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arXiv 0904.3105astro-ph.SRastro-ph.GA
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核合成的终结:早期星系中铅和钍的产生

The End of Nucleosynthesis: Production of Lead and Thorium in the Early Galaxy

Ian U. Roederer, Karl-Ludwig Kratz, Anna Frebel, Norbert Christlieb, Bernd Pfeiffer, John J. Cowan, Christopher Sneden

摘要:

我们研究了27颗贫金属星(-3.1 < [Fe/H] < -1.4)的Pb和Th丰度,它们的重金属(Z > 56)富集仅由快速(r-)核合成过程产生。新的丰度来自HST/STIS,Keck/HIRES和VLT/UVES光谱,并结合文献中的其他测量,以形成一个更完整的图片核合成中产生的最重元素的r-过程。在所有情况下,稀土元素和第3 r-过程峰值元素(La,Eu,Er,Hf和Ir)之间的丰度比是恒定的,相当于缩放的太阳系r-过程丰度分布。我们比较恒星观测与经典的“等待点”近似的r-过程计算。在这些计算中,将23 < log(n_n)< 30范围内的15个加权中子密度分量的叠加拟合到r过程丰度峰上,成功地再现了太阳系稳定同位素分布和低金属丰度星Ba和U之间稳定的重元素丰度模式。在这些天体物理条件下,这是典型的“主”r-过程,我们发现非常好的协议之间的恒星铅r-过程的丰度和我们的模型预测。对于Th/Eu比值非常高的恒星(所谓的锕系元素增强),我们的观测表明,任何核合成偏离主r过程的影响-最多-只有超出第三r过程峰的元素,即Pb,Th和U。我们的理论计算还表明,可能的r-过程丰度“损失”的核裂变是可以忽略不计的同位素沿r-过程之间的路径铅和长寿命的放射性同位素的Th和U。

英文摘要:

We examine the Pb and Th abundances in 27 metal-poor stars (-3.1 < [Fe/H] < -1.4) whose very heavy metal (Z > 56) enrichment was produced only by the rapid (r-) nucleosynthesis process. New abundances are derived from HST/STIS, Keck/HIRES, and VLT/UVES spectra and combined with other measurements from the literature to form a more complete picture of nucleosynthesis of the heaviest elements produced in the r-process. In all cases, the abundance ratios among the rare earth elements and the 3rd r-process peak elements considered (La, Eu, Er, Hf, and Ir) are constant and equivalent to the scaled solar system r-process abundance distribution. We compare the stellar observations with r-process calculations within the classical "waiting-point" approximation. In these computations a superposition of 15 weighted neutron-density components in the range 23 < log(n_n) < 30 is fit to the r-process abundance peaks to successfully reproduce both the stable solar system isotopic distribution and the stable heavy element abundance pattern between Ba and U in low-metallicity stars. Under these astrophysical conditions, which are typical of the "main" r-process, we find very good agreement between the stellar Pb r-process abundances and those predicted by our model. For stars with anomalously high Th/Eu ratios (the so-called actinide boost), our observations demonstrate that any nucleosynthetic deviations from the main r-process affect--at most--only the elements beyond the 3rd r-process peak, namely Pb, Th, and U. Our theoretical calculations also indicate that possible r-process abundance "losses" by nuclear fission are negligible for isotopes along the r-process path between Pb and the long-lived radioactive isotopes of Th and U.

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