Contribution of dust produced by binary merger ejecta
Contribution of dust produced by binary merger ejecta
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DOI：
10.1088/1674-4527/15/1/006
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发表时间：
2015
影响因子：
1.8
通讯作者：
Zhaojun Wang;Chunhua Zhu;G. Lü
中科院分区：
文献类型：
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作者：
Zhaojun Wang;Chunhua Zhu;G. Lü
利用星族合成程序，通过构造一个简单的渐近巨星分支（AGB）、共包络（CE）和双星合并喷出物的尘埃模型，估算了银河系中这些过程的尘埃生成率（DPRs）. AGB星的总DPR为10.67 × 10−4 M yr−1，其中约73%的尘埃颗粒是碳，24%是硅酸盐，3%是铁。来自CE喷出物的总DPR为4.2 × 10−4 M yr−1，其中约83%的尘埃颗粒是硅酸盐，约12%是碳，5%是铁。双星并合喷出物的DPR小于AGB星或CE喷出物的1/3，在某些情况下甚至可以忽略不计。因此，与AGB星和CE喷出物相比，双星合并喷出物产生的尘埃对银河系总尘埃颗粒的贡献较小或可以忽略。
By means of a population synthesis code and by constructing a simple toy model of dust produced by asymptotic giant branch (AGB) stars, common envelope (CE) ejecta and binary merger ejecta, we estimate the dust product rates (DPRs) of these processes in the Milky Way. The total DPR from AGB stars is ∼ 6.7 × 10−4 M⊙ yr−1, in which about 73% of dust grains are carbon, 24% are silicates and 3% are iron. The total DPR from CE ejecta is ∼ 4.2 × 10−4 M⊙ yr−1, in which about 83% of dust grains are silicates, about 12% are carbon and 5% are iron. The DPR from binary merger ejecta is less than 1/3 that from AGB stars or CE ejecta, and it could even be negligible under certain circumstances. Therefore, compared with AGB stars and CE ejecta, the contribution of dust produced by binary merger ejecta to total dust grains in the Milky Way is smaller or can be negligible.