论文标题
关于明亮的年轻脉冲星的潜力
On the potential of bright, young pulsars to power ultra-high gamma-ray sources
论文作者
论文摘要
最近发现了新的超高能量伽马射线源的新人群，光谱延伸了100 TEV，这表明存在银河系PEVATRON-COSMIC-RAY厂加速颗粒到PEV能量。这些来源，除了与螃蟹星云相关联的来源，尚未确定。延伸1度或以上，其中大多数包含多个潜在的对应物，包括超新星残留物，年轻的恒星簇和脉冲星风星云（PWNE），它们可以像Pevatrons一样执行，从而为周围的散射超高能能量伽玛射线结构提供动力。在怪异的情况下，伽马射线是由电子产生的，通过2.7 k CMB辐射的逆康普顿散射在脉冲星风终止冲击下加速。 PULSAR旋转功率对相对论电子的高转化效率与短冷却时间尺度相结合，使伽马射线的发光度达到$l_γ\ sim 0.1 \ dot {e} $的水平。 Pulsar旋转的光度，$ \ dot e $，也确定了单个光子的绝对最大能量：$ e _ {\ rm γ〜 \ rm max} \大约0.9 \ dot e_ {36}^{0.65}^{0.65} ~~ \ rm {pev} $。这种基本约束在Young PWNE的同步加速器能量损失的情况下占主导地位，其典型磁场$ \ $ \ $ \ $ 100 $μ$ G，$ \ dot {e} \ sillesim 10^{37} {37} {37} \ \ \ \ \ \ \ \ \ \ \ rm erg erg/s $。我们通过将$ e _ {\ rmγ〜 \ rm max} $与Lhaaso报告的最高能量光子进行比较的含义讨论了$ e _ {\ rmγ〜 \ rm max} $的含义。每当可能的PWN来源时，我们都会使用LHAASO测量值将上限设置在Nebular磁场上。
The recent discovery of a new population of ultra-high-energy gamma-ray sources with spectra extending beyond 100 TeV revealed the presence of Galactic PeVatrons - cosmic-ray factories accelerating particles to PeV energies. These sources, except for the one associated with the Crab Nebula, are not yet identified. With an extension of 1 degree or more, most of them contain several potential counterparts, including Supernova Remnants, young stellar clusters and Pulsar Wind Nebulae (PWNe), which can perform as PeVatrons and thus power the surrounding diffuse ultra-high energy gamma-ray structures. In the case of PWNe, gamma rays are produced by electrons, accelerated at the pulsar wind termination shock, through the inverse Compton scattering of 2.7 K CMB radiation. The high conversion efficiency of pulsar rotational power to relativistic electrons, combined with the short cooling timescales, allow gamma-ray luminosities up to the level of $L_γ\sim 0.1 \dot{E}$. The pulsar spin-down luminosity, $\dot E$, also determines the absolute maximum energy of individual photons: $E_{\rm γ~\rm max}\approx 0.9 \dot E_{36}^{0.65}~~\rm{PeV}$. This fundamental constraint dominates over the condition set by synchrotron energy losses of electrons for young PWNe with typical magnetic field of $\approx$100$μ$G with $\dot{E} \lesssim 10^{37}\ \rm erg/s$. We discuss the implications of $E_{\rm γ~\rm max}$ by comparing it with the highest energy photons reported by LHAASO from a dozen of ultra-high-energy sources. Whenever a PWN origin of the emission is possible, we use the LHAASO measurements to set upper limits on the nebular magnetic field.
