系外行星光谱在任意取向系统中的旋转致宽：应用于反射光
Rotational broadening of exoplanet spectra in arbitrarily oriented systems: Application to reflected light
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中文总结 AI 辅助
本研究推导了任意对齐系外行星系统的旋转致宽核，用于高分辨率反射光谱分析，发现非对齐系统与顺行对齐轨道的致宽差异可达50 km/s，并可用于测量轨道对齐。
中文摘要 AI 辅助
系外行星的反射光谱包含丰富的信息，我们如今正开始获取这些信息。在高光谱分辨率下，恒星和行星的旋转都会影响反射光谱线的形状。在高分辨率分析中必须考虑这一效应，并且该效应可用于测量系统的轨道对齐程度。在本工作中，我们推导了任意对齐系统中的旋转致宽核，既包括行星所观测到的恒星光谱的致宽核，也包括行星光谱中反射分量的致宽核。随后，我们确定了这些核的参数与系外行星系统标准轨道参数之间的关系。最后，我们展示了这些核的示例，将其与先前的模型进行比较，并探讨了我们的假设所带来的局限性。我们发现，非对齐系统的旋转致宽与顺行对齐轨道所预期的致宽之间的差异可达约50 km/s。我们还强调了本工作中提出的方程和核如何被修改以用于其他用途，例如热发射光谱。
英文摘要
Exoplanet reflection spectra contain a wealth of information, which we are now beginning to access. At a high spectral resolution, the rotation of both the star and the planet affects the shape of the reflected spectral lines. This effect must be accounted for in high-resolution analyses and could be used to measure the orbital alignment of systems. In this work, we derive the rotational broadening kernels for arbitrarily aligned systems, both for the stellar spectrum viewed by the planet and for the reflected component of the planet's spectrum. We then determine the relation between the parameters of the kernels and the standard orbital parameters of an exoplanet system. Finally, we show examples of these kernels, compare them with previous models, and investigate the limitations imposed by our assumptions. We find that the difference in the rotational broadening of a non-aligned system relative to the broadening expected from a prograde aligned orbit can be of the order of 50 km s$^{-1}$. We also highlight how the equations and kernels presented in this work could be modified for other uses, such as thermal emission spectra.
发表机构
- Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）
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