The soft X-ray excess is a major component of many type 1 active galactic nuclei(AGN),especially Narrow Line Seyfert1 (NLS1) galaxies. The radiation of Active galactic nuclei can cover all band.Below 1 $keV$ in the X-ray band, the X-ray data are above the low energy extrapolation of the best fitting 2-10 $keV$ power law by index about $\Gamma\sim2.0$. This is so-called soft X-ray excess. However, the origin of the soft X-ray excess is unclear and difficult to explain. In some previous works that consider the black body radiation from accretion disc can emit the soft X-raylike as the "Big Blue Bump". But according to the standard accretion disc model, if the soft X-ray can be radiated from accretion disc, the mass of black hole must be small as well as the accretion rate should be close or exceed the Eddington accretion rate. However, the observation shows that the sample of AGNs with soft X-ray excess do not obey those conditions. So that it is difficult to use the standard accretion disc model to explain the origin of the soft X-ray excess. At the same time, the blackbody temperature of the soft X-ray excess remains remarkably constant at 0.1-0.2$keV$. Since then, many models are present to explain the origin of the soft X-ray excess, such as reflection and absorption model, "Slim disc", disc wind model, thermal comptonization and so on. But those models more or less have some difficult, so the origin of the soft X-ray excess is still controversial.So we can quest a new scenario to explain the Soft X-ray excess in AGNs. Because magnetic field exist in plasma generally, so it is necessary to consider magnetic field into the radiative processes of the soft X-ray. Under the effect of differential rotation of the accretion disc and turbulence, magnetic field should be tangled to generate magnetic reconnection. Then, electrons are accelerated by shock wave and turbulence triggered by magnetic reconnection, then they take place inverse Compton scattering with the soft photon which generate from accretion disc that contributes soft X-rays. We then apply the model to fit the spectra of AGNs with strong soft X-ray excess.
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