# MHD Accretion-Disk Winds as X-ray Absorbers in AGNs

## Abstract

We present the two-dimensional (2D) ionization structure of
self-similar magnetohydrodynamic (MHD) winds off accretion disks
around irradiated by a central X-ray point source. Based
on earlier observational clues and theoretical arguments, we focus
our attention on a subset of these winds, namely those with radial
density dependence ( is the spherical radial
coordinate).
We employ the photoionization code `XSTAR`

to compute the ionic
abundances of a large number of ions of different elements and then
compile their line-of-sight (LOS) absorption columns. We focus our
attention on the distribution of the column density of the various
ions as a function of the ionization parameter (or
equivalently ) and the angle . Particular attention is
paid to the absorption measure distribution (AMD), namely their
Hydrogen-equivalent column per logarithmic interval, , which provides a measure of the winds’ radial density
profiles. For the chosen density profile the AMD is found to be independent of , in good agreement
with its behavior inferred from the X-ray spectra of several active
galactic nuclei (AGNs).
For the specific wind structure and X-ray spectrum we also compute
detailed absorption line profiles for a number of ions to obtain
their LOS velocities, km s (at ) for Fe xvii and km s (at
) for Fe xxv, in good agreement with the
observation. Our models describe the X-ray absorption properties of
these winds with only two parameters, namely the
mass-accretion rate and LOS angle . The probability
of obscuration of the X-ray ionizing source in these winds decreases
with increasing and increases steeply with the LOS
inclination angle . As such, we concur with previous authors
that these wind configurations, viewed globally, incorporate all the
requisite properties of the parsec scale “torii” invoked in AGN
unification schemes. We indicate that a combination of the AMD and
absorption line profile observations can uniquely determine these
model parameters and their bearing on AGN population demographics.

## 1 Introduction

The issue of accretion as the power source behind Active Galactic Nuclei (AGNs) was decided as early as 1969 (Lynden-Bell, 1969). Since then, a 40-year effort to unravel the physics underlying this process has produced a great body of observational and theoretical work covering a host of the AGN properties and phenomena. However, due to the small angular size of a black hole horizon, whether at the galactic or extragalactic setting, these studies were effectively performed mainly in the spectral (but also the time) domain; the spatial structure of accretion flows, but those of scale of many parsecs, was then inevitably delegated to models, whose validity was determined by their ability to reproduce the spectral and timing observations with sufficient accuracy. At the risk of oversimplifying the issue, the spectral properties of AGNs were basically outlined (among other works) in Sanders et al. (1989) who showed that the Spectral Energy Distribution (SED) of AGNs includes three broad components in the IR, optical-UV and X-ray bands, with roughly equal energy per decade, with the radio comprising only a small fraction of their bolometric luminosity, of order in the Radio-Quiet (RQ) AGNs and in Radio-Loud (RL) AGNs.

Considering that accretion produces most of its power in the last 10 or so Schwarzschild radii, , outside the black hole horizon, barring an inherently non-thermal emission process (as it turns out to be the case with blazars), it is strange that the observed SEDs exhibit roughly constant luminosity per decade. Interestingly, the simplest of assumptions, namely radiation of the AGN bolometric luminosity in black body form by an object (most likely in the form of a cold disk of K) of size a few of a supermassive black hole ( where is the solar mass), implies peak emission at UV frequencies, consistent with the observationally identified UV feature referred to above, known as the Big Blue Bump (BBB); as such, this feature was modeled with emission by a geometrically-thin, optically-thick accretion disk extending usually to the Innermost Stable Circular Orbit (ISCO) of the black hole. Of the other two distinct components the X-rays are generally attributed to emission by an optically-thin, hot ( K) corona overlying this disk and heated by the action of magnetic fields that thread the geometrically-thin disk, in close analogy to the Solar Corona (e.g. Haardt & Maraschi, 1991; Kawanaka, Kato, & Mineshige, 2008). Finally, the IR emission was accounted for as the result of reprocessing the O-UV radiation by a geometrically thick (scale height roughly equal to the local radius , i.e. ), cool, molecular torus at large distances ( pc) from the central engine [an arrangement that presents a bit of a problem, since the temperature of this torus ( K) is much less than the virial temperature of the gas at that distance and would lead to a configuration with ; see Krolik & Begelman (1988). The region between the torus and the accretion disk was thought to be occupied by clouds with velocity widths ranging from tens of thousands to several hundreds of kilometers per second, producing the observed line radiation, with the ensemble of these components encapsulated in the well known cartoon of Urry & Padovani (1995).

While in most models these components are generally thought of as independent, Principal Component Analysis (PCA) of multiwavelength AGN features by Boroson & Green (1992) and Boroson (2002) indicated that most of the variance in the measured optical emission line properties and a broad range of continuum features (radio, optical, X-ray) of AGNs was contained in two sets of correlations, eigenvectors of the correlation matrix. This analysis suggested that the properties of these features are not independent (despite their diverse locations and emission processes) but are well correlated by two single underlying physical parameters through the physics of accretion and the conversion of its power to radiation and outflows. On the other hand, general theoretical arguments suggesting, e.g. a tight correlation between variations in the X-ray and O-UV components, given their implied proximity, were not confirmed by observations (Nandra et al., 1998).

The advent of X-ray instrumentation and in particular X-ray spectroscopy, established the presence of spectral components apparently present across the entire range of compact object masses from galactic black hole candidates (GBHCs) to luminous AGNs, namely outflowing X-ray absorbing matter in our line of sight (LOS) manifested as complex (blueshifted) absorption features of hydrogen equivalent column density cm. The presence of this absorbing material, often referred to as Warm Absorber, was first established in ASCA observations of many AGNs (e.g. Reynolds and Fabian, 1995) and GBHCs (e.g. Miller et al., 2006) which provided clear evidence of highly ionized oxygen O vii (0.739 keV) and/or O viii (0.871 keV) along the LOS. More recently, grating spectra of high-resolving power obtained by Chandra and XMM-Newton have enabled the study of these absorption features in greater detail leading to the conclusion that they are present in a large fraction of AGNs and span a wide range () in ionization parameter (e.g. Holczer, Behar & Kaspi, 2007, hereafter HBK07). Some sources appear to contain low and/or high velocity outflows (e.g. HBK07; Holczer, Behar & Arav, 2009) while a handful of objects exhibit a trans-relativistic outflow (e.g. Chartas et al., 2009; Pounds & Reeves, 2009; Reeves et al., 2009). In addition in both AGNs and GBHCs the observed outflows from at least a number of sources have been suggested to be accelerated magnetically (rather than by another process) off an accretion disk (e.g., see Miller et al. 2006, 2008 for GRO J1655-40; Kraemer et al. 2005 and Crenshaw & Kraemer 2007 for NGC 4151). A brief review of luminous AGN winds is found in Brandt et al. (2009). These facts imply the presence of gas covering a large fraction of the solid angle and distributed over a large range of radii, perhaps the entire range between the X-ray source and the torus, indicating AGNs to be multiscale and multiwavelength objects rather than a class with properties determined only by the power released by accretion in the black hole vicinity. This last point has gained further support with the discovery of the correlation between the accreting black hole mass and the velocity dispersion of the surrounding stellar population (Ferrarese & Merrit, 2000).

