论文标题
部分可观测时空混沌系统的无模型预测
Radio Pulsar Beam Geometry at Lower Frequencies: Bright Sources Outside the Arecibo Sky
论文作者
论文摘要
我们提出脉冲星的发射光束分析和模型，以便在最低频率散射允许的情况下检查脉冲星的几何形状和物理。我们考虑了两名属于Arecibo Sky外面的知识良好的脉冲星人群，这是Jodrell Bank Bank Gould＆Lyne的第一张绘图，调查降至-35°，第二次使用Parkes Surveys在远南进行。这些汇集了1990年代后期众所周知的487个脉冲星的全天空种群，它们都以“ B”名称。我们充分利用核心/双锥发射光束模型来评估其在较低频率下的疗效，并概述了不同的配对等离子源的有效性。分析表明，除了极少数例外，脉冲星射击束可以用两个同心圆锥梁和1 GHz处的常规角度尺寸进行定量建模。此外，较低频率的光束形式在大小上逐渐变化，但在配置上没有变化。 Pulsar发射光束性能强烈划分的，具体取决于等离子体激发在极性Fluxtube内的中心是沿产生圆锥形束的边缘产生核心束或外围的，这似乎在很大程度上取决于其Spindown能量是否大于或少于10 $^{32.5} $ ERGS/s。核心发射统治的脉冲星倾向于沿银河平面和银河中心的方向紧密浓缩。而圆锥形脉冲星在银河经度和纬度上的分布更加均匀。核心主导的脉冲星也往往更遥远，尤其是在内星系区域。
We present pulsar emission beam analyses and models in an effort to examine pulsar geometry and physics at the lowest frequencies scattering permits. We consider two populations of well-studied pulsars that lie outside the Arecibo sky, the first drawing on the Jodrell Bank Gould & Lyne survey down to -35° declination and a second using Parkes surveys in the far south. These assemble the full sky population of 487 pulsars known before the late 1990s which conveniently all have "B" names. We make full use of the core/double-cone emission beam model to assess its efficacy at lower frequencies, and we outline how different pair plasma sources probably underlie its validity. The analysis shows that with a very few exceptions pulsar radio emission beams can be modeled quantitatively with two concentric conal beams and a core beam of regular angular dimensions at 1 GHz. Further, the beamforms at lower frequencies change progressively in size but not in configuration. Pulsar emission-beam properties divide strongly depending on whether the plasma excitation is central within the polar fluxtube producing a core beam or peripheral along the edges generating conal beams, and this seems largely determined by whether their spindown energy is greater or less than about 10$^{32.5}$ ergs/s. Core emission dominated pulsars tend concentrate closely along the Galactic plane and in the direction of the Galactic center; whereas conal pulsars are somewhat more uniformly distributed both in Galactic longitude and latitude. Core dominated pulsars also tend to be more distant and particularly so in the inner Galaxy region.
