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It is widely accepted that X-ray emission in luminous active galactic nuclei(AGNs) originates from hot corona. To prevent the corona from over-cooling bystrong X-ray emission, steady heating to the corona is essential, for which themost promising mechanisms is the magnetic reconnection. Detailed studies of thecoupled disc and corona, in the frame of magnetic field transferringaccretion-released energy from the disc to the corona, reveal that the thermalelectrons can only produce X-ray spectrum with $\Gamma_{\rm 2-10\,keV}>2.1$,which is an inevitable consequence of the radiative coupling of the thermalcorona and disc. In the present work, we develop themagnetic-reconnection-heated corona model by taking into account the potentialnon-thermal electrons accelerated in the magnetic reconnection process, inaddition to the thermal electrons. We show that the features of the structureand spectrum of the coupled disc and corona can be affected by the fraction ofmagnetic energy allocated to thermal electrons. Furthermore, we investigate theeffects of the power-law index and energy range of non-thermal electrons andthe magnetic field on the spectrum. It is found that the X-ray spectrum fromthe Comptonization of the hybrid electrons can be flatter than that fromthermal electrons only, in agreement with observations. By comparing with theobserved hard X-ray data, we suggest that a large fraction ($>40\%$) of themagnetic energy be allocated to the non-thermal electrons in the luminous andflat X-ray spectrum AGNs.

Magnetic-Reconnection-Heated Corona Model: Implication of Hybrid Electrons for Hard X-ray Emission of Luminous Active Galactic Nuclei