Wen-Long Zhang, Wen-Jun Tan, Hao-Tian Lan, Shuang-Xi Yi, Shao-Lin Xiong, Chen-Wei Wang, Shuang-Nan Zhang, C. Guidorzi, R. Maccary, R. Moradi, Cheng-Kui Li, Sheng-Lun Xie, Wang-Chen Xue, Jia-Cong Liu, Zheng-Hang Yu, Yue Wang, Peng Zhang, Yan-Qiu Zhang, Chao Zheng, Jin-Peng Zhang, Fa-Yin Wang
Gamma-ray bursts (GRBs) are the most energetic explosive events in the Universe, yet the physical mechanism of their prompt emission remains a mystery. Especially, it is unclear whether the energy dissipation mechanism in the GRB jet is dominated by kinetic energy or magnetic energy. Here, we studied the pulses in the prompt emission of the second brightest GRB to date, GRB 230307A, which was accurately measured by the Gravitational wave high-energy electromagnetic counterpart all-sky monitor (GECAM), with focus on the cumulative distributions of peak counts and duration of pulses as well as the waiting time between pulses. We find that these cumulative distributions show scale-invariant behavior, well consistent with the prediction of the self-organized criticality (SOC) theory. This is the first robust evidence of an SOC feature in the prompt emission of a single GRB. Moreover, the statistical properties of pulses in the prompt emission of GRB 230307A are very similar to those of solar flares. Our findings suggest that the prompt emission of GRB is powered by the dissipation of magnetic energy in the ultra-relativistic jet, supporting the Poynting-flux-dominated prompt models.