HD 203608，旧星系盘中一个安静的星震目标
HD 203608, a quiet asteroseismic target in the old galactic disk
摘要：
在欧洲南方天文台3.6米望远镜上用光谱仪Harps进行了一次短期观测，以便继续探索F型星的小行星地震特性。事实上，多普勒观测的F型的主序列是苛刻的，目前仍然局限于一个单一的情况下（HD 49933）。将有可能通过一套增强的观测结果与CoRoT飞行任务在类似恒星上获得的光度测量结果进行比较。我们选择了4等F8V恒星HD 203608，以研究旧银盘中低金属丰度恒星的振荡性质。2006年8月与Harps进行了为期5晚的小行星地震观测方案。用仪器提供的在线数据处理软件对光谱进行处理。本文提出了一种新的统计方法来提取傅立叶域中的显著峰。振荡频谱在频率范围[1.5，3.0 mHz]内显示出显著的过剩功率。它在2.5 mHz时具有约120.4 $μ$ Hz的大间距。大间距随频率的变化被清楚地确定，这需要一个适应的渐近发展。模式识别基于15种模式的明确签名，其中$\ell = 0$和1。这一观测显示了对星震制约的潜在诊断。在恒星模型中包括它们显著提高了\cible物理参数的精度，从而在HR图中获得更精确的位置。恒星的年龄现在被确定在$7.25\pm0.07$ Gyr范围内。
英文摘要：
A short observing run with the spectrometer Harps at the ESO 3.6-m telescope was conducted in order to continue exploring the asteroseismic properties of F type stars. In fact, Doppler observations of F type on the main sequence are demanding and remain currently limited to a single case (HD 49933). Comparison with photometric results obtained with the CoRoT mission on similar stars will be possible with an enhanced set of observations. We selected the 4th magnitude F8V star HD 203608, in order to investigate the oscillating properties of a low-metallicity star of the old galactic disk. A 5-night asteroseismic observation program has been conducted in August 2006 with Harps. Spectra were reduced with the on-line data reduction software provided by the instrument. A new statistical approach has been developed for extracting the significant peaks in the Fourier domain. The oscillation spectrum shows a significant excess power in the frequency range [1.5, 3.0 mHz]. It exhibits a large spacing about 120.4 $μ$Hz at 2.5 mHz. Variations of the large spacing with frequency are clearly identified, which require an adapted asymptotic development. The modes identification is based on the unambiguous signature of 15 modes with $\ell = 0$ and 1. This observation shows the potential diagnostic of asteroseismic constraints. Including them in the stellar modeling enhances significantly the precision on the physical parameters of \cible, resulting in a much more precise position in the HR diagram. The age of the star is now determined in the range $7.25\pm0.07$ Gyr.
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