论文标题
核子有效质量和对称能对中微子平均自由路径的影响
Effect of nucleon effective mass and symmetry energy on the neutrino mean free path in a neutron star
论文作者
论文摘要
韩国-IBS-DAEGU-SKKU能量密度功能（KIDS-EDF）模型是由核物质中能量密度的扰动扩张构建的，已成功地用于描述有限核和无限核物质的性质。在目前的工作中，我们扩展了儿童EDF模型的应用，以研究核子有效质量和核对称能对中子星（NSS）（NSS）（NSS）的性质的含义以及与NS成分物质在线性响应近似（LRA）中与NS构成物的相互作用。在固定中微子能量和动量转移时，我们分析了中微子的总差分横截面，中微子平均自由路径（NMFP）和NS Mass-Radius（M-R）关系。与从$ m_n^* /m \ Lessim 1 $的$ M_N^* /M \ Lessim 1 $相比，与从KIDS0，KIDS-A和KIDS-A和KIDS-B型号获得的NMFP相比，KIDS0-M*87和SLY4型号给出了显着的结果，其中$ M_N^* /M \ gtrsim 1 $。对于Kids0，Kids-A和Kids-B型号，我们获得了$λ\ Lessim r _ {\ textrm {ns}} $，表明这些模型可以预测NSS中的慢速NS冷却和中微子捕获。相比之下，KIDS0-M*87和SLY4模型产生$λ\ gtrsim r _ {\ textrm {ns}} $，因此我们希望NS冷却速度更快，并且在NSS中陷入了中微子诱捕的可能性很小。我们还计算NMFP是中微子能量和核物质密度的函数，发现NMFP随着密度和中微子能量的增加而降低，这与在饱和密度下模型中Brussels-Montreal Skyrme（BSK17和BSK17）中获得的结果一致。
The Korea-IBS-Daegu-SKKU energy density functional (KIDS-EDF) models, constructed from the perturbative expansion of the energy density in nuclear matter, have been successfully and widely applied in describing the properties of finite nuclei and infinite nuclear matter. In the present work, we extend the applications of the KIDS-EDF models to investigate the implications of the nucleon effective mass and nuclear symmetry energy for the properties of neutron stars (NSs) and neutrino interaction with the NS constituent matter in the linear response approximation (LRA). At fixed neutrino energy and momentum transfer, we analyze the total differential cross section of neutrino, the neutrino mean free path (NMFP), and the NS mass-radius (M-R) relations. Remarkable results are given by the KIDS0-m*87 and SLy4 models, in which $M_n^* /M \lesssim 1$, and their NMFPs are quite higher in comparison with those obtained from the KIDS0, KIDS-A, and KIDS-B models, which result in $M_n^*/M \gtrsim 1$. For the KIDS0, KIDS-A, and KIDS-B models, we obtain $λ\lesssim R_{\textrm{NS}}$, indicating that these models could predict the slow NS cooling and neutrino trapping in NSs. In contrast, the KIDS0-m*87 and SLy4 models yield $λ\gtrsim R_{\textrm{NS}}$ and thus we expect faster NS cooling and a small possibility of neutrino trapping within NSs. We also calculate the NMFP as a function of the neutrino energy and the nuclear matter density and find that the NMFP decreases as the density and neutrino energy increase, which is consistent with the result obtained in the Brussels-Montreal Skyrme (BSk17 and BSk18) models at saturation density.
