论文标题
PSR J0855 $ - $ 4644负责Dampe暗示的1.4 TEV电子光谱凹凸吗？
Is PSR J0855$-$4644 responsible for the 1.4 TeV electron spectral bump hinted by DAMPE?
论文作者
论文摘要
宇宙射线电子光谱上的Dampe观察表明，$ \ sim $ 1.4 TEV的狭窄过剩。尽管过量可以归因于暗物质颗粒，但据信脉冲星和脉冲星风星云是一个更自然的天体物理起源：从附近脉冲星注射的电子早期注射的电子可能由于辐射能量损失而在光谱中形成类似颠簸的特征。在本文中，通过对附近脉冲星的调查，我们发现了4个脉冲星，这些脉冲星可能对$ \ sim $ 1.4 $ 1.4 TEV COSMIC RAE ELECTRON。其中，PSR J0855 $ - $ 4644的旋转发光度比其他人高出50倍以上，并且大概可以主导它们的电子通量。然后使用对内部紧凑部分（可能代表从PULSAR传输的隧道）对PWN G267.0 $ -01.0的X射线观测来约束由脉冲星注入的高能电子的光谱指数。我们表明，由PSR J0855 $ - $ 4644发布的高能电子确实可以复制Dampe用合理的参数暗示的1.4 TEV光谱功能。
DAMPE observation on the cosmic ray electron spectrum hints a narrow excess at $\sim$ 1.4 TeV. Although the excess can be ascribed to dark matter particles, pulsars and pulsar wind nebulae are believed to be a more natural astrophysical origin: electrons injected from nearby pulsars at their early ages can form a bump-like feature in the spectrum due to radiative energy losses. In this paper, with a survey of nearby pulsars, we find 4 pulsars that may have notable contributions to $\sim$ 1.4 TeV cosmic ray electrons. Among them, PSR J0855$-$4644 has a spin down luminosity more than 50 times higher than others and presumably dominates the electron fluxes from them. X-ray observations on the inner compact part (which may represent a tunnel for the transport of electrons from the pulsar) of PWN G267.0$-$01.0 are then used to constrain the spectral index of high energy electrons injected by the pulsar. We show that high-energy electrons released by PSR J0855$-$4644 could indeed reproduce the 1.4 TeV spectral feature hinted by the DAMPE with reasonable parameters.
