Spectroscopic study of the outer atmosphere of the exoplanet HD 189733 b

在论文的框架内，我建议使用高分辨率光谱研究热木星行星HD 189733 b的大气。已知的太阳系外行星系统的数量不断增加，揭示了各种各样的行星，它们具有不同的质量、密度、轨道结构，因此很可能也有高度不同的大气层。类木行星的轨道离它们的主星——热木星——很近，这是令人惊讶的发现之一。这个应用程序旨在探测和分析热木星行星HD 189733 b的大气，这颗行星因其明亮而活跃的主恒星而从大约一千颗已知的系外行星中脱颖而出。计划的研究基于我在2013年7月1日使用UVES光谱仪获得的一组约250个高分辨率光谱。此外，ESO-和keck -存档的两组数据是可用的，但尚未对大气吸收进行分析。数据缩减后，通过分析Ca II H和K以及H- α线来探测行星大气。此外，我们的数据所涵盖的耀斑将被分析，特别是关于大气质量损失的分析。尽管对HD 189733 b大气的探测已经发表，但大气吸收的强度仍然存在争议。由于在耀斑期间可能会释放出大部分相关的高能辐射，因此可能会有一个暂时可变的大气。因此，为了更好地了解HD 189733 b的大气和质量损失，进一步测量大气吸收是必不可少的。我们的数据具有极高的光度稳定性，可以在分析中包括凌日的颜色依赖性。这为研究活动主恒星的中心到边缘的变化提供了可能，也为研究行星大气的吸收提供了另一种方法。随着已知行星数量的不断增加，待研究的大气也越来越多。

I propose to study the atmosphere of the hot Jovian planet HD 189733 b using high-resolution spectroscopy in the frame of a dissertation. The continuously increasing number of known extrasolar planetary systems reveals an enormous variety of planets with different masses, densities, orbital configurations and, therefore, most likely also highly dissimilar atmospheres. Jovian planets orbiting in close proximity to their host-stars - the hot Jupiters - are among the surprising discoveries.This application aims at the detection and analysis of the atmosphere of the hot Jovian planet HD 189733 b, which stands out from the roughly one thousand known exoplanets for its bright and active host star. The planned study is based on a set of ca. 250 high-resolution spectra, which I obtained on July 1st, 2013 using the UVES spectrograph. Furthermore, two data sets from the ESO- and KECK-archive are available, which have not yet been analyzed with respect to atmospheric absorption.After the data reduction, the planetary atmosphere shall be detected through the analysis of the Ca II H and K and H-alpha lines. Moreover, a flare covered by out data is to be analyzed, in particular with respect to atmospheric mass loss. Although a number of detections of HD 189733 b's atmosphere have been published already, the strength of the atmospheric absorption remains controversial.Because a major fraction of the relevant high-energy emission is potentially released during flares, a temporally variable atmosphere seems likely. Consequently, further measurements of atmospheric absorption are indispensable to better understand the atmosphere and mass loss of HD 189733 b.The extraordinarily high photometric stability of our data allows to include the color dependence of the transit in the analysis. This provides both a possibility to study the center-to-limb variation of the active host-star and another approach to study the planetary atmosphere in absorption.A continuously growing number of known planets ensues an increasing number of atmospheres to be studied.