Rezzolla L, Lamb FK, Shapiro SL
Astrophys J. 2000 Mar 10;531(2):L139-L142. doi: 10.1086/312539.
We show that r-mode oscillations distort the magnetic fields of neutron stars and that their occurrence is likely to be limited by this interaction. If the field is greater, similar1016(Omega/OmegaB) G, where Omega and OmegaB are the angular velocities of the star and at which mass shedding occurs, r-mode oscillations cannot occur. Much weaker fields will prevent gravitational radiation from exciting r-mode oscillations or will damp them on a relatively short timescale by extracting energy from the modes faster than gravitational-wave emission can pump energy into them. For example, a 1010 G poloidal magnetic field that threads the star's superconducting core is likely to prevent the l=2 mode from being excited unless Omega exceeds 0.35OmegaB. If Omega is larger than 0.35OmegaB initially, the l=2 mode may be excited but is likely to decay rapidly once Omega falls below 0.35OmegaB, which happens in less, similar15 days if the saturation amplitude is greater, similar0.1. The r-mode oscillations may play an important role in determining the structure of neutron star magnetic fields.
我们表明，r模振荡会使中子星的磁场发生畸变，并且其出现可能受这种相互作用的限制。如果磁场更强，类似10^16（Ω/ΩB）高斯，其中Ω和ΩB分别是恒星的角速度以及发生质量损失时的角速度，r模振荡就不会发生。弱得多的磁场会阻止引力辐射激发r模振荡，或者会通过比引力波发射向其注入能量更快地从这些模式中提取能量，从而在相对较短的时间尺度上使其衰减。例如，贯穿恒星超导核心的10^10高斯极向磁场很可能会阻止l = 2模式被激发，除非Ω超过0.35ΩB。如果Ω最初大于0.35ΩB，l = 2模式可能会被激发，但一旦Ω降至0.35ΩB以下，它很可能会迅速衰减，如果饱和振幅更大，类似0.1，这种情况会在不到约15天内发生。r模振荡可能在确定中子星磁场结构方面发挥重要作用。
