基于PHOEBE和FASTWIND的大质量恒星光谱补丁模型
Spectroscopic patch model for massive stars using PHOEBE II and FASTWIND
摘要：
大质量恒星在星系的机械和化学演化中起着重要的作用。了解这些恒星的内部过程对于我们了解它们的演化和最终的最终产品至关重要。球面几何的变形在大质量恒星中很常见;然而，目前可用于研究这些系统的工具几乎都是一维的。我们提出了一种新的光谱分析工具，适合于偏离球对称的大质量恒星。该代码（名为SPAMMS）是一个光谱补丁模型，它考虑到系统的三维表面几何形状，以产生在给定的相位和方向的光谱剖面。在使用威尔逊Devinney的代码PHOEBE结合非局部热力学平衡（NLTE）辐射转移代码FASTWIND，我们创建了一个三维网格，代表我们的系统的表面几何形状，我们分配FASTWIND出射强度线轮廓到每个网格三角形，考虑到当地的参数，如温度，表面重力，和半径。然后，这些线轮廓在可见表面上积分，其中考虑到它们的通量贡献和径向速度，从而返回给定相位处的系统的可见表面的最终线轮廓。我们证明，SPAMMS可以准确地再现所观察到的过接触系统的谱线轮廓的形态。此外，我们展示了如何快速旋转的单星的线轮廓不同时，考虑到旋转失真，以及这些可以对所确定的参数的影响。最后，我们证明了代码的能力，再现罗斯特-麦克劳克林和斯特鲁夫-萨哈德效果。
英文摘要：
Massive stars play an important role in the mechanical and chemical evolution of galaxies. Understanding the internal processes of these stars is vital to our understanding of their evolution and eventual end products. Deformations from spherical geometry are common for massive stars; however, the tools that are currently available for the study of these systems are almost exclusively one-dimensional. We present a new spectroscopic analysis tool tailored for massive stars that deviate from spherical symmetry. This code (entitled SPAMMS) is a spectroscopic patch model that takes the three-dimensional surface geometry of the system into account to produce spectral profiles at given phases and orientations. In using the Wilson-Devinney-like code PHOEBE in combination with the non local thermodynamic equilibrium (NLTE) radiative transfer code FASTWIND, we created a three-dimensional mesh that represents the surface geometry of our system and we assigned FASTWIND emergent intensity line profiles to each mesh triangle, which take the local parameters such as temperature, surface gravity, and radius into account. These line profiles were then integrated across the visible surface, where their flux contribution and radial velocity are taken into account, thus returning a final line profile for the visible surface of the system at a given phase. We demonstrate that SPAMMS can accurately reproduce the morphology of observed spectral line profiles for overcontact systems. Additionally, we show how line profiles of rapidly-rotating single stars differ when taking rotational distortion into account, and the effects that these can have on the determined parameters. Finally, we demonstrate the code's ability to reproduce the Rossiter-Mclaughlin and Struve-Sahade effects.
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