From the theoretical point of view, most early AGN treatments were focused on the structure of the innermost regions of the accretion flow and as such they limited themselves to the study of the conditions in a rather narrow range of radii. Nonetheless, several treatments of magnetohydrodynamic (MHD) accretion disk winds, aiming to account for the observed AGN outflows, employed self-similar solutions, which naturally span a large range in radius (e.g. Blandford & Payne 1982, hereafter BP82; Contopoulos & Lovelace 1994, hereafter CL94). Using the structure of these solutions, Köngl & Kartje (1994, hereafter KK94) proposed that the so-called molecular torus of the AGN unification scheme is a dynamical rather than a static object, namely an MHD wind of the type suggested in the above works. KK94 also contented that agreement between model and observation demanded a rather specific type of wind, a particular case of those discussed in CL94, one that we also concentrate on in the present work. At the same time, they noted that the 2D geometry of these winds (with low column at inclination angles , i.e. along the wind axis, and high column at ) provided, in addition, a natural framework for the unification scheme of type I and II Seyfert galaxies proposed by Antonucci & Miller (1985), thereby linking the large scale AGN spectral classification to the dynamics of AGN accretion/outflows.

Self-similar solutions of the accretion flow equations were also provided by Narayan & Yi (1994, 1995a), who considered the structure of hot accretion flows in the regime of low accretion rate, i.e. for accretion rates less than the Eddington value, . Because for these low rates the accretion time scale is shorter than the gas cooling time , in fact , only a fraction of the energy released in the dissipation of the plasma kinetic energy is radiated away with the remainder advected into the black hole (hence the term Advection Dominated Accretion Flows or ADAFs); as a result, the accretion luminosity is then proportional to (rather than ). The high temperature of the inner ADAFs, provides naturally for the hot component required to produce the observed X-ray emission, which, rather than being an independent component, within ADAFs is incorporated in the dynamics of accretion itself (see Narayan & McClintock, 2008, for recent review). More recently, Blandford & Begelman (1999), elaborated further on ADAFs elucidating, among others, the reason for which the Bernoulli integral of ADAFs is positive (a point that had been noted by Narayan & Yi, 1994, 1995a), that being that the viscous stresses transfer outward, in addition to angular momentum, also mechanical energy. They then proposed that this excess energy can be carried away in the form of wind over a large range of radii, thereby leading to configurations similar to those obtained in the more detailed studies of BP82 and CL94, while at the same time maintaining some of the general properties of ADAFs. The combination of radiatively inefficient flows with the simultaneous presence of winds led to the nomenclature Advection Dominated Inflow-Outflow Solutions (ADIOS). Following these pioneering works, many attempts have been made in recent years to reproduce and explain the kinematics and X-ray spectra of the observed outflows in AGNs (see, among others, Proga, 2003; Everett, 2005; Sim, 2005; Schurch & Done, 2007; Dorodnitsyn, Kallman & Proga, 2008; Sim et al., 2008; Schurch, Done & Proga, 2009).

Motivated by these considerations we are taking a closer look at the issue of Warm Absorbers (X-ray absorbing medium) in terms of specific disk-wind models, namely those of CL94. As it will be discussed in more detail later on, these solutions are characterized by a parameter , which determines the distribution of axial current in the wind as a function of the radius; this parameter, in conjunction with the MHD conservation laws and the radial force balance, determines both the radial dependence of the matter density in the wind and the radial dependence of the toroidal magnetic field component . Taking our lead from the works of Behar et al. (2003) and HBK07, in the present work we restrict our attention to wind models with , i.e. the value used also by KK94. This is in a sense a critical value of this parameter because, as discussed in CL94, it leads to winds with toroidal magnetic field and therefore magnetic field energy on the disk that diverges only logarithmically at small and large and as such it can be considered as a “minimum magnetic energy” configuration (KK94); values of lead to configurations with power-law divergence either at small or large . In addition, the choice leads to a wind with radial density profile , i.e. a profile with equal column per logarithmic radial interval (and normalization that depends on the polar angle and the mass-accretion rate ), a fact that is in general agreement with the profiles implied by the ionized absorbers data analysis to date (HBK07). It is worth noting that a similar density profile was invoked by Kazanas, Hua & Titarchuk (1996) and Hua, Kazanas & Titarchuk (1997) to explain the Fourier frequency dependence of the soft-hard X-ray lags observed in GBHCs and in AGNs (Papadakis et al. 2002).

With the wind 2D ( and ) density field as a function of radius and angle provided by the models of CL94 (i.e. ignoring at present effects that can be attributed to other agents that could affect the wind structure) and the assumption of a point X-ray source of a given spectrum at the origin, one can compute their 2D ionization structure and in particular the local column density of specific ionic species as a function of radius and angle. One can also compute the integrated column of each such ion, quantities that can be directly compared to observation (HBK07). This we do in the present work. While a number of issues remain open or are sidestepped in the present self-similar wind models, this is the price to pay in order to limit the number of free parameters to just two (the wind mass flux and the observer inclination angle), a fact that allows the study of the properties of warm absorbers within the global perspective of AGN unification.

Our paper is structured as follows: in §2 we review the MHD wind equations and structure as given in CL94 and make a connection of these winds with flows of the ADAF/ADIOS type by relating the wind density normalization to the ionizing luminosity produced by the idealized point source at the coordinate origin. In §3 we provide the general 2D ionization structure, the local column of specific ions as a function of radius as well as the total ionic column of a given charge state and for each element, as well as the absorption line profiles of selected transitions. In §4 the results are compared to observation, the properties and limitation of the present treatment are discussed and a course for future work is charted.

## 2 Description of the Model

Our wind model consists primarily of two parts: () The
outflow/wind structure originating from a geometrically-thin
accretion disk as described by CL94 and () The computation of
the ionization of the wind plasma under local heating-cooling and
ionization equilibrium, by employing the photoinization code
`XSTAR`

(Kallman & Bautista, 2001). These two steps are self-consistently
coupled in a scheme similar to some previous work in a slightly
different context (e.g. Schurch & Done, 2007; Dorodnitsyn, Kallman & Proga, 2008; Schurch, Done & Proga, 2009). All calculations
are performed under steady-state, axisymmetric conditions as shall
be described in detail in the following sections.

