The properties of the young pulsars and their relations to the supernova remnants (SNRs) have been the interesting topics. At present, 383 SNRs in the Milky Way Galaxy have been published, which are associated with 64 radio pulsars and 46 pulsars with high-energy emissions. However, we noticed that 630 young radio pulsars with the spin periods of less than half a second have been not yet observed the SNRs surrounding or nearby them, which arises a question of that could the two types of young radio pulsars with/without SNRs hold the distinctive characteristics? Here, we employ the statistical tests on the two groups of young radio pulsars with (52) and without (630) SNRs to reveal if they share the different origins. Kolmogorov–Smirnov (K–S) and Mann–Whitney–Wilcoxon (M–W–W) tests indicate that the two samples have the different distributions with parameters of spin period (P), derivative of spin period ($\dot{P}$), surface magnetic field strength (B), and energy loss rate ($\dot{E}$). Meanwhile, the cumulative number ratio between the pulsars with and without SNRs at the different spin-down ages decreases significantly after $\rm 10\!-\!20\, kyr$. So we propose that the existence of the two types of supernovae (SNe), corresponding to their SNR lifetimes, which can be roughly ascribed to the low- and high-energy SNe. Furthermore, the low-energy SNe may be formed from the $\rm 8\!-\!12\, M_{\odot }$ progenitor, e.g. possibly experiencing the electron capture, while the main-sequence stars of $\rm 12\!-\!25\, M_{\odot }$ may produce the high-energy SNe probably by the iron core collapse.

中文翻译：

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有/没有超新星遗迹的年轻射电脉冲星的统计测试：暗示中子星的两个起源

年轻脉冲星的特性及其与超新星遗迹（SNR）的关系一直是有趣的话题。目前，银河系共发布了 383 个 SNR，与 64 个射电脉冲星和 46 个高能发射脉冲星相关。然而，我们注意到630颗自旋周期小于半秒的年轻射电脉冲星尚未观测到它们周围或附近的信噪比，这就产生了一个问题，即有/没有信噪比的两种年轻射电脉冲星是否都成立鲜明的特点？在这里，我们对具有 (52) 和不具有 (630) SNR 的两组年轻射电脉冲星进行统计检验，以揭示它们是否具有不同的起源。Kolmogorov-Smirnov (K-S) 和 Mann-Whitney-Wilcoxon (M-W-W) 检验表明，两个样品具有不同的分布，其参数为自旋周期 (P)、自旋周期导数 ($\dot{P }$)、表面磁场强度 (B) 和能量损失率 ($\dot{E}$)。同时，在$\rm 10\!-\!20\, kyr$ 之后，不同自旋下降年龄的有SNR 和没有SNR 的脉冲星的累积数量比显着降低。因此我们提出两种超新星（SNe）的存在，对应于它们的信噪比寿命，大致可以归结为低能和高能超新星。此外，低能超新星可能由 $\rm 8\!-\!12\, M_{\odot }$ 的祖先形成，例如可能经历电子俘获，而 $\rm 12 的主序星\!-\!25\,