论文标题
原始恒星和合并残余物中的三角洲共和力和超子
Delta-resonances and hyperons in proto-neutron stars and merger remnants
论文作者
论文摘要
在中子星二元合并残留物和超新星的特征的条件下，研究了状态方程（EOS）的方程（EOS）和密集和热$δ$均匀的超核问题。寒冷的，无中微子的状态也被视为对密集物质EOS的天体物理约束的参考。我们的形式主义使用协变量功能（CDF）理论成功地适应了整个$ j^p = 1/2^+$ baryon八位位和$ j^p = 3/2^+$ decouplet的非震动成员，并与密度相关的耦合进行了适当调整到现有的实验室和天文学数据。 $δ$在有限温度下的效果是在中间密度下软化高核物质的EOS并在高密度下加强。在低温下，如果$δ$ -Meson耦合接近核子 - 梅森 - 梅森 - 梅森 - - 梅森 - 梅森耦合，则沉重的baryons $λ$，$Δ^ - $，$δ^ - $，$δ^ - $，$ξ^ - $，$ξ^ - $和$δ^0 $。与Hyperons一样，$δ$谐振的阈值转移到较低的密度，温度的升高表明在低密度亚核状态下的$δ$的明显部分。我们发现，$δ$ res子包含很大一部分的巴元物质，在中微子捕获的制度中的几十MEV的温度下，$ 10 \％$的顺序为$％$ $，因此，可以通过为中心访问或新的频道提供一个新的频道来影响超新星和二元中性星星的二进制中性恒星动态。讨论了等等静态静态，球体对称热恒星的质量关系。
The equation of state (EoS) and composition of dense and hot $Δ$-resonance admixed hypernuclear matter is studied under conditions that are characteristic of neutron star binary merger remnants and supernovas. The cold, neutrino free regime is also considered as a reference for the astrophysical constraints on the EoS of dense matter. Our formalism uses the covariant density functional (CDF) theory successfully adapted to include the full $J^P=1/2^+$ baryon octet and non-strange members of $J^P=3/2^+$ decouplet with density-dependent couplings that have been suitably adjusted to the existing laboratory and astrophysical data. The effect of $Δ$-resonances at finite temperatures is to soften the EoS of hypernuclear matter at intermediate densities and stiffen it at high densities. At low temperatures, the heavy baryons $Λ$, $Δ^-$,$Ξ^-$, $Ξ^0$ and $Δ^0$ appear in the given order if the $Δ$-meson couplings are close to those for the nucleon-meson couplings. As is the case for hyperons, the thresholds of $Δ$-resonances move to lower densities with the increase of temperature indicating a significant fraction of $Δ$'s in the low-density subnuclear regime. We find that the $Δ$-resonances comprise a significant fraction of baryonic matter, of the order of $10\%$ at temperatures of the order of several tens of MeV in the neutrino-trapped regime and, thus, may affect the supernova and binary neutron star dynamics by providing, for example, a new source for neutrino opacity or a new channel for bulk viscosity via the direct Urca processes. The mass-radius relation of isentropic static, spherically symmetric hot compact stars is discussed.
