标题： 利用全局中子星特性探测费米子非对称暗物质核心 显示英文标题

标题： Probing fermionic asymmetric dark matter cores using global neutron star properties

摘要： 不对称暗物质（ADM）有可能在中子星内部积累，并影响其整体性质。 考虑到这种积累的影响，中子星质量-半径测量可以为冷密物质的状态方程（EoS）提供新的见解。 在本文中，我们使用贝叶斯参数估计，利用真实和合成的中子星质量-半径数据来推断结合重子物质和费米子ADM的EoS约束，其中费米子ADM在中子星内部形成核心。 利用目前可用的质量-半径数据，我们发现ADM有效自排斥强度（$g_\chi/m_\phi$）与粒子质量（$m_\chi$）的比值下限可以在68%（95%）的可信水平上被限制为$10^{-6.59}$（$10^{-7.77}$）。 我们还发现，如果中子星质量-半径测量的不确定性降低到2%的水平，那么对$g_\chi/m_\phi$与$m_\chi$比值下限的约束可以分别提高到 68% 和 95% 的可信水平的$10^{-6.49}$和$10^{-7.68}$。 然而，其他所有组合，包括$m_\chi$、$g_\chi$和 ADM 质量分数$F_\chi$（即引力 ADM 质量与中子星引力质量的比值）都是不受约束的。 此外，在压强-能量密度和质量-半径平面上，包含费米子ADM核心可能性的推论与忽略费米子ADM的推论对于$F_\chi \leq 1.7\%$和中子星质量-半径不确定性$\geq 2\%$几乎相同。 因此，我们发现中子星质量-半径测量可以限制$g_\chi/m_\phi$与$m_\chi$的比值，并且具有ADM的中子星与纯重子星无法区分。 这意味着具有ADM的中子星与可用的质量-半径数据的一致性与不具有ADM的中子星同样高。 显示英文摘要

摘要： It is possible for asymmetric dark matter (ADM) to accumulate in neutron star interiors and affect their global properties. Considering the effects of this accumulation, neutron star mass-radius measurements can deliver new insights into the cold dense matter equation of state (EoS). In this paper, we employ Bayesian parameter estimation using real and synthetic neutron star mass-radius data to infer constraints on the combined baryonic matter and fermionic ADM EoS, where the fermionic ADM forms a core in the neutron star interior. Using currently available mass-radius data, we find that the lower bound of the ratio between ADM effective self-repulsion strength ($g_\chi/m_\phi$) and particle mass ($m_\chi$) can be constrained at the 68\% (95\%) credible level to $10^{-6.59}$ ($10^{-7.77}$). We also find that, if neutron star mass-radius measurement uncertainties are reduced to the 2\% level, the constraints on the lower bound of the ratio of $g_\chi/m_\phi$ to $m_\chi$ can be improved to $10^{-6.49}$ and $10^{-7.68}$ at the 68\% and 95\% credible levels, respectively. However, all other combinations, of $m_\chi$, $g_\chi$, and the ADM mass-fraction, $F_\chi$, (i.e., the ratio of the gravitational ADM mass to the gravitational mass of the neutron star) are unconstrained. Furthermore, in the pressure-energy density and mass-radius planes, the inferences which include the possibility of fermionic ADM cores are nearly identical with the inferences that neglect fermionic ADM for $F_\chi \leq 1.7\%$ and neutron star mass-radius uncertainties $\geq 2\%$. Therefore, we find that neutron star mass-radius measurements can constrain the ratio of $g_\chi/m_\phi$ to $m_\chi$ and that neutron stars with ADM are indistinguishable from purely baryonic stars. This implies that neutron stars with ADM are equally as consistent with the available mass-radius data as neutron stars without ADM.