text:
\section{Introduction}
Titarchuk \& Shrader (2005), Paper I, hereafter TSh05,  have shown  that downscattering modification of the primary photon spectrum by an outflowing plasma is a possible mechanism  for producing  the continuum excess in the $\sim10$ keV spectral region. This continuum excess can be formed only  if the energy index of the primary photon spectrum is less than one (see also Sunyaev \& Titarchuk 1980, hereafter ST80).
This is usually attributed to Comptonization by a static reflector, such as a downward- or
obliquely-illuminated accretion disk,  although the overall continuum
form differs from that of the basic Compton reflection form. TSh05 thus suggest, that  in at least some cases, the outflow downscattering effect rather than the standard Compton reflection  mechanism is
responsible for the observed ''excess`` hard-X-ray continuum.

To obtain  a description of the X-ray photon spectrum,  many  authors (see e.g. Gilfanov, Churazov \& Revnivtsev 1999, hereafter
GCR99, Pottschmidt et al. 2003, and etc)
 used an empirical model in which each source spectrum is a sum of power law spectrum with photon index
$\Gamma$ and a multi-temperature disk blackbody. To this continuum, a reflection spectrum after Magdziarz  \& Zdziarski  (1995) was
added.

However,  Shaposhnikov \& Titarchuk (2006), hereafter ST06  argue that these spectral features are results of reprocessing  of the central
 source hard radiation in the outflow (warm wind)
that surrounds the central BH. This  claim is supported by observed  power decay of quasiperiodic oscillations (QPOs) towards the softer states that is presumably a result of reprocessing of time signal in  the extended relatively warm wind (see Fig. 6 in ST06).

The basic idea is that
electron  scattering of photons from a central source
entering the expanding outflow experience a decrease in
energy (downscattering). The magnitude of this decrease is of first order
in $V/c$ and in $E/m_ec^2$ where $V$ is the outflow speed,
c is the speed of light, $E$ is the initial photon energy
and $m_e$ is the electron rest mass.

TSh05 have developed an analytic formulation for the
emergent spectrum resulting from photon diffusion in
a  spherically expanding Comptonizing media,
characterized by two model  parameters: an average number of scatterings in the medium $N_{av}$, and
efficiency the energy loss in the divergent flow $\varepsilon$.
In this formulation of the Radiative Transfer problem, the number of photons
emitted in the wind shell equals that which escape to the Earth
observer  (i.e. the photon number is conserved). Consequently,  if   the high energy photons lose
their energy on the way out but the number of photons is conserved, it  has to result in the accumulation of the photons
at a particular lower energy band.

 The basic idea of the wind photon  downscattering  is depicted in Figure 1. There  presents a simple explanation
of the diverging flow  effect
on the photon propagation through the medium.
A photon emitted outwards near inner boundary and then
scattered at a certain point by an electron moving with velocity ${\bf V}_1$, is
received by an electron moving with velocity ${\bf V}_2$ as shown with
frequency $\nu _2 = \nu _1\left[1+\left({\bf V}_1-{\bf V}_2\right)
\cdot{\bf n}/c\right]$ where ${\bf n}$ is a unit vector along the
path of the photon at the scattering point.  In a diverging flow
$\left({\bf V}_1-{\bf V}_2\right)\cdot{\bf n}/c <0$ and photons are
successively redshifted, until scattered to an observer at infinity.
 The color of photon path  (in Figure 1) indicates
the frequency shift in the rest frame of the receiver (electron or the Earth
observer). On the other hand, referring to the right-hand side of Figure 1,
in a converging flow
$\left({\bf V}_1-{\bf V}_2\right)\cdot{\bf n}/c >0$ and photons are
blueshifted.

In this Paper we present the results of extensive Monte Carlo simulations of the downscattering effects in the
wind (diverging flow). In addition to the scattering, Doppler and Compton effects we include a photoabsorption effect in the diverging flow (wind).
Any photon with energy of about 7-8 keV and higher interacting with outflow plasma is more likely to be absorbed by the flow and be reemitted at energies about
6.4-6.6 keV, depending on the ionization stage of the flow (see Kallman et al. 2004). Laming and Titarchuk (2004), hereafter LT04, calculated the temperature and ionization balance
in the outflow determined by seeking the temperature at which the outflowing gas attains photoionization-recombination equilibrium.
The gas is heated by Compton scattering and photoionizations by photons from the central compact object and is cooled by radiation, ionization,
and adiabatic
expansion losses. The solution of this  problem is  general regarding the calculation of the  temperature and ionization balance in the target
illuminated by the hard radiation. It potentially  has many applications beyond  Astrophysics
(for example, in   Radiation Safety Physics). Our simulations allow us to reveal {\it the spectral, timing and absorption properties of the emergent radiation}.

We  update the analytical results of the downscattering modifications of the continuum obtained by TSh05 (using Fokker-Planck technique)
and we verify them using  the Monte Carlo (MC)
simulated spectra. We demonstrate that the  analytical formulas for the continuum spectra well describe
 the MC spectra almost for any $\beta=V/c\lax 0.8$.

Many authors [e.g. Tanaka et al. (1995); Nandra et al. (1997); Wilms et al. (2001);
Uttley et al. (2004); Miller et al. (2004a,b)]
have found unusual curvature (red-skewed  features) at energies between 2 and 8 keV in X-ray spectra of a number of
galactic and extragalactic BH sources. Significantly the fluxes of these features remain nearly {\it constant}
despite the large changes in
the continuum flux as shown in the observations of MCG-6-30-15, NGC 4051 and others [Markovitz,
Edelson, \& Vaughan (2003)]. This lack of variability means that fast changes (which are almost certain to occur near
the BH) are not obtained.
These observations motivate us to make a detailed study of the spectral line formation in the outflows that  possibly occur in black hole sources.
In this Paper we  demonstrate that  red-skewed  features can be a  result of scattering of iron line photons  in the powerful outflow.

We offer a model in which the hard radiation of the central object illuminates and heats the outflow (wind) region
originated in the outskirts of the disk (well outside the innermost part of the accretion disk near the BH).
The line photons are generated and scattered in the
outflow.
Our basic scenario is illustrated in Figure 1. The
wind originates at a distance $r_{in}$ from the central black hole
and is of a density such as to give a Thomson scattering optical depth $\tau_{\rm T}$
close to unity far from the black hole. The optical depth in the Fe K
continuum is about 1-3 times higher than that due to electron scattering
(assuming a solar abundance of Fe, and depending on charge state, see
Kallman et al. 2004),
and so Fe K$\alpha$ formed by inner shell ionization of Fe ions in the
outflow by the continuum from the central black hole only comes from a
smaller inner region.
In fact,  using the calculations of the  ionization state of the outflow shell
by  LT04,  we find that K$_\alpha-$photon sources are exponentially
distributed  over  a skin at the bottom of the outflow, the skin thickness being $4\%$ of the optical depth of the wind shell.
Furthermore because
the iron photo-absorption opacity $\sigma_K$ is about few times
the Thomson opacity, $\sigma_{\rm T}$, any photon
around the K-absorption edge energy must be absorbed. In fact, these edges are seen with the strong
K$_\alpha$ lines during  X-ray superbursts detected from NS source 4U 1820-30 (see  Figs. 5 and 9 in Strohmayer \& Brown 2002).

A thorough analysis  and review of the diffusion theory of photon propagation
in an optically  thick fluid in bulk outflow
has been provided by Titarchuk, Kazanas \& Becker (2003), hereafter TKB.
They show that  the iron line is produced in an effectively optically thick medium.
Its red wing is the result of multiple scattering,  each scattering producing a first
order $V/c-$redshift. This process produces a red wing
to the line without any particular fine-tuned geometric arrangement.

  The TSh05 and TBK results are obtained using the Fokker-Planck equation [Blandford \& Payne (1981) see
also Lifshitz \& Pitaevsky (1981) for a general treatment of the particle acceleration problem]
which   is valid for $\beta=V/c\ll 1$ and $\tau_{eff}>1$. The MC
method does not have these limitations.

We show the results of MC simulations of scatterings of continuum and monochromatic photons
for various values of plasma temperatures $kT_e$, outflow bulk velocity  $\beta$, and Thomson optical depth
 $\tau$. The details of the MC method applied to the outflow model are given
in \S 2.    We  compare the results of the MC simulated continuum with their analytical description and discuss the downscattering modifications
of the incident spectrum in \S \S3.1-3.2  The results of  the simulated line formation in the outflow and its explanation
using the analytical theory are shown in \S 3.3.
 Examples of the model fits to the XMM data obtained for MCG-6-30-15
and to ASCA archive data of galactic BHs
are shown in \S  4.
The results of the simulations of overall spectra including the scattering, photon absorption effects are presented in \S 5.
Discussion and conclusions follow in \S 6.

\section{Details of the Monte Carlo Method}
Laurent \& Titarchuk (1999), hereafter LT99, simulated the Comptonization of photons
using a Monte-Carlo method in the  Schwarzschild metric.
The geometry used in these simulations consists of a spherical shell harboring a black hole
in its center.  Once given the cloud Thomson optical depth $\tau$,
 $N_e$ is an electron number density measured in
the local rest frame of the flow that is
\begin{equation}
N_e=\tau (r_{\rm S}/r)^{2}/[r_{\rm S}\sigma_T(r_{\rm S}/r_{in} - r_{\rm S}/r_{out})].
\label{electrden}
\end{equation}
Here $\sigma_T $ is the Thomson cross section,
$r_{in}$ and $r_{out}$  are the inner and outer radii of the shell respectively,
and $r_{\rm S}$ is the Schwarzschild radius.
Simulations
made for different values of  $r_{in}$ and $r_{out}$ (that are much greater than the Schwarzschild radius) have shown
no change of the line profile and continuum
provided the shell optical depth remains the same.
We have varied  the shell electron temperature from 0.01 to 1 keV.
Along with the thermal motion of the electrons in the cloud,
we have also taken into account the bulk velocity of the outflow $\beta=V/c$.
In these simulations, the spherical wind has a constant bulk velocity within the flow.
It is worth noting that an increase of the shell temperature from 0.01 to 1 keV
 slightly increases the blue wing of  the observed line, but induces no change in the red wing  that
we are mostly interested in here.

For the timing studies described in the next section
we have also computed   the path length  that each photon  in the simulations  has
covered until it escapes from the shell.

\section{Dowscattering effect in an outflow}
The problem of photon propagation in a fluid in bulk motion has been studied in
detail in a number of papers [see e.g.  Blandford \& Payne (1981),
 Payne \& Blandford (1981),  Nobili, Turolla
\& Zampieri (1993); Titarchuk, Mastichiadis \& Kylafis (1997); TKB; TSh05; Laurent \& Titarchuk (1999), (2001).
In particular, TSh05 present a general formulation and a solution of the spectral
formation in the diverging outflow. They demonstrated
that the resulting spectrum can be formed as a convolution of energy and spatial diffusion
solutions.

To apply these Radiative Transfer results to observational data,
TSh05 have developed a generic analytical formulation which leads to a simple
analytic expression for modification of the emergent
spectrum due to recoil and velocity
divergence effects in the flow.  For the recoil effect, TSh05 extend
the  results by Sunyaev \& Titarchuk (1980), hereafter ST80,
 who show that the downscattering feature, or "bump", can
appear superposed on power-law spectra with energy spectral indices $\alpha<1$
as a result of photon
diffusion through a static cloud.  From ST80 and  calculations presented in TSh05,
one might conclude such bumps are not a necessarily a feature of
disk reflection, but they can  be also formed as a result of the photon
reprocessing  in a relatively cool, ambient plasma characterized by
temperatures of order $10^6$ K.