### 2.1 Self-similar MHD Wind from Accretion Disks

While the detailed formalism of self-similar MHD wind solutions is found in CL94, let us here briefly summarize some of their characteristics. The basic equations of this problem are those of steady-state, nonrelativistic, ideal MHD that include gravity and gas pressure, namely

(1) | |||||

(2) | |||||

(3) | |||||

(4) | |||||

(5) | |||||

(6) |

Here, the plasma wind velocity is assumed to be frozen into the global magnetic field ; is the electric field; is the electric current density; and is the speed of light. The gas pressure and mass density of the wind are related through an equation of state

(7) |

where and are the adiabatic constant and adiabatic index respectively. The assumption of axial symmetry allows one to separate poloidal quantities from toroidal ones as and , with

(8) |

where, is the magnetic flux function. We will henceforth work in spherical coordinates () [note that CL94 used cylindrical ones ()]. Magnetic field lines lie along surfaces of constant value of . Furthermore, under conditions of steady-state, the following quantities are conserved along field lines characterized by the value of

(9) |

(10) |

(11) |

(12) |

(13) |

where is the ratio of mass to magnetic fluxes, is the angular velocity of magnetic field lines, corresponds to the specific angular momentum (it includes magnetic torques), is the specific energy (Bernoulli) integral, and is the specific entropy. Also, is Boltzmann’s constant, and is the Newtonian gravitational potential. The wind velocity field is related to the magnetic field as

(14) |

CL94 first showed that one can obtain general self-similar solutions of the above system of equations of the form

(15) | |||||

(16) | |||||

(17) | |||||

(18) |

Here, is the launch radius of a characteristic field/flow line at the base of the wind at while and are respectively the magnitude of the vertical components of the magnetic field and the initial rotational wind velocity at the same foot point; and are dimensionless with while and denote the angular dependence of the pressure and wind density, respectively. The exponent is a free parameter that controls the radial scaling of the magnetic field. One sees directly that discriminates current-carrying wind configurations (when , grows with ; the wind carries a net axial current) from zero-total-current ones (when , for ; the wind carries a singular axial current and its corresponding return current; see CL94 and references). Obviously,

(19) |

where is dimensionless, , and is the poloidal magnetic flux through radius . The above scalings allow us to obtain the geometry of the poloidal field/flow lines (characterized by the value of ) as

(20) |

Note that the function characterizes the shape of all field/flow lines. That is, all field/flow lines are self-similar to the ‘characteristic’ field/flow line that originates at and on the disk. Self-similarity further implies that

(21) | |||||

(22) | |||||

(23) | |||||

(24) |

(25) |

where is a dimensionless adiabatic constant. The adiabatic speed of sound scales as

(26) |

Finally, one can combine the dimensionless forms of equations (9)-(25) that involve the dimensionless quantities as functions of , and thus express the poloidal projection of the momentum balance equation (5) [the so called generalized Grad-Shafranov (GS) equation] in the form of a second-order ordinary differential equation for as

(27) |

This equation (too complicated to write down explicitly in this paper) is integrated numerically from the surface of the disk (taken for simplicity to lie at ) to axial infinity (). The initial conditions are and , essentially a free-parameter that depends on the details of the internal disk structure, which, for a given value of , is adjusted in order for the wind to cross the Alfvn point (the point at which the the wind poloidal speed becomes equal to the local Alfvn speed - see CL94 for a detailed description) continuously and smoothly. According to equation (20), the form of the solution characterizes the poloidal shape of the field lines, and in particular, the initial condition characterizes the angle the poloidal field/flow lines make with the disk at their foot points [readers can easily verify that this angle is equal to ].

To numerically solve the above wind equation (27) we assume that the plasma is initially in Keplerian rotation at the disk surface with only a small out-of-the-disk velocity component ( at ). As a fiducial solution we fix the following set of parameters as described in CL94; , with kinematic variables , , and . With these initial conditions, the remaining conserved quantities are calculated as , and (see CL94 for details). The only freedom left is the value of that is obtained iteratively so that the wind passes smoothly through the Alfvn surface. This important physical constraint yields . Note that for sufficiently small (a magnetically dominated flow) its velocity is nearly Keplerian, setting the value of , while passing through the Alfvén point fixes and effectively the remaining constants of the flow, with as the one meaningful free parameter.

The obtained wind kinematics are shown in Figure 1a and the magnetic field components in Figure 1b. As discussed in CL94, different values of the exponent allow for distinct streamline geometries in the poloidal plane, which in turn is associated with other observable quantities of the wind (such as the density profile; see following sections). As is initially set up, this wind is launched from a thin Keplerian disk with only a small out-of-the-disk surface velocity component. The magnetic field there is dragged by the rotating plasma () resulting thus in a negative toroidal field component (). As the wind leaves the disk, magnetic torques act on the outflowing plasma and magnetic energy is efficiently converted into kinetic energy of the wind along the symmetry axis. The magnetic field also plays an important role in collimating the wind at large distances. In this particular case the wind is found to end up with terminal velocity roughly a few times the initial rotational speed and remains below fast magnetosonic speed.

The astute reader may note that X-ray heating is likely to produce thermal velocities inconsistent with the self-similarity of the sound speed invoked above (i.e. ; see Fig. 4). We will discuss this in §3.1.

Knowing the wind streamline described by equation (27) one can separately write down radial and angular dependence of the wind number density as

(28) |

where is the number density normalization at the initial characteristic launching radius , is the normalized angular dependence of the wind number density, and is the non-dimensional radial coordinate; is the proton mass and the mean molecular weight of the wind. In what follows, we will take the characteristic radius to be equal to the Schwarzschild radius, namely , taken to be the inner edge of the accretion flow with cm where is the mass of the black hole in units of solar mass . It is well known that free-fall spherical accretion at the Eddington rate () produces Thomson opacity one () at the Schwarzschild radius (). Using this scaling we can express our wind density normalization at the inner edge of the disk as

(29) |

where, is the ratio of of the mass-outflow rate in the wind to the mass-accretion rate , assumed here to be , and is the Thomson cross-section. It is important to note here that because the mass flux in these winds depends in general on the radius, a normalized parameter used throughout this work, , always refers to the mass flux at the innermost value of the flow radius, i.e. at .

Figure 2a exhibits a LOS angle () dependence of the wind density profile from the pole () to the equator () along a characteristic stream line of , normalized to unity at its highest value at , as obtained from the self-similar solution of Figure 1. This distribution illustrates the significant change of the LOS density (and also column density) with inclination angle (over three decades between ). The LOS wind velocity (in units of ) along a characteristic streamline is shown in Figure 2b. We see that increases as the LOS angle becomes smaller (toward the polar region) because the wind is magnetocentrifugally accelerated along the way, and furthermore, the direction of becomes more and more parallel to the total wind velocity as well [e.g. ].

