The gamma-ray halo around Geminga is formed owing to the slow diffusion of the electrons released by the Geminga pulsar wind nebula (PWN). The latest observations from the HAWC and H.E.S.S. Collaborations exhibit complex features in the TeV gamma-ray spectrum of the Geminga halo. We first show that the new results cannot be interpreted by the commonly used simple model, where a single power-law injection spectrum and an energy index of $\ensuremath{\delta}=1/3$ for the diffusion coefficient are assumed. We then propose a two-population electron injection model based on the x-ray observations of the Geminga PWN, which consists of a population of freshly accelerated electrons escaping from the PWN through rapid outflows and a population trapped longer inside the PWN before escaping. The two-population model interprets the HAWC and H.E.S.S. data well, and the goodness of fit improves significantly compared with the single power-law injection model. It also predicts a different energy dependency of the gamma-ray profile from the single power-law injection model, which could be tested by the Large High Altitude Air Shower Observatory in the coming future. We note that a $\ensuremath{\delta}$ slightly larger than 1 is needed to fit the HAWC and H.E.S.S. data consistently. We also discuss the possible improvements by adopting the two-zone diffusion model.
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