\subsection{Time  distributions of escape photons}
In order to understand and explain  the shapes and  the main features of the MC simulated spectra
we attempted to reproduce them using the analytical diffusion approximation.
In framework  of the diffusion theory (TSh05) the resulting spectrum can be presented as a  particular convolution of a primary photon spectrum  $\varphi(z)$ and a time  distribution of escape photons $ {\cal P}(u)$ (see Eq. \ref{emerg}, below).  Here
$u=t/t_{fp}$,  $t$ and
$t_{fp}=l/c$ are the time for photon to escape from the wind  and the mean free path time between two consequent photon scatterings respectively; $z=E/m_ec^2$  is the dimensionless photon energy.
ST80 and Sunyaev \& Titarchuk (1985) hereafter ST85, demonstrate that the photon escape distribution ${\cal P}(u)$  exponentially decays with $u$  as $u>1$  for any bounded configuration, namely ${\cal P}(u)\sim b\exp(-bu)$.

In Figure 2 we present the simulated  time distribution ${\cal P}(t/t_{fp})$ for
optical depth of the wind $\tau$  equal to 4.
As it was found by ST80 and ST85, the time distribution decay exponentially  $\exp (-bt/t_{fp})$ for  $t>t_{fp}$ when the photons propagate in any bounded medium.
This result is used for derivation of the analytical spectra (see Eqs \ref{emerg}).
It means that the best-fit $b-$ parameters obtained by fitting  $\exp (-bt/t_{fp})$ to the time distributions and
those $b-$ parameters obtained by fitting the analytical spectra to the simulated spectra
 are identical within errors  of $b$.
We computed  the $b-$values obtained by these ways and we found they are  identical. This consistency check gives us more confidence of accuracy of our simulations and their analytical description.

In Figure 3  we show the photon distribution for emergent photons over a range of deflecting angles with respect of the  direction of the incident photons.
The outflow shell is radially illuminated be the central source radiation.
The simulations are presented for $\tau=1, ~2,~4$ and  $\beta=0.1$.
In fact, we find in our simulations that  the distribution of the scattering component   weakly depends on  $\tau$.
 Practically, there is little difference
between that related to $\tau=4$, and $\tau=1,~2$. There is only the difference in  the normalization  of the direct (non-scattering) component $A_N$ for which  the ratio of $A_N(\tau=4)/A_N(\tau)=\exp(-4+\tau)$.
The distribution has a strong maximum about $50^{o}$. Thus  we expect that our results for
spherical wind can be applicable for the conical wind if the half-angle of the conical wind is about
$50^o$ or more  (wide open jet or wind).

As we demonstrate in Figure 2  the simulated  escape time distribution in the wind  has an exponential profile which is a typical signature of the photon diffusion propagation in any bounded configuration (ST85). This leads us to conclusion that  we can also treat the radiative transfer in the wind in the framework of the diffusion model (see TSh05).

\subsection{Monte Carlo simulated spectra of the continuum and their analytical description}
For the completeness of the present work  we reproduce some necessary details of the analytical diffusion model  by TSh05.
 Particularly,  the downscattering modification of the incident spectrum $\varphi(E)$ can be obtained using formula (24) in TSh05:
\begin{equation}
{\cal F}_\nu(z,\varepsilon)=\frac{1}{z}
\int_0^{u_{max, \varepsilon}(z)}e^{-4\varepsilon u/3}
\psi^{(\varepsilon)} (z,u)
\varphi[\psi^{(\varepsilon)}(z,u)] {\cal P}(u)du,
\label{emerg}
\end{equation}
where ${\cal P}(u)$ is  the distribution of the photons over their dimensionless escape time $u=t/t_{fp}$,
\begin{equation}
u_{max, \varepsilon}(z)=(3/\varepsilon)\ln(1+\varepsilon/3z)\gg 1,
\label{umax}
\end{equation}
is  a maximal number of scatterings related to the dimensionless energy $z=E/m_ec^2$.
\begin{equation}
z_0=\psi^{(\varepsilon)}(z,u)=(\varepsilon/3)/[(1+\varepsilon/3z)\exp(-\varepsilon u/3)-1],
\label{z0}
\end{equation}
 is the dimensionless photon energy $z_0=E_0/m_ec^2$ at $u=0$
 and $\varepsilon\ll1$ is a coefficient of the diverging term  in the kinetic (Fokker-Planck) equation
(see Eqs. 16, 17 in TSh05 and related  discussion). In fact, $\varepsilon$ is an average relative energy redshift per scattering.
Below (see Eq. \ref{deltaE}), we evaluate these values and verify them using results of   our Monte Carlo simulations.
We find that $\varepsilon\sim \beta/2\tau$ is of  order of $10^{-2}$  for $\beta\lax0.1$ and for  $\tau$ of a few.

This result is a generalization of ST80 and TKB results. ST80 derived the
spectra when the downscattering effects  due to the recoil was taken into account.
It should be noted that the downscattering modification of the spectrum occurs
when photons undergo multiple scatterings $u$.
Thus  we  can expand the integrand function ~~~
$W^{(\varepsilon)}(z,u)=e^{-4\varepsilon u/3}[\psi^{(\varepsilon)} (z,u)]\varphi[\psi^{(\varepsilon)}(z,u)]$ over $u$
in formula (\ref{emerg}):
 \begin{equation}
W^{(\varepsilon)}(z,u)\approx W^{(\varepsilon)}(z,0)+W^{(\varepsilon)\prime}_{u}(z,0)u +
W^{(\varepsilon)\prime\prime}_{u}(z,0)u^2/2 +W^{(\varepsilon)\prime\prime\prime}_{u}(z,0)u^3/3! +...
 \label{expan}
\end{equation}

For the simplest case of the power-law incident spectrum and neglecting the diverging term  in the kinetic (Fokker-Planck) equation
($\varepsilon=0$) the resulting spectrum (Eq. \ref{emerg}) is as follows
\begin{equation}
{\cal F}_E(z)= \frac{A}{z}\int_{0}^{1/z}(1/z-u)^{\alpha-1}{\cal P}(u)du.
\label{powerlaw}
\end{equation}
Using the expansion (\ref{expan}) one can obtain (see Appendix A, Eq. \ref{powerlaw_ap3})
$$
{\cal F}_E(z)= Az^{-\alpha}[ M_{0}(z^{-1})+
\frac{(1-\alpha)}{1!}z M_{1}(z^{-1})+\frac{(1-\alpha)(2-\alpha)}{2!}z^2 M_{2}(z^{-1})+...
$$
\begin{equation}
+\frac{(1-\alpha)(2-\alpha)...(n-\alpha)}{n!} z^{n}M_{n}(z^{-1}) +...],
\label{plexpan}
\end{equation}
 where
\begin{equation}
M_{n}(z^{-1})=b\int_0^{1/z}u^n\exp(-bu)du ~~~~~{\rm~for}~~n=0,~1,~2~...
\label{M_func}
 \end{equation}
Note, the first term in the parenthesis of the right hand side $M_{0}(z^{-1})=1$ for $z\ll 1$ and the second term of that   $(1-\alpha)z M_{1}(z^{-1})$ is positive if energy index of the primary photon spectrum $\alpha<1$. Thus one can expect the photon accumulation bump at low energies for the downscattered power-law spectra for which the  primary photon spectrum  is quite hard (the energy index  $\alpha<1$). Indeed, in the pure scattering  case the photon number is conserved,  so if large   numbers of   the downscattered high energy photons  are removed from the high energy part of the incident spectrum, then they should are seen at lower energies as a so called {\it  downscattering} bump.

In Figures 4, 5 we present the Monte Carlo simulated spectra along with the analytical spectra  (Eq. \ref{plexpan}) for the power-law incident spectra  for $\tau=4$ and  $\tau=2$ respectively.

The downscattering (accumulation) bump and softening of spectrum at high energies are clearly seen in these spectra. As  optical depth increases   more  prominent  bumps are formed in the outflow.
The softening of the analytic  spectra due to the downscattering effect is well described by exponential decay of  moments of the time distribution,
$M_i(1/z)$ $(i=0, 1, 2,..)$ at higher energies (i.e. when $b/z>1$),  see Eqs. (\ref{M_func}), (\ref{M_n}).
The parameter $b$  is only a free parameter to fit the analytical formula,  we fix $\varepsilon=0$
for which $u_{max}=1/z$, see Eq. (\ref{umax}), namely $\lim_{\varepsilon\to0}u_{max}^{\varepsilon}=1/z$.
For $\tau=4$ the analytical spectra (\ref{plexpan}) perfectly represent the simulated spectra for a wide range of the wind
velocities $V=\beta c\lax0.8c$.  It is worth noting that we need not more than 6 terms   of asymptotic series (\ref{plexpan}) to achieve the highest accuracy   of the analytical spectra calculations.

For $\beta = 0.05,~0.1,~0.3,~0.8$ the best-fit parameters $b=0.07,~0.07,~0.11,~0.45$ respectively. The inverse of $b-$parameter, $N_{av}=1/b$ is an average
number of scatterings undergone by the photons in the wind.  For a faster wind the number of scatterings  naturally decreases because  photons are
effectively taken by the outflow and less photons are scattered off outflow electrons.  ST85, calculate b-parameters (and the
average number of scatterings $N_{av}$) for spherical and plane (disk) geometry (Table 1, in ST85, where $\beta$ corresponds to our value $b$).
ST85 present their results for the static case i.e the zero bulk velocity case. Thus we should compare  their results with our results when
$\beta=0.05,~0.1$. Moreover, our wind extended envelope of optical depth  $\tau$ is equivalent to the disk of  half-optical depth  $\tau/2$.
For example, for $\tau=4$, our $b=0.07$ should be related to $0.101$ in ST85 for $\tau=2$. As expected our b-value is smaller (or $1/b$ greater)
than that in ST85, because the empty internal cavity of the wind envelope essentially  amplifies the number of photon  scatterings with respect
to that in a plane disk of the same optical depth.   The scattering effect of the cavity is suppressed when the wind velocity (or $\beta$) increases.
For $\beta=0.3$, the cavity effect and the wind velocity on scattering compensate each other. Our value of $b=0.11$ is very close to that in ST85.

In Figure 5 we show the simulated spectra along with the analytical spectra for $\tau=2$. One can notice that
the best-fit analytical spectra  slightly deviate from  the simulated spectra at high energies.
For $\beta = 0.05,~0.1,~0.3,~0.8$ the best-fit parameters $b=0.13,~0.15,~0.21,~0.62$ respectively. ST85 give the corresponding value of $b=0.234$
(related to our $b$-parameter for $\beta=0.05$).
From this comparison it is evident that the scattering effect of the cavity becomes stronger with the optical depth decrease.
As expected, the analytical spectra as solutions of the diffusion problem in Thomson regime may depart
 from the Monte Carlo simulated spectra for $\tau\lax2$ at high energies where the electron opacity is less than the Thomson opacity.
The central source spectrum (dashed line) is slightly less modified by the scattering in the wind (see MC histogram for the simulated spectrum) than that using the diffusion spectrum (solid line).

Another  interesting case is the downscattering modification of Comptonization spectrum (see e.g. ST80 and Titarchuk
1994). The incident Comptonization  spectrum can be well fitted by a power-law spectrum with an exponential cutoff, namely
 \begin{equation}
\varphi_{comp}(z) \approx Az^{-\alpha}\exp(-z/z_{\ast}).
 \label{comp}
\end{equation}
where  $z_{\ast}=E_{\ast}/m_ec^2$ is the dimensionless photon energy and
the cutoff energy $E_{\ast}$ is related to the Compton cloud electron temperature $kT_e$,
namely $E_{\ast}\approx 2kT_e$.
The downscattering modification of the  spectrum, (see Eq. \ref{intexpan1}) can be written  using the expansion (\ref{expan}).
It can be shown that for $\varepsilon=0$ and $z_{\ast}\to\infty$ formula (\ref{intexpan1}) is reduced to formula (\ref{plexpan}).
In Figures 6 and 7 we present the Monte Carlo simulated spectra for the power-law with exponential-cutoff incident spectra for $\tau=4, ~\tau=2$
respectively  along with the analytically calculated spectra
(see Eqs. \ref{intexpan1}, \ref{nder}-\ref{highz_0vsdu}).
 The  MC simulated spectra are  well described by the analytical  model for all $\beta\lax0.8$. It is worth noting that  the downscattering bumps are not seen in either the simulated nor model spectra.

