一种产生宽带脉冲状偏振的新机制
A new mechanism for generating broadband pulsar-like polarization
摘要：
观测数据暗示脉冲星磁层中存在超光速电流。这样的光源与狭义相对论并不矛盾;它们已经在实验室里被创造出来了。在这里，我们描述了旋转超光速源产生的辐射束的独特特征，并表明：（i）它由观测者离源越远越窄的子束组成：其强度随距离（R）衰减为1/R而不是1/R^2的子束，（ii）其子束的场由三种并发偏振模式表征：两个“正交”的模式和其位置角在子波束上摆动的第三模式桥接其他两个模式，（iii）其整个光束由这种相干子光束的非相干叠加组成，并且具有反映源的贡献部分的方位角分布的强度分布，（光源以光速和零加速度接近观察者的部分），（四）光谱（同步加速器光谱的超光速对应物）比任何其他已知的发射都要宽，并且需要其间距和振幅分别随着频率的增加而代数地增加和减少的振荡，以及（v）其平均偏振度和其线偏振的分数都随着频率的增加而增加，超过观察者落在菲涅尔区内的频率。我们还比较了这些功能与从蟹状星云脉冲星接收到的辐射。
英文摘要：
Observational data imply the presence of superluminal electric currents in pulsar magnetospheres. Such sources are not inconsistent with special relativity; they have already been created in the laboratory. Here we describe the distinctive features of the radiation beam that is generated by a rotating superluminal source and show that (i) it consists of subbeams that are narrower the farther the observer is from the source: subbeams whose intensities decay as 1/R instead of 1/R^2 with distance (R), (ii) the fields of its subbeams are characterized by three concurrent polarization modes: two modes that are 'orthogonal' and a third mode whose position angle swings across the subbeam bridging those of the other two, (iii) its overall beam consists of an incoherent superposition of such coherent subbeams and has an intensity profile that reflects the azimuthal distribution of the contributing part of the source (the part of the source that approaches the observer with the speed of light and zero acceleration), (iv) its spectrum (the superluminal counterpart of synchrotron spectrum) is broader than that of any other known emission and entails oscillations whose spacings and amplitudes respectively increase and decrease algebraically with increasing frequency, and (v) the degree of its mean polarization and the fraction of its linear polarization both increase with frequency beyond the frequency for which the observer falls within the Fresnel zone. We also compare these features with those of the radiation received from the Crab pulsar.
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