Structure and Dynamics of the Quiet Chromosphere

这项调查将解决这样一个问题：顶部安静的太阳色球是永远热(7000K)，温度变化小(5%)，还是主要冷(2000K)，温度漂移大(高达25000K)？目前的两种经验模型，一种是一组与时间无关的稳态发射模型，另一种是对非磁性色球动力学的随时间变化的模拟，得出了截然不同的结论。为了解决这个问题，将采取双管齐下的办法。一方面，将对空间观测进行分析，以确定实际太阳色球中的温度和振荡幅度，另一方面，将开发数值和分析工具，从理论上评估磁流体动力波对色球的加热。

This investigation will address the question: Is the quiet solar chromosphere at the top always hot (7000 K), with small temperature variations (5%), or mainly cold (2000 K), with large temperature excursions (up to 25,000 K)? Two kinds of current empirical models, one a set of time-independent models of the steady emission, the other, a time-dependent simulation of the dynamics of the non-magnetic chromosphere, come to fundamentally different conclusions. To gain a resolution of this problem a two-pronged approach will be employed. On the one hand, space observations are to be analyzed to determine the temperature and the amplitude of oscillations in the actual solar chromosphere, and on the other, numerical and analytic tools will be developed for a theoretical assessment of chromospheric heating by magnetohydrodynamic waves.