For $\tau=4$ and  $\beta = 0.1,~0.3,~0.5, ~0.8$ the best-fit parameters are $b=0.06,~0.10,~0.18,~0.38$ respectively.
For $\tau=2$ and  the same  $\beta$ the best-fit parameters are $b=0.14,~0.21,~0.30,~0.59$ respectively.
It is worth noting that the values of $b-$parameter for small $\beta\lax0.1$ is almost independent of the shape of the incident spectrum
(within the error bar
$\delta b=\pm 0.005$)  and it depends on $\tau$ only.

Comparison of the simulated and analytically calculated spectra leads us to conclude that the simulated spectra can be well described by the analytical model  with only one  free parameter $b$ that is related to the mean number of photon scattering in the wind ($N_{av}=1/b$).
It means that the continuum spectral formation in the pure scattering wind is dictated  by the mean  number of scatterings  $N_{av}$ only but that
the value of $N_{av}$ is determined by the combined effect of the wind optical depth $\tau$ and the dimensionless wind velocity $\beta$.

\subsection{ K$_{\alpha}-$Line formation in the outflow}

Another observational feature of the wind is the strong broad feature of K$_{\alpha}$ line in
the spectrum.  Recently,  Shaposhnikov \& Titarchuk (2006) demonstrate  that these strong iron lines are present in all spectral states of Cyg X-1. Also they  show  that the equivalent
width (EW) of the  K$_{\alpha}$ line increases with the photon
index $\Gamma$ from about 150 eV in the low/hard state to about 1.3 keV in the high/soft and very soft states.

The X-ray photons of the central source
illuminates the wind (see Fig. 1). The wind gas is heated by Compton scattering and photoionizations by photons coming from the central object and is cooled by radiation, ionization,
and adiabatic expansion losses (LT04).
The photons above the K-edge energy are absorbed and  ionize iron atoms which leads to the formation of
the strong K$_{\alpha}$ line.  LT04 calculated ionization, temperature structure and the equivalent widths of Fe K$_{\alpha}$ line formed in the wind.
For the wide set
of parameters of the wind (velocity, the Thomson optical depth $\tau$) and the incident Comptonization spectrum
(the index and the Compton cloud electron temperature) they established
that EW of the line should be about  1 keV and less for the line to  be observed.
LT04 also predicted that in this case the inner radius of the wind should be situated at $(10^{3}-10^{4})/\tau_{0}$ Schwarzschild radii away from the
central object.

\subsubsection{The spectral line redshift in outflow. Analytical Description}

In Figure 1 we show the picture of the line photon propagation in the wind.
At each consecutive scattering the line photon in average loses its energy, in other words it
is redshifted.
A photon emitted near the inner boundary and subsequently scattered
 by an electron moving with velocity ${\bf V}_1$, is
received by an electron moving with velocity ${\bf V}_2$ as shown in Fig. 1.
The change in frequency is
\begin{equation}
 \nu _2 = \nu _1\left[1+\left({\bf V}_1-{\bf V}_2\right)
\cdot{\bf n}/c\right]
\label{energ_change}
\end{equation}
where ${\bf n}$ is a unit vector along the
path of the photon scattered at the next point.

We remind a reader that   in the static and spherical-symmetric  medium  and
where electrons experience a random (Brownian) motion only,   the  mean energy change per scattering, $<\Delta E>$, for photons undergoing quite  a few scatterings is proportional to   square  of electron velocity, namely
$<\Delta E>\propto (V/c)^2$  (see e.g. Rybicki \& Lightman 1979 and ST80).

On the other hand   for photons undergoing numerous
 scatterings in the bulk flow $<\Delta E>$ is just  proportional  to $V/c$.
[see Titarchuk, Mastihiadis \& Kylafis 1997, Appendix D and TKB).
In order to make estimate of the  loss per scattering, one has to find the response of the energy operator of the diffusion kinetic equation (see TKB, Eqs. 3, 18) to a delta-function injection. In Appendix B1 we show that in this  standard diffusion approximation $<\Delta E>$ is proportional to the velocity divergence, namely
\begin{equation}
<\Delta E>\approx -\frac{4}{3}\frac{\nabla ({\bf V}/c)}{\kappa}E_0\sim \frac{8}{3}\frac{\beta}{\tau}E_0
\label{deltaE_divergence}
\end{equation}
where $\kappa$ is the scattering coefficient (or the inverse of the scattering mean free path).
But this method  provides rather a qualitative estimate of the redshift  effect in the outflow than a quantitative one.
The   value of the  numerical factor $4/3$  in equation (\ref{deltaE_divergence}) is not precisely correct,  which suggests that factor $4/3$ should be replaced by the right one; however, the form of the exact equation actually depends on $\beta=V/c$ and $\tau$ in a more complex way.
Formula (\ref{deltaE_divergence}) should be then taken only as an estimate.

A useful result of the  $ <\Delta E>$ estimate is obtained using the scattering geometry method  (see Appendix B2)
\begin{equation}
<\Delta E>\approx -\beta f/(2\tau)\sqrt{1-(f/2\tau)^2} E_0.
\label{deltaE}
\end{equation}
Below  we utilize  the MC simulations to show that   the numerical factor  $f$ in formula (\ref{deltaE}) is   about one.
Comparison of Eqs. (\ref{deltaE_divergence}) and (\ref{deltaE})  leads us to conclude that $<\Delta E>$ is proportional
to $\beta$ but that is overestimated in equation   Eq. (\ref{deltaE_divergence}).

The average energy of photons escaping after $N_{av}=1/b$ scatterings is
\begin{equation}
<E>_{sc}=(1+<\Delta E>)^{1/b}E_0.
\label{E_av_p}
\end{equation}
From here using formula (\ref{deltaE}) we obtain that
\begin{equation}
<E>_{sc}=\{1-\beta f/(2\tau)\sqrt{1-(f/2\tau)^2}\}^{1/b} E_0.
\label{E_av}
\end{equation}

\subsubsection{MC simulated spectral lines in outflow. Evidence of the strong redshift effect in the outflow}

We simulate line profiles for different optical depths of the wind.
In Figure 8 (left hand side panel) we present  examples of the line profiles for
simulations where  we take into account only the pure electron scattering
in the flow, photo-electric absorption being neglected in these simulations.
In Figure 8 (right-hand side panel) we present the spectral profile of the line obtained as a result of the electron scattering
in the flow along with   photo-electric absorption.
When the X-ray  continuum spectrum of the central source illuminates the wind  the seed  $K_{\alpha}-$photons are formed in the innermost part   of the wind.
The photo-absorption profile as a function of energy, calculated by LT04, is related to the specific case of $\beta=0.1$,
  $\alpha=0.5$, $kT_{e}=50$ keV  for which
 the inferred LT04 model parameter $r_{in}\tau/L_{40}=6\times 10^{12}$ cm.

 The model and X-ray continuum parameters are the following: $r_{in}$ is the outflow inner radius, $L_{40}$ is the luminosity of the central source in units $10^{40}$
 erg s$^{-1}$, $\alpha$   is the energy spectral index and  $kT_{e}$ is
 the electron temperature of the Comptonization spectrum
 (see details of the photo-absorption calculations in LT04). We find that the height scale of
 the source exponential distribution, $H$, is only  a small fraction of the inner radius or in other words
   $H/r_{in}\sim0.04\tau$ is a small fraction of the  optical thickness of the outflow.
Thus {\it the sources of K$_\alpha$ is distributed in the innermost part of the flow}.

We simulate  the line profiles  for  $\tau=2, ~4$,
$kT_e = 0.1$ keV,  $\beta =0.1$, and
for an initial seed photon energy $E_{ph} = 6.6$ keV.

One can clearly see  the red-skewed part of the spectrum formed by photons undergoing multiple scatterings, along with the
primary peak formed by photons escaping directly to the observer.
The normalization of the direct non-scattering line component is suppressed for $\tau=2$. The real normalizations are
 $A_N=1.35\times10^6, ~1.29\times10^6$ for the diffusion and diffusion+absorption cases respectively.

In a  situation, when the effect of the photon photoionization and absorption is taken into
account, the red wing of the line (for energies less than 4 keV) and   blue wing (for energies higher 8 keV)
have  to be suppressed  due to high photo-electric absorption
opacities.  Despite  this photo-absorption suppression, the red-skewed shape of the line  is retained.
Thus one can conclude that {\it the red-skewed line profiles are intrinsic signatures of outward propagation of K$_{\alpha}-$photons
generated at the bottom of the outflow due to the outflow illumination by the X-ray  hard radiation of the central source.}

In Figure 9  we show  timing properties of the line propagation in the  outflow
for 5 energy bands for the pure scattering case.
In the plot the time is given in the free path  time units $t_{fp}=l/c$.
Photons escaping from the bottom atmosphere without scattering are at 6.6 keV.
The model parameters used here are
$kT_e = 0.1$ keV, ~$ \beta = 0.1$, $\tau =4$ (upper panel),   and  $\tau=2$ (lower panel).
We show the arrival time of photons at the top of the cloud for five energy bands,
in free path  time units $t_{fp}$.  Soft lags, low energy emission at later times are clearly seen.

It  is also worth noting that TKB predict  soft lags, namely that a photon of initial energy $E_0$ loses its
energy with time, i.e. $E=\exp(-u_{\rm TKB})E_0$ [compare with our formulas (\ref{deltaE}, \ref{E_av}) ]. The dimensionless time variable
(we call it as $u_{\rm TKB}$) used there is  a mathematical variable for a convolution method (see their Eq. 9). It can be interpreted as
a product of  the  number of scatterings $t/t_{fp}$ multiplied  by the mean photon inelasticity $<\Delta E>/E$
(see our Eq. \ref{deltaE}), i.e
 $u_{\rm TKB}= (<\Delta E>/E)(t/t_{fp})$.

The photon distribution  with respect to  escape time integrated over energies can be fitted  with an exponential
law  $b\exp(-bt/t_{fp})$ (shown in Fig. 2). The values of $b=0.057$ and $b=0.144$ for $\tau=4$ and $\tau=2$ respectively
(and consequently the average number of scatterings $N_{av}=1/b$) are very close to $b$ (or $N_{av}$) obtained
from the best-fit analytical spectrum for the same values of $\beta$ and $\tau$.

We also check  the analytical estimate of the average redshift of the line energy using formula (\ref{E_av}) and
that obtained from our simulations with the  values  $<E>_{sc}=4.56$ keV and $<E>_{sc}=5.27$ keV  for $\tau=4$ and $\tau=2$ respectively.
On the other hand keeping in mind the values of $b$,  related to a given $\tau$ we can obtain the same values of $<E>_{sc}$ as the simulated ones using formula
(\ref{E_av}) with  $f=1.3, ~f=1.7$  for $\tau=2$ and $\tau=4$ respectively.
These values  of $f>1$  are expected in the framework of our analytical  estimate of $<E>$.
 (see details of the derivation in Eq. (\ref{l_r}).
 It is worth noting that now we can  calculate $\varepsilon=<\Delta E>/E_0$
that follows from formula (\ref{deltaE}) using $f$ inferred from our simulations.
They are $\varepsilon=0.03,$ and $0.04$ for $\tau=2,~4$  respectively and for $\beta=0.1$.

