be vaporized in less than a second .

想了解磁力线重连事件中究竟发生了些什麽事情，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。

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 .