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Phase-Resolved Studies of the High-Energy Gamma-Ray Emission from the Crab, Geminga, and Vela Pulsars

机译:来自螃蟹,双子座和Vela脉冲星的高能伽马射线发射的相位分辨研究

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摘要

Using the first three and a half years of observations from the Energetic Gamma Ray Telescope (EGRET) on board the Compton Gamma Ray Observatory (CGRO), phase-resolved analyses are performed on the emission from the three brightest high-energy gamma-ray pulsars, Crab, Geminga, and Vela. For each pulsar, it is found that there is detectable high-energy gamma-ray emission above the galactic diffuse background throughout much of the pulsar rotation cycle. A hardness ratio is introduced to characterize the evolution of the spectral index as a function of pulsar phase. While the hardest emission from the Crab and Vela pulsars comes from the bridge region between the two gamma-ray peaks, the hardest emission from Geminga corresponds to the second gamma-ray peak. For all three pulsars, phase-resolved spectra of the pulse profile components reveal that although there is a large variation in the spectral index over the pulsar phase interval, the high-energy spectral turnover, if any, occurs at roughly the same energy in each component. The high-energy gamma-ray emission from the Crab complex appears to include an unpulsed ultra-soft component of spectral index ~ -4.3 which dominates the total emission below 100 MeV. This component is consistent with the expected emission from the tail end of the Crab nebula synchrotron emission.
机译:利用康普顿伽玛射线天文台(CGRO)上的高能伽玛射线望远镜(EGRET)进行的前三年半的观测,对三个最亮的高能伽玛射线脉冲星的发射进行了相分辨分析,螃蟹,Geminga和Vela。对于每个脉冲星,发现在整个脉冲星自转周期的大部分时间内,在银河漫射本底以上都有可检测的高能伽马射线发射。引入硬度比来表征光谱指数随脉冲星相位的变化。来自蟹状脉冲星和维拉脉冲星的最强发射来自两个伽马射线峰之间的桥接区域,而来自盖明加的最硬发射对应于第二个伽马射线峰。对于所有三个脉冲星,脉冲轮廓分量的相分辨谱显示,尽管在脉冲星相间隔上光谱指数有很大变化,但高能谱转换(如果有的话)在每个脉冲中的能量大致相同零件。 Crab配合物的高能伽马射线发射似乎包括光谱指数〜-4.3的无脉冲超软组分,该组分在总能量低于100 MeV时占主导地位。该分量与蟹状星云同步加速器尾部的预期发射一致。

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