Neutron-Rich Nuclei in Heaven and Earth
Neutron-Rich Nuclei in Heaven and Earth
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天地间的富中子核
DOI：
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发表时间：
2005
期刊：
影响因子：
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通讯作者：
J. Piekarewicz
中科院分区：
文献类型：
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作者：
B. G. Todd;J. Piekarewicz
引入了一种精确校准的相对论参数化方法来计算有限原子核的基态性质、线性响应和中子星的结构。虽然在精神上类似于成功的NL3参数集，但它产生了一个相当柔软的状态方程-对于对称核物质和对称能量都是如此。这种软化似乎是精确描述具有不同中子质子比的几种集体模式所必需的。该模型预测了K = 230 MeV的对称核物质不可压缩性和R n - R p = 0的208 Pb中子蒙皮厚度。21调频。此外，这种软化对中子星性质的影响如下：模型预测中子星的极限质量为mmax = 1。72 M⊙，半径R = 12。66公里的“标准”M = 1。4个M⊙中子星，没有（核子）直接在质量低于M =1的中子星中冷却。3米⊙。
An accurately calibrated relativistic parametrization is introduced to compute the ground state properties of finite nuclei, their linear response, and the structure of neutron stars. While similar in spirit to the successful NL3 parameter set, it produces an equation of state that is considerably softer — both for symmetric nuclear matter and for the symmetry energy. This softening appears to be required for an accurate description of several collective modes having different neutron-to-proton ratios. Among the predictions of this model are a symmetric nuclear-matter incompressibility of K = 230 MeV and a neutron skin thickness in 208 Pb of R n − R p = 0 . 21 fm. Further, the impact of such a softening on the properties of neutron stars is as follows: the model predicts a limiting neutron star mass of M max = 1 . 72 M ⊙ , a radius of R = 12 . 66 km for a “canonical” M = 1 . 4 M ⊙ neutron star, and no (nucleon) direct Urca cooling in neutrons stars with masses below M =1 . 3 M ⊙ .