Abstract—The distribution of young pulsars in the log(dP/dt)–log(tc) diagram that have a characteristic age tc < ~5 × 10⁶ yr and a period derivative dP/dt > ~10^–16 is analyzed. Six clusters-stripes are revealed for the first time, along which the long-term evolution tracks of individual pulsars pass. The mean track in a stripe corresponds to the long-term regular evolution for a typical pulsar of this stripe. The clusters-stripes population composition is analyzed by object types. Rotating radio transients (RRATs) are present in all clusters-stripes at tc > 10⁵ yr. It turns out that three stripes contain objects of only one of the three numerous (≥10) known types: magnetars, pulsars with a high magnetic field, and Vela-like pulsars. In three other clusters-stripes, objects of the indicated three types are not found. The following object classification in the composition of six clusters-stripes is proposed: magnetars (M), pulsars with a high magnetic field (HB), pulsars with a sub-high magnetic field (S-HB), Vela-type pulsars (V), sub-Vela pulsars (SV), and low magnetic field pulsars (LB). Four pulsars that are outside the stripes are referred to peculiar. Analytical formulas are presented for calculating evolution parameters in the log(dP/dt)–log(tc) diagram. As a result of the optimal fitting of the mean clusters-stripes track by the appropriate empirical function, long-term regular values of the braking index and the second derivative of the period are estimated for 327 pulsars for the first time. As a consequence of the clusters-stripes presence, the “striped” distribution of the dipole magnetic field at pulsar birth indicates the intervality in the mass distribution of pulsar progenitor stars. The recent supernovae explosion models (Pejcha & Thomson, 2015) also produce an interval mass distribution of progenitors generating neutron stars, which confirm that pulsar clusters-stripes do exist and their origin can be naturally explained.

摘要—分析了具有年龄tc < 〜5 ×10 ⁶ yr和周期导数dP / dt >〜10 ^–16的log（dP / dt）-log（tc）图中的年轻脉冲星的分布。首次揭示了六个星团-条带，各个脉冲星的长期演化轨迹都沿着该星团通过。条纹中的平均轨迹对应于该条纹的典型脉冲星的长期规则演化。通过对象类型分析群集-条纹种群组成。在tc > 10 ^5时所有簇-条纹中都存在旋转无线电瞬变（RRAT）年。事实证明，三个条纹仅包含三种已知（≥10）已知类型中的一种的物体：磁星，具有强磁场的脉冲星和类似Vela的脉冲星。在其他三个群集条纹中，找不到指定的三种类型的对象。提出了六个簇-条纹组成的目标分类：磁星（M），具有高磁场（HB）的脉冲星，具有亚高磁场的脉冲星（S-HB），Vela型脉冲星（V ），亚Vela脉冲星（SV）和低磁场脉冲星（LB）。条纹之外的四个脉冲星称为奇异脉冲星。给出了用于计算log（dP / dt）–log（tc）中的演化参数的解析公式）图。由于通过适当的经验函数对平均簇-条纹轨迹进行了最佳拟合，首次为327个脉冲星估算了制动指数的长期规则值和该周期的二阶导数。由于存在簇条纹，脉冲星诞生时偶极子磁场的“条纹”分布表明脉冲星祖星质量分布的间隔。最近的超新星爆炸模型（Pejcha＆Thomson，2015）还产生了产生中子星的前体的间歇质量分布，这证实了脉冲星团-条纹的确存在并且其起源可以自然解释。