摘要
Chemical abundances of very metal-poor s-rich stars contain excellent information to set new constraints on models of neutron-capture processes at low metallicity. Using the parametric approach based on the radiative s-process nucleosynthesis model, we obtain the mass fraction q of 13 C-pocket, the overlap factor r, the neutron exposure per interpulse △τ, and the component coefficients of the s-process and the r-process for 25 s-rich stars, respectively. We find that q deduced for the lead stars is comparable to the overlap factor r, which is larger than the standard case （hereafter ST case） of the AGB model （q - 0.05） about 10 times, and AT are about 10 times smaller than the ST case （AT = 7.0 mbarn^-1）. Although the two parameters obtained for the lead stars are very different from the ST case of the AGB stellar model, it is worth noting that the total amounts of 13 C in metal-poor condition are close to the ST case. The above relation is a significant evidence for the primary nature of the neutron source and the lead stars could be polluted by low-mass AGB stars. Because interpulse period declines with increasing stellar mass, for high-mass AGB star, the neutron irradiation may be terminated due to their shorter interpulse period. Thus the neutron exposure per interpulse of the larger AGB stars should be about 10 times smaller than the ST case. In this ease, the primary nature of the neutron source also exists.
Chemical abundances of very metal-poor s-rich stars contain excellent information to set new constraints on models of neutron-capture processes at low metallicity. Using the parametric approach based on the radiative s-process nucleosynthesis model, we obtain the mass fraction q of 13 C-pocket, the overlap factor r, the neutron exposure per interpulse △τ, and the component coefficients of the s-process and the r-process for 25 s-rich stars, respectively. We find that q deduced for the lead stars is comparable to the overlap factor r, which is larger than the standard case （hereafter ST case） of the AGB model （q - 0.05） about 10 times, and AT are about 10 times smaller than the ST case （AT = 7.0 mbarn^-1）. Although the two parameters obtained for the lead stars are very different from the ST case of the AGB stellar model, it is worth noting that the total amounts of 13 C in metal-poor condition are close to the ST case. The above relation is a significant evidence for the primary nature of the neutron source and the lead stars could be polluted by low-mass AGB stars. Because interpulse period declines with increasing stellar mass, for high-mass AGB star, the neutron irradiation may be terminated due to their shorter interpulse period. Thus the neutron exposure per interpulse of the larger AGB stars should be about 10 times smaller than the ST case. In this ease, the primary nature of the neutron source also exists.
基金
Supported by the National Natural Science Foundation of China under Nos 10673002, 10847119 and 10778616, the Natural Science Foundation of Hebei Provincial Education Department under Grant No 2008127, and the Science Foundation of Hebei Normal University under Grant No L2007B07.
