关于射电望远镜的脉宽统计。I.脉冲间发射的重要性
On the pulse--width statistics in radio pulsars. I. Importance of the interpulse emission
摘要：
我们对脉冲星射电辐射的不同性质进行了蒙特卡罗模拟，如：脉冲星周期、脉冲宽度、倾角和脉冲间辐射（IP）的发生率。我们使用最近可用的脉冲星周期P，脉冲轮廓宽度W和磁倾角α的大数据集。我们还编制了有史以来最大的脉冲间发射脉冲星数据库，分为双极（DP-IP）和单极（SP-IP）情况。它们在P-P点图上的分布强烈地表明了磁轴从最初的随机取向长期排列。利用现有的脉冲星观测数据集（P、W、α和IP）、不同的脉冲星射电束模型rho = rho（P）以及脉冲星周期和倾角的不同试验分布函数，通过Kolmogorov-Smirnov显著性检验，导出了脉冲星重要参数的可能母源分布函数。最适合的母周期分布函数是对数正态分布，但不能排除伽马函数分布。对导出的模型分布函数的最强约束是要求间隔脉冲的数量恰好（在1 σ误差内）处于观察到的发生水平。我们发现，一个合适的模型分布函数的倾角是复杂的三角函数，它有两个局部极大值，一个附近的0度和90度附近的其他。前者和后者意味着正确的IP发生率。脉冲星光束不太可能显著偏离圆形横截面。我们发现，描述脉冲星光束覆盖的整个球体的一部分（也称为聚束部分）的平均聚束因子fb的上限约为10%。这意味着银河系中中子星的数量可能被低估了。
英文摘要：
We performed Monte Carlo simulations of different properties of pulsar radio emission, such as: pulsar periods, pulse-widths, inclination angles and rates of occurrence of interpulse emission (IP). We used recently available large data sets of the pulsar periods P, the pulse profile widths W and the magnetic inclination angle alpha. We also compiled the largest ever database of pulsars with interpulse emission, divided into the double-pole (DP-IP) and the single-pole (SP-IP) cases. Their distribution on the P - Pdot diagram strongly suggests a secular alignment of the magnetic axis from the originally random orientation. We derived possible parent distribution functions of important pulsar parameters by means of the Kolmogorov-Smirnov significance test using the available data sets (P, W, alpha and IP), different models of pulsar radio beam rho = rho(P) as well as different trial distribution functions of pulsar period and the inclination angles. The best suited parent period distribution function is the log-normal distribution, although the gamma function distribution cannot be excluded. The strongest constraint on derived model distribution functions was the requirement that the numbers of interpulses were exactly (within 1sigma errors) at the observed level of occurrences. We found that a suitable model distribution function for the inclination angle is the complicated trigonometric function which has two local maxima, one near 0 deg and the other near 90 deg. The former and the latter implies the right rates of IP occurrence. It is very unlikely that the pulsar beam deviates significantly from the circular cross-section. We found that the upper limit for the average beaming factor fb describing a fraction of the full sphere (called also beaming fraction) covered by a pulsar beam is about 10%. This implies that the number of the neutron stars in the Galaxy might be underestimated.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
