发表机构
Institute of Physics, National Academy of Sciences of Belarus; ICRANet; ICRANet-Minsk, Institute of Physics, National Academy of Sciences of Belarus（白俄罗斯国家科学院物理研究所; 国际相对论天体物理中心; 明斯克国际相对论天体物理中心，白俄罗斯国家科学院物理研究所）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文发现新生夸克星的电磁辐射主要来自电子层（等离子体频率约40 keV），而非被抑制的夸克等离子体；冷却经历两个阶段：光球层黑体辐射（温度从几MeV降至22 keV）和40 keV窄谱特征，可被X射线天文台探测。
AI 中文摘要
长期以来人们认为新生夸克星是低效的辐射体，因为夸克等离子体频率极高，抑制了从整个频谱到几十MeV能量的电磁辐射。本文表明，显著的电磁辐射反而可以来自夸克星的电子层（electrosphere），那里的等离子体频率低得多，约为40 keV。因此，新生夸克星的冷却预计会经历两个截然不同的观测阶段。在第一阶段，黑体辐射来自电子层附近产生的光学厚相对论性风的光球层。在恒星形成后的几天内，光球层温度从几MeV降至约22 keV。在第二阶段，黑体谱演化为以40 keV为中心的窄特征，辐射逐渐减弱。这种谱演化提供了围绕致密天体物理对象的电子层的特征信号，并可能被当前或未来的X射线天文台探测到。
英文摘要
It has long been believed that newborn quark stars are inefficient emitters because the quark plasma frequency is so high that it suppresses electromagnetic radiation across the entire spectrum up to energies of several tens of MeV. Here, we show that significant electromagnetic emission can instead originate from the electrosphere of a quark star, where the plasma frequency is much lower, approximately 40 keV. As a result, the cooling of a newborn quark star is expected to proceed through two distinct observational epochs. During the first epoch, blackbody radiation is emitted from the photosphere of an optically thick relativistic wind generated near the electrosphere. Over the course of a few days following the star's formation, the photospheric temperature decreases from several MeV to about 22 keV. During the second epoch, the blackbody spectrum evolves into a narrow feature centered around 40 keV, and the emission gradually fades. This spectral evolution provides a characteristic signature of the electrosphere surrounding compact astrophysical objects and may be detectable with current or future X-ray observatories.
CommentsAccepted as a Letter to Physical Review D
