论文标题
北半球明亮恒星的化学成分：星形行星连接
Chemical Composition Of Bright Stars In The Northern Hemisphere: Star-Planet Connection
论文作者
论文摘要
为了实现行星和星际研究任务的目的，例如NASA过境系外行星调查卫星（TESS）太空望远镜的目标，准确的出色大气参数以及详细的化学成分作为输入。 We have observed high-resolution spectra for all 848 bright (V<8 mag) stars that are cooler than F5 spectral class in the area up to 12 deg surrounding the northern TESS continuous viewing zone and uniformly determined the main atmospheric parameters, ages, orbital parameters, velocity components, and precise abundances of up to 24 chemical species (C(C2), N(CN), [O I], Na I, Mg i，al i，si i，si i，ca i，ca ii，ca i，sc i，sc i，ti i，ti i，v i，cr i，cr i，cr i，mn i，fe i，fe i，fe ii，co i，ni i，ni i，cu i，cu i，cu i and zn i）持续740个慢慢旋转的星星。对我们的样本中25个行星托管恒星的分析使我们得出了以下结论：托管高质量行星的矮星比具有低质量行星的星星更富含金属。我们发现略微负C/O和Mg/Si斜向朝着具有高质量行星的恒星。我们的样本中的所有低质量行星均显示出正$δ$ [el/fe]与冷凝温度斜率相比，尤其是具有大量各种行星的恒星。高质量行星宿主具有多样的斜率，但是在更丰富的金属，较旧和凉爽的恒星中，积极的元素丰度斜率更为常见。
In fulfilling the aims of the planetary and asteroseismic research missions, such as that of the NASA Transiting Exoplanet Survey Satellite (TESS) space telescope, accurate stellar atmospheric parameters and a detailed chemical composition are required as input. We have observed high-resolution spectra for all 848 bright (V<8 mag) stars that are cooler than F5 spectral class in the area up to 12 deg surrounding the northern TESS continuous viewing zone and uniformly determined the main atmospheric parameters, ages, orbital parameters, velocity components, and precise abundances of up to 24 chemical species (C(C2), N(CN), [O I], Na I, Mg I, Al I, Si I, Si I, Ca I, Ca II, Sc I, Sc II, Ti I, Ti II, V I, Cr I, Cr II, Mn I, Fe I, Fe II, Co I, Ni I, Cu I, and Zn I) for 740 slowly rotating stars. The analysis of 25 planet-hosting stars in our sample drove us to the following conclusions: the dwarf stars hosting high-mass planets are more metal rich than those with low-mass planets. We find slightly negative C/O and Mg/Si slopes toward the stars with high-mass planets. All the low-mass planet hosts in our sample show positive $Δ$[El/Fe] versus condensation temperature slopes, in particular, the star with the large number of various planets. The high-mass planet hosts have a diversity of slopes, but in more metal rich, older, and cooler stars, the positive elemental abundance slopes are more common.
