text:
\section{Introduction}

Spectral and temporal properties of galactic and extra-galactic black holes
suggest time dependence of various degrees.  Imaging a black hole accretion disk
would therefore not be accurate without inclusion of the time dependence of
various disk components. There is a class of stellar mass black hole
candidates, known as the outbursting sources, which totally changes its disk configurations
in a matter of few days, when it goes through transitions of its spectral states from
hard to hard intermediate to soft intermediate and then soft states during their
rising phase. Recently, through fits of data with Two Component Advective Flow (TCAF) solution
as prescribed by Chakrabarti \& Titarchuk (1995; hereafter, CT95), the accretion rates
of the halo and disk components, the sizes of the hot electron cloud (`Compton cloud') etc.
were all shown to be highly variable. The Compton cloud in this solution is the
inner part of the advective halo, puffed up due to slowing down by the centrifugal barrier,
which not only inverse Comptonizes the soft photons to produce high energy X-rays, but also
produces outflowing matter just as a normal boundary layer. The disk component on the
equatorial plane supplies soft photons. In the absence of the CENBOL
as in the soft state, the flow behaves as a standard thin disk with the inner edge
close to the inner stable circular orbit or ISCO (Shakura \& Sunyaev, 1973) and no jets or outflows
are seen.  In class-variable sources, such as  GRS 1915+105, temporal variation in
significant count rates and state transitions such as (burst-on and burst-off states)
are seen in a matter of few seconds (Muno et al. 1999). This source also exhibits strong
relativistic radio jets (Fender et al. 1999). Along with the monotonic changes in the CENBOL sizes, the
frequency of the Quasi-Periodic Oscillations (QPOs) is also seen to change
monotonically (Chakrabarti et al. 2005). Theoretical work which forms the basis of TCAF
is in Chakrabarti (1996) and references therein.

The time dependent simulations (Giri, Garain \& Chakrabarti 2013
and references therein) show the formation of two components in the flow
with the Keplerian disk on the equatorial plane and advective halo surrounding it
formed the shock and outflows exactly as envisaged in CT95. Outflows are intrinsically associated with
accretion mechanism (see C90 and Chakrabarti 1996 for further details) in this solution. The explicit
ratio of mass outflow rate to the inflow rate was first computed in Chakrabarti (1999)
and was found to strongly depend on the compression ratio at the shock.
From Fig. 4 of Giri \& Chakrabarti (2012), it is clear that the ratio of the outflow to
the inflow rate increases with decreasing viscosity parameter and the inviscid flow
produces maximum outflows. In outbursts or class variable sources, outflows are found to be
sporadic and highly variable. Thus, it is very important to have the
time dependent spectra and images of TCAF where outflows are self-consistently
generated from the CENBOL itself. Cooling via Comptonization is an essential mechanism by which the
CENBOL reduces its size making the spectrum softer. While the CENBOL lasts,
rough agreement between the cooling and compressional heating timescales causes it
to oscillate and produce the so-called QPOs (Chakrabarti et al. 2015 and references
therein). Detailed hydrodynamic simulations in presence of Compton cooling
are in Ghosh, Garain \& Chakrabarti (2011) and Garain, Ghosh \& Chakrabarti
(2014) where effects of cooling on the spectra, shock location and the formation of
QPOs are described.

Theoretical efforts for imaging of accretion disks started with the pioneering
work by Luminet (1978) who drew the image of a standard Keplerian  disk around a
Schwarzschild black hole (Shakura-Sunyaev, 1973). The method of image construction was done from the
observers end. This technique is very useful as photons were not lost while
tracking them from the observer. Following this, Fukue \& Yokohama (1988) published
the colored version of the image. With that, they also studied the occultation
effect on accretion disk light curve. A few years later, Viergutz (1992) generalized
the transfer functions for Kerr geometry. Marck (1996), for the first time, produced
the Keplerian disk image using the actual Ray-Tracing mechanism. Bromley et al. (2001)
added polarization determination. Dexter \& Agol (2009) first published `geokerr', a
public code to compute images in Kerr geometry. `GYOTO' (Vincent et al., 2011),
`YNOGK' (Yang \& Wang, 2013), `GRTRANS' (Dexter, 2016) came into public domains. The
focus of these works was to prepare one to interpret results from the Event
Horizon Telescope (EHT) whose objective is to identify the horizon of the supermassive
black hole at the centre of our Galaxy.

Armitage \& Reynolds (2003), first performed MHD simulation of Keplerian disk and
produced the images where the disk structure remained the same at all the time.
More recently, Broderick \& Loeb (2009) presented results where simulated images
of force free jets (Tchekhovskoy et al. 2008) launched from M87 are shown for various
model parameters and polarization maps of the magnetically driven jets are obtained.
However, under TCAF paradigm, one does not have to introduce magnetic field to generate
outflows. The hydrodynamic inflow produces time varying outflows self-consistently. Magnetic
field may be useful for collimation and acceleration purposed further out.

GRMHD simulations in the context of our Galactic centre were mostly performed
(Ohsuga et al. 2005; Noble et al. 2007; M\`oscibrodzka et al. 2009, 2011; Dexter et al. 2010;
Hilburn et al. 2010; Dexter \& Fragile 2012; Dolence et al. 2012; Shcherbakov, Penna
\& McKinney 2012, S\c adowski et al. 2013, Roelofs et al. 2017) considering a very
low accretion rate as applicable. Cooling term was neglected as appropriate for Sgr A*.
In fact, Dibi et al. (2012) added the cooling term and found the effect to be negligible in case
Sgr A*. Drappeau et al. (2013) constrained the mass accretion rate to be $\sim10^{-9}~M_{\odot}/yr$
with a highly spinning central black hole. This accretion rate is much lower
than that of the earlier result ($\sim10^{-5}~M_{\odot}/yr$) predicted by Coker \& Melia
(1997). A detailed review on the simulations and observational possibilities of the black hole
shadow of Sgr A* was presented by Falcke \& Markoff (2013). But, most of the earlier studies were
based on the RIAF model to simulate spectra and images of Sgr A* only. However, there exists
a large number of SMBHs in Radio Loud Quasars, Seyfert galaxies, where the accretion rate
could be substantially high (Bian \& Zhao, 2003) and thus formation of disk and cooling becomes
important. Another situation which might induce a sudden high mass inflow is from tidal
disruption of neighboring object (Gillessen et al. 2012).

Chatterjee, Chakrabarti \& Ghosh, (2017a, hereafter CCG17a) showed the static images of TCAF
with general relativistic thick disks acting as the Compton cloud and relativistic
Keplerian disk (Page \& Thorne, 1974) acting as the source of seed photons. Images for various disk
rates and inclination angle are shown with their observable spectral counterparts.
The variation of optical depth of the CENBOL medium is achieved by changing the
halo rate ($\dot{m}_h$). They have shown that by increasing the optical depth, the Keplerian
disk from the other side is completely blocked by the CENBOL medium. Also, with increasing
inclination angle, the spectral hardening can be seen in their work. Following the
same geometry, Chatterjee, Chakrabarti \& Ghosh, 2017b, (hereafter CCG17b) simulated
the time lags of various energy bins and compare the simulated results with the
observed counterparts.

