High Time Resolution Infrared Observations of the Crab Nebula Pulsar and the Pulsar Emission Mechanism
High Time Resolution Infrared Observations of the Crab Nebula Pulsar and the Pulsar Emission Mechanism
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蟹状星云脉冲星的高时间分辨率红外观测及脉冲星发射机制
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发表时间：
1997
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通讯作者：
C. Pennypacker
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作者：
S. Eikenberry;G. Fazio;S. Ransom;J. Middleditch;J. Kristian;C. Pennypacker
我们提出了新的，高信噪比的蟹状星云脉冲星的近红外观测使用固态光电倍增管仪器的多镜望远镜。我们的观测覆盖了J（1.25 μm）、H（1.65 μm）和K（2.2 μm）红外波段，时间分辨率为20 μs。加上哈勃太空望远镜高速光度计进行的可见光和紫外线观测，我们有高时间分辨率的观测，覆盖十多个波长。我们提出了在这个波长范围内的脉冲轮廓，我们分析了作为波长的函数的脉冲形状，包括峰到峰的相位分离，峰值半高宽（FWHM），和峰值半高宽（HWHM）。我们还创建了脉冲星发射的相位平均和相位分辨的彩色光谱。我们发现，峰-峰相位分离显示出随波长增加的显着趋势，与脉冲星发射机制的模型大致一致。峰1和2的FWHM也显示出随波长增加的趋势，再次与模型定性一致。然而，峰1和峰2的HWHM在它们的波长依赖性方面从前沿到后沿显示出显著差异。目前的脉冲星发射模型没有预测到这种行为，并且分量HWHM值的不同波长依赖性使人们对FWHM测量的有用性提出了质疑。我们的光谱分析表明，红外-紫外去红的相位平均色谱基本上是平坦的超过十年的频率。这与X射线和γ射线区域形成鲜明对比，在X射线和γ射线区域，光谱急剧下降。峰1和峰2的色谱也基本上是平坦的，但两者的比率显示出与恒定值的统计学显著变化。最后，峰1和峰2的色谱显示从前缘到后缘的显著差异。与HWHM一样，目前的脉冲星发射模型无法预测这种行为。
We present new, high signal-to-noise near-infrared observations of the Crab Nebula pulsar using the Solid State Photomultiplier instrument on the Multiple Mirror Telescope. Our observations cover the J (1.25 μm), H (1.65 μm), and K (2.2 μm) infrared wavebands and have 20 μs time resolution. Together with visible and UV observations made by the Hubble Space Telescope High-Speed Photometer, we have high time resolution observations covering over a decade in wavelength. We present the pulse profiles over this wavelength range, and we analyze the pulse shape as a function of wavelength, including the peak-to-peak phase separation, the peak full width half-maxima (FWHM), and the peak half-width half-maxima (HWHM). We also create both phase-averaged and phase-resolved color spectra of the pulsar emission. We find that the peak-to-peak phase separation shows a significant trend for an increase with wavelength, in rough agreement with models of the pulsar emission mechanism. The FWHM for peaks 1 and 2 also show a trend for increase with wavelength, again in qualitative agreement with the models. However, the HWHM for peaks 1 and 2 show significant differences in their wavelength dependences from the leading to trailing edges. This behavior is not predicted by current pulsar emission models, and the different wavelength dependences of the component HWHM values call into question the usefulness of FWHM measurements. Our spectral analyses show that the IR-UV dereddened phase-averaged color spectrum is essentially flat over more than a decade in frequency. This is in clear contrast to the X-ray and γ-ray regimes, where the spectrum is falling steeply. The color spectra of peaks 1 and 2 are also essentially flat, but the ratio of the two shows statistically significant variations from a constant value. Finally, the color spectra of peaks 1 and 2 show significant differences from the leading to trailing edges. As with the HWHM, this behavior is not predicted by current pulsar emission models.