AI 中文总结
本文基于Hartle-Thorne度规计算致密星吸积能量，发现转动修正和参考系拖拽效应有限，并推导出与物态无关的表达式，结果与现有估计偏差显著。
AI 中文摘要
我们计算了物质从薄吸积盘内边缘落到致密星上时，通过吸积过程获得的能量。我们采用基于Hartle-Thorne度规的受控慢转动展开方法，发现对于中子星，通常只有描述参考系拖拽的度规的领头阶转动修正才是显著的。然而，对于磁化中子星的吸积，当吸积盘大致延伸到共转半径时，即使参考系拖拽效应也较小。基于一般守恒定律，我们推导出简单的、与物态方程无关的自转加速和加热能量的表达式，一致地包含了相关的转动、相对论和核效应，并发现对于观测到的吸积毫秒源，这些结果可能与目前使用的估计值存在显著偏差。
英文摘要
We compute the energy gained by accretion onto a compact star due to matter falling from the inner edge of a thin accretion disk. We employ a controlled slow-rotation expansion based on the Hartle-Thorne metric and find that in neutron stars in general only leading order rotational corrections to the metric, describing frame dragging, are sizable. However, for accretion onto a magnetized neutron star, where the disk roughly extends to the co-rotation radius, even frame dragging effects are minor. Based on general conservation laws we then derive simple, equation-of-state-independent expressions for the spin-up and heating energy, consistently including the relevant rotational, relativistic and nuclear effects, and find that in observed accreting millisecond sources the results can strongly deviate from presently employed estimates.
Comments11 pages, 8 figures