In this paper, for the first time, we present time dependent images of TCAF
with Comptonization and outflows. Basic simulation process by hydrodynamic TVD
code is explained \S 2. Thermodynamic properties of CENBOL and Keplerian
disk are presented in \S 3. Section deals with Monte-Carlo simulation of Comptonization
and cooling mechanism. The spectra, time dependent images with and without
cooling effects are presented in the results section. Convolved images of accretion
disk at different spectral states are presented. We discuss our results and conclude
this paper in the final section.

\section{Time Dependent Simulations of TCAF}
Hydrodynamic simulation procedure is similar to what has been earlier reported in Ryu et al. (1997),
Giri et al. (2010), Giri \& Chakrabarti (2012, 2013), Giri, Garain \& Chakrabarti (2015).
Governing equations of TVD are explicitly presented by Ryu et al. 1996; Molteni et al.
1996; Giri \& Chakrabarti 2012. The conservation equation of mass, momentum and energy for an
axisymmetric, inviscid, non-magnetic flow takes the following form
\begin{equation}
\frac{\partial \boldsymbol {q}}{\partial t} + \frac{1}{r} \frac{\partial\boldsymbol {F_1}}{\partial r} +
\frac{\partial\boldsymbol {F_2}}{\partial r} + \frac{\partial\boldsymbol {G}}{\partial z} = \boldsymbol {S},
\end{equation}
where
$\boldsymbol{q}= \left (\begin{array}{c}
\rho\\
\rho v_r\\
\rho v_{\theta}\\
\rho v_{z}\\
E
\end{array} \right ) $ is the state vector,  \\
$\boldsymbol{F_1}= \left (\begin{array}{c}
\rho v_{r}\\
\rho v_{r}^{2}\\
\rho v_{r}v_{\theta}\\
\rho v_{r}v_{z}\\
(E+\rho)v_{r}
\end{array} \right ), $
$\boldsymbol{F_2}= \left (\begin{array}{c}
0\\
p\\
0\\
0\\
0
\end{array} \right ), $

$\boldsymbol{F_2}= \left (\begin{array}{c}
\rho v_{z}\\
\rho v_{r}v_{z}\\
\rho v_{\theta}v_{z}\\
\rho v_{z}^2 + p\\
(E+\rho)v_{z}
\end{array} \right )$ are the flux functions.

The source function is defined as\\
$\boldsymbol{S}= \left (\begin{array}{c}
0\\
\frac{\rho v_{\theta}^2}{r}-\frac{\rho r}{2(\sqrt{r^2+z^2}-1)^2\sqrt{r^2+z^2}}\\
-\frac{\rho v_{r}v_{\theta}}{r}\\
-\frac{\rho z}{2(\sqrt{r^2+z^2}-1)^2\sqrt{r^2+z^2}}\\
-\frac{\rho (rv_{r}+zv_{z})}{2(\sqrt{r^2+z^2}-1)^2\sqrt{r^2+z^2}}
\end{array} \right ). $

The energy density $E=p/(\gamma -1)+\rho(v_{r}^2+v_{\theta}^2+v_{z}^2)/2$ is the sum
of thermal and kinetic energy of the infalling matter. The equation corresponding
to energy density can be extracted as
\\

$
\frac{\partial {E}}{\partial t} + \frac{1}{r} \frac{\partial {(E+\rho)v_{r}}}{\partial x} +
+ \frac{\partial {(E+\rho)v_{z}}}{\partial z} =
-\frac{\rho (rv_{r}+zv_{z})}{2(\sqrt{r^2+z^2}-1)^2\sqrt{r^2+z^2}}.
$
\\

During cooling, change in $E$ directly modifies the flow configurations following Eqn (1).

The gravitational field, as far as the hydrodynamics is concerned, is assumed to follow the
Paczy\'nski \& Wiita (1980) pseudo-Newtonian potential which is given by,
\begin{equation}
\phi(r,Z)=-\frac{GM_{bh}}{r-r_g}
\end{equation}
where $G$ is the universal gravitational constant, $M_{bh}$ is the mass of the black hole kept at
$10~M_{\odot}$ throughout the simulation and $r_g=\frac{2GM_{bh}}{c^2}=1$ is the Schwarzschild radius
and $r=\sqrt{r^2+Z^2}$. Velocity of light is denoted by $c$. The flow is considered to be adiabatic
and axisymmetric with the black hole sitting at centre of the cylindrical co-ordinate system
defined by $(r,\theta,Z)$. In our current simulation, we have ignored viscosity to
have the strong and hot shock and consequently highest outflow rate. Thus, the specific
angular momentum $\lambda$ is constant everywhere. Also, from C89 and C90, it is known that for
a steady state situation the specific energy $\varepsilon$ is also constant.
Matter is injected at the outer boundary with specific energy $\varepsilon=0.003$
(in units of $c^2$) and specific angular momentum $\lambda=1.8$ )in units of $c r_g$.

TVD scheme was originally developed by Harten (1983) to solve the hyperbolic equations present in
the hydrodynamic conservation equations. This method works on the second order accuracy by
modifying first order flux function to use the non-oscillatory results in the second order
solutions. The details of the code were presented in Ryu et al. (1995, 1997) where the code is
modified to suit black hole accretion.

Our computational domain is defined as: $0<r<100$ and $0<Z<100$ in $r-Z$ plane with a grid
resolution of $512\times512$. So, each grid size is $\delta r=0.195 r_g$ and $\delta Z=0.195 r_g$.
The black hole absorption boundary is kept at $1.5 r_g$ after which all informations about the
matter as well as photons are lost. Before starting the simulation, entire grid is filled with a low floor density
($10^{-8}$ where the injected density is $1$ in code unit) to avoid any numerical singularities.
At the outer boundary sub-Keplerian
matter is allowed to flow through. During the accretion, the matter follows the inviscid hybrid
accretion mechanism (Chakrabarti 1990) and forms a shock at a specified position.
We assume axisymmetry and perform our hydro-simulation on the first quadrant of the r-Z plane.
The black hole is located at the origin of the r-Z coordinate system.
The initial pressure is chosen such that the sound speed as of the interior material is same as
the incoming matter. Also, inside the computational domain, all the velocity components are set to
zero initially. The simulation result does not depend on the chosen initial condition as the
initial matter is washed away by the incoming matter in a few dynamical time. On the right
radial boundary, we use an inflow boundary condition. Incoming matter enters the computational
domain through this boundary. Since the density of the incoming matter is chosen to be unity, it
has $10^{8}$ times higher pressure and it rushes towards the central black hole practically through
vacuum until it hits the centrifugal barrier.

Total dynamical time scale for this simulation is $4000$ which in physical units ($\frac{2GM_{BH}}{c^3}\times f_{t}$,
where $f_{t}$ contains informations of each time) is about $40$s. In the present context, the hydrodynamical
simulation has been performed for Galactic black hole candidates. However, these results will also hold for
supermassive or intermediate mass black holes.