In Figure 10 we present the emergent line profiles for   different values  of $\tau$ and $\beta$.
Spectral lines as a function of $\tau$ are for $\beta=0.1$, and that as a function of
$\beta$ for $\tau=2$.
The source photons are generated at the bottom of the cloud and the cloud temperature is kept fixed at $kT_e=0.1$ keV.
The red wing of the line profile is  insensitive to the temperature of the flow if $kT_e< 1$
keV. On the other hand, the blue wing becomes broader with $kT_e$,  but its relative width is still  smaller than that of
the red wing.
In fact, the blue wing  is affected for energies higher than K-edge ($>8$ keV)
if  the photo-absorption is taken into account (see  the left lower panels of Fig. 10). In general,
the photo-absorption narrows the line profile
(compare the lines profiles in the upper and lower panels of Fig. 10).

The line profiles  depend quite strongly on $\tau$ and $\beta$.
The shape of the red wing below  the broad peak (see  Fig. 10)
follows a power law with  index which is a strong function of $\tau$ and $\beta$.
Our calculated indices are in agreement with
the TKB results for $\beta<0.5$ and $\tau_{eff}=3\beta\tau>1$.   In TKB, the photon indices are equal to $\Gamma=2+\lambda_k^2$,
where $\lambda_k^2$ are eigenvalues  calculated using their equation (30).

When $\beta\sim 1$
the spectrum of scattered photons becomes flat even for $\tau=2$.
The relativistic spherical outflow completely washes out the bump induced by scatterings (see the right panels of Fig. 10).
However, for  relatively small $\beta$, the power law tails still remain steep for higher $\tau$ (see the left panels of Fig. 10).
This is very similar to the results obtained by TKB.

\section{Comparison of MC simulated line profiles with the data}

In Figures 11 and 12 (the left panel) we present the results of  fitting our model to the XMM (EPIC) data of Wilms et al. (2001) obtained during the observation of
the bright Seyfert 1 galaxy MCG-6-30-15. These observations were focused on the broad Fe K$\alpha$ line at
$\sim 6.4$ keV. For MCG 6-30-15   we fit the continuum with a power law of
index 1.8 and compare the residuals with our model.
The best-fit  parameters of the pure scattering model we found are $E_{ph} = 6.51$ keV, ~$kT_e = 0.1$ keV,
$\tau =1.2, ~\beta = 0.02$. We generated the primary photons  at the bottom of outflow. If we take into account the LT04 model for  the photo-absorption along with
electron scattering, then the best-fit parameters become $E_{ph} = 6.51$ keV, ~$kT_e = 0.1$ keV,
$\tau =1.7, ~\beta = 0.02$.

 The best-fit model spectrum is very similar to the steep spectrum presented in Fig. 10 for $\beta=0.01$ (black curve in the
 lower panel). The quality of the fits  strongly depends on the outflow optical depth $\tau$ and bulk velocity
$\beta$. It is less sensitive to the outflow temperature $kT_e$ unless $kT_e\lax0.1$ keV.
It is important to note that  using our diverging outflow model we confirm  Fabian's (1994) finding
that velocity of the warm absorber outflow is about 5000 km s$^{-1}$ in MCG-6-30-15.

We fitted the red-skewed iron line profiles for four galactic sources XTE J1550-564, GRO J1655-40, Cyg X-1 and GRS
1915+105 obtained by Miller et al. (2004b). All of these data can be fitted by our model.
In Figures 11 and 12 (the right hand panel) we show an example
of these fits to the data.   For GRO J1655-40 for the pure scattering model
 we find that optical depth $\tau=2.0$ and  an outflow velocity  is $ \beta = 0.1$,  much higher than that for MCG 6-30-15 and $E_{ph} = 7.1$ keV.
If we take into account the photo-absorption along with scattering in our model, then the best-fit parameters are $\tau=3.3$, $\beta=0.25$ and  $E_{ph} = 7.1$ keV.
It is worth noting that the fit in this case is not so good as that in the case of the pure scattering model. It can mean that the iron abundance in GRO J1655-40 is less than cosmic
abundance. In fact, LT04 calculated the photoabsorption cross-sections for the cosmic abundances.

As we have  pointed out, the MC simulated line profiles are  independent of the outflow size
and are determined by four  parameters $\tau$, $\beta$, $kT_e$ and $E_0$. The  size of the outflow
shell can be determined by timing characteristics such as variability timescales and time lags.
Our model predicts soft time lags, i.e. the time lags become longer as energy decreases.
Time lags are scaled with the light crossing time, $t_{cross}$,
from one to  a few $t_{cross}$. Unfortunately  time lag information is not yet available
for all  sources analyzed. The only available information at present is the lack of the iron line variability
with respect to the continuum for a number of extragactic sources [Markovitz, Edelson \& Vaughan (2003)].
Thus one can suggest that  these line
features are formed in a more extended configuration than the source of the continuum (which is presumably a Compton cloud close
to the compact object). Here we demonstrate how our model can be used in the  analysis of the line data.
The detailed interpretation of the line data using our outflow model  will be presented in a separate publication.

\section{Outflow  reprocessing of X-ray continuum spectra: MC simulated spectra}
 We also  study the modification of the central source X-ray spectrum in the warm outflow as a result of photoionization and
 downscattering.  In Figure 13 we present the  simulations
 for different values of $\tau=2,~4$ and $\beta=0.1, ~0.3$.
 The results of simulations are shown as $E^2 F(E)$ diagrams, where $F(E)$ is a photon spectrum.
 In these simulations, the incident (central source) spectrum is approximated by the
 sum of two components: a blackbody shape radiation presumably coming from the inner part of the accretion disk,
 and a power-law with an exponential cutoff coming from the Compton cloud (corona).
  The parameters used for this input spectrum are the color temperature of the blackbody component $kT_{bb} = 1.2$ keV,
  the power-law photon index  $\Gamma=1.5$ (energy index $\alpha=0.5$) , and the cutoff $E_{cutoff}= 50$  keV. As shown in Comptonization theory (see e.g. ST80, Titarchuk 1994) the exponential cutoff energy $E_{cutoff}$ of the unsaturated Comptonization spectrum
 is approximately $2kT_e$ where $kT_e$ is the plasma temperature of the Compton cloud.  The  temperature of spherically symmetric wind is  $kT_e = 0.1$ keV.

For the X-ray spectrum of the central source we assume that the photon numbers are the same for the blackbody and hard
components. In fact, the ratio of the photon numbers depends on the illumination of the Compton cloud by the source of blackbody radiation.

 The photoelectric effect is taken into account in these simulations.

When a photoelectric event occurred, we drew a random number to firstly determine if this event
occurs in the K shell of iron. The probability
of fluorescence is about 30 \%.
The fluorescence photon is then  propagated into the cloud in the same way as the input central
object spectrum.

In the simulated spectra one can clearly see features of the strong fluorescent K$_{\alpha}$ line and the deep K-edge formed in the wind.
The prominent bump around 25 keV is a combined effect of photoionization and downscattering in the wind.
The wind modification of the spectra is very sensitive to the optical depth of the wind $\tau$ and $\beta$.
For example, for a given $\beta=0.1$ (or the wind velocity $0.1c$ ) the depth of K-edge is broader and much deeper for $\tau=4$ than  for $\tau=2$.
As expected the width of the line increases with $\beta$ (compare the spectrum for $\beta=0.1$ with that for $\beta=0.3$).
It is important to emphasize that the shape of K$_{\alpha}$  line consists of narrow and broad components. These narrow and broad line  features of the line
are really  observed in Cyg X-1 (see review of the K$_\alpha$ line observations in Cyg X-1 in the introduction section of ST06).

The shape of the spectrum for $\tau=4$ and $\beta=0.3$ is very similar to the observed spectrum of Cyg X-3 (TSh05 and Trudolyubov, 2006, private communication).
We present the interpretation of Cyg X-3 data based on the results of our simulations elsewhere.

\section{ Discussion and Conclusions}

It is important to point out  that  Thomson optical depth of outflow is an order of unity
when the mass outflow rate $\dot M_{out}$
is an order of the Eddington mass accretion rate $\dot M_{\rm Edd}$ and higher
(see e.g. formula 4 in King \& Pounds 2003).

Recent {\it XMM-Newton} observations of bright quasars (Pounds et al., 2003a,b; Reeves et al., 2003) give strong evidence
for powerful outflows from the nucleus with mass rates $\dot M_{out}\sim \dot M_{\odot}$ yr$^{-1}\sim \dot M_{\rm Edd}$ and
velocity $V\sim0.1c$ (i.e. $\beta=0.1$) in the form of blueshifted X-ray absorption lines. These outflows closely resemble those
recently inferred in a set of ultraluminous X-ray sources with extremely soft spectral components
(Mukai et al. 2003; Fabbiano et al. 2003).
It is also worth noting the recent  observations of the strong outflows from GRO J1655-40
(Miller et al. 2006) and the Nucleus of the Seyfert 1 Galaxy NGC 3783 using
an intensive HST/Chandra/FUSE monitoring (Crenshaw et al. 2004) and the recent Chandra observations  of highly obscured AGN (Levenson et al. 2004) reported in the AAS HEAD meeting in  2004. In particular, Levenson et al. analyze new Chandra observations
 of three
Compton thick Seyfert 2s with obscuring column densities that exceed $10^{24}$ cm$^{-2}$. They report that the Fe K$_\alpha$ line is very
prominent in these examples with equivalent width $>1$ keV.
 Thus one can  conclude that powerful mass outflows from
Eddington-limited accreting compact objects appear to be a very widespread phenomenon.
King \& Pounds (2003) and Begelman, King \& Pringle (2006)  argue that the powerful outflows
 may provide the high luminosity observed in quasars and ULXs, and imply that such objects have a major effect on their surroundings.
They further suggest that the powerful outflow phenomena have barely been explored, and the field promises to be fruitful.

It is out of the scope of this paper to study the  consequences of the X-ray  radiation for hydrodynamics of these outflows.
Our goal is to elaborate the spectroscopic tools for probing the outflow physical conditions such as column density
(the outflow optical depth) temperature and iron ionization charge state. Moreover the photoionization modeling of the outflow (see LT04) permits the
determination of its distance from the central black hole.

We have presented  the Monte Carlo simulations of the radiative transfer of
monochromatic photons and continuum photons within a diverging outflow, a problem which is also of observational
interest, in view of the observations of broad, redshifted Fe lines and downscattering bumps (so called ``reflection features'') in
extragalactic and galactic black hole  candidate spectra.
We also provide an analytic description of the simulated spectra which allows us to understand, in  detail,
 the effect of  the dowscattering modification of the central source spectrum.

In the  form presented the derived formulae of the resulting spectra can be easily used  as an efficient  analytical tool for the spectral data analysis.
We demonstrate that the strength of the downscattering bump is determined by the average number of scattering that photons undergo in the wind.
From our simulations of the pure scattering wind model we find that the average number of scattering $N_{av}=b^{-1}$
suffered by the photons in the wind  of optical depth $\tau\gax 2$ is $\gax \tau^2$ for $\beta\lax 0.1$ (see \S 3 for details).
On the other hand the average number of scatterings $N_{av}$ decreases when the velocity of the wind increases.
A larger  fraction of the photons are rather carried out by the flow than scattered  there
when velocities are higher than $0.1c$.

The outflow leads to a  redshift of the photon energy  producing a broad, red
component (see Fig. 1 for illustration of this redshift effect) not unlike those of the Fe K$\alpha$ lines observed.
We demonstrate analytically and numerically  (using Monte Carlo simulations) that the mean photon energy change per scattering  in the outflow $<\Delta E>$ is the first order effect with respect of $V/c$, namely $ <\Delta E>\propto-V/c$.
We  further emphasize
that the red-skewed line features appear   when the line photons are generated very close to the bottom
of the outflow due to the outflow illumination by the X-ray  hard radiation of the central source.

