AI 中文总结
研究原中子星演化中色超导相情况，通过将原中子星条件纳入RG一致的NJL模型状态方程，沿重子数等值线追踪恒星构型，揭示了四种核心演化情景，发现特定参数化下稳定色超导相仅在窄高质量区域的冷中子星中维持。
AI 中文摘要
在高密度和中等温度下，强子物质预计会经历一级相变进入色超导（CSC）状态。原中子星描述了核心坍缩超新星爆发后最初几秒到几分钟内的最早演化阶段，因此有潜力评估在如此高密度和中等温度下CSC相的出现情况。为解决此问题，我们在最近开发的RG一致的NJL模型中，将原中子星条件（包括中微子捕获和中微子透明条件）纳入包含色超导相的状态方程中。由于原中子星的总重子数在其后期演化中守恒，沿着重子数等值线追踪从热原中子星的初始质量到最终冷中子星的恒星构型，使我们能够研究在这条轨迹上的任何一点是否能形成色超导相。通过描绘核心坍缩超新星从捕获中微子的诞生状态冷却到冷的、中微子透明的最终状态这个热熔炉中的多维转变，我们揭示了四种不同的核心演化情景——我们的原中子星演化的“小甜点”：从CSC相延迟坍缩到黑洞、持续的CSC相、消失的CSC相和短暂的CSC相。对于我们对强子和CSC状态方程的特定参数化，我们发现对于一个狭窄的高质量区域，稳定的色超导相只能在最终的冷中子星中维持。
英文摘要
At high densities and moderate temperatures, hadronic matter is expected to undergo a first-order phase transition into a color-superconducting (CSC) state. A proto-neutron star describes the earliest evolutionary stages during the first seconds to minutes after core-collapse supernovae and therefore has the potential to assess the appearance of CSC phases at such high densities and moderate temperatures. To address this, we incorporate proto-neutron star conditions, considering neutrino-trapped and neutrino-transparent ones, into the equation of state including color-superconducting phases in a recently developed RG-consistent NJL model. Since the total baryon number of a proto-neutron star is conserved during its later evolution, tracking stellar configurations from an initial mass of the hot proto-neutron star to the final cold neutron star along isolines of baryon number allows us to investigate whether color-superconducting phases can form at any point along this trajectory. By mapping this multidimensional transition in the hot furnace of a core-collapse supernovae cooling from a neutrino-trapped birth state to a cold, neutrino-transparent final state, we reveal four distinct core evolution scenarios-our "petit four" of proto-neutron star evolution: a delayed collapse from the CSC phase to a black hole, a persistent CSC phase, a vanishing CSC phase, and a fleeting CSC phase. For our specific parameterization of the hadronic and the CSC equation of state, we find that a stable color-superconducting phase can only be sustained in the final cold neutron star for a narrow, high-mass region.
Comments14 pages, 9 figures, comments are welcome
