论文标题
重复和非重复的快速无线电爆发的光度 - 持续关系关系和发光函数
Luminosity-duration relations and luminosity functions of repeating and non-repeating fast radio bursts
论文作者
论文摘要
快速无线电爆发（FRB）是神秘的无线电爆发，其时间比例大约为毫秒。在观察中鉴定了两个人群，即重复重复和不重复的FRB。但是，这两者及其起源之间的差异仍然被神秘。在这里，我们显示了时间集成的光度 - 持续时间（$l_ν$ - $ w _ {\ rm int，REST} $）关系和Luminosity函数（LFS）在FRB目录项目中重复和不重复的FRB。显然，这两个种群在$L_ν$ - $ W _ {\ rm int，REST} $平面具有独特的LFS，即重复frb的$L_ν$和更长的$ w _ {\ rm int，REST} $，LF较低的LF。与非重复的FRB相反，重复FRB在$l_ν$和$ w _ {\ rm int，REST} $之间没有任何明确的相关性。这些结果表明两者的物理起源基本不同。 The faint ends of the LFs of repeating and non-repeating FRBs are higher than volumetric occurrence rates of neutron-star mergers and accretion-induced collapse (AIC) of white dwarfs, and are consistent with those of soft gamma-ray repeaters (SGRs), type Ia supernovae, magnetars, and white-dwarf mergers.这表明了两种可能性：（i）（i）微弱的非重复的FRB源自中子星级合并或AIC，实际上在祖细胞的生命中重复，或（ii）（ii）微弱的非重新培养的FRB源自任何SGRS，任何SGRS，IA型超新星，磁铁，磁铁和白色WARF MERGERS型。重复和不重复的FRB的LF的明亮末端低于任何祖细胞的候选者，这表明明亮的FRB是由祖细胞的一小部分产生的，无论重复如何。否则，它们可能起源于未知的祖细胞。
Fast radio bursts (FRBs) are mysterious radio bursts with a time scale of approximately milliseconds. Two populations of FRB, namely repeating and non-repeating FRBs, are observationally identified. However, the differences between these two and their origins are still cloaked in mystery. Here we show the time-integrated luminosity-duration ($L_ν$-$w_{\rm int,rest}$) relations and luminosity functions (LFs) of repeating and non-repeating FRBs in the FRB Catalogue project. These two populations are obviously separated in the $L_ν$-$w_{\rm int,rest}$ plane with distinct LFs, i.e., repeating FRBs have relatively fainter $L_ν$ and longer $w_{\rm int,rest}$ with a much lower LF. In contrast with non-repeating FRBs, repeating FRBs do not show any clear correlation between $L_ν$ and $w_{\rm int,rest}$. These results suggest essentially different physical origins of the two. The faint ends of the LFs of repeating and non-repeating FRBs are higher than volumetric occurrence rates of neutron-star mergers and accretion-induced collapse (AIC) of white dwarfs, and are consistent with those of soft gamma-ray repeaters (SGRs), type Ia supernovae, magnetars, and white-dwarf mergers. This indicates two possibilities: either (i) faint non-repeating FRBs originate in neutron-star mergers or AIC and are actually repeating during the lifetime of the progenitor, or (ii) faint non-repeating FRBs originate in any of SGRs, type Ia supernovae, magnetars, and white-dwarf mergers. The bright ends of LFs of repeating and non-repeating FRBs are lower than any candidates of progenitors, suggesting that bright FRBs are produced from a very small fraction of the progenitors regardless of the repetition. Otherwise, they might originate in unknown progenitors.