\section{Density and Temperature Profile of the Electron Cloud}
CENBOL is a region of hot electron cloud where inverse Comptonization  of soft photons
originated from the Keplerian disk occurs. The electrons in this region are ultra-relativistic. So, $\gamma=4/3$
is a good assumption for this region. Number density (per $cm^3$) and temperature (in the kilo electron Volt)
of the electrons are supplied for each grid. The pressure and density is related via polytropic equation
of state $p=K\rho^{\gamma}$, where $p$ is the pressure, $K$ the entropy constant and $\rho$ is the density
of the flow. From this, we can write $T\propto \rho^{1/3}$, where $T$ is the temperature of the electron
cloud. In our studies, the maximum number density of electron is $\sim 10^{19}~per~cm^3$ and temperature is
$\sim 250~keV$. Hydrodynamical simulation changes the configuration of CENBOL region for each time stamp. The
variation of electron cloud geometry with number density and temperature as given in the color bar are presented in
Figs. 1.

\begin{figure*}
\centering
\vbox{
\includegraphics[height=5.5cm,width=8.0cm]{image01a.eps}\hskip 0.5cm
\includegraphics[height=5.5cm,width=8.0cm]{image01b.eps}}
\caption{Electron Density (in the units of number per $cm^3$ shown in log scale, left panel)
and temperature (in the units of keV, right panel) distribution in the post-shock region at
(a) $t=14.25s$, (b) $t=14.35s$, (c)  $t=14.45s$, (d) $t=14.55$, (e) $t=14.65s$ and (f) $t=14.75s$.}

\end{figure*}

From Fig. 1, the region of outflows can be distinctly seen as a region where temperature and electron
number density drops rapidly. Over the time, the geometry of the CENBOL region changes as hydrodynamical
simulation progresses. One can easily differentiate between Fig. 1a and Fig. 1f as the amount of outflow increased
substantially in the time passed. The inner isobaric contours of the CENBOL region (Figs. 1a-f)
behave similar to thick disks (Abramowicz et al. 1978; Kozlowski et al. 1978; Paczy\'nski \& Wiita 1980; Begelman, Blandford
\& Rees 1982; Chakrabarti, 1985a) as pointed out by Molteni, Lanzafame \& Chakrabarti (1994, hereafter MLC94).

The TVD method simulates a true accretion mechanism. The injected matter washes away the
initial low floor matter and attains a quasi steady state. Inflowing matter undergoes a shock due
to the centrifugal barrier. After the shock, matter starts to flow towards black hole. The mass
absorption rate through the black hole boundary ($1.5~r_g$) is represented in the Fig. 2. It can
be seen that the mass absorption rate after the transient phase saturates at $\sim75\%$ of the
injected mass.

\begin{figure}
\vskip 0.4cm
\centering
\vbox{
\includegraphics[width=1.0\columnwidth]{image02.eps}}
\caption{Fraction of mass absorption (circle-black), outflows (triangle-red) and the ratio of outflowing
matter to that of absorption (square-green) through the inner boundary with time are shown. Injected
halo rate ($\dot{m}_h$) is kept fixed at $0.1$.}
\end{figure}

First simulation of this kind was performed by MLC94 followed by Molteni, Ryu \& Chakrabarti 1996 (MRC96), Giri \&
Chakrabarti 2012, 2013 (GC12, GC13). The outflows are generated out of
inflowing sub-Keplerian matter forming a shock due to centrifugal barrier.
The oscillation of the shock front after attaining a steady state and the consequence
of that on light curves are well studied in MLC94 and Giri et al. (2010) and Garain et al. (2013).
This formation of shock induces a temperature rise in the post-shock region which acts
as the base of the outflows or Jets. Due to the increase of temperature in the post shock
region, force due to gradient of pressure pushes matter outward along the vertical
direction. This creates the outflows. In HD simulations, this is not well collimated.
One may require magnetic effects for collimation (Chakrabarti, 2013).
To show details, we have shown the post-shock region only. The
sub-Keplerian flow of the pre-shock region has much lower density and optical depth as
compared to the post-shock region (GC13). Maximum number of scatterings occur in the
post-shock region and for an observer trying to capture the image of an accretion disk
in presence of the outflows, the last scattering surface of the CENBOL will appear as
the shape of the Compton cloud.

\subsection{Keplerian Disk Acting as the Soft Photon Source}

In order not to include a time dependence in the Keplerian disk, we put it on the equatorial plane, whose
purpose is to supply soft photons as per Page \& Thorne (1974) prescription. We employ the Monte-Carlo simulations
to compute the resulting spectrum which includes the original source photons from this Keplerian disk as well as those
scattered from the CENBOL and the outflows. The Keplerian disk is truncated at the inner edge at the CENBOL surface
and the outer edge is extended up to $100~r_g$ for simulation purpose.

\begin{equation}
\begin{aligned}
F(r) =
\frac{F_c(\dot{m}_d)}{(r-3/2)r^{5/2}}  \\
\times \bigg[\sqrt{r}-\sqrt{3/2}+
\frac{\sqrt{3/2}}{2}log\bigg(\frac{(\sqrt{r}+\sqrt{3/2})(\sqrt{3}-\sqrt{3/2})}
{(\sqrt{r}-\sqrt{3/2})(\sqrt{3}+\sqrt{3/2})}\bigg)\bigg]\\
 \\ and \\
T(r)= \bigg(\frac{F(r)}{\sigma}\bigg)^{1/4}
\end{aligned}
\end{equation}
where, $F_c(\dot{m}_d)=\frac{3m\dot{m}_d}{8\pi r_{g}^3}$, $\dot{m}_d$ is
the Keplerian disk accretion rate in Eddington unit, $\sigma=\frac{2\pi^5k_{B}^4}{15h^3c^3}$
is the Stefan-Boltzmann constant.

Photon flux emitted from the Keplerian disk surface of radius  $r$ to $r+\delta r$ is written as,
\begin{equation}
n_{\gamma}(r)=\bigg[\frac{4\pi}{c^2} \bigg(\frac{k_bT(r)}{h}\bigg)^3 \times \zeta (3)\bigg]~cm^{-2}s^{-1},
\end{equation}
where, $\zeta (3)=\sum^\infty_1{l}^{-3} = 1.202$ is the Riemann zeta function.
So, the rate of photons emitted from the radius $r$ to $r+\delta r$ is given by,
\begin{equation}
dN(r) = 4\pi r\delta rn_{\gamma}(r),
\end{equation}
where the Keplerian disk height $H(r)$ is considered as $0.1$
(since $\frac{H(r)}{r} << 1$ for Keplerian disk region).

The disk is divided into several annuli of radial width $D(r) = 0.1$  and of mean
temperature $T(r)$. The exact number of photons come to be around $\sim 10^{39}$ --$10^{40}$ per
second for a disk rate of $\dot{m}_d=0.1$. With increasing disk rate this number increases
rapidly. Using a weightage factor $f_W=\frac{dN(r)}{N_{comp(r)}}$ where $N_{comp}(r) = 10^9$,
we bundle these photons to save computational time.

Soft photon energy is calculated using Planck distribution law for $T(r)$.
Photon number density ($n_\gamma(E)$) which corresponds to an energy $E$ is given by,
\begin{equation}
n_\gamma(E) = \frac{1}{2 \zeta(3)} b^{3} E^{2}(e^{bE} -1 )^{-1}.
\end{equation}
The process is similar to the earlier works presented by Ghosh, Chakrabarti \&
Laurent (2009); Chatterjee, Chakrabarti \& Ghosh (2017a, 2017b).

\section{Monte-Carlo Simulation of Comptonization}

In Monte-Carlo process, the photons inside the CENBOL region are assumed to follow straight line trajectories
in between two scatterings. This enhances the Computational efficiency without sacrificing science. This has been pointed out by
Laurent \& Titarchuk (1999). The Keplerian disk emits seed photons with six random number associated
with position and velocity. In reality, the Keplerian disk should have the maximum flux along
Z-axis and minimum along the equatorial plane. This has been implemented by assuming
$F_{\nu}=\int I_{\nu}\mathrm{cos}\theta d\Omega$. Inside the CENBOL region,
a critical optical depth ($\tau_c$) is set up using random number corresponding to each
scattering. The next scattering would occur if the optical depth of a particular photon crosses $\tau_c$.