An important result of our simulations
(see also TKB's results) is the natural suppression of a blue wing in the iron line  feature without
the need to invoke any specific geometric arrangement for the emission.
The illumination of the outflow from inside by the X-ray radiation, is  natural  for a compact source
geometry, where the X-ray radiation  originates from the innermost part of the source
(a Compton  cloud  along with a disk).
The powerful wind  presumably starts in  outskirts of the source (see Everett \& Ballantyne 2004 for the
wind model).
In  our model  the red-wing  photons have undergone numerous  scatterings
in an (effectively) optically thick medium, with
an associated first order redshift in each  scattering.
It is not surprising that
the blue wing,  as a result of the second order $(v/c)^2$ effect,  is weak for $kT_e\lax$ keV
and $\beta=V/c\lax0.1$.

{\it This red-skewed line  is a  natural consequence of the first order Doppler effect
 in the presence of multiple scattering and photo-absorption events in the wind.

It does not require  any particularly fine tuned geometric arrangement}.

LT04 find the self-consistent temperature and ionization structure
of the wind shell as a function of the parameter (radius/luminosity, $r_{in}\tau/L_{40}$ where $r_{in}$ is
the inner outflow radius and $L_{40}$ is X-ray luminosity in units of $10^{40}$ erg s$^{-1}$)
for a given Thomson optical depth of
the shell. It is evident that the ionization parameter $L_{40}/nor^2$ is constant  through the shell (i.e.
for $r>r_{in}$) if the velocity of the wind is
constant through the flow.  Thus  the LT04 solution allows one to determine the size of the shell base for a given
luminosity of which the red-skewed line is observed. LT04 derive the range of parameter $r_{in}/L_{40}$
where the outflow-produced  stable solution exist. The allowed $r_{in}/L_{40}$ values are concentrated around $10^{12}-10^{13}$ cm.

{\it Our model predicts the soft lags to be a function of $E/E_0$, $\beta$ and $\tau$}.
The combination of the red-skewed features along with the soft time lags
that strongly depends on $\beta$, $\tau$ and $kT_e$ are intrinsic signatures of any diverging outflow.

The demonstrated application of our outflow model to  data   points out a potentially
powerful spectral  diagnostic for probes of the outflow-central object connection in Galactic and
extragalactic BH sources.
Particularly, analyzing  MCG-6-30-15 data (see \S4) we infer that bulk outflow  velocity is about 6000  km s$^{-1}$.
On the other hand  the OVII edge in the warm absorber of MCG-6-30-15 indicates that the flow along line of sight is
about $5000\pm1000$ km s$^{-1}$ (Fabian et al. 1994).
Thus  using a new X-ray spectroscopic method [our diverging (outflow) model]
  we confirm  the early finding (that used UV spectroscopy)
  that velocity of the warm absorber outflow of MCG-6-30-15 is about 5000 km s$^{-1}$.

L.T. acknowledges the support of this work by the Center for Earth Observing
an Space Research of the George Mason University. L.T. also appreciates  productive  discussions
with Ralph Fiorito, Stuart Wick, Phil Uttley, Martin Laming and Chris Shrader.
We also acknowledge discussion of the paper results with
the referee
and his/her constructive and interesting suggestions.

redpajama_set_name: RedPajamaArXiv


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text:
Bears president/CEO Ted Phillips to retire at season's end
Bryan Perez September 2, 2022 September 2, 2022
The Athletic's Dan Pompei dropped a bombshell Friday morning with the breaking news that Chicago Bears president and CEO, Ted Phillips, will retire at the end of the 2022 season. Phillips, who's worked for the Bears for 39 years (23 years in his current role), was instrumental in the Soldier Field renovation and has led the charge in the Bears' stadium project at Arlington Heights.
"When COVID came, it changed a lot of dynamics and gave me some time to reflect on my life, my work life," Phillips told The Athletic. "I came to the conclusion that, my gosh, almost 40 years is a long time. It's time to hand over the baton and give myself the gift of time. You know how this business can be, a lot of hours and time away from family. I just turned 65 years old. I feel good. My health is good. I felt it was time to slow down and do whatever I want to do."
Phillips has been an easy target for disgruntled Bears fans through the years. Chicago's lost more game than it's won under his watch, which led to a reshuffling of the football organization last offseason. General manager Ryan Poles reports directly to George McCaskey, a stark contrast from past regimes that first went through Phillips for football decisions.
The Bears have already begun a search for Phillips' replacement. For a complete breakdown of the Ted Phillips news, check out Pompei's article here.
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text:
De Ridderlijke Duitsche Orde in de protestantse Balije Utrecht is een liefdadige ridderlijke orde die alleen Nederlandse protestantse edellieden toelaat.
De orde is in de Reformatie afgesplitst van de katholieke Duitse Orde.

In 1518 bezat de Balije van Utrecht, een van de veertien balijen van de grote en rijke Duitse Orde, veertien commanderijen. De orde werd bestuurd door een landcommandeur vanuit het Duitse Huis binnen de muren van de stad Utrecht. Sinds de orde het Duitse Huis in 1992 heeft kunnen terugkopen is dat na een onderbreking van twee eeuwen weer het hoofdkwartier van de balije.

De veertien commanderijen
De commanderij van Middelburg of Zandvoord (1248/71-in 1581 verkocht)
De commanderij van Katwijk (en Valkenburg) (1241-vanaf 1388 in Katwijk gevestigd en vanaf 1599 samengevoegd met Leiden)
De commanderij van Leiden (1268 -rond 1650)
De commanderij van Maasland of Hofdijk (1241-heden)
De commanderij van Schoonhoven (1395-1578)
De commanderij van Schelluinen (1220-1700)
De commanderij van Tiel of Hemert (voor 1256-heden, vanaf 1328 in Tiel gevestigd)
De commanderij van Rhenen (1277-1630)
De commanderij van Doesburg (1286-1657)
De commanderij van Dieren (1218-heden, vanaf 1434 behorend aan de balije Utrecht)
De commanderij van Ootmarsum. Deze werd tussen 1262 en 1454 aan de balije Westfalen afgestaan, ze werd in 1811 geseculariseerd wat inhield dat ze verdween, maar werd in 2006 weer hersteld, nu als deel van de Utrechtse Balije.
De commanderij van Nes (voor 1243-1604 door de Staten van Friesland geseculariseerd)
De commanderij van Schoten of Schoterburen (voor 1299-heden)
De commanderij van Bunne of Bonne (1272-1563)

De commanderijen waren kleine beheerscentra met eigen inkomsten uit voornamelijk pacht en kerkelijke inkomsten (aan veel commanderijen was een parochiekerk verbonden). De commandeur bestuurde het geheel en de op de commanderij levende priester- en ridderbroeders wijdden zich aan gebed en het beheer van de goederen.

De periode van de kruistochten lag in de zestiende eeuw al lang in het verleden en overal in Europa keken de vorsten met enige hebzucht naar de enorme bezittingen van de nutteloos geworden ridderorden. Zo werden militaire orden als de rijke Spaanse Orde van Calatrava binnen de machtssfeer van de koning gebracht. De Duitse Orde heeft dit lot, althans in Nederland, kunnen ontlopen.
De Staten van Utrecht verboden in 1581 de katholieke eredienst en alle katholieke orden en instellingen. Hun bezittingen vielen toe aan de Staten van Utrecht.
De Duitse Orde kon desondanks blijven bestaan, omdat landcommandeur Jacob Taets van Amerongen de Staten beloofde dat alle ridders protestant zouden worden. Daarmee verviel in theorie ook het verplichte celibaat van de ordebroeders. Het protestantisme wijst het celibaat af, maar het kapittel stond de Ridders van de Duitse Orde in haar Balije pas in 1638 toe om te trouwen.
De Staten werden de grootmeester en beschermden als soevereine opvolgers van de afgezworen heer der Nederlanden Filips II de Duitse Orde.

De protestantisering van de orde verliep zeer geleidelijk. De laatste katholieke landscommandeur, Diederik de Bloys van Treslong, trad pas in 1619 af. Zijn opvolger Jasper van Lynden was de eerste van de sindsdien steeds protestantse bestuurders van de balije, maar de laatste katholieke commandeurs verdwenen pas in het midden van de 17e eeuw.

De ridders en commandeurs legden in de middeleeuwen, zoals in een kruisridderorde gebruikelijk, een gelofte van armoede, een gelofte van kuisheid en een gelofte van gehoorzaamheid af. Men kon dus spreken van ridder-monniken. De reformatie maakte geleidelijk een einde aan de naleving van deze geloften. Ten minste een van de landcommandeurs van de Utrechtse Balije woonde op het terrein van het Duitse Huis samen met zijn concubine en zijn bastaardkinderen. In strijd met de gelofte bezaten commandeurs een eigen vermogen waarover zij ook testamentair beschikten zodat hun bezit niet langer automatisch toeviel aan hun orde. De officiële opheffing van het celibaat in 1637 wordt gezien als de definitieve breuk tussen de protestants geworden Utrechtse Balije en de katholiek gebleven balijen die onder het gezag van de Duitsmeester als katholiek instituut bleven voortbestaan.

Het losmaken van de Balije uit het juridische en economische geheel van de Duitse Orde heeft veel tijd gekost. Opvallend is dat de commanderijen van de balije Alden Biesen en de commanderij Ootmarsum, hoewel op het grondgebied van de Republiek der Vereenigde Nederlanden gevestigd, tot de Duitse, katholieke, organisatie behoorden.

De orde was nu een in veler ogen nutteloos maar lucratief instituut geworden. De twaalf commandeurs woonden op hun eigen kastelen en havezathen maar verdeelden wel onderling een groot deel van de inkomsten. De "grote prijs" was de rijke commanderij van Dieren die daarom na 1620 door de leden van de familie Nassau werd opgeëist.
De kerken en huizen van de orde geraakten in verval omdat de commandeurs daar niet meer resideerden.
De orde liet protestantse edelen met "Duits", dat wil zeggen Nederlands of Duits, bloed en vier adellijke kwartieren in haar midden toe als "ridders-expectant". Uit deze heren werd dan, zo er door overlijden een commanderij vrij kwam, een nieuwe commandeur gekozen.
De Orde hield zich nog wel actief bezig met weeshuizen en verschafte geld aan de diaconieën in haar commanderijen. Deze deden op hun buurt aan armenzorg.

Een bijzondere plaats in de geschiedenis van de orde neemt landcommandeur Unico Wilhelm des H.R. Rijksgraaf van Wassenaer-Obdam (1692-1766) in. Hij hervormde de balije grondig. Zijn reorganisaties maakte de orde, zo schrijft J.A. van Zelm van Eldik, aan de vooravond van de revolutieperiode tot een goed functionerend instituut.

De Bataafse republiek verbood de adellijke orde niet en de bezittingen werden door een administrateur beheerd. In 1807 werd het Duitse Huis, min of meer vrijwillig en met recht van eerste koop, aan de regering van Lodewijk Napoleon afgestaan. Het koninkrijk Holland kwam niet aan het regelen van de Duitse Orde, die had moeten toezien hoe de Duitse tak van de orde in 1809 door Napoleon; die adellijke orden verafschuwde, werd opgeheven. In 1811 volgde de Balije Utrecht. Gelukkig voor de Duitse Orde pleegden de hier ten lande met de liquidatie van de orde belaste ambtenaren passief verzet tegen de Franse keizer en schoven ze de verkoop van de goederen op de lange baan.

