arXiv 1602.080082016-02astro-ph.SR

太阳双星HIP 100963的高精度分析

High precision analysis of the solar twin HIP 100963

Jhon Yana Galarza, Jorge Meléndez, Ivan Ramírez, Amanda I. Karakas, Martin Asplund, Fan Liu

发表信息：: A&A 589, A17 (2016)
DOI：: 10.1051/0004-6361/201527912

摘要：

方法.我们使用凯克一号望远镜上的HIRES摄谱仪获取HIP 100963和太阳的高分辨率（R $\approx$ 70000）光谱，该光谱具有高信噪比（S/N $\approx$ 400 - 650/像素），用于差异丰度分析。我们利用微分光谱平衡测量了铁谱线的等效宽度，从而确定了恒星参数。我们通过相对于太阳的差异丰度分析确定了挥发性、难熔性和中子俘获元素的组成。结果我们发现的恒星参数是$T_{\rm{eff}}=5818 \pm 4$ K、log $g = 4.49 \pm 0.01$ dex、$v_{t} = 1.03 \pm 0.01 $ $\rm{km\ {s}}^{-1}$和[Fe/H] $ = -\ 0.003 \pm 0.004$ dex。这些低误差允许我们计算精确的质量（$1.03^{+0.02}_{-0.01}$ M $_{\odot}$）和年龄（2.0 $\pm$ 0.4 Gyr），使用Yonsei-Yale等时线获得。利用我们的[Y/Mg]比值，我们确定了$2.1 \pm 0.4$ Gyr的年龄，与用等时线计算的年龄一致。我们的等时线年龄也同意从恒星活动确定的年龄（2.4 $\pm$ 0.3 Gyr）。我们研究的丰度模式与冷凝温度（$\rm{T_{cond}}$）考虑到GCE的校正。我们表明，中子捕获元素的增强解释的贡献从$s$ -和$r$ -过程。锂的丰度与其他太阳双胞胎中的锂年龄密切相关。结论.我们确认HIP 100963是一个太阳双星，并证明其丰度模式是关于太阳的GCE校正后。这颗恒星还显示出$s-$和$r$过程元素的富集，以及恒星演化导致的锂的耗尽。

英文摘要：

Methods. We used the HIRES spectrograph on the Keck I telescope to acquire high-resolution (R $\approx$ 70000) spectra with a high signal-to-noise ratio (S/N $\approx$ 400 - 650 per pixel) of HIP 100963 and the Sun for a differential abundance analysis. We measured the equivalent widths (EWs) of iron lines to determine the stellar parameters by employing the differential spectroscopic equilibrium. We determined the composition of volatile, refractory, and neutron-capture elements through a differential abundance analysis with respect to the Sun. Results. The stellar parameters we found are $T_{\rm{eff}}=5818 \pm 4$ K, log $g = 4.49 \pm 0.01$ dex, $v_{t} = 1.03 \pm 0.01 $ $\rm{km\ {s}}^{-1}$ , and [Fe/H] $ = -\ 0.003 \pm 0.004$ dex. These low errors allow us to compute a precise mass ($1.03^{+0.02}_{-0.01}$ M$_{\odot}$) and age (2.0 $\pm$ 0.4 Gyr), obtained using Yonsei-Yale isochrones. Using our [Y/Mg] ratio, we have determined an age of $2.1 \pm 0.4$ Gyr, in agreement with the age computed using isochrones. Our isochronal age also agrees with the age determined from stellar activity (2.4 $\pm$ 0.3 Gyr). We study the abundance pattern with condensation temperature ($\rm{T_{cond}}$) taking corrections by the GCE into account. We show that the enhancements of neutron-capture elements are explained by contributions from both the $s$- and $r$-process. The lithium abundance follows the tight Li-age correlation seen in other solar twins. Conclusions. We confirm that HIP 100963 is a solar twin and demonstrate that its abundance pattern is about solar after corrections for GCE. The star also shows enrichment in $s-$ and $r$-process elements, as well as depletion in lithium that is caused by stellar evolution.

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