论文标题
Y型和Z型的前硅碳化物颗粒：其锶和同位素成分和恒星起源
Presolar Silicon Carbide Grains of Types Y and Z: Their Strontium and Barium Isotopic Compositions and Stellar Origins
论文作者
论文摘要
我们报告了Y（11）和Z（7）的18种前晶粒的SR和BA同位素组合物，通常认为罕见的类型是在低于 - 摩尔金属性渐近性渐近性巨型分支（AGB）恒星中形成的。我们发现，Y和Z晶粒显示出比主流晶粒更高的88SR/87SR和更可变的138BA/136BA比。 According to FRANEC Torino AGB models, the Si, Sr, and Ba isotopic compositions of our Y and Z grains can be consistently explained if the grains came from low mass AGB stars with 0.15 Zsun <= Z < 1.00 Zsun, in which the 13C neutron exposure for the slow neutron-capture process is greatly reduced with respect to that required by MS grains for a 1.0 Z8 AGB star.这种情况与基于Ti同位素的先前发现一致，但无法解释MS，Y和Z粒的难以区分的MO同位素组合物。
We report the Sr and Ba isotopic compositions of 18 presolar SiC grains of types Y (11) and Z (7), rare types commonly argued to have formed in lower-than-solar metallicity asymptotic giant branch (AGB) stars. We find that the Y and Z grains show higher 88Sr/87Sr and more variable 138Ba/136Ba ratios than mainstream (MS) grains. According to FRANEC Torino AGB models, the Si, Sr, and Ba isotopic compositions of our Y and Z grains can be consistently explained if the grains came from low mass AGB stars with 0.15 Zsun <= Z < 1.00 Zsun, in which the 13C neutron exposure for the slow neutron-capture process is greatly reduced with respect to that required by MS grains for a 1.0 Z8 AGB star. This scenario is in line with the previous finding based on Ti isotopes, but it fails to explain the indistinguishable Mo isotopic compositions of MS, Y, and Z grains.
