Inhomogeneous Stellar Atmospheres

我们对太阳色球的大部分知识都是基于起源于热等离子体的光谱特征。然而，色球非常不均匀，也包含相对较冷的区域。来自CO的红外波段将被观察，以研究太阳和其他恒星中这种较冷的气体。将构建数值模拟，以便结合热等离子体的观测来理解这些观测。这项工作将阐明太阳色球的热源这一难以捉摸的问题。

Most of our knowledge of the chromosphere of the sun is based on spectral features which originate in hot plasmas. However, the chromosphere is very inhomogeneous and also contains relatively cool regions. The infrared bands from CO will be observed to study this cooler gas in the sun and other stars. Numerical simulations will be constructed to understand these observations in conjunction with observations of the hot plasma. This work will shed light on the elusive question of the source of heating of the solar chromosphere.