We choose Klein-Nishina scattering cross section $\sigma$ which is given by:
\begin{equation}
\sigma = \frac{2\pi r_{e}^{2}}{x}\left[ \left( 1 - \frac{4}{x} - \frac{8}{x^2} \right)
ln\left( 1 + x \right) + \frac{1}{2} + \frac{8}{x} - \frac{1}{2\left( 1 + x \right)^2} \right],
\end{equation}
where, $x$ is given by,
\begin{equation}
x = \frac{2E}{m c^2} \gamma \left(1 - \mu \frac{v}{c} \right),
\end{equation}
$r_{e} = e^2/mc^2$ is the classical electron radius and $m$ is the mass of the electron. This yields
Thomson scattering cross section ($\sigma_{T}$) in low frequencies and Compton scattering cross
section ($\sigma_{C}$) in higher frequencies like X-rays and $\gamma$-Rays. Between each pair of
scatterings, the gravitational red-shift modifies the energy of the photon. This process
continues until it leaves the CENBOL region or get sucked by the black hole. The process
is similar to that presented in GCL09; Ghosh, Garain, Chakrabarti, Laurent, 2010; Ghosh, Garain,
Giri, Chakrabarti, 2011 (hereafter GGGC11); CCG17a, CCG17b.

\begin{figure}
\vskip 0.7cm
\centering
\vbox{
\includegraphics[width=1.0\columnwidth]{image03.eps}}
\caption{Spectra obtained after Comptonization. (a) The spectra at $t=14.25s$ (Black-Solid),
$t=14.45s$ (Red-Dotted) and $t=14.75s$ (Green-Dot-Dashed)~and~ injected (Blue-Dot-Dash-Dash) spectrum.
(b) Injected spectrum (Black-Solid), composite spectrum (Red-Dashed), Reflected Spectrum
(Blue-Dot-Dash-Dash), Outflow spectrum (Green-Dot-Dashed). (c) Inclination dependence
of reflected spectra. The inclination bins are $0^{\circ}-20^{\circ}$ (Black-Solid), $40^{\circ}-60^{\circ}$
(Red-Dotted), $70^{\circ}-90^{\circ}$ (Green-Dot-Dashed). (d) Outflow spectra at $t=14.25s$
(Black-Solid), $t=14.45s$ (Red-Dotted) and  $t=14.75s$ (Green-Dot-Dashed). Note that the outflow spectra
changed significantly due to the increase in the outflow rate.
Disk accretion rate $\dot{m}_d=0.1$ is kept fixed throughout the simulations.}
\end{figure}

After Comptonization, the spectra at various times are presented in Fig. 3.
Fig. 3a shows the Comptonized spectra of TCAF at $t=14.25s$, $t=14.45s$~and~$t=14.75s$.
The temporal variation in the thermodynamic variables of TCAF has been shown
in Fig. 1. In the absence of cooling, the Compton cloud remains hot.
Thus, the variations in spectra are very small. The Blue-dot-dot-dashed curve
in Fig. 3a represents the injected spectra. In (b), various components such as the net spectrum (red-dashed),
injected spectrum (solid-black), reflected spectrum  caused by rescattering of Comptonized radiation by the Keplerian
disk before it reaches the observer (blue-dot-dot-dashed) and outflow
spectrum (green-dot-dashed) are shown at $t=14.45s$. It can be clearly seen
from Fig. 3b that the reflected spectrum contributes more to the net spectrum than
the outflows spectrum. Fig. 3c shows the reflected spectrum at three inclinations
($0^\circ-22.5^\circ$ (black-solid), $45^\circ-67.5^\circ$ (red-dashed) and $67.5^\circ-
90^\circ$ (green-dot-dashed)) at time $t=14.45s$. The hard energy contribution in
reflected spectra increases with inclination angles while the soft energy contribution
decreases. This is an expected result for the reflected component as the reflection dominates
at high inclinations. With the
increase of the outflow rate, the spectral contribution of
the outflow also increases. In Fig. 3d, the outflow spectra have been plotted for
$t=14.25s$~(black-solid), $t=14.45s$~(red-dotted) and~$t=14.75s$~(green-dot-dashed).

\subsection{Cooling Process}
During Comptonization, the photons either gain or lose energy. In the context of accretion physics,
the electrons in the CENBOL region is at much higher temperature than that of the photons coming from a Keplerian disk.
So, mostly inverse Compton scattering dominates and the signature of that is prominent in the
emergent spectra. We supply a steady state hydrodynamical configuration obtained from TVD code
where the density and temperature of the cloud is defined in each grid. After the scattering,
the electron from a particular grid may loose or gain $\Delta E$ amount of energy which is
transferred to the photon via Compton mechanism. In a particular state, after all the
scatterings by the injected photons, the energy of the entire grid is modified to generate a new
hydrodynamical state where the lose or gain of energy from each grid has been accounted. By this
process the final temperature of the cloud steadily decreases. The final temperature of the
electron cloud in a particular grid is expressed as,
\begin{equation}
k_BT_{new}(ir,iz) = k_BT_{old}(ir,iz) - \frac{\Delta E}{3dN_e(ir,iz)},
\end{equation}
where $T_{new}$ and $T_{old}$ are updated and old temperature of electron cloud. $dN_e(ir,iz)$ is
the number density of the electron in a particular grid denoted by $ir$ and $iz$ and $k_B$ is
the Boltzmann constant. Details of this process of cooling is earlier presented in Ghosh, Garain,
Giri \& Chakrabarti 2011 (GGGC11); Garain, Ghosh \& Chakrabarti 2012 (GGC12) and Garain, Ghosh
\& Chakrabarti 2014 (GGC14).

\begin{figure}
\centering
\vbox{
\includegraphics[width=1.0\columnwidth]{image04.eps}}
\caption{(a-c) Electron number density (in per $cm^3$, upper panel), and (b-d) temperature (in the units of keV,
lower panel) distribution in the post-shock region at $t=14.25s$. Compton cooling collapses the post-shock
region (a,c): initial stage of cooling, (b,d): after the cooling process is completed. The shock moves
inward due to loss of post-shock pressure. Disk rates $\dot{m}_d=0.1$ and $\dot{m}_h=0.1$ are kept constant
throughout.}
\end{figure}

In Fig. 4, we see that the shock location moves inward as the Compton cooling
starts to affect the post-shock region. Panels (a) and (d) show the CENBOL region
which has almost the same electron density and temperature as Fig. 1 (a). We have
considered this particular data file to see the effect of Compton cooling. Fig 4(a) is presented
when cooling just started to work. Then, after a few iterations cooling starts to reduce the
CENBOL size. Spectra softens as the size of hotter Compton cloud becomes smaller. Finally, the
Compton cloud reduces more which makes the accretion disk spectra to be in soft state.
The corresponding spectra of Panel (b) and (d) suggest the CENBOL region is
so small that a very few numbers of soft photons are intercepted by the cloud. Thus, the spectrum
softens and spectral slope increases. The effect of cooling on the outflows are
also visible from Fig. 4. With the inclusion of cooling, the amount of matter outflow rate
($R_{\dot{m}}$) reduces drastically.

