The Infrared to Gamma-Ray Pulse Shape of the Crab Nebula Pulsar
The Infrared to Gamma-Ray Pulse Shape of the Crab Nebula Pulsar
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DOI：
10.1086/303616
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发表时间：
1996-07
期刊：
影响因子：
--
通讯作者：
S. Eikenberry;G. Fazio
中科院分区：
文献类型：
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作者：
S. Eikenberry;G. Fazio
我们分析了蟹状星云脉冲星在近红外，光学，紫外，X射线和γ射线波段的脉冲形状，包括以前未发表的ROSAT HRI脉冲轮廓。我们发现，除了先前已知的趋势的能量密度的桥梁和峰2增加与能量相对于峰1的能量密度，有一个小的，但统计上显着的趋势，都减少与能量相对于峰1在近红外范围。我们发现，脉冲轮廓的两个峰值之间的相位分离作为能量的函数在七十年的能量几乎连续地减小。我们发现，峰的半峰全宽在这个能量范围内是显着可变的，但没有任何明确的模式的可变性。我们发现，Eikenberry等人发现的两个峰的半高处的前缘和后缘半宽的能量依赖性之间的差异。也继续超过70年的能量。我们发现，峰2的尖形反转红外/光学和X射线/γ射线带之间的方向，而峰1的尖形显示X射线和γ射线带之间的反转方向的弱证据。最后，我们发现，许多脉冲形状参数显示在0.5-1 eV的能量的最大值或最小值，这意味着一个重要的变化发生在脉冲星的发射在这个能量附近。这些复杂的现象中有许多是目前的脉冲星发射模型无法预测的，这为这种模型的发展提出了新的挑战。
We analyze the pulse shape of the Crab Nebula pulsar in the near-infrared, optical, ultraviolet, X-ray, and γ-ray bands, including a previously unpublished ROSAT HRI pulse profile. We show that, in addition to the previously known trend for the fluences of the bridge and peak 2 to increase with energy relative to the fluence of peak 1, there is a small but statistically significant trend for both to decrease with energy relative to peak 1 over the near-infrared range. We find that the phase separation between the two peaks of the pulse profile decreases nearly continuously as a function of energy over seven decades of energy. We show that the peaks' full widths at half-maximum are significantly variable over this energy range, but without any clear pattern to the variability. We find that the differences between the energy dependences of the leading and trailing edge half-widths at half-maximum of both peaks found by Eikenberry et al. also continue over seven decades of energy. We show that the cusped shape of peak 2 reverses direction between the infrared/optical and X-ray/γ-ray bands, while the cusped shape of peak 1 shows weak evidence of reversing direction between the X-ray and γ-ray bands. Finally, we find that many of the pulse shape parameters show maxima or minima at energies of 0.5-1 eV, implying that an important change in the pulsar emission is occurring near this energy. Many of these complex phenomena are not predicted by current pulsar emission models, and offer new challenges for the development of such models.