Energetics and diagnostics of hot star disks

许多类型的大质量恒星旋转速度很快，往往与恒星周围的气体物质有关；有时还存在尘埃和分子。通常，这种物质可以在我们从恒星观察到的光中被探测到。通常，这种物质具有盘状分布，但形成和维持这些盘状分布的过程还不是很清楚。因此，我的研究将主要集中在两种特定类型的热星，Be星和B[e]星，它们与盘状分布的物质有关。这些恒星代表着我们严重缺乏知识的重要恒星群。与太阳相比，这些恒星每秒以光的形式向周围释放大约100到100万倍的能量，这有助于塑造它们母星系的演化。由于大质量恒星消耗能量的速度如此之快，而且它们的质量只有太阳质量的大约十倍，因此它们的寿命必然很短。当大质量恒星在其作为恒星的生命接近尾声时耗尽其能量供应时，可能会发生爆炸，从而进一步丰富其环境中的能量和化学元素。我的研究重点是构建这些盘状区域的计算机模型。这些模型预测来自这些天体的光线中的细节，然后将这些预测与实际观测进行比较。这种分析使我能够破译这些恒星周围的物理条件，如温度、密度和风速，这样我就可以尝试了解是什么过程形成和维护这些盘状区域，并了解这些恒星在其生命周期中对其环境的影响。

Many types of massive stars rotate rapidly and are often associated with gaseous matter surrounding the star; sometimes dust and molecules are also present.  This material can be detected in the light we observe from the star. Often, this material has a disk-like distribution, but the processes which form and maintain these disks are not well understood.    My research will concentrate primarily on two particular types of hot stars, the Be stars and the B[e] stars, which are associated with disk-like distributions of material.  These stars represent an important group of stars for which our knowledge is severely lacking.  Compared to the Sun, these stars emit approximately a hundred to a million times more energy each second to their surroundings in the form of light which helps to shape the evolution of their parent galaxy. Since massive stars spend their supply of energy at such a large rate, and since their masses are only approximately ten times the mass of the Sun, they necessarily have short lifetimes. When massive stars have exhausted their energy supply near the end of their lifetime as a star, explosions can occur which further enrich their environments with both energy and chemical elements. My research focuses on constructing computer models of these disk-like regions.  The models predict details in the light that come from these objects, and then these predictions are compared with actual observations.  This analysis allows me to decipher the physical conditions surrounding these stars, such as temperature, density, and wind speed, so that I can try to understand what processes form and maintain these disks-like regions, and to understand the effects these stars have on their environments during their lifetimes.