AI 中文总结
研究通过用介质势修正FKM的IdylliQ模型解决中子星超子难题，受超核数据和中微子诱导的超子FSI约束，得出多个结果，包括修正后的超子起始点、相关条件及对TOV软化、核心奇异度的影响等，还指出dMmax/dUY可区分两种解决方案。
AI 中文摘要
夸克物质在统计上解决了中子星超子难题：中子填充低动量d夸克相空间，将S = -1阈值从μB = MY转变为2MY - MN，并在Fujimoto - Kojo - McLerran（FKM）机制中通过1/NC³抑制残余软化。我们用介质势修正FKM的IdylliQ模型，受超核数据和中微子诱导的超子FSI约束，发现：（i）修正后的起始点，μB^起始 = (2MY - MN) + 2UY - UN，UY权重为2，每10MeV的dn起始/dUY≈0.3nz，杠杆作用翻倍。（ii）自洽中子势以 -2的权重进入，因此保护需要UN(n起始)≤ +96MeV。（iii）对于处于β平衡的轻子，Σ⁻（dds）的起始变为μe≥258MeV + US - UN，在2Msun核心内从未达到：Σ⁻从第一个超子变为被禁止，Σ的顺序反转。（iv）在FKM假设族中，KY≥Kbu的延续使TOV软化在0.05Msun以下，对于实际相互作用的恒星在0.025Msun以下，比强子模型低4 - 8倍。在该族中这是一个上限；一般来说是下限，因为高于Kbu的超子被省略。（v）在校准到Mmax = 2.12Msun的相互作用低密度区域，核心奇异度由(UL(nz), cΛ)控制：当UL(nz) = -28MeV时，一旦超饱和YNN翻转超过几MeV阈值c*Λ，最大质量恒星无超子。预计的SBND + DUNE FSI精度确定了UL(nz)，但cΛ起决定性作用，中微子数据对此盲目：有重离子先验时，P（无超子核心） = 0.90，仅先验时为0.89，由先验主导而非测量。最敏锐的可观测量是微分的：dMmax/dUY比平均场模型小一个数量级，可区分这两种解决方案。
英文摘要
Quarkyonic matter resolves the neutron-star hyperon puzzle statistically: neutrons fill low-momentum $d$-quark phase space, shifting the $S=-1$ threshold from $\muB=M_Y$ to $2M_Y-M_N$ and suppressing residual softening by $1/\Nc^3$ in the Fujimoto--Kojo--McLerran (FKM) mechanism. We dress FKM's IdylliQ model with in-medium potentials, constrained by hypernuclear data and neutrino-induced hyperon FSI, and find: (i) the dressed onset, $\muB^{\rm onset}=(2M_Y{-}M_N)+2U_Y-\UN$, carries $U_Y$ at weight 2, with $dn_{\rm onset}/dU_Y\simeq0.3\,\nz$ per $10\MeV$, twice the leverage. (ii) A self-consistent neutron potential enters at weight $-2$, so protection needs $\UN(n_{\rm onset})\lesssim+96\MeV$. (iii) With leptons in $β$ equilibrium, the $Σ^-$ ($dds$) onset becomes $\mue\ge258\MeV+\US-\UN$, never reached inside a $2\,\Msun$ core: $Σ^-$ switches from first hyperon to forbidden and the $Σ$ ordering inverts. (iv) The $\kY\ge\kbu$ continuation gives TOV softening below $0.05\,\Msun$ in the FKM ansatz family and below $0.025\,\Msun$ for the realistic interacting star, $4$--$8$ below hadronic models. In the family this is a ceiling; generally it is a floor, since hyperons above $\kbu$ are omitted. (v) In an interacting low-density sector calibrated to $\Mmax=2.12\,\Msun$, core strangeness is controlled by $(\UL(\nz),c_Λ)$: at $\UL(\nz)=-28\MeV$, the maximum-mass star is hyperon-free once the supra-saturation $YNN$ turn-over exceeds a few-MeV threshold $c^*_Λ$. Projected SBND+DUNE FSI precision pins $\UL(\nz)$ but leaves $c_Λ$ -- to which neutrino data are blind -- decisive: with the heavy-ion prior, $P({\rm hyperon\mbox{-}free\ core})=0.90$, versus $0.89$ from priors alone, prior-dominated rather than measured. The sharpest observable is differential: $d\Mmax/dU_Y$ is an order of magnitude smaller than in mean-field models, discriminating the two resolutions.
Comments9 pages, 6 figures