De Orde in het Koninkrijk der Nederlanden
Koning Willem I gaf de Balije Utrecht haar bezittingen, voor zover nog niet verkocht, weer terug. In een van de eerste wetten van het Koninkrijk der Nederlanden, op 8 augustus 1815, werd de Duitse Orde, ondanks een tegenstribbelende Staten-Generaal, erkend. De koning wees de titel van hoog- of grootmeester na enige aarzeling af, maar verkreeg wel het aggregatierecht. Alle benoemingen en bevorderingen in de Duitse Orde geschieden sindsdien bij Koninklijk Besluit. Opvallend is dat de orde geen regerende vorsten en geen prinsen der Nederlanden in haar midden heeft opgenomen.

De orde heeft tot 1945 ook Duitse ridders-expectanten en commandeurs gekend. Koning Willem III heeft zelfs tegen het grote aantal Duitse voordrachten geprotesteerd. Na 1871 werden er nog elf Duitse edelen tot kapittelridders benoemd. In 1937 werd vastgelegd dat de er geen Duitse onderdanen meer in de orde zouden worden opgenomen. In 1946 werden de Duitse leden geschrapt uit het ledenregister. De enige Duitse commandeur, Wolf Dietrich von Trotha, die sinds 1935 lid van het kapittel was, trof hetzelfde lot.

Mogelijke ridders-expectanten worden vaak al bij hun geboorte als "edelexpectant" aangemeld. Op hun 21e verjaardag kunnen zij als ridder-expectant tot de orde toetreden. Op hun dertigste jaar zijn zij verkiesbaar in het kapittel. Het entreegeld bedraagt 1200 gulden.
De kapittelridders worden niet tot ridder geslagen, maar leggen een eed af.
Het kapittel bestaat uit de landcommandeur, de coadjutor, elf commandeurs en de eerste en tweede kapittelridder.

De eis dat de Nederlandse ridders expectanten "zestien kwartieren oude adel niet besmet met bastaardij" moesten aantonen, werd afgezwakt tot "vier kwartieren met twee grootvaders van families die al vóór 1795 jaar tot de adel behoorden". Het kapittel achtte ook deze toelatingseis aan het begin van de 21e eeuw onhoudbaar en vroeg de Hoge Raad van Adel om een advies over nieuwe toelatingseisen, omdat het "voortbestaan van de orde" niet meer gegarandeerd kan worden.

Mede op grond van een reeds in 2003 uitgebracht advies van de Hoge Raad van Adel inzake aanpassing van de
toelatingseisen, waar het de eis van vier adellijke kwartieren betreft, stelde de Ridderlijke Duitsche
Orde, Balije van Utrecht, in 2006 nieuwe statuten vast. Sindsdien is slechts één adellijk kwartier paternel (aan de vaderszijde)
van vóór 1795 en één adellijk kwartier maternel (aan de moederszijde) zonder ouderdomsgrens vereist.

In 1992 werd het Duitse Huis gedeeltelijk teruggekocht. De orde heeft in Nederland 130 verpachte boerderijen en 1430 hectare landbouwgrond, waarvan het grootste deel in de provincie Utrecht. Uit de pachtopbrengsten wordt jaarlijks 1,2 miljoen euro uitgekeerd aan goede doelen.

Activiteiten van de Ridderlijke Duitsche Orde in de protestantse Balije Utrecht

De dagelijkse leiding over de activiteiten berust bij de secretaris van de Duitse Orde. Er is ook een "Dirigerende commissie" waarvan de landcommandeur J.R. baron de Vos van Steenwijk, de coadjutor ir. B.W. baron Bentinck tot Buckhorst en de commandeurs mr. R.G.M.C. ridder van Rappard, drs. J-A.F. baron de Vos van Steenwijk en ds. B.F. baron van Verschuer deel uitmaken.

Voor bijzondere hulpverlening aan behoeftigen werd door de Duitse Orde de "Johan van Drongelenstichting" (vernoemd naar een voormalig Landcommandeur) opgericht. Per jaar worden ongeveer 500 aanvragen voor hulp en schuldsanering behandeld.
Met twee andere Utrechtse fondsen werd een fonds voor individuele materiële noodhulp opgericht. Dit fonds, de "Stichting N(oodhulp) U(trecht)" kan, doordat de gemeente Utrecht de administratie voor haar rekening neemt, al haar middelen inzetten ter leniging van individuele noden in de stad. Het jaarlijks budget hiervoor ligt rond de € 120.000. Deze vorm van hulp voorziet in een grote behoefte.
Ook wordt een substantieel deel van het jaarlijkse budget van de orde besteed aan bijdragen voor het aanschaffen van aangepaste vervoermiddelen of aanpassingen aan woningen; aanvullingen op voorzieningen die de overheid geeft in het kader van de Wet voorzieningen gehandicapten.

Ook in grotere projecten, te denken is aan het financieel helpen realiseren van huizen voor stervensbegeleiding (het Johannes Hospitium Vleuten) of opvangcentra voor zwerfjongeren ("Singelzicht" in Utrecht), is de orde betrokken.
Hoewel het overgrote deel van de middelen wordt besteed in het binnenland, is jaarlijks een kleine ton beschikbaar voor buitenlandse projecten. In toenemende mate wordt daarbij de aandacht gericht op gebieden waarmee de orde van oudsher banden heeft zoals de Baltische Staten, Kaliningrad en Polen.
De orde geeft ook geld voor medisch-wetenschappelijk onderzoek.
Het Vicariefonds wordt gebruikt om het reformatorisch-christelijke gedachtegoed te bevorderen en draagt bij aan Klinische Pastorale Vorming (KPV), buitenlandse studiereizen, sabbaticals en bijdragen in promotiekosten voor predikanten.

Heraldiek
De commandeurs en de landcommandeur van de orde palen, of kwartileren, wanneer dat heraldisch, gezien de stukken, beter uitkomt, hun eigen wapen met dat van de Duitse Orde. In de 17e eeuw was het daarvoor gebruikte kruis nog van een zilveren zoom voorzien. In de loop der eeuwen werd het kruis eenvoudiger van snit en tegenwoordig is het een eenvoudig Latijns kruis.
De vele in het Duitse Huis bewaard gebleven wapens en portretten van de landscommandeurs zijn een rijke bron van heraldische kennis. Dat geldt ook voor de honderden uitgegeven kwartierstaten van de ridders-expectanten die, zelf of vertegenwoordigd door hun vader, "op hun woord van edelman" een document met hun wapen en dat van hun adellijke grootouders overleggen.

Ordekleding
De orde bezat tot voor enige jaren als ordekleding een kostbaar uniform van witte stof met zwarte omslagen, hoge kaplaarzen, zwaard en kraagspiegel. Daarbij werden een witte mantel en een witgevederde hoed gedragen. Tegenwoordig wordt de mantel over een jacquet of rokkostuum gedragen. De ridders-expectanten dragen een klein kruis aan een zwart lint in het knoopsgat. De commandeurs dragen een kruis aan een zwart lint om de hals en een zilveren, zwart gemaakt, kruis op hun borst.
De landcommandeur draagt zijn kruis aan een gouden keten. Er zijn geen vrouwelijke leden.

De landcommandeurs sinds 1620

(35) Hendrik Casimir I van Nassau-Dietz, 1620-1640.

(36) Willem Frederik van Nassau-Dietz, 1641-1664.

(37) Floris Borre van Amerongen, 1664-1675.

(38) Heinrich von Solms, 1675-1693.

(39) Hendrik Casimir II van Nassau-Dietz, 1693-1696.

(40) Godard van Reede van Athlone, 1697-1703.

(41) Frederik Borre van Amerongen, 1703-1722.

(42) Willem van Lintelo, 1723-1732.

(43) Evert Jan Benjamin van Goltstein, 1732-1744.

(44) Lucas Willem van Broeckhuysen, 1744-1748.

(45) Hendrik van Iselmuden, 1748-1751.

(46) Frederik Willem Torck, 1753-1761.

(47) Unico Wilhelm van Wassenaer, 1763-1766.

(48) Frans Steven Carel van Randwijck, 1766-1785.

(49) Karl Ludwig von Anhalt-Bernburg-Schaumburg, 1786-1806.

(50) Jan Walraad van Welderen, 1806-1807.

(51) Arend van Raesfelt van Elsen, 1807.

(52) Volker Rudolf Bentinck van Schoonheeten, 1807-1820.

(53) Adriaan Wolter Willem Sloet van Sinderen, 1820-1824.

(54) Godert Willem de Vos van Steenwijk, 1824-1830.

(55) Rudolph Hendrik van Iselmuden, 1831-1834.

(56) Floris Willem Sloet tot Warmelo, 1834-1838.

(57) Albert Carel Snouckaert van Schauburg, 1838-1841.

(58) Carl Wilhelm Georg Johan Theodor Bodelschwingh-Plettenberg, 1841-1850.

(59) Otto Anna van Bylant, 1850-1857.

(60) Boudewijn Reynt Wouter Sloet van Hagendorp, 1857-1863.

(61) Frederik Louis Wilhelm van Brakell, 1863-1865.

(62) Hendrik Rudolph Willem van Goltstein van Oldenaller, 1865-1868.

(63) Alexander Carel Jacob Schimmelpenninck van der Oye, 1868-1877.

(64) Jan Derk van Rechteren van Ahnen, 1877-1886.

(65) François Maximiliaan van der Duyn, 1886-1889.
Otto van Dedem, 1889-1894.

(66) Reinhard Jan Christiaan van Pallandt van Rosendael, 1894-1899.

(67) Emilius Johan van Pallandt, 1899-1914.

(68) Alexander Schimmelpenninck van der Oye, 1914-1918.

(69) Anne Willem Jacob Joost van Nagell, 1918-1936.

(70) Otto Jacob Eiffelanus van Wassenaer van Catwijck, 1936-1939.

(71) Karel Gerrit Willem van Wassenaer, 1939-1946.

(72) Frand Johan Julius van Heemstra, 1946-1958.

(73) Bernhard Frederik van Verschuer, 1958-1971.

(74) Hendrik Jan van Nagell, 1971-1977.

(75) Paul Anthony van der Borch, 1977-1992.

(76) Albert van Harinxma thoe Slooten, 1992-

(78) Rudolph Everhard Willem van Weede

(79) Anthon Gerrit Aemile van Rappard

(80) Jan Reint de Vos van Steenwijk

De portretten van de landcommandeurs

De Duitse Orde heeft na 1556 portretten van de landcommandeurs vanaf het jaar 1239 laten maken. De anonieme schilder, "Meester van het Duitse Huis" genoemd, schilderde uiteraard fictieve portretten van de oudste landcommandeurs. De afgebeelde personen zijn wel herkenbaar aan hun wapenschild. Alleen de grootmeester en de Deutschmeister zijn met hun vaandel of commandovlag afgebeeld.

De rij opent met een groot crucifix en een fictief portret van de in 1239 regerende grootmeester Coenraat van Thüringen, daarop volgen de Deutschmeister Bodo van Hohenlohe en de oudste meester van het Utrechtse huis van de Duitse Orde. Al de in 1556 geschilderde portretten hebben hetzelfde formaat en de afgebeelde personen zijn allen in min of meer dezelfde knielende en biddende houding afgebeeld. Allen dragen een harnas en ook hun helmen zijn afgebeeld. Op hun bidbank is hun wapen afgebeeld. Latere portretten uit de periode waarin de orde protestants was tonen de landcommandeurs geknield achter een kist of meubel. Protestanten gebruiken immers geen bidbanken.

