论文标题
缓慢旋转的，分层的中子星的R模式
The r-modes of slowly rotating, stratified neutron stars
论文作者
论文摘要
唯一在全球型，旋转，牛顿恒星中存在的R模式是基本的$ l = | m | $ solutions，其中$ l $和$ m $是描述该模式的角度依赖性的球形谐波$ y_l^m $的索引。这与恒星模型形成鲜明对比，该模型在其整个内部都非 - 脑部的模型，该模型托有所有$ l \ geq | m | $扰动，包括径向泛滥。实际上，中子恒星用局部正压区域进行了分层。因此，我们探讨了分层如何改变恒星支持R模型的能力。我们考虑了全局分层的情况，并随着恒星接近压缩性的方式检查模式的行为。在此限制下，我们发现除了基本$ L = | M | $扰动之外，其他所有内容都会改变字符并成为通用惯性模式。将分析限制在$ L = | M | $扰动中，我们开发了R模式方程，以考虑显示出局部正交性的出色模型。我们对此类模型的结果表明，R模式泛音差异并连接惯性模式。为了查看哪种R模式持续存在并保留其特征在逼真的中子星中，这些计算将需要完全相对。
The only r-modes that exist in a globally barotropic, rotating, Newtonian star are the fundamental $l = |m|$ solutions, where $l$ and $m$ are the indices of the spherical harmonic $Y_l^m$ that describe the mode's angular dependence. This is in stark contrast to a stellar model that is non-barotropic throughout its interior, which hosts all the $l \geq |m|$ perturbations including radial overtones. In reality, neutron stars are stratified with locally barotropic regions. Therefore, we explore how stratification alters a star's ability to support r-modes. We consider the globally stratified case and examine the behaviour of the modes as the star gets close to barotropicity. In this limit, we find that all but the fundamental $l = |m|$ perturbations change character and become generic inertial modes. Restricting the analysis to $l = |m|$ perturbations, we develop the r-mode equations in order to consider stellar models that exhibit local barotropicity. Our results for such models show that the r-mode overtones diverge and join the inertial modes. In order to see which r-modes persist and retain their character in realistic neutron stars, these calculations will need to be brought into full general relativity.
