非偶极磁场和中子星进动对脉冲星制动指标的影响
The influence of nondipolar magnetic field and neutron star precession on braking indexes of radiopulsars
摘要：
某些脉冲星的制动指数值$n = Ω\ddotΩ / \dotΩ^2 \sim \pm (10^3 ÷10^4) $异常。结果表明，这些值可能与非偶极磁场有关。中子星的进动导致角速度矢量$\vecΩ$沿中子星磁偶极矩$\vec{m}$方向以角速度$\vecΩ_{p}$旋转（在与中子星相关的参考系中）。该过程可引起通过内部间隙的电流的改变，并因此引起具有与进动周期$T_{p} = 2π/ Ω_{p}$相同的时间尺度的电流损耗。这是由于内隙中的电流由Goldreich-Julian电荷密度$ρ_{GJ} = -\frac{\vecΩ \cdot \vec{B}}{2πc}$决定的，而电荷密度$ρ_{GJ} = -\frac{\vecΩ \cdot \vec{B}}{2πc}$取决于小尺度磁场方向与角速度$\vecΩ$之间的夹角。中子星表面附近的脉冲星管是弯曲的。在目前的文件中，它被认为是唯一的内部间隙与稳定的，电子电荷限制流制度。
英文摘要：
Some of radiopulsars have anomalous braking index values $n = Ω\ddotΩ / \dotΩ^2 \sim \pm (10^3 ÷10^4) $. It is shown that such values may be related with nondipolar magnetic field. The precession of neutron star lead to rotation (in reference frame related with neutron star) of vector of angular velocity $\vecΩ$ along direction of neutron star magnetic dipole moment $\vec{m}$ with angular velocity $\vecΩ_{p}$. This process may cause the altering of electric current flow through inner gap and consequently the current losses with the same time scale as precession period $T_{p} = 2π/ Ω_{p}$. It occurs because of electric current in inner gaps is determined by Goldreich-Julian charge density $ρ_{GJ} = -\frac{\vecΩ \cdot \vec{B}}{2πc}$, which are depend on angle between direction of small scale magnetic field and angular velocity $\vecΩ$. It is essential that pulsar tubes nearby neutron star surface are curved. In current paper it is considered the only inner gaps with steady, electron charge limited flow regime.
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