9个宽带射电星多波长观测与超光速旋转分布型扩展流发射光谱的比较
Comparison of multiwavelength observations of 9 broad-band pulsars with the spectrum of the emission from an extended current with a superluminally rotating distribution pattern
摘要：
本文报道了9颗具有射电至$X$或$γ$射线波段多波长数据的恒星的观测光谱（蟹、船帆座、Geminga、B 0656 +14、B1055-52、B1509-58、B1706-44、B1929+10、和B1951+32）与由扩展的偏振电流产生的辐射的光谱进行比较，扩展的偏振电流的分布图案旋转得比光快（真空中的\it}。结果表明，通过从观测资料中推断两个自由参数的值，（与常规脉冲星磁层中的等离子体频率和电子回旋频率的值一致的值），并且通过调整描述各个频带中的源谱的幂律的谱指数，我们可以用一个单一的发射过程来定量地计算每个脉冲星整个光谱的{ \em}。这种发射过程（同步加速器-谢连科夫过程在真空中的体积分布源的推广）产生振荡辐射光谱。因此，脉冲星光谱在紫外或$X$射线波段（通常被解释为热辐射的表现）的钟形峰在本模型中表现为构成蟹状星云脉冲星射电光谱中观测到的发射波段的相同振荡的高频最大值。同样地，在$10^{18}-10^{21}$ Hz附近，光谱的梯度突然变陡-1，这似乎是脉冲星辐射的一个普遍特征：这个特征反映了观测者的位置在频率相关的瑞利距离上的转变。此外，本模型的自由参数的推断值表明，脉冲星的旋转频率越低，观测到的光谱强度越向高频加权。
英文摘要：
The observed spectra of 9 pulsars for which multiwavelength data are available from radio to $X$- or $γ$-ray bands (Crab, Vela, Geminga, B0656+14, B1055-52, B1509-58, B1706-44, B1929+10, and B1951+32) are compared with the spectrum of the radiation generated by an extended polarization current whose distribution pattern rotates faster than light {\it in vacuo}. It is shown that by inferring the values of two free parameters from observational data (values that are consistent with those of plasma frequency and electron cyclotron frequency in a conventional pulsar magnetosphere), and by adjusting the spectral indices of the power laws describing the source spectrum in various frequency bands, one can account {\em quantitatively} for the entire spectrum of each pulsar in terms of a single emission process. This emission process (a generalization of the synchrotron-Ćerenkov process to a volume-distributed source in vacuum) gives rise to an oscillatory radiation spectrum. Thus, the bell-shaped peaks of pulsar spectra in the ultraviolet or $X$-ray bands (the features that are normally interpreted as manifestations of thermal radiation) appear in the present model as higher-frequency maxima of the same oscillations that constitute the emission bands observed in the radio spectrum of the Crab pulsar. Likewise, the sudden steepening of the gradient of the spectrum by -1, which occurs around $10^{18}-10^{21}$ Hz, appears as a universal feature of the pulsar emission: a feature that reflects the transit of the position of the observer across the frequency-dependent Rayleigh distance. Inferred values of the free parameters of the present model suggest, moreover, that the lower the rotation frequency of a pulsar, the more weighted towards higher frequencies will be its observed spectral intensity.
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