论文标题
制定缓慢旋转中子星的R模式问题
Formulating the r-mode problem for slowly rotating neutron stars
论文作者
论文摘要
我们回顾了分层恒星中惯性R模型的问题，借鉴了成熟中子恒星中组成分层的更精确描述。结果突出了传统的问题方法的问题，使我们重新考虑了非野星中子星的R模型的计算策略。我们概述了处理问题的两种策略。对于中度至缓慢旋转的中子星，唯一可行的替代方法可能是从一开始就以数字解决问题，而有意义的慢旋转计算可以针对已知最快的旋转恒星进行（这可能接近通过重力波排放的驱动不稳定）。我们证明了后一种方法导致问题与正压惯性模式结束但不完全相同。我们还建议，对问题的这些重新构建可能会解决与旋转相对论中子恒星共旋转点相关的奇异行为的长期问题。为了指导未来的重力波搜索，需要解决此问题。
We revisit the problem of inertial r-modes in stratified stars, drawing on a more precise description of the composition stratification in a mature neutron star. The results highlight issues with the traditional approach to the problem, leading us to rethink the computational strategy for r-modes of non-barotropic neutron stars. We outline two strategies for dealing with the problem. For moderate to slowly rotating neutron stars the only viable alternative may be to approach the problem numerically from the outset, while a meaningful slow-rotation calculation can be carried out for the fastest known spinning stars (which may be close to being driven unstable by the emission of gravitational waves). We demonstrate that the latter approach leads to a problem close, but not identical, to that for barotropic inertial modes. We also suggest that these reformulations of the problem likely resolve the long-standing problem of singular behaviour associated with a co-rotation point in rotating relativistic neutron stars. This issue needs to be resolved in order to guide future gravitational-wave searches.