\begin{figure}
\vskip 0.7cm
\centering
\vbox{
\includegraphics[width=1.0\columnwidth]{image05.eps}}
\caption{Variation of spectrum due to Compton cooling. Panel (a) corresponds
to the injected soft spectrum where solid-black is the same spectrum as injected
to the without cooling cases. Dotted-red corresponds to the injected spectra at final
stage (Fig. 4b,d). The corresponding emergent Comptonized spectra are presented
in Panel (b) where solid-black (same as Fig. 3) and dotted-red (for CENBOL represented
in Fig. 4b,d) curves showing the spectral softening due to Compton cooling.}
\end{figure}

Fig. 6 represents the outflows spectra for two different CENBOLs. Black-solid one is same as
the spectra presented for $t=14.25s$ in Fig. 3d. This is the input TVD file on which Compton
cooling started to act. The CENBOL reduces the its size due to cooling. And outflows component
vanishes with cooling. The outflow spectra shrinks more and more and the it softens. Basically, all
photons in the outflows spectra for the to particular case comes from the base of the jet which is
CENBOL itself.  In this paper, our goal is to show the variation of images and spectra when
cooling is included. A very detailed study of the effect of cooling on outflows has already
been reported in GGC12.

\begin{figure}
\centering
\vbox{
\includegraphics[width=1.0\columnwidth]{image06.eps}}
\caption{Emergent outflow spectra for corresponding density and temperature
distribution shown in Fig. 4. Black-Solid curve shows the outflows spectrum
directly from the output of the TVD code (same as the black curve shown in
Fig. 3d). Red-dashed represents outflow spectra of the TCAF after final
stage of cooling.
}
\end{figure}

\section{Ray-Tracing Process}
In Schwarzschild geometry, the non vanishing components Christoffel symbol yield geodesic
equations from the field equation,
\noindent
\begin{equation}
\frac{d^2x^{\mu}}{dp^2}+ {\Gamma}_{\nu\lambda}^{\mu}\frac{dx^{\nu}}{dp}\frac{dx^{\lambda}}{dp} = 0,
\end{equation}
where ${\mu} = [0,1,2,3]$; $x^{0} = t$, $x^{1} = r$, $x^{2} = \theta$ and $x^{3} = \phi$,
$p$ is the Affine parameter. The four coupled, second order differential equations for photons
can be reduced to three using energy $P_t=E=(1-\frac{1}{r})\frac{dt}{dp}$ and
angular momentum $P_{\phi}=L=r^{2}\mathrm{sin}^{2}\theta\frac{d\phi}{dp}$ definitions
(Chandrasekhar, 1985). So, three geodesic equations which dictate the trajectory of photons
can be written as
\begin{equation}
\begin{aligned}
\frac{d^2r}{dt^2} + \frac{3}{2r(r-1)}\bigg(\frac{dr}{dt}\bigg)^2 - \\ (r-1)\bigg(\frac{d\theta}{dt}\bigg)^2 -
 (r-1)r\mathrm{sin}^2{\theta}\bigg(\frac{d\phi}{dt}\bigg)^2
+ \frac{r-1}{2r^3} = 0,\\
\frac{d^2\theta}{dt^2} + \frac{2r-3}{r(r-1)}\bigg(\frac{d\theta}{dt}\bigg)\bigg(\frac{dr}{dt}\bigg)
- \mathrm{sin}{\theta}\mathrm{cos}{\theta}\bigg(\frac{d\phi}{dt}\bigg)^2 = 0 ~\mathrm{and}\\
\frac{d^2\phi}{dt^2} +\frac{2r-3}{r(r-1)}\bigg(\frac{d\theta}{dt}\bigg)\bigg(\frac{dr}{dt}\bigg)
 + 2\mathrm{cot}{\theta}\bigg(\frac{d\theta}{dt}\bigg)\bigg(\frac{d\phi}{dt}\bigg) = 0.
\end{aligned}
\label{eq:xdef}
\end{equation}

Velocity components are derived using Tetrad formalism (Park 2006) and are given by,
\begin{equation}
\begin{aligned}
v^{\hat{r}}=\frac{d\hat{r}}{dt}=\frac{r}{(r-1)}\frac{dr}{dt},
~v^{\hat{\theta}}=\frac{d\hat{\theta}}{dt}=\frac{r\sqrt{r}}{\sqrt{(r-1)}}\frac{d\theta}{dt}\\
\mathrm{and} ~
v^{\hat{\phi}}=\frac{d\hat{\phi}}{dt}=\frac{r\sqrt{r}\mathrm{sin}{\theta}}{\sqrt{(r-1)}}\frac{d\theta}{dt}.
\end{aligned}
\label{eq:xdef}
\end{equation}

The redshift factor added to connect the source and the observer frame is given by the relation
\begin{equation}
1+z= \frac{E_{em}}{E_{obs}}=\frac{(P_{\alpha}u^{\alpha})^{em}}{(P_{\alpha}u^{\alpha})^{obs}},
\end{equation}
where, $E_{em}$ and $E_{obs}$ are the energy of emitted and observed photons respectively.
The observed and emitted fluxes are related via the fourth power of redshift factor
\begin{equation}
F_{k}^{obs}= \frac{F_{k}^{disk}}{(1+z)^4}.
\end{equation}
This relationship between the observed flux and the observed temperature can be expressed as,
\begin{equation}
T_{k}^{obs} = \bigg(\frac{F_{k}^{obs}}{\sigma}\bigg)^{1/4}.
\end{equation}
Doppler boosting is added during the emitter-observer frame transformation.
The Ray-Tracing process and formation of images are done in the same way as
as reported earlier in CCG17a, CCG17b.

\section{Results}

\subsection{Time Dependent Images without Cooling}
The static images of TCAF in presence of Comptonization were presented in CCG17a. The Compton
cloud was modelled using natural angular momentum description of General Relativistic thick disks given by
Chakrabarti (1985a). The variations of images and spectra were presented for various inclination angles and
disk accretion rates. They show that due to steep variation of density and temperature inside the CENBOL,
the image does not have sharp edges. On the top of that, for an increasing optical depth of the CENBOL region, the photons from
the Keplerian disk region located opposite to the observer are blocked. In the present case, where TVD code
was used to create the CENBOL and the outflow self-consistently, the optical depth of the CENBOL medium allows
a fraction of photons from the Keplerian disk to pass through the Compton cloud without getting scattered.
This can be seen in each panels presented in Fig. 7 \& Fig. 8.

\begin{figure}
\centering
\vbox{
\includegraphics[width=1.00\columnwidth]{image07.eps}}
\caption{Images of TCAF (in $log(T_{obs})$ scale) seen from an inclination angle of $70^\circ$
in presence of outflows at time $t=14.25s$ ~and~$t=14.75s$. Colorbar is in the range
$10^{6.0}-10^{6.5}$ Kelvin.}
\end{figure}

Figure 7 is drawn at (a) $t=14.25s$~and~ (b) $t=14.75s$. In panel (a), the amount of outflow is much less as
compared to the panel (b). The photons emitted by the base of the lower jet are mostly blocked by the optically
thick Keplerian disk. In Fig. 7a, a very low number of photons is visible from the lower
jet. Due to reflection symmetry of the outflows, these photons are also visible in the upper part of
the outflows. However, due to Lorentz boosting in the upper jet, its observed temperature
is enhanced and it is overall brighter. The sonic surface of the outflow is the cap-like curved
bright surface. The flow is subsonic and hotter below this surface.
We include the photons in this plot which are emitted from the regions with optical depth
greater than unity. This creates a special shape for the base of the outflow.

