论文标题
R-Process Alliance：几乎完整的R-Process丰度模板，该模板源自R的紫外线光谱法，R-Process-heanced Metal-Poor Star HD 222925
The R-Process Alliance: A Nearly Complete R-Process Abundance Template Derived from Ultraviolet Spectroscopy of the R-Process-Enhanced Metal-Poor Star HD 222925
论文作者
论文摘要
我们提出了金属贫困（[Fe/H] = -1.46 +/- 0.10）的几乎完全快速的中子捕获过程（R-Process）化学清单r-process-enhanced（[EU/Fe] = +1.32 +/- 0.08）HALO HALO HALO HD 222925。此次数超过任何对象。它包括31 <= z <= 90的42个元素，包括在R-Process增强的恒星中很少检测到的元素，例如Ga，ge，se，se，cd，in，sn，sn，sn，sb，sb，sb，sb，te，w，re，re，os，os，ir，ir，pt和au。我们从对哈勃太空望远镜上的空间望远镜成像仪收集的紫外光谱中的404个吸收线的分析中得出了这些丰度，并以前分析了光谱。一系列附录讨论了这些行的原子数据和拟合的质量。从BA到PB的R过程元素（包括第三R-Process峰的所有元素）与太阳能R-Process残差表现出显着的一致性，其标准偏差仅为0.08 DEX（17％）。相比之下，从GA到TE的较轻元素之间的偏差范围近1.4个DEX，它们显示出从GA到SE，NB到CD的不同趋势，以及通过TE到TE。 R-Process对GA，GE以及小的贡献，SE是最轻的元素，其生产由R-Process主导。灯笼分数（X_LA）= -1.39 +/- 0.09，对于R-Process-Enhanced恒星来说是典型的，并且比GW170817 Neutron-Star-Star合并事件的Kilonova高。我们主张采用这种模式作为太阳R-Process-元素残差的替代方法，当时与观测值面对重型元素核合成的未来理论模型。
We present a nearly complete rapid neutron-capture process (r-process) chemical inventory of the metal-poor ([Fe/H] = -1.46 +/- 0.10) r-process-enhanced ([Eu/Fe] = +1.32 +/- 0.08) halo star HD 222925. This abundance set is the most complete for any object beyond the solar system, totaling 63 metals detected and 7 with upper limits. It comprises 42 elements from 31 <= Z <= 90, including elements rarely detected in r-process-enhanced stars, such as Ga, Ge, As, Se, Cd, In, Sn, Sb, Te, W, Re, Os, Ir, Pt, and Au. We derive these abundances from an analysis of 404 absorption lines in ultraviolet spectra collected using the Space Telescope Imaging Spectrograph on the Hubble Space Telescope and previously analyzed optical spectra. A series of appendices discusses the atomic data and quality of fits for these lines. The r-process elements from Ba to Pb, including all elements at the third r-process peak, exhibit remarkable agreement with the Solar r-process residuals, with a standard deviation of the differences of only 0.08 dex (17%). In contrast, deviations among the lighter elements from Ga to Te span nearly 1.4 dex, and they show distinct trends from Ga to Se, Nb through Cd, and In through Te. The r-process contribution to Ga, Ge, and As is small, and Se is the lightest element whose production is dominated by the r-process. The lanthanide fraction, log(X_La) = -1.39 +/- 0.09, is typical for r-process-enhanced stars and higher than that of the kilonova from the GW170817 neutron-star merger event. We advocate adopting this pattern as an alternative to the Solar r-process-element residuals when confronting future theoretical models of heavy-element nucleosynthesis with observations.
