Authors
Zhen Cao, F Aharonian, Y X Bai, Y W Bao, D Bastieri, X J Bi, Y J Bi, W Bian, A V Bukevich, C M Cai, W Y Cao, Zhe Cao, J Chang, J F Chang, A M Chen, E S Chen, G H Chen, H X Chen, Liang Chen, Long Chen, M J Chen, M L Chen, Q H Chen, S Chen, S H Chen, S Z Chen, T L Chen, X B Chen, X J Chen, Y Chen, N Cheng, Y D Cheng, M C Chu, M Y Cui, S W Cui, X H Cui, Y D Cui, B Z Dai, H L Dai, Z G Dai, Danzengluobu, Y X Diao, X Q Dong, K K Duan, J H Fan, Y Z Fan, J Fang, J H Fang, K Fang, C F Feng, H Feng, L Feng, S H Feng, X T Feng, Y Feng, Y L Feng, S Gabici, B Gao, C D Gao, Q Gao, W Gao, W K Gao, M M Ge, T T Ge, L S Geng, G Giacinti, G H Gong, Q B Gou, M H Gu, F L Guo, J Guo, X L Guo, Y Q Guo, Y Y Guo, Y A Han, O A Hannuksela, M Hasan, H H He, H N He, J Y He, X Y He, Y He, S Hernández-Cadena, B W Hou, C Hou, X Hou, H B Hu, S C Hu, C Huang, D H Huang, J J Huang, T Q Huang, W J Huang, X T Huang, X Y Huang, Y Huang, Y Y Huang, X L Ji, H Y Jia, K Jia, H B Jiang, K Jiang, X W Jiang, Z J Jiang, M Jin, S Kaci, M M Kang, I Karpikov, D Khangulyan, K Koennonkok, D Kuleshov, K Kurinov, B B Li, Cheng Li, Cong Li, D Li, F Li, H B Li, H C Li, Jian Li, Jie Li, K Li, L Li, R L Li, S D Li, T Y Li, W L Li, X R 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, D B Liu, H Liu, H D Liu, J Liu, J L Liu, J R Liu, M Y Liu, R Y Liu, S M Liu, W Liu, X Liu, Y Liu, Y Liu, Y N Liu, Y Q Lou, Q Luo, Y Luo, H K Lv, B Q Ma, L L Ma, X H Ma, J R Mao, Z Min, W Mitthumsiri, G B Mou, H J Mu, A Neronov, K C Y Ng, M Y Ni, L Nie, L J Ou, P Pattarakijwanich, Z Y Pei, J C Qi, M Y Qi, J J Qin, A Raza, C Y Ren, N Ruangpongsiri, D Ruffolo, A Sáiz, D Semikoz, L Shao, O Shchegolev, Y Z Shen, X D Sheng, Z D Shi, F W Shu, H C Song, Yu V Stenkin, V Stepanov, Y Su, D X Sun, H Sun, Q N Sun, X N Sun, Z B Sun, N H Tabasam, J Takata, P H T Tam, H B Tan, Q W Tang, R Tang, Z B Tang, W W Tian, C N Tong, L H Wan, C Wang, G W Wang, H G Wang, J C Wang, K Wang, Kai Wang, Kai Wang, L P Wang, L Y Wang, L Y Wang, R Wang, W Wang, X G Wang, X J Wang, X Y Wang, Y Wang, Y D Wang, Z H Wang, Z X Wang, Zheng Wang, D M Wei, J J Wei, Y J Wei, T Wen, S S Weng, C Y Wu, H R Wu, Q W Wu, S Wu, X F Wu, Y S Wu, S Q Xi, J Xia, J J Xia, G M Xiang, D X Xiao, G Xiao, Y L Xin, Y Xing, D R Xiong, Z Xiong, D L Xu, R F Xu, R X Xu, W L Xu, L Xue, D H Yan, T Yan, C W Yang, C Y Yang, F F Yang, L L Yang, M J Yang, R Z Yang, W X Yang, Z H Yang, Z G Yao, X A Ye, L Q Yin, N Yin, X H You, Z Y You, Q Yuan, H Yue, H D Zeng, T X Zeng, W Zeng, X T Zeng, M Zha, B B Zhang, B T Zhang, C Zhang, F Zhang, H Zhang, H M Zhang, H Y Zhang, J L Zhang, Li Zhang, P F Zhang, P P Zhang, R Zhang, S R Zhang, S S Zhang, W Y Zhang, X Zhang, X P Zhang, Yi Zhang, Yong Zhang, Z P Zhang, J Zhao, L Zhao, L Z Zhao, S P Zhao, X H Zhao, Z H Zhao, F Zheng, W J Zhong, B Zhou, H Zhou, J N Zhou, M Zhou, P Zhou, R Zhou, X X Zhou, X X Zhou, B Y Zhu, C G Zhu, F R Zhu, H Zhu, K J Zhu, Y C Zou, X Zuo, LHAASO Collaboration
Published in
Physical review letters. Volume 136. Issue 25. Pages 251002. Jun 26, 2026.
Abstract
Large- or medium-scale cosmic ray anisotropy at TeV energies has not previously been confirmed to vary with time. Transient anisotropy changes have been observed below 150 GeV, especially near the passage of an interplanetary shock and coronal mass ejection containing a magnetic flux rope ejected by a solar storm, which can trigger a geomagnetic storm with practical consequences. Here, we report the first observation of transient large-scale anisotropy in TeV cosmic ray ions using data from the Large High-Altitude Air Shower Observatory. We analyze hourly skymaps of the transient cosmic ray intensity excess or deficit, the gradient of which indicates the direction and magnitude of transient large-scale anisotropy across the field of view. We observe enhanced anisotropy above typical hourly fluctuations with >5σ significance during some hours of November 4, 2021, in separate datasets for four primary cosmic ray energy ranges of median energy from E=0.6 to 2.8 TeV. The gradient varies with energy as E^{γ}, where γ=-0.5. At a median energy ≤1.0 TeV, this gradient corresponds to a dipole anisotropy of at least 0.9%, or possibly a weaker anisotropy of higher order. This new type of observation opens the opportunity to study interplanetary magnetic structures using air shower arrays around the world, complementing existing in situ and remote measurements of plasma properties.
PMID:
42430624
Bibliographic data and abstract were imported from PubMed on 11 Jul 2026.
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