带自转的I型X射线暴模型
Type I X-Ray Burst Models With Rotation
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中文总结 AI 辅助
本文首次揭示自转是塑造快速旋转系统I型X射线暴特性的关键因素，离心力与自转诱导混合机制会改变爆发的复发时间、能量及光变曲线形态，为相关研究提供了新的关键影响因素。
中文摘要 AI 辅助
I型X射线暴由密近双星系统中吸积中子星表面的不稳定热核燃烧提供能量，这类短暂的X射线闪发光变曲线具有1-10秒的上升时间、10-100秒的持续时间，以及数小时至数天的复发周期，是银河系中最频繁的恒星爆发事件，典型能量约为10^39-10^40erg，属于超新星和经典新星之后最强大的天文瞬变事件。迄今为止，银河系中已确认约120个爆发X射线双星，已有多项研究针对这类事件的动力学展开，重点是重现观测到的复发周期和光变曲线形状。本文首次表明，自转是塑造快速旋转系统中I型X射线暴特性的关键因素；离心力与经向环流、剪切诱导湍流扩散等一系列自转诱导混合机制的加入，会降低表面重力，缩短复发时间并降低爆发能量；自转还会改变这类事件中核活动的范围，影响光变曲线的形态，快速旋转中子星的光变曲线明显更宽。
英文摘要
Type I X-ray bursts are powered by unstable thermonuclear burning on the surface of accreting neutron stars in close binary systems. These brief X-ray flashes, with light curves featuring rise times of $1-10$ s, durations of $10-100$ s, and recurrence periods of hours to days, represent the most frequent stellar explosions in our Galaxy. With typical energies of $\sim 10^{39}-10^{40}$ erg, they rank among the most powerful astrophysical transients after supernovae and classical novae. To date, roughly 120 bursting X-ray binaries have been identified in the Milky Way. Several studies have been conducted to characterize the dynamics of these events, with emphasis on reproducing the observed recurrence periods and light curve shapes. In this paper we show, for the first time, that rotation is a key factor shaping the properties of Type I X-ray bursts in rapidly spinning systems. The inclusion of centrifugal forces, together with a suite of rotationally-induced mixing mechanisms, such as meridional circulation and shear-induced turbulent diffusion, reduce surface gravity, shortening the recurrence times and lowering burst energies. Rotation also modifies the extent of the nuclear activity during these events and affects the morphology of their light curves, which are distinctly broader for rapidly rotating neutron stars.
