论文标题
揭示身份不明的伽马射线源的性质4FGL J1908.6+0915E，HESS J1907+089+089/HOTS J1907+091和3HWC J1907+085在Magnet Sgr Sgr 1900+14的天空区域
Unveiling the nature of the unidentified gamma-ray sources 4FGL J1908.6+0915e, HESS J1907+089/HOTS J1907+091, and 3HWC J1907+085 in the sky region of the magnetar SGR 1900+14
论文作者
论文摘要
超新星残留物（SNR），恒星形成区域（SFR）和脉冲星风星云（PWNE）是银河系pevatrons的主要候选者。非热高能量（He，$ \ varepsilon> 100 \ textrm {Mev} $）和非常高的能量（vhe，$ \ varepsilon> 100 \ textrm {gev} $）$γ$γ$-γ$-γ$-γ$-γ$ -DRAIES应该是这些来源的ray ray ray ray ray ray ray ray ray ray rays应该是加速过程的有点表现。我们研究了从Magnetar Sgr 1900+14的天空区域中解释He和Vhe $γ$射线的可能性，这是在上述来源加速的宇宙射线的签名。为此，我们模拟了从扩展的费米 - lat源4FGL J1908.6+0915E中的$γ$ ray排放，扩展的Vhe H.E.S.S.源候选人热点J1907+091，以及点状的HAWC TEV源3HWC J1907+085，它们在空间上与SNR G42.8+0.6，Magnetar SGR 1900+14和星形形成区域W49A相吻合。模拟是在辐射模型中进行的。我们表明，原则上，观察到的$γ$ - 射线从Magnetar Sgr 1900+14区域的排放量可以包括来自所有三种（潜在混乱）来源的不同强度的贡献。在详细的情况下，考虑了磁性连接但仍未发现的SNR和PWN的考虑，但对辐射Cr颗粒的能量储备非常有严重要求 - $ 10^{51} d _ {\ textrm {\ textrm {\ textrm {10kpc}}}}^{2} $ erg sim sim sim sim $ d c。可以由新生儿毫秒磁铁产生的与磁体相关的超诺伐氏菌和/或磁铁磁星云残留物提供此类能量储备，其中旋转能量$ e _ {\ textrm {rot}}} \ sim 10^{52} {52} {52} \ textrm {erg {erg {erg} $。
Supernova remnants (SNRs), star formation regions (SFRs), and pulsar wind nebulae (PWNe) are prime candidates for Galactic PeVatrons. The nonthermal high-energy (HE, $\varepsilon>100 \textrm{ MeV}$) and very high-energy (VHE, $\varepsilon>100 \textrm{ GeV}$) $γ$-ray emission from these sources should be a promising manifestation of acceleration processes. We investigate the possibility to explain the HE and VHE $γ$-ray emission from the sky region of the magnetar SGR 1900+14 as a signature of cosmic rays accelerated in above mentioned sources. To this end, we simulate the $γ$-ray emission from the extended Fermi-LAT HE source 4FGL J1908.6+0915e, the extended VHE H.E.S.S. source candidate HOTS J1907+091, and the point-like HAWC TeV source 3HWC J1907+085, which are spatially coincident with the SNR G42.8+0.6, the magnetar SGR 1900+14 and the star forming region W49A. The simulations are performed within the hadronic and leptonic models. We show that the observed $γ$-ray emission from the region of the magnetar SGR 1900+14 can, in principle, include contributions of different intensities from all three types of (potentially confused) sources. The considered in detail cases of a magnetar-connected but still undetected SNR and a PWN are the most promising ones, but with a serious requirement on the energy reserve of radiated CR particles - of order of $10^{51}d_{\textrm{10kpc}}^{2}$ erg for sources at a distance of $d\sim 10$ kpc. Such energy reserve can be provided by the magnetar-related Hypernova and/or magnetar wind nebula remnant created by the newborn millisecond magnetar with the large supply of rotational energy $E_{\textrm{rot}}\sim 10^{52}\textrm{ erg}$.