\begin{figure*}
\centering
\vbox{
\includegraphics[width=2.0\columnwidth]{image08.eps}}
\caption{Images of TCAF (in $log(T_{obs})$ scale) in presence of outflows at $t=14.25s$,
$t=14.35s$, $t=14.45s$, $t=14.55s$, $t=14.65s$~and~$t=14.75s$. Colorbar is in the range $10^{6.0}-
10^{6.5}$ Kelvin and inclination of the observer is at $80^\circ$. Asymmetry in the shape
is due to difference in Doppler shifts in upper and lower jet components.}
\end{figure*}

Figure 8 shows the dynamical evolution of outflows at $t=14.25s$, $t=14.35s$, $t=14.45s$,
$t=14.55s$, $t=14.65s$~and~$t=14.75s$. The mass outflow increases with time in this case. The images
with gravitationally bent rays have been drawn from the perspective of an observer placed at an
inclination angle of $80^\circ$. The asymmetry of outflows become prominent in this Figure also. The
energy range is chosen in such a way that the observer temperature variation of the Keplerian
disk can be found easily.

\begin{figure}
\centering
\vbox{
\includegraphics[width=1.0\columnwidth]{image09.eps}}
\caption{Grid averaged images of TCAF (in $log(T_{obs})$ scale) in presence of outflows at time $t=14.65s$.
Colorbar is in the range $10^{5.4}-10^{6.7}$ Kelvin for panel (a) and $10^{6.7}-10^{10.3}$ Kelvin for panel
(b). The observer is placed at $70^\circ$. For higher energy range detectors, the Keplerian disk and
upper part of jet becomes completely invisible to an observer.}
\end{figure}

Figure 9 shows energy dependent images of TCAF. With a higher energy detector which
works best in the energy range of $1.0-100$ keV, the Keplerian disk might not be seen for disk
rates lower than $0.1$. With increasing $\dot{m}_d$, the disk may reappear. So, for
an outbursting source, whose accretion rates change on a daily basis, the images will change for
any particular energy range of detector. These pictorial changes will be due to the physical
variations of accretion disk geometry which will be triggered by the thermodynamical properties
(see, CT95 for details) of the disk.

In Panel (b), we see the top part of the outflows is also missing in
a high energy observation. This is due to the velocity profile of the outflowing electrons.
Most of the photons suffer downscattering during their collision in the outflowing electrons.
In Panel 3d, we see that the Jet spectra extends upto $1000$ keV. But, in reality,
in our model of non-magnetic jets, maximum hard photons in the Jet spectra are contributed
only from the base of the jet. The photons that are coming from below the equatorial plane are mostly
reflected or absorbed by optically thick Keplerian
disk. So, up to $70^\circ$, visibility of the base of a lower jet is screened by the Keplerian
disk itself. But, at $80^\circ$, as in Fig. 8, both sides become visible to the
observer.

\subsection{Observed Spectra}
The source spectrum  as presented in the Fig. 3a has a peak
at $0.6$ keV. This has been modified due to photon bending and shifted to a lower value for
an observer at higher inclination angle. In the observed spectrum of Keplerian disk has a
peak at $0.3$ keV for $80^\circ$ inclination angle (Fig. 10). The
corresponding characteristic temperature ranges from $10^{6.0}-10^{6.6}$ Kelvin and this
is visible in Fig. 9a for $70^\circ$. The observed spectral variation of the black body
part with an inclination angle remains almost the same as reported in CCG17a.

\begin{figure}
\centering
\vbox{
\includegraphics[width=0.8\columnwidth]{image10.eps}}
\caption{Observed spectra of TCAF seen from inclination angles $10^\circ$, $50^\circ$
and $80^\circ$ in presence of Outflows. Increase in the hard photon contribution with inclination
angle is visible. However, with the inclusion of outflows, the spectral slope increases with
increasing the inclination angle.}
\end{figure}

From Fig. 10, we see that the contribution of hard photons increases with inclination
angle. But, the spectral slope is less for low inclination angle. This is to be contrasted
with our earlier studies (see CCG17a) where the outflow component has not been added.
Without the outflows, the hard photons in powerlaw component increases and the slope
of the spectrum decreases with increasing inclination angle. With the inclusion of
outflows, the spectral slope increases with increasing inclination angle. But, the
contribution of hard photons increases  more significantly when the observer moves to
a higher inclination angle.

\subsection{Images with Cooling}
To demonstrate the effects of Compton cooling, we consider first  the
data file from hydrodynamic simulations at $t=14.25s$. The electron number density and
temperature profile of the post-shock region after Compton cooling is presented
in Fig. 4. Corresponding spectrum in Fig. 5 shows the spectral softening due
to cooling. From Fig. 11, we see that the size of the CENBOL region is
substantially reduced due to cooling effect and the optical depth of CENBOL
region is so low that very few soft photons from Keplerian disk are intercepted
in the Compton cloud. This is the reason of spectral softening. With the inclusion of
Compton cooling the outflow drastically reduces its size. This effect can also be visible
in the images of TCAF. As the CENBOL size is reduced, the inner edge of the truncated Keplerian
disk moves radially inwards.

\begin{figure}
\centering
\vbox{
\includegraphics[width=0.45\columnwidth]{image11a.eps}
\includegraphics[width=0.45\columnwidth]{image11b.eps}}
\caption{Images of TCAF (in $log(T_{obs})$ scale) as seen from the inclination angle of $50^\circ$,
$70^\circ$ in presence of Compton cooling. Colorbar is in the range $10^{5.6}-10^{6.6}$ K. If the
outflows are absent, dark central region of black hole just starts to appear to an observer at $50^\circ$ and
becomes clearer if the onlooker moves to a lower inclination angle.}
\end{figure}

\vskip 0.5cm

\subsection{Realistic Observed Image with a finite beamwidth}

Figure 12, panel (a) shows a convolved image of a Keplerian disk with the inner edge
at $3$ and outer edge at $50$. Convolution is over a beam width of (a) $\sim 20 r_g$
and (d) $\sim 5 r_g$.  Corresponding spectrum for this image gives a pure soft spectrum
(see CT95 and SS73 for further details).
The intensity variation due to the disk and the black hole can be seen. In Panels (b,e),
the images show an accretion disk with
CENBOL (same as Fig. 9(i) of CCG17a).
 In this case, the spectrum is hard and the CENBOL surface completely screens the inner
region close to the black hole. This case was studied in CCG17a. In Panel (c,f)
outflows are strong as in an intermediate states and the convolutions show complex
structure. If the inclination angle is very low, then possibly the black hole horizon
could be seen, but in the present case of high inclination angle, the identification of
horizon would be difficult, especially if integrated over time. The images we just presented are
relevant for our galactic center under a sudden high mass inflow induced by
tidal disruption. Various measurements (Markoff et al. 2007 and
references therein) suggested that the jet from the Sgr A* is around $75^\circ$ away
from our line of sight. Assuming this is along the perpendicular direction  with respect to the accretion plane, and
assuming radio intensity roughly tracks the disk/jet as discussed above, the Galactic centre
should also show images similar to the panels Fig. 12(a-f).
Our conclusion is that we may not be able to discern the horizon itself, but some
features as in our Fig. 12(a-f) should be visible. Similarly the presence and absence of accretion disk
with change in accretion rates should be seen.

