标题： 利用全球中子星属性探测费米子不对称暗物质核心 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聚并对它们的全局属性产生影响。 考虑到这种积聚的影响，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，我们利用真实的和合成的中子星质量-半径数据进行贝叶斯参数估计，以推断结合的重子物质和费米子ADM状态方程的约束条件，其中费米子ADM在中子星内部形成一个核心。 使用目前可用的质量-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（$m_\chi$）之比的下限可以在68%（95%）可信度水平上限制为$10^{-6.59}$（$10^{-7.36}$）。 我们还发现，如果中子星质量和半径的测量不确定性降低到2%，那么对 $g_\chi/m_\phi$ 与 $m_\chi$ 比值下限的约束可以提高到分别在68%和95%可信度水平下的 $10^{-6.5}$ 和 $10^{-7.29}$。然而，所有其他组合，包括 $m_\chi$、$g_\chi$ 和 ADM 质量分数 $F_\chi$（即中子星引力 ADM 质量与引力质量之比），都未受到约束。 此外，在压强-能量密度和平面图-质量平面中，包含费米子ADM核心可能性的推论与忽略$F_\chi \leq 1.7\%$和中子星质量-半径不确定性的$\geq 2\%$的推论几乎相同。 因此，我们发现中子星质量-半径测量可以约束某些场景中的ADM，并且中子星核心中存在ADM与不存在ADM同样与当前数据一致。 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 $10^{-6.59}$ ($10^{-7.36}$). We also find that, if neutron star mass-radius measurement uncertainties are reduced to the 2% level, the constraints on lower bound on the ratio of $g_\chi/m_\phi$ to $m_\chi$ can be improved to $10^{-6.5}$ and $10^{-7.29}$ 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 ADM in some scenarios and that the presence of ADM in neutron star cores is as equally consistent with current data as the absence of ADM.