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We conducted a comprehensive investigation of the brightest-of-all-time GRB221009A using new insights from very high energy (VHE) observations from LHAASOand a complete multiwavelength afterglow dataset. Through data fitting, weimposed constraints on the jet structure, radiation mechanisms, and burstenvironment of GRB 221009A. Our findings reveal a structured jet morphologycharacterized by a core+wing configuration. A smooth transition of energywithin the jet takes place between the core and wing, but with a discontinuityin the bulk Lorentz factor. The jet structure differs from both the case ofshort GRB 170817A and the results of numerical simulations for long-durationbursts. The VHE emission can be explained by the forward-shock synchrotronself-Compton radiation of the core component, but requiring a distinctivetransition of the burst environment from uniform to wind-like, suggesting thepresence of complex pre-burst mass ejection processes. The low-energymultiwavelength afterglow is mainly governed by the synchrotron radiation fromthe forward and reverse shocks of the wing component. Our analysis indicates amagnetization factor of 5 for the wing component. Additionally, by comparingthe forward shock parameters of the core and wing components, we find apotential correlation between the electron acceleration efficiency and both theLorentz factor of the shock and the magnetic field equipartition factor. Wediscuss the significance of our findings, potential interpretations, andremaining issues.

Jet Structure and Burst Environment of GRB 221009A