Characterizing Kepler asteroseismic targets
Characterizing Kepler asteroseismic targets
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DOI：
10.1111/j.1365-2966.2010.17978.x
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发表时间：
2010-11
影响因子：
4.8
通讯作者：
J. Molenda–Żakowicz;D. Latham;G. Catanzaro;A. Frasca;S. Quinn
中科院分区：
文献类型：
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作者：
J. Molenda–Żakowicz;D. Latham;G. Catanzaro;A. Frasca;S. Quinn
只要有高精度的数据，就可以用星震方法详细研究恒星的结构和演化。我们使用我们的高分辨率（R > 20 000）光谱观测确定了44个开普勒小行星地震目标的有效温度（T eff），表面重力（log g），金属丰度和投影旋转速度（v sin i）;这些参数将用于计算这些恒星的小行星地震模型和解释开普勒光变曲线。我们使用互相关的方法来测量我们的目标的径向速度（RV），而大气参数推导使用ROTFIT码和频谱合成方法。我们发现了三个双线光谱双星，HIP 94924，HIP 95115和HIP 97321 -对于最后一个系统，我们提供了轨道解，我们报告了两个可疑的单线光谱双星，HIP 94112和HIP 96062。对于所有的恒星从我们的样本，我们得出RV，v sin i，Teff，log g和金属丰度，并为六颗恒星，我们进行了详细的丰度分析。对33个目标进行了光谱分类。最后，我们表明，早期型的星星HIP 94472旋转缓慢（v sin i = 13公里s-1），我们确认其分类为上午光谱类型，这使得它成为一个有趣的和有前途的目标，为asteroseismic建模。本文报道的结果与开普勒输入目录（KIC）中的信息的比较表明，迫切需要验证和改进的KIC中列出的大气参数。这种改进对于充分利用开普勒提供的数据至关重要，只有通过详细的地面研究才能实现。
Stellar structure and evolution can be studied in great detail by asteroseismic methods, provided data of high precision are available. We determine the effective temperature (T eff ), surface gravity (log g), metallicity and the projected rotational velocity (v sin i) of 44 Kepler asteroseismic targets using our high-resolution (R > 20 000) spectroscopic observations; these parameters will then be used to compute asteroseismic models of these stars and to interpret the Kepler light curves. We use the method of cross-correlation to measure the radial velocity (RV) of our targets, while atmospheric parameters are derived using the ROTFIT code and spectral synthesis method. We discover three double-lined spectroscopic binaries, HIP 94924, HIP 95115 and HIP 97321 - for the last system, we provide the orbital solution, and we report two suspected single-lined spectroscopic binaries, HIP 94112 and HIP 96062. For all stars from our sample we derive RV, v sin i, T eff , log g and metallicity, and for six stars, we perform a detailed abundance analysis. A spectral classification is done for 33 targets. Finally, we show that the early-type star HIP 94472 is rotating slowly (v sin i = 13 km s -1 ) and we confirm its classification to the Am spectral type which makes it an interesting and promising target for asteroseismic modelling. The comparison of the results reported in this paper with the information in the Kepler Input Catalogue (KIC) shows an urgent need for verification and refinement of the atmospheric parameters listed in the KIC. That refinement is crucial for making a full use of the data delivered by Kepler and can be achieved only by a detailed ground-based study.