Rezzolla等人[ApJ 531（2000），L139; Phys. Rev. D 64（2001），104013; Phys. Rev. D 64（2001），104014]将注意力集中在与r模相关的二阶长期漂移上，并声称它会导致磁场增强和磁化中子星中r模不稳定性的抑制。我们批判性地修正了这些结果。我们提出了一个特殊的二阶r-模式的解决方案与消失的长期漂移，从而驳斥了一个广泛认为的声明，长期漂移是一个不可避免的功能的r-模式。如果$B\ll B_{\mathrm{crit}}\approx 10^{17}\,(ν/600\,\mathrm{Hz})$ G（$ν$是自旋频率），则该非漂移解不受磁场$B$的影响，并且不导致磁场的长期演化。对于一般的二阶r模解，漂移不一定为零，但可以表示为两个解的叠加：一个描述非振荡星的微分转动演化（描述长期漂移;对于非磁化星，它是圆柱上分层的任意定常旋转;磁化星的微分自转在Alfvén时间尺度上演化，并可能导致磁能增强），另一种是上述的非漂移r模解。这种表示使我们能够得出结论，磁场能量的增强受到差分旋转的初始能量的限制，该初始能量比r模式的总能量小得多（对于因子$\propto α^2$，其中$α$是模式振幅）。因此，由漂移引起的磁场增强不能抑制r模式不稳定性。结果可以推广到任何介质中的任何振荡模式，如果该模式具有$B=0$的非漂移解。
英文摘要：
Rezzolla et al. [ApJ 531 (2000), L139; Phys. Rev. D 64 (2001), 104013; Phys. Rev. D 64 (2001), 104014] draw attention to the second order secular drift associated with r-modes and claimed that it should lead to magnetic field enhancement and suppression of r-mode instability in magnetized neutron stars. We critically revise these results. We present a particular second order r-mode solution with vanishing secular drift, thus refuting a widely believed statement that secular drift is an unavoidable feature of r-modes. This non-drifting solution is not affected by magnetic field $B$, if $B\ll B_{\mathrm{crit}}\approx 10^{17}\,(ν/600\,\mathrm{Hz})$ G ($ν$ is a spin frequency) and does not lead to secular evolution of magnetic field. For general second order r-mode solution the drift does not necessarily vanish, but the solution can be presented as a superposition of two solutions: one describes evolution of differential rotation in nonoscillating star (which describes secular drift; for nonmagnetized star it is arbitrary stationary rotation stratified on cylinders; for magnetized star differential rotation evolves on the Alfvén timescale and may lead to magnetic energy enhancement), and another one is non-drifting r-mode solution mentioned above. This representation allows us to conclude that enhancement of magnetic field energy is limited by initial energy of differential rotation, which is much less (for a factor $\propto α^2$, where $α$ is mode amplitude) than the total energy of r-mode. Hence, magnetic field enhancement by drift cannot suppress r-mode instability. Results can be generalized for any oscillation mode in any medium, if this mode has non-drifting solution for $B=0$.
Explaining the thermal emission of old neutron stars with rotochemical heating and magnetized superconducting protons
Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学）；Universidad Metropolitana de Ciencias de la Educación（教育与科学都市大学）；Institut de Recherche en Astrophysique et Planétologie (IRAP)（天体物理学与行星学研究所在）；Indiana University（印第安纳大学）
Relativistic Mean-Field Treatment of Pulsar Kick from Neutrino Propagation in Magnetized Proto-Neutron
本文用微扰法计算了在强磁场作用下，热而致密的超声波中子星物质中中微子的散射和吸收。我们在完全相对论平均场论中计算了吸收截面。我们发现中微子的吸收强度存在显著的角度依赖性，即在平行于磁场的方向上减弱，而在相反的方向上增强。对于2 x 10^{17} G的内部磁场，中微子吸收的这种不对称性估计高达整个中微子动量的2.2%。与这种不对称性相关联的脉冲星反冲速度被证明是可比的观察到的速度。
