Neutrino Reactions on 4He and the r-Process
Neutrino Reactions on 4He and the r-Process
复制标题
4He 中微子反应和 r 过程
DOI：
10.1086/309634
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发表时间：
1995
期刊：
影响因子：
--
通讯作者：
B. Meyer
中科院分区：
文献类型：
--
作者：
B. Meyer
来自开尔文-亥姆霍兹冷却中子星星的中微子驱动风，核合成的r过程可能在其中发生。中微子决定了物质的膨胀率、每个重子的熵以及风物质中的中子丰度。中微子驱动风核合成的一些模型已经成功地再现了太阳r过程的同位素模式和产额。然而，这些模型中以前没有包括的一个效应是中微子与丰富的4 He核的相互作用。这种相互作用往往会通过允许太多种子核的组装来抑制r过程，从而破坏模型产量和太阳系丰度之间的良好一致性。为了恢复这种良好的一致性，有必要对现有模型进行一些修改。
Neutrinos from a Kelvin-Helmholtz-cooling neutron star drive the winds in which the r-process of nucleosynthesis possibly occurs. The neutrinos establish the matter expansion rate, the entropy per baryon, and the neutron richness in the wind material. Some models of the nucleosynthesis in neutrino-driven winds have successfully reproduced the solar r-process isotopic patterns and yields. An effect not previously included in these models, however, is the interaction of neutrinos with the abundant 4He nuclei. Such interactions tend to inhibit the r-process by allowing the assembly of too many seed nuclei, thereby destroying the good agreement between model yields and solar system abundances. In order to restore that good agreement, it is necessary to postulate some modification or modifications to current models.