| Literature DB >> 34261813 |
Zhen Cao, F Aharonian, Q An, L X Bai, Y X Bai, Y W Bao, D Bastieri, X J Bi, Y J Bi, H Cai, J T Cai, Zhe Cao, J Chang, J F Chang, B M Chen, E S Chen, J Chen, Liang Chen, Liang Chen, Long Chen, M J Chen, M L Chen, Q H Chen, S H Chen, S Z Chen, T L Chen, X L Chen, Y Chen, N Cheng, Y D Cheng, S W Cui, X H Cui, Y D Cui, B D'Ettorre Piazzoli, B Z Dai, H L Dai, Z G Dai, D Della Volpe, X J Dong, K K Duan, J H Fan, Y Z Fan, Z X Fan, J Fang, K Fang, C F Feng, L Feng, S H Feng, Y L Feng, B Gao, C D Gao, L Q Gao, Q Gao, W Gao, M M Ge, L S Geng, G H Gong, Q B Gou, M H Gu, F L Guo, J G Guo, X L Guo, Y Q Guo, Y Y Guo, Y A Han, H H He, H N He, J C He, S L He, X B He, Y He, M Heller, Y K Hor, C Hou, X Hou, H B Hu, S Hu, S C Hu, X J Hu, D H Huang, Q L Huang, W H Huang, X T Huang, X Y Huang, Z C Huang, F Ji, X L Ji, H Y Jia, K Jiang, Z J Jiang, C Jin, T Ke, D Kuleshov, K Levochkin, B B Li, Cheng Li, Cong Li, F Li, H B Li, H C Li, H Y Li, Jian Li, Jie Li, K Li, W L Li, X R Li, Xin Li, Xin Li, Y Li, Y Z Li, Zhe Li, Zhuo Li, E W Liang, Y F Liang, S J Lin, B Liu, C Liu, D Liu, H Liu, H D Liu, J Liu, J L Liu, J S Liu, J Y Liu, M Y Liu, R Y Liu, S M Liu, W Liu, Y Liu, Y N Liu, Z X Liu, W J Long, R Lu, H K Lv, B Q Ma, L L Ma, X H Ma, J R Mao, A Masood, Z Min, W Mitthumsiri, T Montaruli, Y C Nan, B Y Pang, P Pattarakijwanich, Z Y Pei, M Y Qi, Y Q Qi, B Q Qiao, J J Qin, D Ruffolo, V Rulev, A Saiz, L Shao, O Shchegolev, X D Sheng, J Y Shi, H C Song, Yu V Stenkin, V Stepanov, Y Su, Q N Sun, X N Sun, Z B Sun, P H T Tam, Z B Tang, W W Tian, B D Wang, C Wang, H Wang, H G Wang, J C Wang, J S Wang, L P Wang, L Y Wang, R N Wang, Wei Wang, Wei Wang, X G Wang, X J Wang, X Y Wang, Y Wang, Y D Wang, Y J Wang, Y P Wang, Z H Wang, Z X Wang, Zhen Wang, Zheng Wang, D M Wei, J J Wei, Y J Wei, T Wen, C Y Wu, H R Wu, S Wu, W X Wu, X F Wu, S Q Xi, J Xia, J J Xia, G M Xiang, D X Xiao, G Xiao, H B Xiao, G G Xin, Y L Xin, Y Xing, D L Xu, R X Xu, L Xue, D H Yan, J Z Yan, C W Yang, F F Yang, J Y Yang, L L Yang, M J Yang, R Z Yang, S B Yang, Y H Yao, Z G Yao, Y M Ye, L Q Yin, N Yin, X H You, Z Y You, Y H Yu, Q Yuan, H D Zeng, T X Zeng, W Zeng, Z K Zeng, M Zha, X X Zhai, B B Zhang, H M Zhang, H Y Zhang, J L Zhang, J W Zhang, L X Zhang, Li Zhang, Lu Zhang, P F Zhang, P P Zhang, R Zhang, S R Zhang, S S Zhang, X Zhang, X P Zhang, Y F Zhang, Y L Zhang, Yi Zhang, Yong Zhang, B Zhao, J Zhao, L Zhao, L Z Zhao, S P Zhao, F Zheng, Y Zheng, B Zhou, H Zhou, J N Zhou, P Zhou, R Zhou, X X Zhou, C G Zhu, F R Zhu, H Zhu, K J Zhu, X Zuo.
Abstract
The Crab Nebula is a bright source of gamma-rays powered by the Crab Pulsar's rotational energy, through the formation and termination of a relativistic electron-positron wind. We report the detection of γ-rays from this source with energies from 5 × 10-4 to 1.1 petaelectronvolts (PeV), with a spectrum showing gradual steepening over three energy decades. The ultra-high-energy photons imply the presence of a PeV electron accelerator (a pevatron) in the nebula, with an acceleration rate exceeding 15% of the theoretical limit. We constrain the pevatron's size between 0.025 and 0.1 pc, and magnetic field ≈110 μG. The production rate of PeV electrons, 2.5 × 1036 erg s-1, constitutes 0.5% of the pulsar spin-down luminosity, although we cannot exclude a contribution of PeV protons to the production of the highest energy γ-rays.Year: 2021 PMID： 34261813 DOI： 10.1126/science.abg5137
Source DB: PubMed Journal: Science ISSN： 0036-8075 Impact factor: 47.728