\begin{figure*}
\centering
\vbox{
\includegraphics[width=2.0\columnwidth]{image12.eps}}
\caption{Convolved images of TCAF at different states. 2D Gaussian distribution is
considered for convolution with spreading diameter (hypothetical beam width of the instrument)
of $20~r_g$ (for upper panel) and $5~r_g$ for lower
panel. Panels (a,d) are for a pure Keplerian disk (hard state with weak outflow) with outer edge
at $50~r_g$. Panels (b,e) show
images of TCAF without outflows with outer edge at $50~r_g$ (Soft state). Panels (c,f) depict images
of TCAF with outflows having outer edges up to $100~r_g$. Inclination angle is $80^\circ$ for all
panels. Intensity variation close to the black hole could be seen only when the beam width is around
$5~r_g$.}
\end{figure*}

The convolved images presented in Fig. 12 suggest a low spatial resolution of about $5~r_g$
will be able to distinguish features in the hole-disk system, unless the object has a very low
inclination. Integrated counts from the central region is plotted in Fig. 13b for the Keplerian disk only.
A spatial resolution of $5~r_g$ shows double-peaked curve in just resolved condition. Figure 13a shows
unresolved count distribution when $20 r_g$ is used instead. Considering the possibilities
of high mass inflow onto Sgr A*, in its flaring state, we expect an X-Ray image similar
to Fig. 8 which is difficult to resolve at a high inclination. Thus,
probing inner region to capture the event horizon can be difficult in this state. Future projects
which aim at capturing the image of an event horizon will not be able detect the difference in the intensity
of disk to that of the hole unless the object is in the soft state. Otherwise, only
low inclination disks would show the even horizon in any spectral states, even in presence of
outflows. Of course, this conclusion is valid only if the radio emission roughly tracks the inflow-outflow features as
observed in our numerical simulations.

\begin{figure}
\centering
\vbox{
\includegraphics[width=1.00\columnwidth]{image13.eps}}
\caption{Difference in counts from central region received by detectors with spatial resolution of
$20~r_g$ (curve (a)) and of $5~r_g$ (curve (b)). This is case is for a pure Keplerian disk
presented in Fig. 12(a,d).}
\end{figure}
\vskip 0.5cm

\section{Discussions and Conclusion}
Recent study of the effects of the photon bending on standard and two component
accretion disk spectra and images was made by CCG17a. Earlier, static images of
Two component advective flows were presented where we discussed how the Keplerian
disk (valid for soft states only) and the two component disks with its intrinsic
Compton cloud at the inner edge would look like from various angles. However, a
realistic advective flow  will be time dependent and also will have outflows as
the outflow and inflow solutions are always treated with a common footing (Chakrabarti,
1989). This outflow must come out from the post-shock region or CENBOL which behaves
as the Compton cloud around a black hole or a neutron star. This has also been
shown by numerical simulations through numerous works referred to in the earlier
Sections. The outflow could be time varying and the image of the disk would, in
general, vary with time.

In the present paper, we have employed numerical simulations of hydrodynamic process to
generate time dependent accretion disk configurations. At every time step, Monte-Carlo
simulation was done to compute the effects of Comptonization and to obtain the spectrum.
We produced images of the CENBOL with the jet as well as the composite spectra
when the effects of cooling due to Comptonization was turned off or turned on. We
find that with cooling effects the CENBOL collapses to a smaller size and the outflow
is also reduced as in a soft state. In presence of outflows, we draw images of an accretion
disk where the Compton cloud or CENBOL is showing temporal variation of its physical
shape and internal properties. With these, the images depict the outflows which are
self-consistently produced from the inflowing matter. We showed the combined effects
of the disk and the jet and particularly how they would look like in different
X-ray energies. Doppler shift was seen to break the symmetry as expected, but
the photon bending made it even more asymmetric.

Though our simulations are carried out in regions which emit X-rays, and this
will remain true for higher mass black holes also, but the efforts are on to
observe the event horizon in radio waves which have higher spatial resolutions.
On the other hand, both the radio and the Comptonization track the high energy
electron distribution. So we believe that our simulations will have relevance for
radio observations as well. However, intensity of synchrotron photon in
radio band depends on the magnetic field strength and are expected to be primarily originated
from the post shock region. Thus, our X-ray images without the cooler
Keplerian disk, can be treated as radio images. We showed, using two different spatial resolutions,
that one requires a resolution of $\sim 5 r_g$ in order to separate distinct features
in disk-jet systems when high inclination objects are observed, unless the object
is in a soft state and only has the Keplerian disk. However, the obscuration of the
central region is not done when viewed at low inclination angle and the event horizon
should be observable at any spectral state if the beam width is low enough.
The images are of particular interest where the mass accretion rate onto central
engine is high enough, such as RL Quasars, Seyfert 1 galaxies. The current
findings would hold for LLAGNs, like Sgr A*, for high mass inflow induced by tidal
disruptions. Considering the future possibilities of observing such Galactic black holes and SMBHs, we
present an example of a high inclination system, to impress how the inclination
basically removes the chances of observing the horizon, especially, when the
jets are active. In the absence of jets and outflows, however, the horizon can be
discerned. This result will be of importance for future missions which could exclude
high inclination Seyfert 2 AGNs and GBHs such as GRS 1915+105, H 1743-322, GRO 1655-40.

In the spectral study using Monte Carlo simulations, we see effects of
photon bending in the multi-color soft photon component. The peak was seen at a lower
energy due to redshifts at an inclination of $70^{\circ}$. We also find that the
spectra harden at higher inclination angles. Of course, a major result, though
expected, in our simulation is that when the cooling is included, the CENBOL itself shrinks
and consequently the spectra become softer. Further simulations including the effects
of synchrotron radiation, Compton cooling and viscosity are being carried
out and will be reported elsewhere.

\section{Acknowledgements}
This research was possible in part due to a grant from Ministry of Earth Sciences
with Indian Centre for Space Physics.

redpajama_set_name: RedPajamaArXiv


text:
Mr. Ranchu – Goldfish Care
All About Goldfish
Golfish History
Goldfish Varieties
Goldfish Nutrition
Goldfish illness and Treatment
Carp pox
Cotton Mouth
Fin Rot
Hole in the Head
Ich a.k.a White Spot
Lice & Worms
Pop Eye
Swim Bladder Disease
All about goldfish care & facts
GoldFish History
2016-04-25 Mr. Ranchu Comments 0 Comment
Goldfish was one of the earliest fish to be domesticated, and it's one of the most common kept aquarium fish. It was domesticated in China more than a thousand years ago, and several distinct breeds have since been developed. Goldfish breeds vary greatly in size, body shape, fin configuration and colouration (various combinations of white, yellow, orange, red, brown, and black are known).
Goldfish is a member of Carp family. Some of these normally gray or silver species have a tendency to produce red, orange or yellow colour mutations; this was first recorded during the Jin Dynasty ( Ancient China).
During the Tang Dynasty, it was popular to raise carp in ornamental ponds and water garden . A natural genetic mutation produced gold (actually yellowish orange) rather than silver colouration.
By the Song Dynasty, the domestication of goldfish was firmly established. In 1162, the empress of the Song dynasty ordered the construction of a pond to collect the red and gold variety. By this time, people outside the imperial family were forbidden to keep goldfish of the gold (yellow) variety.
The first occurrence of fancy-tailed goldfish was recorded in the Ming dynasty and thy began to raised it indoor. In 1603, Goldfish was introduced to Japan and to Portugal and from there to the other parts of Europe.
During the 1620s, goldfish were highly regarded in southern Europe because of their metallic scales, and symbolised good luck and fortune. It became tradition for married men to give their wives a goldfish on their one-year anniversary, as a symbol for the prosperous years to come.
Goldfish were first introduced to North America around 1850 and quickly became popular in the United States.
All About Goldfish, Golfish History
Goldfish Behavior: Knowing your little pet:)
Goldfish Diet

