THE GALACTIC POPULATION OF YOUNG γ-RAY PULSARS
THE GALACTIC POPULATION OF YOUNG γ-RAY PULSARS
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DOI：
10.1088/0004-637x/727/2/123
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发表时间：
2010-09
期刊：
影响因子：
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通讯作者：
K. Watters;R. Romani
中科院分区：
文献类型：
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作者：
K. Watters;R. Romani
我们已经模拟了银河系的年轻恒星人口，并与费米LAT样本进行了比较，限制了这些自旋动力物体的出生特性，光束和演化。利用与观测到的自旋和脉冲特性分布相一致的定量测试，我们发现，短诞生周期P0 ≤ 50 ms和γ射线束产生于外磁层，由单极主导，是强烈的首选。模拟的无线电探测和无线电安静的对象的相对数量与数据吻合得很好。虽然样本是局部的，但外推到整个银河系意味着γ射线脉冲星的出生率为1/（59年）。这被证明是在很好的协议与估计的银河系核心崩溃率和本地密度的OB星星的祖先。如果费米LAT观测持续10年，我们给出了预期的年轻脉冲星探测的数量的预测。相对于未分辨的毫秒双星的潜在重要贡献，我们发现年轻的双星对银河系γ射线背景的贡献很小。
We have simulated a Galactic population of young pulsars and compared with the Fermi LAT sample, constraining the birth properties, beaming and evolution of these spin-powered objects. Using quantitative tests of agreement with the distributions of observed spin and pulse properties, we find that short birth periods P0 ≈ 50 ms and γ-ray beams arising in the outer magnetosphere, dominated by a single pole, are strongly preferred. The modeled relative numbers of radio-detected and radio-quiet objects agrees well with the data. Although the sample is local, extrapolation to the full Galaxy implies a γ-ray pulsar birthrate 1/(59 yr). This is shown to be in good agreement with the estimated Galactic core collapse rate and with the local density of OB star progenitors. We give predictions for the numbers of expected young pulsar detections if Fermi LAT observations continue 10 years. In contrast to the potentially significant contribution of unresolved millisecond pulsars, we find that young pulsars should contribute little to the Galactic γ-ray background.