Inhomogeneous Stellar Atmospheres

恒星的特征通常是 温度从内部（其中温度通常是 数百万开氏度）到表面（温度 是数千或数万开氏度）。 在阳光下 和其他具有表面的恒星（即，光球）温度 大约6000 K和更少的温度急剧上升， 透明的，最外层由于能量沉积从 磁表面活动 在太阳中， 温度开始上升，传统上被称为 色球层 最近，导致这种情况的过程 温度反转被称为“分子冷却 因为CO和其他分子的辐射冷却 似乎是他干的 主要研究者（PI）建议研究以下地区： 晚型恒星大气中的逆温， 将它们与太阳的太阳进行比较。 观测输入数据 将是这些恒星的空间未分辨光谱，PI 和他的合作者们在过去三年里积累的。 这些数据将由计算机代码处理， 分子非局部热力学平衡（NLTE）问题。

Stars are generally characterized by a decrease in their temperature from the interior (where the temperature is typically millions of degrees Kelvin) to the surface (where the temperature is thousands or tens of thousands of degrees Kelvin). In the sun and other stars with surface (i.e., photospheric) temperatures of roughly 6000 K and less the temperature rises sharply in the transparent, outermost layers due to energy deposited from magnetic surface activities. In the sun, the region in which the temperature starts rising has traditionally been known as the chromosphere. More recently, the processes giving rise to this temperature inversion have been called the "molecular cooling catastrophes" because radiative cooling by CO and other molecules appears to be responsible for it. The Principal Investigator (PI) proposes to study the regions of temperature inversion in the atmospheres of late-type stars and compare them to those of the sun. The observational input data will be spatially-unresolved spectra of these stars, which the PI and his collaborators have accumulated over the past three years. This data will be processed by computer codes capable of solving the molecular non-local thermodynamic equilibrium (NLTE) problem.