Een aantal van de panelen is tijdens de beeldenstorm, in de stad Utrecht betrof het waarschijnlijk de beeldenstorm van 7 maart 1580, beschadigd geraakt. De gezichten werden kapot gekrast maar werden later weer overgeschilderd.
De portretten hebben sindsdien vrijwel altijd in een van de zalen van de orde gehangen. Ze worden nu in het Duitse Huis in Utrecht bewaard vanwaaruit ze in 2015 naar het Centraal Museum in Utrecht zijn gebracht voor een tentoonstelling over de Duitse Orde. De portrettenreeks is na 1592 aangevuld met portretten van de landscommandeurs. Na landscommandeur Hendrik Jan baron van Nagell, die zich in 1971 nog volgens de traditie in harnas had laten portretteren, wordt naar een nieuwe vorm voor de portretten gezocht. Urban Larsson, een van de in de 20e eeuw aangezochte schilders weigerde een portret van een man in harnas te schilderen, zo werd Albertus baron van Harixma thoe Sloten in 1996 in mantel en zwart jacquet afgebeeld. Paulus Anthony baron van der Borch tot Verwolde, heer van Vorden  en Anthon Gerrit Aemile ridder van Rappard  kozen voor een portret in het in onbruik geraakte officiële kostuum van de Duitse Orde.
Na het portret van de tussen 1615 en 1619 geportretteerde landcommandeur Diederik Bloys van Treslong dragen alle landcommandeurs een groot zwartgeëmailleerd kruis van de orde, meestal aan een gouden keten, maar in de late 18e en vroege 19e eeuw ook wel aan een zwart lint om de hals.

De oudere portretten zijn in veel gevallen zwaar gerestaureerd en vaak overgeschilderd. De orde heeft vaak, maar niet altijd, voor portretschilders uit Utrecht gekozen.

Literatuur
 F.J.W. FABIUS, De Ridderlijke Duitse Orde van verleden tot heden. [Z.j., ca. 1958].
 P. J. D'ARTILLAC BRILL, Beknopte geschiedenis der Nederlandse ridderorden. 's-Gravenhage, 1958.
 J.W. JONGEDIJK, Ridderlijke Orden in Nederland. Zaltbommel, 1965.
 J.A. VAN ZELM VAN ELDIK, Moed en deugd. Ridderorden in Nederland. Deel I. Zutphen, 2003.
 Dr. Daantje MEUWISSEN, Gekoesterde traditie, de portretreeks met de landcommandeurs van de Utrechtse Balije van de Ridderlijke Duitse Orde, Hilversum 2011
 Renger E. DE BRUIN, Bedreigd door Napoleon. De Ridderlijke Duitse Orde, Balje van Utrecht, 1753-1838, Uitg. Verloren, 2012.
 Huib J. ZUIDERVAART, Ridders, priesters en predikanten in Schelluinen. De geschiedenis van een commanderij van de Ridderlijke Duitse Orde, Balje van Utrecht, Uitg. Verloren, 2013.
 Jerem VAN DUIJL, Goederenverwerving van het Duitse Huis in Utrecht 1218-1536, Uitg. Verloren, 2022.

Externe link

 Officiële website RDO Balje van Utrecht

Voetnoten

Duitse
Duitse
Utrecht

redpajama_set_name: RedPajamaWikipedia


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Ferry Cross The Mersey
Defecting between the major parties is something I find a little incomprehensible in general. The funny thing is that most of the individual decisions are even less easy to understand. As we might expect, the BBC has taken to reporting council level defections which is how I found out about this oddity.
Here's what the BBC reports.
Mr Jobling, who was first elected in 2003 and is a member of Merseyside Police Authority, said the proposed cuts to the police force had really bothered him.
So lemme get this straight. A Lib Dem defects to Labour because of proposed cuts to the police force. This is confounding on so many levels? To name 3
1. Why was he a Lib Dem in the first place if policing is his number one issue?
2. Where did he get the idea that Labour is the law n order party?
3. Why did he have to wait so long to jump ship? It's been clear for months that due to the previous Labour overspending, budgets would need to contract in all departments but health and international development.
In a word, odd.


text:
Anyone caught drink-driving in NSW can now lose their licence immediately under a tough new penalty regime that will also see offenders fined almost $600. First time, low-range drink-drivers from May 20 can be slapped with an on-the-spot suspension of their licence for three months and a fine of $561. Roads Minister Andrew Constance says NSW is taking a "zero-tolerance" approach to drink and drug-driving. READ ALSO: "This means anyone caught drink-driving in NSW, at any level, including low-range, can now lose their licence immediately," the minister said in a statement on Monday. "This reform makes it clear if you break the law, you will pay the price. We are taking a zero-tolerance approach to drink and drug driving." Drivers found with drugs in their system will face the same penalties if the offence is confirmed by laboratory analysis. Some 68 people died in alcohol-related crashes on NSW roads last year. Drug-driving resulted in a similar number of deaths. Assistant Police Commissioner Michael Corboy said the reform would protect road users by ensuring swift and certain penalties. "Alcohol is one of the major factors in crashes that kill or injure people on NSW roads. The 0.05 blood alcohol limit has been in place for almost 38 years. There are no more excuses," Assistant Commissioner Corboy said. AAP
/images/transform/v1/crop/frm/silverstone-feed-data/6c77d878-4e56-4ff6-a3d5-4a0800b6f255.jpg/r0_74_800_526_w1200_h678_fmax.jpg
May 6 2019 - 2:10PM
Immediate loss of licence for all drink drivers under new laws
Heather McNab
Anyone in NSW found drink-driving will immediately lose their licence for three months from May 20.
Anyone caught drink-driving in NSW can now lose their licence immediately under a tough new penalty regime that will also see offenders fined almost $600.
First time, low-range drink-drivers from May 20 can be slapped with an on-the-spot suspension of their licence for three months and a fine of $561.
Roads Minister Andrew Constance says NSW is taking a "zero-tolerance" approach to drink and drug-driving.
Man admits to dangerous driving after head-on crash
Gas flares could run for 30 hours straight as company checks pipeline
All the photos from Saturday's Westpac Rescue Helicoper Ball
"This means anyone caught drink-driving in NSW, at any level, including low-range, can now lose their licence immediately," the minister said in a statement on Monday.
"This reform makes it clear if you break the law, you will pay the price. We are taking a zero-tolerance approach to drink and drug driving."
Drivers found with drugs in their system will face the same penalties if the offence is confirmed by laboratory analysis.
Some 68 people died in alcohol-related crashes on NSW roads last year. Drug-driving resulted in a similar number of deaths.
Assistant Police Commissioner Michael Corboy said the reform would protect road users by ensuring swift and certain penalties.
"Alcohol is one of the major factors in crashes that kill or injure people on NSW roads. The 0.05 blood alcohol limit has been in place for almost 38 years. There are no more excuses," Assistant Commissioner Corboy said.
Discuss "Immediate loss of licence for all drink drivers under new laws"


text:
Christian Schools and the City: An Introduction
jarmoluk / Pixabay
This summer, Erik Ellefsen asked if I might write a piece kicking off a new series for CACE about Christian Schools in the City. While today I work with The Gospel Coalition, a group aimed primarily at church leaders, I continue to see Christian education as strategic for the gospel's advance in our nation's cities.
I am not only a product of Christian education myself but I have served at two urban Christian schools in Minneapolis. First as a teacher at a leading Christian school (Minnehaha Academy) and then in senior leadership at a classical Christ-centered school for disadvantaged youth. I remain involved at both schools. The second, Hope Academy, will be one of the six schools this series will profile.
But I first want to address the question of why engaging the city is essential for the future of Christian schooling.
There are three key reasons—cultural, missiological, and visceral. All three are drawn from a wonderful address given by Dr. Tim Keller to the Lausanne Congress on World Evangelization back in 2010 in Cape Town, South Africa.
First, culturally. We live in a more urbanized world than at any time in history, and if we have the goal of having our shared life shaped by the gospel and the kingdom, we must focus on cities. More than ever before, the economic and cultural forces that shape our world are being shaped not by nation-states, but by cities.
Second, missiologically. Cities are strategic to God's mission because there are four kinds of people who disproportionately live in the city: young adults, unreached peoples, cultural elites, and the poor. All of them have children who will need to be educated.
Young Adults – The younger generation all around the world, and increasingly in America, disproportionately want to live in cities.
Unreached peoples – Unreached people around the world are much more reachable in cities. Keller notes that when people "immigrate from rural areas or from other countries, they break their kinship ties, and are in a more pluralistic environment…they are far more open to the gospel than they would have been in their previous habitat."
Cultural elites – Cities are where cultures are shaped. Keller stresses that "people who tend to make the films, write the books, do the business deals" live in cities.
The poor – Here Keller cites the fact that one third of people moving into cities around the world live in shanty towns or (in developed nations) economically disadvantaged neighborhoods. God's people have always shared God's particular burden for the poor.
Third, viscerally. Keller here cites God's encounter with Jonah over his reluctance to go to Ninevah. When Jonah grieves over the small plant that was giving him shade that then dies—God chastizes Jonah. God, Keller argues, loves people more than plants, and cities are where people are. In cities, he says, "you have more image of God per square inch than anywhere else in the world".
The city is central to God's mission culturally, missiologically, and viscerally. The Christian schools and leaders that will be profiled in this series all share Dr. Keller's conviction that if we want human life and culture to be shaped at all by Jesus Christ, we simply must have excellent Christian schools that serve the children of the city.
Over the coming weeks, leaders of these schools will share their approach as well as lessons learned. They may prioritize different segments in their respective city, but our hope is that their stories and their schools might inspire you to see Christian schooling as a key part of God's mission in your city.
The leaders you will hear from and their schools are: Russ Gregg, Head of School of Hope Academy (Minneapolis, MN), Jesse Kell, Executive Director of Elijah House Academy (Richmond, VA), Jake Becker, Headmaster of The City School (Philadelphia), John Booy, founder and President of The Potter's House (Grand Rapids, MI); Ben Sciacca, Head of School at Restoration Academy in Fairfield, Alabama; Frank Guerra of Boston Trinity Academy (Boston, MA), Andrew Hart, Head of School of The Oaks Academy (Indianapolis, Indiana) and others.
Dan Olson
Dan Olson (@danjolson) is the Executive Director of the Spreading Hope Network after servings as director of advancement for The Gospel Coalition. Prior to TGC, Dan spent nine years involved in urban ministry and development with Hope Academy (Minneapolis). He received his BA from Wheaton College in Illinois and his MA in theological studies from Regent College in Vancouver. He lives in Minneapolis with his wife, Lucy, and their four kids.
Future of Christian Education
Hope Academy and Minneapolis
Preparing Our Kids For The Innovation Era


text:
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A little while ago we wrote about a case called Cape v Dring. It wasn't a family case at all, in fact it was something to do with asbestos, and the reason we wrote about it was because it dealt with the principles that apply to applications for sight of documents...
"I hurt you because I love you" – what did TV's Silent Witness get right and wrong about the treatment of domestic violence in the family courts?
No one is ever going to give the BBC TV show Silent Witness any prizes for being particularly factually accurate (what do you MEAN forensic pathologists don't actually run around solving crimes!?). But who cares, right? It's good, dramatic telly. That was all well and...
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text:
Dhaneshwor Temple () is 1 km south of the town Banepa. This is a temple of Shiva.

