NICER中子星中的暗能量与暗物质：对推断状态方程的影响
NICER neutron stars with dark energy and dark matter: effects on the inferred equation of state
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中文总结 AI 辅助
本研究对比含暗能量或暗物质核心的中子星与纯重子星，发现暗能量模型受观测约束更强，且质量-半径观测无法探测暗物质核心，需其他探针。
中文摘要 AI 辅助
[摘要删节] 在这项工作中，我们比较了核心中存在暗能量或暗物质的中子星，并将其与具有相同中心能量密度的纯重子星进行对比。通过这一比较，我们发现暗能量模型比暗物质模型受到中子星观测的约束更强，这表明中子星可以对暗能量参数施加强有力的限制。我们考虑了四种构型：由分段多方（PP）状态方程（EoS）描述的纯重子中子星；混合有玻色子或费米子非对称暗物质（ADM）核心的重子星；以及具有暗能量核心和重子壳层的恒星，其中暗能量由修正的Chaplygin暗流体（MCDF）描述。利用PSR J0740$+$6620、PSR J0437$-$4715和PSR J0030$+$0451的质量和半径，我们采用贝叶斯推断来研究考虑玻色子/费米子ADM和MCDF核心如何影响推断的中子星性质。我们发现，与PP和ADM混合模型相比，MCDF核心更显著地拓宽了中子星质量-半径和压力-能量密度的后验分布。此外，MCDF的EoS参数可以被紧密约束。虽然玻色子和费米子ADM核心降低了推断的最大质量，但对于ADM质量分数$F_\chi \leq 5\\%$，它们的后验与PP模型的后验强烈重合。这些结果表明，当前的质量-半径观测不能排除MCDF核心，但可以将MCDF参数空间约束到狭窄区域。然而，对于所有探索的质量分数，ADM混合中子星在观测上与纯重子星仍然相同，即使质量-半径不确定性得到改善。这表明仅凭质量-半径测量不足以探测中子星内部的ADM核心，需要独立的天体物理或粒子物理探针。
英文摘要
[Abridged] In this work, we compare neutron stars where dark energy or dark matter are present in the core, contrasting them against purely baryonic stars with the same central energy density. From this comparison, we find that the dark energy models are more constrained by neutron star observations than the dark matter models, suggesting that neutron stars can place strong constraints on dark energy parameters. We consider four configurations: purely baryonic neutron stars described by a piecewise polytropic (PP) equation of state (EoS), baryonic stars admixed with bosonic or fermionic asymmetric dark matter (ADM) cores, and stars with a dark energy core and baryonic shell, where the dark energy is described by the modified Chaplygin dark fluid (MCDF). Using the masses and radii of PSR J0740$+$6620, PSR J0437$-$4715, and PSR J0030$+$0451, we employ Bayesian inference to investigate how accounting for bosonic/fermionic ADM and MCDF cores affects the inferred neutron star properties. We find that MCDF cores, more than PP and ADM admixed models, substantially broaden neutron star mass-radius and pressure-energy density posterior distributions. Moreover, the MCDF EoS parameters can be tightly constrained. While bosonic and fermionic ADM cores decrease the inferred maximum mass, their posteriors strongly coincide with those of the PP model for ADM mass-fractions $F_χ\leq 5\%$. These results demonstrate that current mass-radius observations cannot rule out MCDF cores, but they can constrain the MCDF parameter space to narrow regions. ADM admixed neutron stars, however, remain observationally identical to purely baryonic stars for all explored mass-fractions, even with improved mass-radius uncertainties. This suggests that mass-radius measurements alone are insufficient to detect ADM core inside neutron stars and that independent astrophysical or particle physics probes will be required.
发表机构
- University of New Hampshire（新罕布什尔大学）
- Foundational Questions Institute (FQxI)（基础问题研究所）
- University of Amsterdam（阿姆斯特丹大学）
机构由 AI 辅助整理，请以论文原文为准。
