Radiation pressure on dust explains the Low Ionized Broad Emission Lines
  in Active Galactic Nuclei
  Broad emission lines are the most characteristic features in the spectra of
active galaxies. They mostly show either a single-peaked or double-peaked
profiles; and originate from a complex dynamics of the likely discrete clouds
moving in a spatially extended region so-called Broad Line Region (BLR). We
follow a non-hydrodynamical single-cloud approach to the BLR dynamics based on
the dust-driving model of Czerny & Hryniewicz. We previously showed in details
that the 2.5D version of the model could provide us with the 3D geometry of the
BLR. In this paper, we provide a large grid of results based on which we aim at
testing the model with calculation of the spectral line generic profiles. We
show that the shape of profiles not only depends on the accretion rate of the
source, the black hole mass, and the viewing angle, but also it is most
significantly affected by the adopted dust-to-gas mass ratio that regulates the
strength of the radiation pressure. We also show that the model can
appropriately explain the low ionized broad emission lines of the mean spectrum
of quasars, such as MgII and Hbeta.
