Empirical neutron star mass formula based on experimental observables
Empirical neutron star mass formula based on experimental observables
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DOI：
10.1103/physrevc.107.035802
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发表时间：
2023-03
影响因子：
3.1
通讯作者：
H. Sotani;T. Naito
中科院分区：
文献类型：
--
作者：
H. Sotani;T. Naito
给出了中心密度小于核饱和密度三倍的中子星的质量和引力红移与中子皮厚度或偶极子极化率的关系的经验公式，特别是讨论了8种Skyrme型有效相互作用.用我们的公式可以估计中子星的质量及其引力红移，而中子星的半径也可以通过结合所得到的公式来估计在几美元的误差之内。根据得到的经验公式，我们发现中子星的质量和半径对中子皮厚度比偶极子极化率对中子皮厚度的影响更敏感。
We derive the empirical formulae expressing the mass and gravitational redshift of a neutron star, whose central density is less than threefold the nuclear saturation density, as a function of the neutron-skin thickness or the dipole polarizability of $ {}^{208} \mathrm{Pb} $ or $ {}^{132} \mathrm{Sn} $, especially focusing on the 8 Skyrme-type effective interactions. The neutron star mass and its gravitational redshift can be estimated within $ \approx 10 \, \% $ errors with our formulae, while the neutron star radius is also expected within a few $\%$ errors by combining the derived formulae. Owing to the resultant empirical formulae, we find that the neutron star mass and radius are more sensitive to the neutron-skin thickness of $ {}^{208} \mathrm{Pb} $ than the dipole polarizability of $ {}^{208} \mathrm{Pb} $ or $ {}^{132} \mathrm{Sn} $.