新生奇异星的对光度与冷却：色味锁定和双味色超导夸克
Pair luminosity and cooling of newborn strange star: Color-flavor-locked and two-flavor color superconducting quarks
AI总结：
研究由色超导夸克构成的热奇异星早期热演化，考虑中微子冷却和施温格过程等，表明施温格光度是温度通用函数，奇异星表面冷却快，对光度随时间下降，分析了中微子与电子 - 正电子对光度及能量关系。
AI中文摘要：
继之前的工作，本文考虑由处于两种不同配对状态（双味色超导体（2SC）和色味锁定（CFL）相）的色超导夸克构成的热奇异星的早期热演化，计入中微子冷却以及施温格过程导致的电子 - 正电子对产生。我们表明，对于夸克化学势\(\mu_q>280\) MeV，电球层中的施温格光度是温度的通用函数，与夸克物质相无关。奇异星表面在所有情况下冷却都比其内部快，导致对光度随时间快速下降，在奇异星形成后1秒时不超过\(10^{46}\) erg/s。除了具有大能隙参数\(\Delta>60\) MeV的CFL相（其中中微子发射受到强烈抑制）外，中微子光度在所有情况下都主导对光度。电子 - 正电子对发射的总能量总是小于中微子发射的能量，但对于大能隙参数它们变得相当。
英文摘要：
Following the previous wor k[1] here we consider early thermal evolution of hot strange stars made of color superconducting quarks in two different pairing states: two-flavor color superconductor (2SC) and color-flavor-locked (CFL) phases, taking into account cooling by neutrinos and electron-positron pair creation due to the Schwinger process. We show that Schwinger luminosity in the electrosphere is a universal function of temperature, independent of quark matter phase for quark chemical potential $μ_q>280$ MeV. The surface of a strange star in all the cases cools faster than its interior. This leads to a fast decrease of pair luminosity with time, so that it does not exceed $10^{46}$ erg/s at 1 second after strange star formation. Neutrino luminosity dominates over pair luminosity in all the cases except for the CFL phase with a large gap parameter $Δ>60$ MeV, where there is a strong suppression of neutrino emission. The total energy emitted in electron-positron pairs is always smaller than the energy emitted in neutrinos, but they become comparable for the large gap parameter.
