## 2. Modeling line profilesIn our model a viscous, geometrically thin, and warped - because of the Bardeen-Petterson effect - accretion disk is irradiated by a point-like central source. We use a cylindrical coordinate system, centered at the black hole (Fig. 1). The irradiating source is located at above the disk plane, along the black hole axis instead of at the exact center, as this is a more realistic situation. The profiles of HFI emission as a result of the reprocessing of the central hard X-ray radiation are obtained. The disk thickness is neglected in the computations - it does not affect the profile shapes significantly as the semithickness to radius ratio is usually much less than the tilt angle. All relativistic corrections are also neglected, because they are small while our goal is to obtain qualitative results only. The disk is assumed to be optically thick to visual light and X-rays - no emission from the lower surface (probably also illuminated) can reach an observer located above the X-Y plane.
## 2.1. Geometry of nonplanar disksSince the precession velocity is small compared to the Keplerian
orbital velocity , the disk is a
stationary structure and can be treated as being composed of
concentric rings, laying in different planes. Warp waves can propagate
through the disk surface if
(Papaloizou & Pringle 1983), where
is the dimensionless viscosity
parameter (Shakura & Sunyaev 1973), but this is not the case for
AGN accretion disks, where is
usually assumed to be 0.1-1. Each disk ring is defined by two Eulerian
angles and
(Fig. 1) and its radius
For a stationary twisted accretion disk,
and
are slowly varying functions of the
radial distance Here the dimensionless parameter
if the semithickness-to-radius ratio of theaccretion disk is about
0.01 (Collin-Souffrin & Dumont 1990),
, and
## 2.2. Illumination and line profilesIn order to explore the nonplanar disk illumination and the
resulting line profiles we created a simple code. The input parameters
are: the initial inclination angle ,
the angles defining the line of sight, the ionizing luminosity
, the source height
and the black hole mass
. For small inclinations of the disk,
the deviation angle of a disk point
(P) is also small () and the
following approximation is valid: ;
; see Fig. 1. The disk is divided
into about elements, each defined by
its dimensions ,
and coordinates For all elements the following value is calculated: In the calculation of the total HFI luminosity, shadowing of the elements by the inner parts of the disk must be taken into account. This has been done as follows: The contribution of each element to the total HFI luminosity from the disk is equal to (Eq. (2)) only in case that there does not exist another element with and is 0 in the opposite case. - the hard X-ray luminosity, is close to the bolometric luminosity if the continuum extends up to with a spectral index close to 1. is the line response to the ionizing flux, i.e. it represents the probability that an absorbed X-photon produces an HFI -photon. It depends on the physical parameters of the emitting layers, taking into account the saturation of the lines (due to the limited number of line-emitting atoms), the absorbed fraction of hard radiation (if the column density of the absorbing gas , not all hard radiation is absorbed), etc. It also may depend slightly on the incident flux - the reprocessing is not necessarily a linear process (Eq. (2)). In our computations we used this dependence as given by Collin-Souffrin & Dumont (1989, 1990b). In their work is presented in a multifunctional form, taking into account all effects mentioned. To obtain the profile of the line emission from the whole disk we have to calculate the Doppler shift of each element, i. e. the projection () of the Keplerian velocity onto the line of sight. is given approximately by: where and are the angles defining the direction to the observer. The whole profile can be constructed by adding contributions of all elements, taking into account their Doppler shifts. © European Southern Observatory (ESO) 1999 Online publication: July 16, 1999 |