In terms of the scalings of our wind model, the total equivalent hydrogen column density of wind over the LOS length scale of is given by

(30) | |||||

where the wind is considered to extend from an inner radius over a length scale of along the LOS. One should note that the configurations have the interesting property of equal column density per decade of radius, i.e. [as can be seen from Fig. 2a, is an excellent fit to the angular dependence of the density for where is measured in degrees]. For and these winds have a column density of cm per decade of radius. As a result, configurations that extend over a number of decades in radius can be quite optically-thick in these directions even for .

### 2.2 The Wind Ionization Structure

With the poloidal field configuration obtained by solving
equation (27) and the corresponding wind kinematics, we now
are in a position to consider its ionization structure assuming the
presence of a point-like X-ray source at the origin. To this end we
employ the photoionization code `XSTAR`

version 2.1kn9, which
solves simultaneously for the ionization balance and thermal
equilibrium of the locally illuminated wind.

The implementation of the above code involves a number of issues and leads to certain wind observables, amongst which are the following: () The ionization is locally determined by the photon flux per electron flux; a proxy for that is the ionization parameter , with being the luminosity of the ionizing source; () The computation of the ionizing flux requires the transfer of radiation from the source through the LOS wind, given that part of it can be removed by scattering and absorption; () Given that our wind models produce, in addition to the density , also the wind velocity field we are then able to compute also detailed absorption line profiles; () The broad range of the wind density with radius leads to ions with very diverse ionization states, whose distribution per logarithmic interval, the AMD, discussed in HBK07 and Behar (2009), can be used to determine the wind radial profile. We will discuss each one of these issues in detail below.

#### The Ionization Parameter

With the density profile at hand, the wind ionization structure, i.e. the local value of , requires also an expression for the X-ray luminosity. Since the models we present are global, i.e. they cover a large number of decades in radius, it makes more sense that we do not detach the ionizing luminosity from the global wind dynamics. In order to do so we need a prescription that connects the wind mass flux rate and the ionizing luminosity . The simplest assumption is that , i.e. to assume that the wind mass rate is proportional to the accretion rate onto the black hole (we assume they are equal), resulting in luminosity proportional . If this were indeed true, then the ionization structure of the wind would be independent of the accretion rate, since would drop out of the expression for the ionization parameter [c.f. eqn. (29)]. However, this is contrary to observations (e.g. Ueda et al., 2003; Tueller et al., 2008), which indicate that the probability of source obscuration decreases with increasing source luminosity (one should note, however, that obscuration may be also due to gas in galactic mergers; e.g. Hopkins et al., 2005). To incorporate this fact, we provisionally adopt the prescription , even though any power near 2 or greater would qualitatively suffice. We note that prescription would be appropriate for flows such as those discussed in Narayan & Yi (1995b) (provided that ; is the usual disk viscosity parameter) with otherwise; considering that the latter case is valid for only a small range in than the former, we adopt the former, bearing in mind its limits of applicability. Expressing the luminosity in terms of its Eddington value we can write

(31) |

where erg s is the Eddington luminosity of a one solar mass an accreting object and is the efficiency of conversion of mass into radiation for . Given the ionizing luminosity , and assuming the source to be point-like, located at the coordinate origin, the local value of the ionization parameter (ratio of ionizing flux per electron flux) is

(32) |

Using the luminosity, density and radius scalings given above this reads as

(33) |

Equation (33) thus provides the explicit dependence of the ionization parameter of the corresponding wind as a function of the accretion rate , the (normalized) distance from the source and the LOS angle for steady-state accretion at a rate into the black hole and actual mass outflow rate (at radius ) in the wind. Figure 3 shows poloidal color maps of (a) the wind density and (b) the ionization parameter for the parameters used to produce Figure 1 along with a number of contour curves (dotted curves with values) and the flow streamlines (solid curves). The diagonal dashed straight lines denote the self-similar surface of the Alfvn point. Here, we have assumed and erg s, which for implies . As seen, we obtain a non-recollimating, non-oscillating wind which asymptotically behaves as where as [or in cylindrical coordinates ; see CL94]. We would like to stress that the field line geometry depends on the wind’s conserved quantities in the model. As a consequence the obtained wind properties (shown here in Figs. 1 to 3) can change quite a bit.

In the context of our accretion-disk wind scenario the outflows are necessarily more opaque near the launching disk surface () at smaller radius as expressed in equation (28). Density profile along a magnetic field follows exactly the one shown in Figure 2a. There are several points to note about equation (33) and Figure 3b: () If distances are scaled by the Schwarzschild radius, , and the accretion rate by its Eddington value, , the ionization parameter, , depends primarily on the normalized accretion rate and ; as a result, our analysis and the corresponding ionization structure of the wind, are applicable to accreting black holes of any size. Note that, had one assumed , the expression for would be independent even of ; we believe that this would be in disagreement with observation; The ionization parameter is much higher near the central engine (e.g. within a few hundreds to thousands Schwarzschild radii) with the wind highly ionized in this region and for a given it drops precipitously with ; For a given , the value of drops with distance (with for our favorite value of ); () increases linearly with increasing accretion rate , implying decreasing source obscuration for high values of as seen in equation (30), in agreement with observation (Tueller et al., 2008); () The wind is fully ionized in regions sufficiently close to the central engine thus no contribution to the absorption lines in the spectrum.

One should note that, as written, the expression of equation (33) is a local one, i.e. it does not take into account neither the absorption of the X-ray radiation in its propagation along the LOS wind nor the corresponding re-emission, both of which would modify the local ionizing spectrum, and thus also the global ionization structure shown in Figure 3b here. These effects are small at small values of the radius ( and for relatively hard spectra ), where the ionization of the gas is high and its absorption depth small at all energies; they become more significant at larger radii and they are taken into detailed consideration in our model calculations as discussed below.

It should also be cautioned at this point, that while is the primary parameter that determines the ionization
state of the X-ray illuminated gas, the latter depends also on the
spectrum of the incident radiation, as the resulting electron
temperature is roughly equal to the mean photon energy of the
ionizing radiation. In the calculations presented herein we assume a
single power-law with an energy spectrum between 13.6 eV and 13.6 keV and
as a fiducial model (e.g. Sim et al., 2008). More realistic incident
spectral distributions (those used, e.g.,
in Everett, 2005; Sim, 2005; Schurch & Done, 2007) can be easily accommodated within
`XSTAR`

likely leading to results that are not substantially
different from those of the next sections, although we defer such
studies to future publications.

