Pulsar braking indices, glitches and energy dissipation in neutron stars
Pulsar braking indices, glitches and energy dissipation in neutron stars
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DOI：
10.1111/j.1365-2966.2006.10893.x
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发表时间：
2006-08
影响因子：
4.8
通讯作者：
Melek Baykal
中科院分区：
文献类型：
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作者：
Melek Baykal
几乎所有具有异常正�测量(对应于5 10−7范围内的异常制动指数)的脉冲星以及在毛刺或干扰�测量之后的脉冲星，都遵循船帆脉冲星最初记录的？�和毛刺参数之间的定标。负的二阶导数值可以理解为遗漏或仍未解决的故障。根据船帆脉冲星的模型，我们讨论了正负制动指标的毛刺率和先验概率。这一行为支持了中子星地壳和内部超流体组件之间普遍存在的非线性动力学耦合。自旋速率为·�的中子星的动力学能量耗散的隐含下限为·Ediss>；1.7×10−6·EROT。对于作为脉冲星死线以外的旋转磁偶极子而自转的老中子星，估计了由于动力能量耗散而产生的热发光和表面温度。
Almost all pulsars with anomalous positive ¨ � measurements (corresponding to anomalous braking indices in the range 5 10 −7 ) as well as post-glitch or interglitch ¨ � measurements, obey the scaling between ¨ � and glitch parameters originally noted in the Vela pulsar. Negative second derivative values can be understood in terms of glitches that were missed or remained unresolved. We discuss the glitch rates and a priori probabilities of positive and negative braking indices according to the model developed for the Vela pulsar. This behaviour supports the universal occurrence of a non-linear dynamical coupling between the neutron star crust and an interior superfluid component. The implied lower limit to dynamical energy dissipation in a neutron star with spindown rate ˙ � is ˙ Ediss > 1.7× 10 −6 ˙ Erot. Thermal luminosities and surface temperatures due to dynamical energy dissipation are estimated for old neutron stars which are spinning down as rotating magnetic dipoles beyond the pulsar death line.