太阳邻域太阳型恒星精确和均匀的丰度图：化学年代学分析
Accurate and homogeneous abundance patterns in solar-type stars of the solar neighbourhood: a chemo-chronological analysis
摘要：
本文报道了太阳附近25颗太阳型恒星中C、Na、Mg、Si、Ca、Sc、Ti、V、Cr、Mn、Fe、Co、Ni、Cu、Zn、Sr、Y、Zr、Ba、Ce、Nd和Sm的丰度及其与年龄、运动学和轨道参数的关系。基于高分辨率和高S/N比数据的光谱分析与太阳不同，并应用于原子线EW和C和C2光谱合成。我们进行了一项统计研究，使用树聚类分析，寻找群体的恒星共享相似的丰度模式。我们推导出Teff，log（g），和[Fe/H]的误差为30 K，0.13 dex，和0.05 dex，分别。[X/Fe]的平均误差为0.06 dex。年龄来自理论的HR图和运动学运动组的成员资格。我们确定了四个恒星群：太阳上丰度（<[X/H]> = +0.26 dex），太阳下丰度（<[X/H]> = -0.24 dex）和中间值（<[X/H]> = -0.06和+0.06 dex），但具有不同的化学模式。共享太阳金属量、年龄和银河系轨道的恒星可能有非太阳丰度，这是其出生云化学不均匀性或迁移的影响。[Cu/Fe]与[Ba/Fe]的趋势似乎存在，与文献中先前的权利要求一致，并且[Sm/Fe]与[Ba/Fe]的趋势也可能存在。没有观察到涉及C、Na、Mn和Zn的这种相关性。[Mg[Sc/Fe]、[Sc/Fe]和[Ti/Fe]随年龄增加而增加。[Mn[Cu/Fe]和[Cu/Fe]在太阳年龄之前先向年轻恒星增加，然后减少，我们解释这一结果可能与SN Ia随时间变化的产额和弱s过程有关。[Sr[Y/Fe]、[Y/Fe]、[Sr/Mg]、[Y/Mg]、[Sr/Zn]和[Y/Zn]随年龄的增加而线性增加。[Zr/Fe]、[Ce/Fe]、[Nd/Fe]、[Ba/Mg]、[Ba/Zn]和[Sr，Y，Ba/Sm]增加，但仅限于比太阳年轻的恒星。最陡峭的负年龄关系是由于[Ba/Fe]，但仅适用于比太阳年轻的恒星。
英文摘要：
We report the abundances of C, Na, Mg, Si, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Zn, Sr, Y, Zr, Ba, Ce, Nd, and Sm in 25 solar-type stars in the solar neighbourhood, and their correlations with ages, kinematics, and orbital parameters. The spectroscopic analysis, based high resolution and high S/N ratio data, was differential to the Sun and applied to atomic line EWs and to C and C2 spectral synthesis. We performed a statistical study using a tree clustering analysis, searching for groups of stars sharing similar abundance patterns. We derived Teff, log(g), and [Fe/H] with errors of 30 K, 0.13 dex, and 0.05 dex, respectively. The average error in [X/Fe] is 0.06 dex. Ages were derived from theoretical HR diagrams and memberships in kinematical moving groups. We identified four stellar groups: with over-solar abundances (<[X/H]> = +0.26 dex), under-solar abundances (<[X/H]> = -0.24 dex), and intermediate values (<[X/H]> = -0.06 and +0.06 dex) but with distinct chemical patterns. Stars sharing solar metallicity, age, and Galactic orbit possibly have non-solar abundance, an effect either of chemical heterogeneity in their natal clouds or migration. A trend of [Cu/Fe] with [Ba/Fe] seems to exist, in agreement with previous claims in the literature, and maybe also of [Sm/Fe] with [Ba/Fe]. No such correlation involving C, Na, Mn, and Zn is observed. [Mg/Fe], [Sc/Fe], and [Ti/Fe] increase with age. [Mn/Fe] and [Cu/Fe] first increase towards younger stars up to the solar age, and then decrease, a result we interpret as possibly related to time-varying yields of SN Ia and the weak s-process. [Sr/Fe], [Y/Fe], [Sr/Mg], [Y/Mg], [Sr/Zn], and [Y/Zn] linearly increase towards younger stars. [Zr/Fe], [Ce/Fe], [Nd/Fe], [Ba/Mg], [Ba/Zn], and [Sr,Y,Ba/Sm] increase but only for stars younger than the Sun. The steepest negative age relation is due to [Ba/Fe], but only for stars younger than the Sun.
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