#### Radiative Transfer in the Wind

As noted above, equation (33) is strictly valid when the
attenuation of the radiation field by the wind itself is small; it
is used in the computation of the ionization state only for the
innermost, highly ionized regions of the wind, while at larger radii
we use the absorbed radiation field is employing `XSTAR`

for
the computation of the relevant opacities; the method is described
below and it is very similar to the recent work of, e.g.,
Schurch & Done (2007), Dorodnitsyn, Kallman & Proga (2008) and Schurch, Done & Proga (2009).
Since at present we are interested mainly in the absorption
properties of the above configuration, whose Thomson opacity is
generally small, we treat the gas along the LOS independently as a
collection of radially discrete slabs of constant (local) density,
and the total column depends only on the LOS angle in
accordance with Figure 2a. At large distances
where the value of the ionization parameter drops and He and H
opacities become important, we let `XSTAR`

subdivide each
zone as necessary for the proper treatment of the radiative
transfer; since in this case the absorption mean-free path at the
characteristic frequencies is much smaller than the local radius,
the plane parallel geometry employed by `XSTAR`

for this
purpose is adequate.

With the ionizing luminosity and a spectrum specified at ,
the entire LOS wind with the radial length scale of is divided up into a number of (plane parallel)
slabs/zones (typically ) of logarithmically-equal thickness
in radius; i.e. .
Then, using `XSTAR`

we calculate the absorption and emission
coefficients within, say, the -th zone, using as input the
(properly normalized) output spectrum of the -th zone, . We
thus obtain the forwardly emitted spectrum in emission lines
and in continuum by
computing the free-free, free-bound and bound-bound atomic
transitions within the -th zone (see `XSTAR`

manual),
while we ignore for this calculation the part of the backward
directed flux. We also compute the fraction of the radiation flux of
the -th zone, , that is transmitted through the -th
zone, , given by

(34) |

where is the optical depth (including continuum and line photoabsorption as well as Thomson scattering) of the -th zone, with being the total hydrogen equivalent column of this slab. Finally, we produce the (properly normalized) spectrum of the -th zone, by adding the forwardly emitted and transmitted spectra, i.e.

(35) |

with the process being iterated with in place of , to compute and so on.

#### Modeling Absorption Line Profiles

The above procedure can be applied to a specific atomic transition to produce the resulting line profile and an absorption feature since this is the dominant process along the observer’s LOS to the point-like ionizing source. The corresponding emission is distributed isotropically and makes a negligible contribution to specific intensity at the particular frequency. The radiation transfer of a specific feature is dominated by the optical depth of the wind at the specific frequency , which is expressed by

(36) |

with the line photoabsorption cross-section

(37) |

where is the oscillator strength of the transition between the th and th levels of an ionic species and is the Doppler broadening factor estimated by relative to the centroid (rest-frame) frequency with being either thermal or turbulent velocity of the medium, assuming that the overall absorption profiles are well approximated locally by the Voigt function (e.g. Mihalas, 1978; Kotani et al., 2000; Hanke et al., 2009). This represents a line profile whose centroid is dominated by the Doppler broadening while the wings are characterized by the damping/Lorentzian profile and defined by

(38) |

In the above expression, we use where is the Einstein coefficient and is the dimensionless frequency spread about the transition frequency. Irrespective of their thermal or turbulent velocities, the winds we consider provide a well defined velocity shear between two adjacent slabs, whose effect on the radiative transfer of a line photon is very similar to that of the turbulent velocity. To rid the situation of as much unwanted uncertainty as possible we then consider the thermal and turbulent broadenings to be negligible and we consider only the shear broadening, so that

(39) |

with being the LOS velocity shear. In addition to the broadening, the velocity of the absorbing medium shifts also the transition frequency blueward as where is the flow velocity along LOS and is the overall observed frequency. With these considerations the expression for the dimensionless frequency spread about the specific transition reads

(40) |

#### Modeling the Absorption Measure Distribution (AMD)

In a wind model with well-defined density as a function of radius along the LOS, it is natural to use the value of , the parameter that determines the presence (or not) of a given ion, as a proxy for the radius along the wind in order to study the structure of its ionization. Then the hydrogen equivalent column of specific ions, , as a function of can be used to determine the wind density distribution as a function of radius. This has been precisely the approach of HBK07, who defined the AMD as the hydrogen equivalent ion column density per logarithmic ionization parameter interval; in view of our specific wind models, this has the following dependences [Eqns. (30) and (33)]

(41) |

Therefore, depending on the specific run of the wind density with radius (via ), the AMD is constant, i.e., independent of the radius or ionization parameter of the plasma when , while it scales as , i.e., monotonically increasing with ionization for the BP82 models ().

## 3 Results

In this section we discuss in detail the implementation of the procedures described above and the ensuing results concerning the properties of individual atomic transitions as well as their dependence on the parameters of the problem. In particular we focus on specific ionic charge states that are important in that they can serve as spectroscopic diagnostics of the ionization state of the wind medium. Because of the specific, continuous decrease of the MHD wind density inherent to the accretion-origin wind scenario, our models span a wide range of ionization parameter space and hence a large number of the corresponding atomic transitions (in absorption). Their global properties are encapsulated in the AMD, namely the distribution of (locally) absorbing column per logarithmic ionization parameter interval, a quantity originally introduced by HBK07, which can and has been compiled for a number of AGNs using comprehensive fits to the ensemble of absorption features in their entire X-ray spectrum (Behar, 2009). Furthermore, given that to each ionization state of the plasma corresponds also a specific wind velocity, there exists a correlation between the presence of a specific atomic transition and the corresponding plasma velocity. Employing this generic property, we demonstrate a progressive absorption of the incident X-ray by matter outflowing at the different velocities (as discussed in §2.2), to produce the eventual absorption line profile of specific transitions. Finally, because of the strong dependence of the wind column density along the LOS angle , as discussed in §2.1, we consider two representative cases for comparison [employing always the field geometry and the parameters used in producing Figs 1-3], namely (high latitude LOS) and (low latitude LOS).

Considering the underlying complexity of the observed broad-band SEDs of AGNs we have decided to adopt the simple prescription of a single power-law form for the ionizing flux discussed above and use different values of its slope to simulate the diversity of observed AGN SEDs. This approach, while it should be viewed with caution vis-á-vis the detailed properties of the wind ionization, we believe that it is sufficient in capturing the trends of the winds’ ionization properties with changes in the overall AGN SED. The photoionization calculations we present include the most important elements (H, He, Ca, Na, O, Ne, Mg, Si and Fe) with abundances set to the solar values (Grevesse, Noels & Sauval, 1996). Based on this set-up the major characteristics of our hydromagnetic wind are listed in Table 1 which we shall discuss in subsequent sections.

