标题： 中间质量恒星的新理论产额 显示英文标题

标题： New theoretical yields of intermediate mass stars

摘要： 我们给出了初始质量在0.8到8 M$_{\odot}$之间、初始金属丰度为Z = 0.001、0.004、0.008、0.02和0.04的恒星理论的H、$^{4}$He、$^{12}$C、$^{13}$C、$^{14}$N和$^{16}$O的产量。我们使用日内瓦小组的演化轨迹结合一个合成热脉冲AGB（渐近巨星支）演化模型，详细追踪了化学演化和质量损失，直至AGB末期，包括第一次、第二次和第三次物质下沉阶段。所使用的大多数关系都是依赖于金属丰度的，以便与具有不同初始丰度的恒星进行现实比较。热底部燃烧（HBB）的影响以近似方式包含在内。 我们计算中的自由参数包括 AGB 阶段恒星的质量损失尺度参数 $\eta_{AGB}$ （采用 Reimers 公式）、吸积的最小核心质量 M$_{c}^{min}$ 和第三次吸积效率 $\lambda$。 根据先前广泛的建模结果， $\eta_{AGB}$ = 4，M$_{c}^{min}$ = 0.58 \mss ，而 $\lambda = 0.75$ 包括 HBB 与银河盘和麦哲伦云中 AGB 恒星的观测结果最为一致。 我们将 AGB 最终阶段预测的丰度与银河盘中行星状星云的观测值进行了比较，结果显示具有上述参数的模型与观测结果非常吻合。 本文提出的中等质量恒星的金属丰度相关产额非常适合用于银河化学演化模型。 显示英文摘要

摘要： We present theoretical yields of H, $^{4}$He, $^{12}$C, $^{13}$C, $^{14}$N, and $^{16}$O for stars with initial masses between 0.8 and 8 M$_{\odot}$ and initial metallicities Z = 0.001, 0.004, 0.008, 0.02, and 0.04. We use the evolutionary tracks of the Geneva group up to the early asymptotic giant branch (AGB) in combination with a synthetic thermal-pulsing AGB evolution model to follow in detail the chemical evolution and mass loss up to the end of the AGB including the first, second, and third dredge-up phases. Most of the relations used are metallicity dependent to make a realistic comparison with stars of different initial abundances. The effect of Hot Bottom Burning (HBB) is included in an approximate way. The free parameters in our calculations are the mass loss scaling parameter $\eta_{AGB}$ for stars on the AGB (using a Reimers law), the minimum core mass for dredge-up M$_{c}^{min}$, and the third dredge-up efficiency $\lambda$. As derived from previous extensive modeling, $\eta_{AGB}$ = 4, M$_{c}^{min}$ = 0.58 \mss, and $\lambda = 0.75$ including HBB are in best agreement with observations of AGB stars both in the Galactic disk and the Magellanic Clouds. We compare the abundances predicted during the final stages of the AGB with those observed in planetary nebulae in the Galactic disk and show that the model with the aforementioned parameters is in good agreement with the observations. The metallicity dependent yields of intermediate mass stars presented in this paper are well suited for use in galactic chemical evolution models.