论文标题
harps-n的差距程序在TNG上。 xxxv。过渡系外行星宿主星的基本特性
The GAPS Programme with HARPS-N at TNG. XXXV. Fundamental properties of transiting exoplanet host stars
论文作者
论文摘要
系外观特性取决于恒星特性：要准确地了解行星，有必要尽可能准确，精确地了解恒星。我们的直接目的是以均匀且准确的方式表征27个在Gaps程序中观察到的27个过境行星托管恒星的样本。我们确定了恒星参数（有效温度，表面重力，旋转速度）和26个元素的丰度（li，c，c，n，o，na，mg，al，si，s，s，ca，ca，ca，sc，ti，ti，cr，cr，cr，cr，cr，cr，mn，mn，mn，mn，co，ni，ni，ni，ni，zn，y，y，y，zr，zr，ba，ba，la，la，nd，nd，eu）。我们的研究基于高分辨率HARPS-N@TNG和FEROS@ESO光谱和统一技术。我们从GAIA数据中得出运动特性，并以元素比为化学时钟在系外行星宿主星年时代估计。我们的恒星的TEFF为4400-6700 K，而[Fe/H]在-0.3和0.4 dex内。锂存在于7颗星中。 [x/h]和[x/fe]丰度与[fe/h]与银河化学演化一致。 [X/Fe]与凝结温度的依赖性相对于恒星和运动学特性进行了严格的分析。所有具有测量C和O丰度的目标均显示C/O <0.8，与岩石形成矿物中存在的Si兼容。大多数靶标显示1.0 <mg/si <1.5，与橄榄石和辉石之间分布的Mg兼容。 HAT-P-26是拥有最低质量行星的目标，显示最高的Mg/Si比。从我们的化学分析分析中，我们发现了银河系磁盘中年龄与位置之间的一致性。我们注意到，更高密度行星是在金属富含恒星附近的趋势，并暗示了某些挥发物的较高巨大的巨大质量，对于较低的质量行星。我们不能排除我们的部分结果也可能与银河磁盘中恒星的位置有关。我们从与宿主星的化学成分相关的行星的组成中追踪行星迁移方案
Exoplanetary properties depend on stellar properties: to know the planet with accuracy and precision it is necessary to know the star as accurately and precisely as possible. Our immediate aim is to characterize in a homogeneous and accurate way a sample of 27 transiting planet-hosting stars observed within the GAPS program. We determined stellar parameters (effective temperature, surface gravity, rotational velocity) and abundances of 26 elements (Li,C,N,O,Na,Mg,Al,Si,S,Ca,Sc,Ti,V,Cr,Fe,Mn,Co,Ni,Cu,Zn,Y,Zr,Ba,La,Nd,Eu). Our study is based on high-resolution HARPS-N@TNG and FEROS@ESO spectra and uniform techniques. We derived kinematic properties from Gaia data and estimated for the first time in exoplanet host stars ages using elemental ratios as chemical clocks. Teff of our stars is of 4400-6700 K, while [Fe/H] is within -0.3 and 0.4 dex. Lithium is present in 7 stars. [X/H] and [X/Fe] abundances vs [Fe/H] are consistent with the Galactic Chemical Evolution. The dependence of [X/Fe] with the condensation temperature is critically analyzed with respect to stellar and kinematic properties. All targets with measured C and O abundances show C/O<0.8, compatible with Si present in rock-forming minerals. Most of targets show 1.0<Mg/Si<1.5, compatible with Mg distributed between olivine and pyroxene. HAT-P-26, the target hosting the lowest-mass planet, shows the highest Mg/Si ratio. From our chemo-dinamical analysis we find agreement between ages and position within the Galactic disk. We note a tendency for higher density planets to be around metal-rich stars and hints of higher stellar abundances of some volatiles for lower mass planets. We cannot exclude that part of our results could be also related to the location of the stars within the Galactic disk. We trace the planetary migration scenario from the composition of the planets related to the chemical composition of the hosting stars