Parameter | Fiducial Value () | Physical Significance |
---|---|---|

Mass of the central black hole in units of | ||

Power-law index of the incident spectrum (in energy) | ||

erg s | Incident X-ray luminosity | |

Radius of the innermost foot point of the wind | ||

1 | Scaling of magnetic fields | |

0.1 | Dimensionless (conserved) mass-accretion rate | |

0.5 | Outflow (wind) rate relative to mass-accretion rate | |

0.2 | Radiative efficiency | |

Dimensionless LOS Inner radius of the wind | ||

cm | Density of the wind at | |

LOS length scale of wind | ||

8.62 / 8.3 | Ionization parameter at | |

(Fe xvii) | km s | Characteristic LOS velocity of Fe xvii |

(Fe xvii) | Ionization parameter of Fe xvii | |

(Fe xvii) | LOS distance of Fe xvii | |

(Fe xxv) | km s | Characteristic LOS velocity of Fe xxv |

(Fe xxv) | Ionization parameter of Fe xxv | |

(Fe xxv) | LOS distance of Fe xxv | |

(O vii) | km s | Characteristic LOS velocity of O vii |

(O viii) | km s | Characteristic LOS velocity of O viii |

cm | Local wind column density per slab | |

cm | Integrated wind column density over |

See the text for the template parameter values in detail.

### 3.1 Absorption Measure Distribution (AMD)

The unique characteristic of any wind model ionized by a point-source located at its origin is the radial distribution of density and therefore the corresponding distribution of the ionization states of the different elements seen in absorption in the source continuum. A particular wind model is therefore characterized by the distribution of the ionization states of the different elements, their velocities and the distribution of their column densities or their (local) equivalent hydrogen column ; these determine the run of the wind’s density and velocity with the radius . For example, in the accelerating phase of a spherical wind, both the ionization parameter and the velocity increase with distance and “freeze” once it has achieved its terminal velocity, while the column density of ions decreases faster than if an ion is present in the wind accelerating stage, leveling off to once terminal velocity is achieved.

The characteristic properties of the winds presented in §2 are drastically different from those of spherical winds. In particular: () The ionization parameter and the corresponding LOS velocity decrease with distance as and respectively to encompass a large number of ionization states of many elements at different velocities. () The specific column density per decade of radius translates for any element to a (local) equivalent hydrogen column that is independent of the radius .

For a given wind model and ionizing spectrum, one can produce the
corresponding AMD profiles, i.e. the global distribution of its
ionization properties which can then be compared to observations. We
do so in this section and compare the results to the recent AMD
analysis of IRAS 13349+2438 observations (HBK07). The results of our
calculations are shown in Figure 4 where we present the
AMD for the wind models, with the plotted as a
function of for in (a) and in
(b). Also superimposed is the plasma (gas) temperature
computed by `XSTAR`

under local thermal equilibrium conditions
along with the analytic self-similar (SS) temperature (). The ionized wind temperature decreases monotonically from K down to K as decreases from
to a range relevant to the
observable ionic states of the major elements. For reference, the
corresponding (dimensionless) LOS distance from the
central engine is also shown in the upper x-axis where in this run
cm. As seen, the local column densities
of the irradiated ions (shown here are the six major elements: N, O,
Ne, Mg, Si and Fe) are found to be all distributed at constant value
of over many decades of (and therefore a similar
range in LOS distance too), namely cm for and
cm for , reflecting the different wind density at
these different LOS (see Fig. 2a). This results in
an integrated column of cm for
and cm for over
. The constant value of AMD is a
unique characteristic of the models with the value
corresponding to case (a) () in good agreement with
the observed AMD of IRAS 13349+2438 analyzed by HBK07.

As shown here, the computed temperature has a radial dependence
(gradient) close to the desired one for , but it
is constant for . However, because the thermal
pressure is smaller than the wind ram pressure over the entire
domain, the thermal pressure effects on the wind density profiles
are not significant. We have also compared the heating/cooling time
scales of `XSTAR`

and were found to be shorter than the local
dynamical time scale , indicating that the temperature
distributions of Figure 4 are indeed correct, even
though not dynamically important. We have obtained by another
calculation a wind solution similar to Figure 4 in the
cold-flow limit ().

It should be noted that the decrease of at high values
of is due to the fact that `XSTAR`

by default does not
provide the column density of fully ionized (bare) ions. This
apparent decrease is just due to the fact that all considered
elements become progressively (completely) ionized at high
values. At the other end of the plot, i.e. for small values of
, appears to decrease too because the wind becomes
too cold (gas temperature of K) to participate
in radiative processes, i.e. each species turns neutral, an
ionization state also not included in the calculation of the
hydrogen equivalent column. The calculated AMD is otherwise
constant, as expected. The fact that the corresponding
is the same in this regime irrespective of the elements used in the
computation is a testimony that our models implement `XSTAR`

correctly, so that the sum of the abundances of all ions of any
element, when corrected for the elemental abundance, yields the same
value of . We also see that the (relatively) lighter
elements (say, oxygen) become fully ionized at lower than
heavier ones (say, iron), also as expected. In essence, the overall
trend of the model AMD in both LOS cases (a) and (b) appears to be
very similar to one another (i.e. constant value of
independent of ionization state) except for the fact that the local
column for in (a) is about a factor of lower than that for in (b) because of the angular
dependence of the wind density function (also see
Fig. 2a).

It is also of interest to show the differential form of Figure 4, i.e. the columns of specific charge states of a given ionic element . This is shown in Figure 5 for iron again for two different LOS. This figure shows the emergence of various ionization states of iron (shown here are Fe iii, Fe vi, Fe x, Fe xiii, Fe xvii, Fe xx, Fe xxv and Fe xxvi) along with the corresponding LOS velocity for in (a) and in (b) corresponding to Figure 4. As discussed above, the higher ionization states are present at the inner sections of the wind (smaller ), being replaced by lower ionization ions at larger radii with their columns given in absolute values instead of the hydrogen-equivalent values . One should note that the maximum value (peak) of for a specific charge state is approximately constant until one gets to the lowest ionization states, located at the largest distances (see, e.g., Murray & Chiang, 1998, for a similar transition) because the fraction of neutral iron relative to the total iron starts increasing as mentioned earlier for Figure 4. Of interest is also the LOS wind velocity that corresponds to a given value of . While decreases like at high values of (as and ), it deviates from this dependence at the largest radii because of the additional reduction of the X-ray flux due to absorption. The velocity at which each ion has its maximum column and the range in over which it has substantial column are of interest because they determine the absorption line profile of the specific ion. Thus, in the case of (a) , higher charge states such as Fe xxv are found to be blueshifted by a relatively high outflow velocity, km s at () while lower charge states such as Fe xvii are blueshifted by only km s at (). We emphasize that the latter (Fe xvii) line velocity and column density are also in good agreement with those of IRAS 13349+2438 (HBK07). For in comparison, the column density increases times but the corresponding line velocity and ionization stage remains roughly the same (but at smaller distances) because both the poloidal velocity and its projection to the LOS are smaller at lower latitudes (see Fig. 2b).

To conclude this section, we show in Figure 6 the column densities of specific charge states of oxygen again for two different LOS at (a) and (b) , along with the corresponding velocities overplotted as in Figure 5. As expected the corresponding outflow velocities are smaller for O vii ( km s at or ) and larger O viii ( km s at or ) for (a) , while similarly for (b) we find km s at () for O vii and km s at () for O viii, with the former having lower column per ion than the latter, as expected.

