论文标题
由假设X17玻色子介导的核力量的中子星形结构
Neutron star structure with nuclear force mediated by hypothetical X17 boson
论文作者
论文摘要
报告的$ {17〜} $ MEV玻色子是针对$^{8} $ be和$^{4} $ anomaly的解释的，它是在其对中子星结构的可能影响的背景下进行了调查的。使用不同的不可压缩性值K $ _ {0} $ = 245 MEV和K $ _ {0} $ = 260 MEV并求解tolman-oppenheeimer-volkoff方程，我们估计$ {m _ proge afffro {tolov， $ {11.5〜} $ km至$ {14〜} $ km之间的跨度$ {r} $的非旋转中子星。从纯净 - NN脱离具有10 \％质子的混合物，并模拟由于超子引起的状态方程的可能软化，我们看到我们的估计极限非常适合最新报告的研究，来自中子星星合并，GW190814
A reported ${17~}$MeV boson, which has been proposed as an explanation to the $^{8}$Be and $^{4}$He anomaly, is investigated in the context of its possible influence to neutron stars structure. Implementing a $m_{X}$=17 MeV to the nuclear equation of state using different incompressibility values K$_{0}$=245 MeV and K$_{0}$=260 MeV and solving Tolman-Oppenheimer-Volkoff equations, we estimate an upper limit of ${M_{TOV}\thickapprox 2.4M\odot}$ for a non rotating neutron star with span in radius ${R}$ between ${11.5~}$km to ${14~}$km. Moving away from pure - NN with admixture of 10\% protons and simulating possible softening of equation of state due to hyperons, we see that our estimated limits fit quite well inside the newest reported studies, coming from neutron stars merger event, GW190814
