On the energetics and number of gamma-ray pulsars
On the energetics and number of gamma-ray pulsars
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DOI：
10.1086/187166
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发表时间：
1994-01
期刊：
影响因子：
--
通讯作者：
C. Dermer;S. Sturner
中科院分区：
文献类型：
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作者：
C. Dermer;S. Sturner
为了解释已知伽玛射线脉冲星的能量学和数量，我们研究了一个具有极盖加速度的近对准脉冲星模型。在该模型中，自旋下光度转换为伽马射线光度的效率随着自旋下光度的降低而增加，这是Ulmer最近强调的趋势。预测的伽马射线通量与点P(exp 3/4)/P(exp 5/4) d（exp 2）成正比，其中P为周期，点P为周期导数，d为到脉冲星的距离。对于初始自旋周期约为10 ~ 30ms，中子星极磁场约为1 ~ 4tg，该模型解释了已观测到的发射能量大于100 MeV的伽马射线的5颗脉冲星的数量和年龄分布。考虑了脉冲星研究的意义。
We examine a nearly aligned pulsar model with polar cap acceleration in order to explain the energetics and number of the known gamma-ray pulsars. In this model, the efficiency of converting spin-down luminosity to gamma-ray luminosity increases with decreasing spin-down luminosity, a trend recently emphasized by Ulmer. The predicted gamma-ray flux is proportional to dot P(exp 3/4)/P(exp 5/4) d(exp 2), where P is the period, dot P is the period derivative, and d is the distance to the pulsar. For initial spin periods between approximately equals 10 and 30 ms and neutron star polar magnetic fields between approximately equals 1 and 4 TG, this model accounts for the number and age distribution of the five pulsars which have been observed to emit gamma rays at energies greater than 100 MeV. Implications for pulsar studies are considered.