具有自旋张开角关联的脉冲星双星双折射率
Pulsar Binary Birthrates with Spin-Opening Angle Correlations
摘要：
脉冲星双星的经验出生率估计取决于脉冲星光束对向的天空比例：脉冲星光束比例。这个比例取决于脉冲星的张角和它的自旋轴和磁轴之间的失准角。以前的估计仅使用两个卫星的平均值，即PSR B1913+16和B1534+12。我们探讨出生率的预测取决于假设的开放角度和对齐，使用的激励分布定义一个有效的光束校正因子，f_{b,eff}。对于大多数已知的参数，我们期望f_{b,eff}小于6。我们还计算了PSR J 0737 - 3039 A和J1141-6545的f_{b,eff}，将当前可用的约束应用于其梁几何形状。我们对紧PSR-NS双星、宽PSR-NS双星和紧PSR-WD双星的后验出生率预测中位数分别为89/Myr、0.84/Myr和34/Myr。对于自旋周期在10 ms和100 ms之间的卫星，我们在一系列合理的波束校正因子上将我们的后验出生率分布P（R）边缘化。我们的预测是强大的，几个替代失调角分布模型之间的变化不大。[删节]
英文摘要：
Empirical birthrate estimates for pulsar binaries depend on the fraction of sky subtended by the pulsar beam: the pulsar beaming fraction. This fraction depends on both the pulsar's opening angle and the misalignment angle between its spin and magnetic axes. Previous estimates use the average value for only two pulsars, i.e. PSRs B1913+16 and B1534+12. We explore how birthrate predictions depend on assumptions about opening angle and alignment, using empirically-motivated distributions to define an effective beaming correction factor, f_{b,eff}. For most known pulsars, we expect f_{b,eff} to be less than 6. We also calculate f_{b,eff} for PSRs J0737-3039A and J1141-6545, applying the currently available constraints for their beam geometry. Our median posterior birthrate predictions for tight PSR-NS binaries, wide PSR-NS binaries, and tight PSR-WD binaries are 89/Myr, 0.84/Myr, and 34/Myr, respectively. For pulsars with spin period between 10 ms and 100 ms, we marginalized our posterior birthrate distribution P(R) over a range of plausible beaming correction factors. Our predictions are robust, changing little between several alternative misalignment angle distribution models. [ABRIDGED]
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