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arXiv 1202.1379astro-ph.SR
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roAp星振荡的单表面近似以外的线轮廓变化的数值模拟

Numerical simulations of line-profile variation beyond a single-surface approximation for oscillations in roAp stars

Takashi Nomura, Jun Naito, Hiromoto Shibahashi

备注：
PASJ, 64, 9 (2012), in press. 18 pages, 16 figures
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摘要：

在过去的十年中，大多数对roAp星的观测都关注光的变化。最近，一些新的，惊人的光谱观测结果，具有高时间分辨率，高光谱色散，高信噪比成为可用。由于在roAp星中发现的振荡是高泛音的，振荡的垂直波长是如此之短，以至于每条光谱线的振幅和相位的变化高度依赖于线轮廓的水平。因此，对roAp星光谱线变化的分析可能为我们提供有关这些恒星大气垂直结构的新信息。为了提取这样的信息，超过一个单一的表面近似的线轮廓变化的数值模拟是必要的。我们进行了数值模拟的线轮廓的变化，考虑到有限的线形成层的厚度。我们证明了这种治疗是多么有效，通过比较模拟与观察到的线轮廓。

英文摘要：

Prior to the last decade, most observations of roAp stars have concerned the light variations. Recently some new, striking results of spectroscopic observations with high time resolution, high spectral dispersion, and a high signal-to-noise ratio became available. Since the oscillations found in roAp stars are high overtones, the vertical wavelengths of the oscillations are so short that the amplitude and phase of the variation of each spectroscopic line are highly dependent on the level of the line profile. Hence, analyses of the variation of the spectroscopic lines of roAp stars potentially provide us with new information about the vertical structure of the atmosphere of these stars. In order to extract such information, a numerical simulation of the line-profile variation beyond a single-surface approximation is necessary. We carried out a numerical simulation of line-profile variation by taking account of the finite thickness of the line forming layer. We demonstrated how effective this treatment is, by comparing the simulation with the observed line profiles.

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