References

External links
   KMC plan goes up in smoke

Hindu temples in Bagmati Province
Buildings and structures in Kavrepalanchok District


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text:
package org.apache.hawq.pxf.service;

import com.google.common.base.Ticker;
import org.apache.hadoop.security.UserGroupInformation;
import org.junit.Before;
import org.junit.Test;
import org.mockito.invocation.InvocationOnMock;
import org.mockito.stubbing.Answer;

import java.io.IOException;
import java.util.concurrent.atomic.AtomicLong;

import static junit.framework.TestCase.assertTrue;
import static org.junit.Assert.assertEquals;
import static org.junit.Assert.assertFalse;
import static org.junit.Assert.assertNotEquals;
import static org.junit.Assert.assertNotNull;
import static org.mockito.Matchers.any;
import static org.mockito.Mockito.doThrow;
import static org.mockito.Mockito.mock;
import static org.mockito.Mockito.never;
import static org.mockito.Mockito.times;
import static org.mockito.Mockito.verify;
import static org.powermock.api.mockito.PowerMockito.when;

public class UGICacheTest {
    private static final long MINUTES = 60 * 1000L;
    private UGIProvider provider = null;
    private SessionId session = null;
    private UGICache cache = null;
    private FakeTicker fakeTicker;

    static class FakeTicker extends Ticker {
        private final AtomicLong nanos = new AtomicLong();

        @Override
        public long read() {
            return nanos.get();
        }

        long advanceTime(long milliseconds) {
            return nanos.addAndGet(milliseconds * UGICache.NANOS_PER_MILLIS) / UGICache.NANOS_PER_MILLIS;
        }
    }

    @Before
    public void setUp() throws Exception {
        provider = mock(UGIProvider.class);
        when(provider.createProxyUGI(any(String.class))).thenAnswer(new Answer<UserGroupInformation>() {
            @Override
            public UserGroupInformation answer(InvocationOnMock invocation) {
                return mock(UserGroupInformation.class);
            }
        });

        session = new SessionId(0, "txn-id", "the-user");
        fakeTicker = new FakeTicker();
        cache = new UGICache(provider, fakeTicker);
    }

    @Test
    public void getUGIFromEmptyCache() throws Exception {
        UserGroupInformation ugi = cache.getUserGroupInformation(session);
        assertNotNull(ugi);
        verify(provider).createProxyUGI("the-user");
    }

    @Test
    public void getSameUGITwiceUsesCache() throws Exception {
        UserGroupInformation ugi1 = cache.getUserGroupInformation(session);
        UserGroupInformation ugi2 = cache.getUserGroupInformation(session);
        assertEquals(ugi1, ugi2);
        verify(provider, times(1)).createProxyUGI("the-user");
        assertCacheSize(1);
    }

    @Test
    public void getUGIWithEquivalentSessionsReturnsTheSameInstance() throws Exception {
        SessionId session2 = new SessionId(0, "txn-id", "the-user");
        UserGroupInformation ugi1 = cache.getUserGroupInformation(session);
        UserGroupInformation ugi2 = cache.getUserGroupInformation(session2);
        assertEquals(ugi1, ugi2);
    }

    @Test
    public void getTwoUGIsWithDifferentTransactionsForSameUser() throws Exception {
        SessionId otherSession = new SessionId(0, "txn-id-2", "the-user");
        UserGroupInformation proxyUGI1 = cache.getUserGroupInformation(session);
        UserGroupInformation proxyUGI2 = cache.getUserGroupInformation(otherSession);
        assertNotEquals(proxyUGI1, proxyUGI2);
        verify(provider, times(2)).createProxyUGI("the-user");
        assertCacheSize(2);
        // getting a new UGI instance for each transaction ID is not strictly necessary, but allows
        // us to expire UGIs for transactions that have finished. If we reused one UGI per user,
        // it might never get to expire from the cache, and eventually Kerberos might invalidate
        // the UGI on its end.
    }

    @Test
    public void getTwoUGIsWithDifferentUsers() throws Exception {
        SessionId otherSession = new SessionId(0, "txn-id", "different-user");
        UserGroupInformation proxyUGI1 = cache.getUserGroupInformation(session);
        UserGroupInformation proxyUGI2 = cache.getUserGroupInformation(otherSession);
        assertNotEquals(proxyUGI1, proxyUGI2);
        verify(provider, times(1)).createProxyUGI("the-user");
        verify(provider, times(1)).createProxyUGI("different-user");
        assertCacheSize(2);
        assertStillInCache(session, proxyUGI1);
        assertStillInCache(otherSession, proxyUGI2);
    }

    @Test
    public void anySegmentIdIsValid() throws Exception {
        int crazySegId = Integer.MAX_VALUE;
        session = new SessionId(crazySegId, "txn-id", "the-user");
        UserGroupInformation proxyUGI1 = cache.getUserGroupInformation(session);
        assertNotNull(proxyUGI1);
        assertStillInCache(session, proxyUGI1);
    }

    @Test
    public void ensureCleanUpAfterExpiration() throws Exception {
        UserGroupInformation ugi1 = cache.getUserGroupInformation(session);
        cache.release(session, false);
        fakeTicker.advanceTime(UGICache.UGI_CACHE_EXPIRY + 1000);

        SessionId session2 = new SessionId(0, "txn-id", "the-user-2");
        cache.getUserGroupInformation(session2); // this triggers cleanup of ugi1
        assertNoLongerInCache(session, ugi1);
        cache.release(session2, true);
        assertCacheSize(0);
    }

    @Test
    public void ensureExpiredUGIIsNotCleanedUpIfItIsStillReferenced() throws Exception {
        SessionId session2 = new SessionId(0, "txn-id", "the-user-2");
        UserGroupInformation stillInUse = cache.getUserGroupInformation(session);
        fakeTicker.advanceTime(UGICache.UGI_CACHE_EXPIRY + 1000);

        // at this point, stillInUse is expired but still in use
        cache.getUserGroupInformation(session2); // trigger cleanup
        assertStillInCache(session, stillInUse);
        cache.release(session, false);
        fakeTicker.advanceTime(UGICache.UGI_CACHE_EXPIRY + 1000);

        cache.getUserGroupInformation(session2);

        verify(provider, times(1)).destroy(stillInUse);
    }

    @Test
    public void putsItemsBackInTheQueueWhenResettingExpirationDate() throws Exception {
        SessionId session2 = new SessionId(0, "txn-id", "the-user-2");
        SessionId session3 = new SessionId(0, "txn-id", "the-user-3");

        UserGroupInformation ugi1 = cache.getUserGroupInformation(session);
        fakeTicker.advanceTime(UGICache.UGI_CACHE_EXPIRY - 1000);
        UserGroupInformation ugi2 = cache.getUserGroupInformation(session2);
        cache.release(session2, false);
        fakeTicker.advanceTime(UGICache.UGI_CACHE_EXPIRY - 1000);
        cache.release(session, false);
        fakeTicker.advanceTime(2 * MINUTES);
        cache.getUserGroupInformation(session3);

        assertStillInCache(session, ugi1);
        assertNoLongerInCache(session2, ugi2);
    }

    @Test
    public void releaseWithoutImmediateCleanup() throws Exception {
        UserGroupInformation ugi1 = cache.getUserGroupInformation(session);

        cache.release(session, false);
        assertStillInCache(session, ugi1);
    }

    @Test
    public void releaseWithImmediateCleanup() throws Exception {
        UserGroupInformation ugi1 = cache.getUserGroupInformation(session);

        cache.release(session, true);
        assertNoLongerInCache(session, ugi1);
    }

    @Test
    public void releaseWithImmediateCleanupOnlyCleansUGIsForThatSegment() throws Exception {
        UserGroupInformation ugi1 = cache.getUserGroupInformation(session);

        SessionId differentSeg = new SessionId(999, "txn-id", "user");
        UserGroupInformation ugi2 = cache.getUserGroupInformation(differentSeg);

        cache.release(differentSeg, false); // ugi2 is now unreferenced
        cache.release(session, true);
        assertNoLongerInCache(session, ugi1);
        assertStillInCache(differentSeg, ugi2);
        assertCacheSize(1);
    }

    @Test
    public void releaseResetsTheExpirationTime() throws Exception {
        UserGroupInformation reference1 = cache.getUserGroupInformation(session);
        cache.getUserGroupInformation(session);

        cache.release(session, true);
        fakeTicker.advanceTime(UGICache.UGI_CACHE_EXPIRY + 1000);
        cache.release(session, false);
        fakeTicker.advanceTime(UGICache.UGI_CACHE_EXPIRY - 1000);

        assertStillInCache(session, reference1);
    }

    @Test
    public void releaseAnExpiredUGIResetsTheTimer() throws Exception {
        UserGroupInformation ugi1 = cache.getUserGroupInformation(session);
        fakeTicker.advanceTime(UGICache.UGI_CACHE_EXPIRY + 1000);
        cache.release(session, false);

        assertStillInCache(session, ugi1);

        fakeTicker.advanceTime(UGICache.UGI_CACHE_EXPIRY - 1000);
        SessionId session2 = new SessionId(0, "txn-id", "the-user-2");
        cache.getUserGroupInformation(session2); // triggers cleanup
        assertStillInCache(session, ugi1);
    }

    @Test
    public void releaseAndReacquireDoesNotFreeResources() throws Exception {
        cache.getUserGroupInformation(session);
        cache.release(session, false);
        UserGroupInformation ugi2 = cache.getUserGroupInformation(session);
        fakeTicker.advanceTime(UGICache.UGI_CACHE_EXPIRY + 1000);
        UserGroupInformation ugi3 = cache.getUserGroupInformation(session);
        // this does not clean up any UGIs because our ugi is still in use.
        assertEquals(ugi3, ugi2);
        verify(provider, times(1)).createProxyUGI("the-user");
        verify(provider, never()).destroy(any(UserGroupInformation.class));
        assertStillInCache(session, ugi2);
    }

    @Test
    public void releaseAndAcquireAfterTimeoutFreesResources() throws Exception {
        UserGroupInformation ugi1 = cache.getUserGroupInformation(session);

        cache.release(session, false);
        fakeTicker.advanceTime(UGICache.UGI_CACHE_EXPIRY + 1000);
        assertStillInCache(session, ugi1);
        UserGroupInformation ugi2 = cache.getUserGroupInformation(session);
        verify(provider).destroy(ugi1);
        assertNotEquals(ugi2, ugi1);
        assertStillInCache(session, ugi2);
    }

    @Test
    public void releaseDoesNotFreeResourcesIfUGIIsUsedElsewhere() throws Exception {
        UserGroupInformation ugi1 = cache.getUserGroupInformation(session);
        cache.getUserGroupInformation(session); // increments ref count to 2

        cache.release(session, true);
        fakeTicker.advanceTime(60 * MINUTES);
        // UGI was not cleaned up because we are still holding a reference
        assertStillInCache(session, ugi1);
    }

    @Test
    public void releasingAllReferencesFreesResources() throws Exception {
        UserGroupInformation ugi1 = cache.getUserGroupInformation(session);
        UserGroupInformation ugi2 = cache.getUserGroupInformation(session);

        assertEquals(ugi1, ugi2);

        cache.release(session, true);
        assertStillInCache(session, ugi1);
        cache.release(session, true);
        // at this point, the initial UGI has been freed.
        assertNoLongerInCache(session, ugi1);
    }

    @Test(expected = IOException.class)
    public void errorsThrownByCreatingAUgiAreNotCaught() throws Exception {
        when(provider.createProxyUGI("the-user")).thenThrow(new IOException("test exception"));
        cache.getUserGroupInformation(session);
    }

    @Test
    public void errorsThrownByDestroyingAUgiAreCaught() throws Exception {
        UserGroupInformation ugi1 = cache.getUserGroupInformation(session);
        doThrow(new IOException("test exception")).when(provider).destroy(ugi1);
        cache.release(session, true); // does not throw
    }

    @Test(expected = IllegalStateException.class)
    public void releaseAnEntryNotInTheCache() {
        // this could happen if some caller of the cache calls release twice.
        cache.release(session, false);
    }

    private void assertStillInCache(SessionId session, UserGroupInformation ugi) throws Exception {
        assertTrue(cache.contains(session));
        verify(provider, never()).destroy(ugi);
    }

    private void assertNoLongerInCache(SessionId session, UserGroupInformation ugi) throws Exception {
        assertFalse(cache.contains(session));
        verify(provider, times(1)).destroy(ugi);
    }

    private void assertCacheSize(int expectedSize) {
        assertEquals(expectedSize, cache.size());
        assertEquals(expectedSize, cache.allQueuesSize());
    }
}

redpajama_set_name: RedPajamaGithub