One should note that the precise correlations between the wind variables and the observables (i.e. , ) in the present model are primarily a function of the specified mass-accretion rate and LOS angle as well as the incident X-ray spectral index and therefore the model has the freedom to alter the resulting AMD distributions depending on the intrinsic properties of AGNs (here we focused on IRAS 13349+2438 as a case study).

### 3.2 Absorption Line Spectra

As discussed in the previous subsection and exhibited plainly in Figures 5 and 6, specific charge states of the different elements are present at different values of to which correspond different values of column density and velocity. We have also indicated that the simplest assumption about the optical depth of a specific transition is that it is determined by the velocity shear of the wind, a quantity that is also calculable within our models [see equation (37)]. Armed with this information we present in this section the profiles of specific atomic transitions in absorption. With the spectral emissivity and velocity given, we are also in a position to calculate the corresponding emission profiles. However, since the most prominent AGN lines lie in the O-UV part of the spectrum, a comprehensive approach would require also a more precise model of the UV part of the spectrum; as such we defer line emission to a future work.

A demonstration of the progressive effect of absorption on the transmitted spectra is presented in Figure 7. This figure exhibits the spectra between 1 eV and 10 keV of the radiation transmitted past the innermost slab 1 (power-law) through the subsequent slabs indicated by the values of for two different LOS angles, (a) and (b) . Absorption by the consistently ionized wind becomes apparent first at energies keV, becoming progressively deeper and shifting to lower energies as the radiation propagates through larger wind column. Absorption also increases with the inclination angle as one would qualitatively expect. Note that in this simplistic model the incident radiation includes only the X-ray power-law continuum ignoring all the other (potentially rather important) components. Also, it ignores emission that eventually may come into our LOS due to reflection and scattering in the wind. For this reason, the deep absorption imprinted in Figure 7 should not be interpreted literally in a quantitative sense, but as a qualitative indicator of the absorption as a function of along a given LOS.

Let us turn our attention to specific atomic transitions, namely those of Fe xvii and Fe xxv of column with velocity as a function of as given in Figure 5 and shear given by our model. Using the expressions for the photoionization cross-section and Voigt function [eqns. (36)- (38)] one can construct the characteristic absorption profiles; these include both the Doppler blueshift due to LOS velocity and the line broadening of the Voigt function in equation (38). Figure 8 shows a sequence of the simulated absorption line for Fe xvii with the rest-frame wavelength at Å (upper panels) and Fe xxv with the rest-frame wavelength at Å (lower panels) for two LOS angles, (left panels) and (right panels). We focus here on these prominent iron charge states because they are less contaminated by other adjacent spectral features. We adopted the following values for the relevant atomic data: and s for Fe xxv/Fe xvii, respectively. The figure provides the spectra transmitted through increasing wind column along the LOS. The absorption line obtains its largest blueshift and broadest contribution by ions at the higher values of , becoming progressively deeper, less blue-shifted and narrower as the contribution to the absorption is affected by regions of lower (larger ) which provide the highest column of the specific ion (and also smaller velocities and shear). Again, the spectra are broader and deeper for the higher LOS angles reflecting higher (local) velocities at specific values of and higher overall columns.

In concluding this section we would like to point out the work of Gabel et al. (2003) on the UV absorption features of NGC 3783 which were found to have velocity structure in agreement with that of the corresponding X-ray ones, thereby arguing for the consistency of the entire wind structure. Also, Collinge et al. (2001) have found that the low ionization Fe absorption features of NGC 4051 had corresponding UV absorption features, while the high ionization, higher velocity X-ray absorption features of the spectrum lacked an equivalent UV absorption, indicating the absence of these ions in the higher ionization, higher velocity plasma.

## 4 Summary and Discussion

In this work we have presented a detailed study of the ionization
structure of model MHD winds off accretion disks; this is our first
attempt to model within this context the recent observations of
absorption features in the ASCA, XMM and Chandra X-ray
spectra, the so-called warm absorbers. To this end we have employed
the self-similar 2D hydromagnetic wind models developed by CL94 that
provide the fluid 2D density and velocity fields, which we coupled
to photoionization calculations using `XSTAR`

. Our
consideration of magnetocentrifugal (MHD) winds/outflows in this
work has been motivated and supported in part by recent
observational implications that at least in a number of AGNs and
GBHCs the inferred driving mechanism of the observed X-ray ionized
wind medium is magnetic rather than thermal or radiative (e.g., see
Miller et al. 2006, 2008 for GRO J1655-40; Kraemer et al. 2005 and
Crenshaw & Kraemer 2007 for NGC 4151).

Given the scope of our paper, our model wind is necessarily overly simple. It ignores a host of issues that affect the structure of winds off accretion disks and replaces them with the self-similar models of CL94. The interested reader can get a feeling of the multitude and complexity of the issues not addressed in the present treatment by looking at the works of, e.g., Proga (2003) and Proga & Kallman (2004) (and references therein) and also Ohsuga (2009, for disks with several distinct values of the accretion rate ). These include, among others, the radiative transfer in the wind, the ensuing effects of radiation pressure and also the influence of the vertical gradient of in the launching of the wind. As shown in these references the winds can be radiation driven in the inner part of the disk (due to the increased flux at this spatial domain) while being magnetically launched at larger radii. In this respect our model winds are quite different in structure and variability from the more realistic winds of Proga (2003) at small radii, while they should be more similar to those of his at larger radii where radiation pressure is smaller and the wind is magnetically launched. Realistic models must by necessity consider the transition of the underlying disk from radiation pressure, at small , to gas pressure dominance at larger radii; this fact would likely force a different choice of our boundary condition and therefore yield a field geometry that breaks the self-similarity of our solutions. Wind models very similar to those used herein but with the inclusion of the effects of the radiation pressure that break the self-similarity were discussed by KK94 and Everett (2005).

One should therefore view our models with the above caveats in mind. The significance and assumptions of the models we propose is basically justified a posteriori by their ability to interpret the observations. Self-similarity is one of the fundamental assumptions of our model winds. However, whether exactly self-similar or not, any model that would attempt to account the entire range of ionic species shown e.g. in Behar (2009) must by necessity cover a very broad range in the photoionization parameter . Then, the column of each such ion provides a measure of the corresponding hydrogen equivalent column as a function of , i.e. the AMD. These two quantities () can then be employed to provide a measure of the gas density as a function of the distance from the X-ray source. Barring the possibility of several independent regions at different distances but similar columns as indicated by the functional form of the AMD (one could consider this is possibility at the risk of introducing an inordinate number of free parameters), models with radial density profiles as those considered here are a natural consequence of the AMD obtained by the Chandra observations.

