  In the unification scheme of active galactic nuclei (AGN), Seyfert 1s and
Seyfert 2s are intrinsically same, but they are viewed at different angles.
However, the Fe K\alpha emission line luminosity of Seyfert 1s was found in
average to be about twice of that of Seyfert 2s at given X-ray continuum
luminosity in the previous work (Ricci et al. 2014). We construct an accretion
disc-corona model, in which a fraction of energy dissipated in the disc is
extracted to heat the corona above the disc. The radiation transfer equation
containing Compton scattering processes is an integro-differential equation,
which is solved numerically for the corona with a parallel plane geometry. We
find that the specific intensity of X-ray radiation from the corona changes
little with the viewing angle \theta when \theta is small (nearly face-on), and
it is sensitive to \theta if the viewing angle is large (\theta> 40 degrees).
The radiation from the cold disc, mostly in infrared/optical/UV bands, is
almost proportional to cos\theta when \theta< 40 degrees, while it decreases
more rapidly than cos\theta when \theta> 40 degrees because of strong
absorption in the corona in this case. For seyfert galaxies, the Fe K\alpha
line may probably be emitted from the disc irradiated by the X-ray continuum
emission. The observed equivalent width (EW) difference between Seyfert 1s and
Seyfert 2s can be reproduced by our model calculations, provided Seyfert 1s are
observed in nearly face-on direction and the average inclination angle of
Seyfert 2s ~65 dgrees.
