HD 65949：罗塞塔石碑或红鲱鱼
HD 65949: Rosetta Stone or Red Herring
摘要：
HD 65949是一颗B星晚期的恒星，在3984[A]处有异常强烈的Hg II，但它不是一颗典型的HgMn星。Re II光谱具有非凡的强度。基于Teff = 13100K和log（g）= 4.0的模型，在此推导出58个元素的丰度或上限。偶Z元素到镍显示出与太阳丰度的微小偏差。奇Z元素通过铜的异常大多很小。在铁峰之外，发现了一个巨大的散射，最重元素的丰度模式类似于太阳物质的N=126 r过程峰，尽管细节上不太清楚。对于Z > 30的元素，我们发现丰度过剩与二次电离势有显著的相关性。这表明光球层或近光球层过程的相关性。我们探讨了一个模型与质量吸积的外来物质，其次是更普遍接受的分化扩散。该模型导致了一些对未来工作提出挑战的预测。可能的第一和第二质量接近3.3和1.6 M（太阳），间隔约为1.5 m。0.25古猿阿新的原子结构计算在两个附录中给出。
英文摘要：
HD 65949 is a late B star with exceptionally strong Hg II at 3984[A], but it is not a typical HgMn star. The Re II spectrum is of extraordinary strength. Abundances, or upper limits are derived here for 58 elements based on a model with Teff = 13100K, and log(g) = 4.0. Even-Z elements through nickel show minor deviations from solar abundances. Anomalies among the odd-Z elements through copper are mostly small. Beyond the iron peak, a huge scatter is found. The abundance pattern of the heaviest elements resembles the N=126 r-process peak of solar material, though not in detail. We find a significant correlation of the abundance excesses with second ionization potentials for elements with Z > 30. This indicates the relevance of photospheric or near-photospheric processes. We explore a model with mass accretion of exotic material followed by the more commonly accepted differentiation by diffusion. That model leads to a number of predictions which challenge future work. Likely primary and secondary masses are near 3.3 and 1.6 M(solar), with a separation of ca. 0.25 AU. New atomic structure calculations are presented in two appendices.
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