Inhomogeneous Stellar Atmospheres

我们对太阳色球层的大部分了解都是基于 起源于热等离子体的光谱特征。 但 色球层非常不均匀， 凉爽的地区。 我们将观察CO的红外波段来研究 太阳和其他恒星中较冷的气体。 数值模拟 将被构造来理解这些观察， 对热等离子体的观测 这项工作将阐明 太阳的热源这个难以捉摸的问题 色球层

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.