射电脉冲星磁层的斯托克斯层析成像。II。毫秒脉冲星
Stokes tomography of radio pulsar magnetospheres. II. Millisecond pulsars
摘要：
毫秒级双星（MSP）的射电偏振特性与非回收双星有很大不同。特别是，许多MSP的位置角（PA）摆动偏离旋转矢量模型预测的S形，即使在相对论像差占，表明它们具有非偶极磁几何形状，可能是由于吸积的历史。斯托克斯层析成像使用斯托克斯参数的相位图作为诊断工具来推断脉冲星的磁几何形状和方向。本文将斯托克斯层析成像技术应用于金属表面微粒，推广了处理脉冲间发射的技术。我们提供了具有电流修改偶极场、填充芯和空心锥束以及两个经验线性极化模型的MSP的斯托克斯相位图和PA摆动的查找表图集。我们比较我们的查找表，从15 MSP的数据，并发现，斯托克斯相位画像的电流修改偶极子近似匹配几个MSP的PA摆动是平坦或不规则的，不能与标准的轴对称旋转矢量模型。PSR J1939+2134和PSR J0437 $-$ 4715详细建模。PSR J1939+2134的0.61GHz数据与发射高度为$r_\text{LC}$、发射高度为$(α, i) = (22 \pm 2^\circ, 80 \pm 1^\circ)$的电流修正偶极子拟合良好。PSR J1939+2134在1.414GHz和PSR J0437 $-$ 4715在1.44GHz的拟合不太准确，表明这些物体可能具有更复杂的磁场几何形状，例如局部表面异常或极磁山。
英文摘要：
The radio polarization characteristics of millisecond pulsars (MSPs) differ significantly from those of non-recycled pulsars. In particular, the position angle (PA) swings of many MSPs deviate from the S-shape predicted by the rotating vector model, even after relativistic aberration is accounted for, indicating that they have non-dipolar magnetic geometries, likely due to a history of accretion. Stokes tomography uses phase portraits of the Stokes parameters as a diagnostic tool to infer a pulsar's magnetic geometry and orientation. This paper applies Stokes tomography to MSPs, generalizing the technique to handle interpulse emission. We present an atlas of look-up tables for the Stokes phase portraits and PA swings of MSPs with current-modified dipole fields, filled core and hollow cone beams, and two empirical linear polarization models. We compare our look-up tables to data from 15 MSPs and find that the Stokes phase portraits for a current-modified dipole approximately match several MSPs whose PA swings are flat or irregular and cannot be reconciled with the standard axisymmetric rotating vector model. PSR J1939+2134 and PSR J0437$-$4715 are modelled in detail. The data from PSR J1939+2134 at 0.61\,GHz can be fitted well with a current-modified dipole at $(α, i) = (22 \pm 2^\circ, 80 \pm 1^\circ)$ and emission altitude 0.4 $r_\text{LC}$. The fit is less accurate for PSR J1939+2134 at 1.414\,GHz, and for PSR J0437$-$4715 at 1.44\,GHz, indicating that these objects may have a more complicated magnetic field geometry, such as a localized surface anomaly or a polar magnetic mountain.
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