Intermediate-mass Asymptotic Giant Branch Stars and Sources of 26Al, 60Fe, 107Pd, and 182Hf in the Solar System
Intermediate-mass Asymptotic Giant Branch Stars and Sources of 26Al, 60Fe, 107Pd, and 182Hf in the Solar System
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太阳系中质量渐近巨分支星和 26Al、60Fe、107Pd 和 182Hf 的来源
DOI：
10.3847/1538-4357/836/1/126
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发表时间：
2016
期刊：
影响因子：
--
通讯作者：
M. Lugaro
中科院分区：
文献类型：
--
作者：
G. Wasserburg;Amanda I Karakas;Amanda I Karakas;M. Lugaro;M. Lugaro
我们探讨的可能性，短寿命的放射性核素l，e，d，和f推断是目前在原太阳云起源于3-8渐近巨星分支（AGB）星。初始质量大于1的AGB星模型由于热底部燃烧（HBB）而大量产生l。相比之下，e、d和f是由中子俘获产生的：d和f在模型中，e在更高质量的模型中。我们混合恒星产量从太阳金属丰度AGB模型到云的太阳质量和成分，以调查是否有可能解释的丰度的四个放射性核素在太阳的诞生使用一个单一的值之间的混合比的AGB产量和初始云材料。我们发现，AGB星，经验有效的HBB（）不能提供一个解决方案，因为他们产生太少的f和d相对于l和e。较低质量的AGB星不能提供一个解决方案，因为它们产生的l相对于d和f太少。对于质量在（4-5.5）之间的AGB星，只要HBB比我们的模型中的强，并且（α，n）中子源被轻度激活，就可以找到一个自洽的解。如果恒星是放射性核素的来源，那么它们存在于原太阳云中的一些基础需要探索，因为恒星的寿命比分子云的寿命长。
We explore the possibility that the short-lived radionuclides l, e, d, and f inferred to be present in the proto-solar cloud originated from 3–8 asymptotic giant branch (AGB) stars. Models of AGB stars with initial mass above are prolific producers of l owing to hot bottom burning (HBB). In contrast, e, d, and f are produced by neutron captures: d and f in models and e in models with higher mass. We mix stellar yields from solar-metallicity AGB models into a cloud of solar mass and composition to investigate whether it is possible to explain the abundances of the four radioactive nuclides at the Sun’s birth using one single value of the mixing ratio between the AGB yields and the initial cloud material. We find that AGB stars that experience efficient HBB ( ) cannot provide a solution because they produce too little f and d relative to l and e. Lower-mass AGB stars cannot provide a solution because they produce too little l relative to d and f. A self-consistent solution may be found for AGB stars with masses in between (4–5.5 ), provided that HBB is stronger than in our models and the (α, n) neutron source is mildly activated. If stars of are the source of the radioactive nuclides, then some basis for their existence in proto-solar clouds needs to be explored, given that the stellar lifetimes are longer than the molecular cloud lifetimes.
影响因子：
5
作者：
Matthes, Maximilian;Fischer-Goedde, Mario;Kleine, Thorsten
通讯作者：
Kleine, Thorsten
影响因子：
56.9
作者：
Kruijer, T. S.;Touboul, M.;Kleine, T.
通讯作者：
Kleine, T.