The wind ionization structure was followed in 1D as described in §2.2, namely along the observer’s LOS, assuming the ionizing source to be point-like. Clearly, a more comprehensive treatment of this problem should take into account also the backward emitted radiation which will reach the observer from the regions of the disk on the other side of the black hole, as well as the scattered radiation, whose effects could be significant. We plan to return to these issues in a future publication.

The 2D structure of the winds considered in our analysis implies, at a minimum, a two-parameter description of the absorption features. However, the self-similarity of the problem simplifies further the treatment by allowing the separation of the and variables with the wind density obtaining the form . The parameter is a most important parameter of these models because it determines both the radial dependence of the ionization parameter and the wind column density per decade of radius along a given direction (LOS). In the models examined in the present work we restricted our study to the value , which leads to a radial density profile . This is an interesting profile in that it provides for an ionization parameter with a similar dependence, i.e. , and most importantly, with equal column per decade in radius, across the entire range in radius and the corresponding range in ; as a result, ionic species of very different ionization properties, existing over a wide range of ionization parameter (and radius), have roughly comparable column densities, independent of the distance and are therefore possible to detect. As noted in CL94, the value of determines also the axial current distribution in radius within the wind, with the corresponding magnetic energy per unit length at the wind base being also constant per (cylindrical) decade in radius. It is worth comparing our work with that of KK94, who used the same type of MHD wind with the value of as we do herein: while these authors focused their study on the effects of dust on radiation transfer, we focus our attention on the effects of the ionizing radiation on the X-ray spectra of AGNs, in particular on the ionized absorbers. KK94 also noted in passing the relevance of their models to the X-ray AGN spectra well ahead of the detailed outflow observations made with Chandra.

While the structure of the wind in and is provided by the models of CL94, for the remaining parameters of our models, namely the normalization of the wind density and the X-ray luminosity of the ionizing source we have chosen to use the scalings of ADAFs, or better ADIOS; as a result the X-ray luminosity is proportional to the square of the (normalized) accretion rate at the inner edge of the disk rather than simply , assumed in standard accretion disks. Therefore, restricting ourselves to models with , the global ionization structure of a given wind, including the normalization of the column density, depends only on two parameters, namely and the observer’s inclination angle . This parametrization provides an extremely economical set of assumptions concerning not only the outflows, i.e. the wind ionization structure seen in absorption in detailed X-ray spectra, but also for the entire (radio-quiet) AGN unification picture: Figure 2 which exhibits the normalization of the wind density as a function of along the magnetic field line of , makes apparent the difference in column between face-on and edge-on views, implying that the wind, if extending to sufficiently large radii, can in fact serve as the proposed molecular torus associated with AGN unification, a point originally made by KK94, also for winds with ; it is of interest to note that the few objects for which sufficiently detailed observations exit are consistent values (HBK07; Behar, 2009). Within this same context and ionizing luminosity considerations, one should note the dependence of source obscuration on the X-ray luminosity, namely its reduced value for objects accreting at a higher fraction of their Eddington rate , which apparently is in general agreement with observations. It remains to be seen whether these notions can withstand the scrutiny of more consistent and encompassing observational tests.

At this point we would like to stress the importance of the AMD in the study of AGN outflows/winds, a quantity enunciated by HBK07 and modeled in detail in the preceding sections. Analyses similar to those of HBK07 and Behar (2009) are indispensable because they produce a consistent analysis of the entire set of absorption features in the AGN X-ray absorption spectra. At the same time they underscore the unique value of X-ray spectroscopy which, in a wavelength band of decades, can encapsulate the properties of ions that span orders of magnitude in ionization parameter and, for models with , a similar range in radius; at the same time, measurement of their absorption columns yields the equivalent hydrogen column of the flow, , over a similar range in radius, thereby going a long way toward the determination of the physics underlying the outflow dynamics. The fact that the AMD analyses to date are roughly independent of provide support to our use of the or models, reiterating that a similar density profile was invoked on the basis of AGN and GBHC timing properties (Papadakis, Nandra & Kazanas, 2001; Kazanas, Hua & Titarchuk, 1996).

We have thus presented a concrete example of the AMD dependence on for our models with and two different values of the observer’s inclination angle (see table 1 for details). As expected we found the AMD to be constant, i.e. independent of , over many decades in this parameter (i.e. the local column density is independent of ionization states of ions). With , equation (30) implies cm (yielding a total column of cm) for and cm (total of cm) for over erg cm s, in good agreement with the observed AMD of IRAS 13349+2438 (HBK07; Behar, 2009) and also some other AGNs detailed below. One should note that these values depend primarily on and and are independent of the black hole mass. The mass of the object gets involved only as a measure of its total luminosity, which does not appear in the expression for , implying that these models could in principle be applicable also in GBHCs. High quality X-ray absorption data are in fact available for the GBHC GRO J1655-40 and were used to argue for magnetic driving of the wind in this system too (Miller et al., 2006, 2008). These spectra are distinguished from those of AGNs by the prominent absence of low ionization state ions. This is to be expected given that the presence of the companion star limits the extent of the disk to roughly half the distance between the two objects or cm. Given that the Schwarzschild radius of the compact object is cm the entire disk size covers only a range of in radius; considering (based on Fig. 4) that in the inner region of the wind ( cm) major elements (even heavier species) are almost fully ionized, one would expect the presence of ions over only a factor of 1000 in , in rough agreement with the observation.

Given that our models provide also the complete velocity field of the MHD wind we have also produced a sequence of synthetic absorption profiles as described in §2.2 and shown in §3.2. We have done so for two charge levels of Fe, namely Fe xxv and Fe xvii. With our fiducial model predicting the Fe xvii column to be maximum at erg cm s, we then infer the corresponding LOS velocity (see Fig. 5) to be km s in excellent agreement with the observed values of IRAS 13349+2438. It is important to note that the model produces not only the correct velocity at the maximum value of but also the observed normalization for the same inclination angle. It is therefore possible with measurements of the combined line widths and column densities to reproduce within the present models both , and , thereby providing a complete specification of these winds. In addition to IRAS 13349+2438, the nearby bright Seyfert MCG 6-30-15 has been observed to show, as one of the multiple ionization zones, an X-ray ionized absorber with an outflow velocity of km s at and cm (e.g. Young et al., 2005; Holczer, Behar & Arav, 2009) also in good agreement with our model results for (see Fig. 5). Clearly, a different choice of a set of conserved quantities (wind variables) in the model would produce a slightly different field line geometry in which the resulting MHD outflow could in principle obtain higher LOS velocities (perhaps by factors of magnitudes), and this will be studied in detail in a future work.

As noted above our model is quite successful in reproducing the observed AMD of IRAS 13349+2438. More recently, Behar (2009) presented a compilation of the AMD of a number of AGN with