redpajama_set_name: RedPajamaCommonCrawl


Manix™ 2 Marbled Carbon Fi - Spyderco, Inc.	Page 1173 – Spyderco, Inc.
This limited-edition Exclusive version of the Spyderco Manix™ 2 was specially produced for the Fradon Lock Company and boasts a truly unique combination of features and materials. Its blade is precision machined from CPM® 4V® powder metal tool steel. Specifically developed for applications requiring a superior blend of strength, wear resistance and toughness, CPM 4V is also a product of Crucible® Industries' particle metallurgy process, which ensures a uniform distribution of the steel's alloys and a fine, homogenous microstructure.
To maximize the performance potential of this steel, this knife features a hollow-ground blade that balances a strong spine and a thin terminal edge that will maintain its high-performance edge geometry over years of use and sharpening. The exceptionally keen PlainEdge™ blade has a beautiful satin finish and a fully accessible Trademark Round Hole™ for swift, ambidextrous one-handed opening.
The other remarkable feature of this Manix 2 Exclusive is its handle, which features solid marbled carbon fiber scales. Lightweight and exceptionally strong, this state-of-the-art material is both practical and visually stunning. All other features of this knife are consistent with the best-selling standard version of the Manix 2, including a high-strength Ball-Bearing Lock™ mechanism and a reversible tip-up carry clip.


text:
Don't Eat the Dirt... is an EP by Sky Cries Mary, released in 1990 through Lively Art.

Track listing

Personnel
Musicians
Jon Auer – drums, piano, engineering and mixing on "Spanish Castle Magic"
Alfred Butler – bass guitar on "Hellbound for Heaven" and "Tongues"
Scott Mercado – drums on "Hellbound for Heaven" and "Tongues"
Roderick Wolgamott Romero – vocals
Stephan Byron-Salit – guitar on "Hellbound for Heaven" and "Tongues"
Ken Stringfellow – bass guitar on "Spanish Castle Magic" and
Production and additional personnel
Steve Fisk – engineering and mixing on "Hellbound for Heaven" and "Tongues"
Pascal Magnier – engineering, mixing

References

External links

1990 EPs
Sky Cries Mary albums

redpajama_set_name: RedPajamaWikipedia


That's the community we want to be in.
Although they primarily live in Georgia, Art & Diane love the convenience of Waterset, especially for visiting family in Sarasota. "[Waterset is] close to a big city, close to Sarasota where our family is, yet it seems like a small and nice community to live in….This is a great spot between Sarasota and Tampa," says Diane.
This is a great spot between Sarasota and Tampa.
When you drive into Waterset, you get a feeling of home and of community.
We're excited about being here.
We found the perfect model for us.
Overall, it's clear that although this is Art & Diane's second house, Waterset is a place that truly feels like home.


text:
Travel Soccer Age Groups
Please look at the chart that follows to determine your child's 'soccer age', and as always, if you have questions, see the club explanation of the age chart or contact the registrar.
2018-2019 Soccer Age Group Chart
August 1, 2018 to July 31, 2019 (Soccer Year)
Birth Month\Birth Year
What soccer age group is my kid in?
In 2015 US Soccer adopted rules to determine soccer age groups by birth year. Soon after US Soccer adopted the age changes, New Jersey Youth Soccer followed suit as did the leagues that our club participates in. MUSA promotes all players playing age appropriate. In some situations, players will play up. These situations are the exception the rule and decisions are made on a case by case basis after being reviewed by members of the MUSA board of directors.
Do I have to play in my age group or can I move up or down?
U9(2009) and older age groups
In the U9 and older age groups, players are allowed by NJYS/SJSL rules to play up but in an effort to have a competitive club in all age groups playing up will be the exception rather than the rule. If your son or daughter is unusually large or unusually skilled for his or her age, he or she may be able to "play up". Such decisions are made with the approval of MUSA Travel Directors. We feel that our club is large enough that we offer teams with a variety of skill levels from the most skilled to the new comer at all age groups and there is no need for players to play up. In some situations, players may be asked to play up so as to provide opportunities for more children to play soccer. In all cases, MUSA does its best to place players with similarly skilled players.
Unlike the other age groups, there is a minimum age for U8. U8 teams do not permit players who are younger than U8 to play on them.
Birth Year Trainer
2011 Jeff Stefano
2010 Angelo DiBartolo
2009 PJ Chew
Mike Gibson
Ken Keim
Clay Pierce
2008 Dave Medland
2007 Tim Donnelly
2006 Rick Difilippo
2005 Joe Clark
JP Blanchett
2007 Colleen McGardy
Travel Soccer Links
NJYS Carding


text:
Waterloo, Canada
http://www.opentext.com
OpenText Corporation develops and sells software products aimed at addressing information management requirements, including the management of large volumes of content, compliance with regulatory requirements, and mobile and online experience management. OpenText has grown primarily by acquisition. Some of the product families that are now part of OpenText include Actuate, Artesia, Captaris, Cordys, GXS, Hummingbird, Livelink, Reddot, and Vignette.
Iknow became an OpenText partner in 2009 when OpenText acquired Vignette Corporation.
OpenText Big Data Analytics
https://www.opentext.com/products-and-solutions/products/analytics/opentext-big-...
OpenText Big Data Analytics is a high-performing big data and predictive solution for business analysts. Big Data Analytics is a feature of Analytics Suite that can access, blend, explore and analyze data quickly without depending on IT or data experts. Big Data Analytics combines an analytical columnar database that easily integrates disparate data sources, with built-in statistical techniques for profiling, mapping, clustering, forecasting, creating decision trees, classification and association rules, doing regressions, and correlations. Users can get a 360 degree view of their business, explore billions of records in seconds and apply advanced and predictive analytics techniques all in a drag-and-drop experience, with no complex data modeling or coding required.
OpenText Information Hub
https://www.opentext.com/products-and-solutions/products/analytics/opentext-info...
The OpenText™ Information Hub (iHub) feature of Analytics Suite is a scalable analytics and data visualization platform that enables IT leaders and their teams to design, deploy, and manage secure, interactive web applications, reports, and dashboards fed by multiple data sources. iHub supports high volumes of users, and its integration APIs enable embedded analytic content in any app, displayed on any device.
OpenText Magellan
https://www.opentext.com/products-and-solutions/products/analytics/opentext-mage...
OpenText Magellan is a flexible, artificial intelligence-powered analytics platform that combines open source machine learning with advanced analytics, enterprise-grade business intelligence, and ability to acquire, merge, manage and analyze structured and unstructured big data and content stored in your enterprise information management (EIM) systems. Magellan enables machine-assisted decision making, automation, and business optimization.
OpenText Decisiv
https://www.opentext.com/products-and-solutions/products/discovery/decisiv
OpenText Decisiv is an enterprise search engine that goes beyond keywords to search multiple repositories at once to find key documents, view projects, and identify internal subject-matter experts. Decisiv provides unified concept search across the enterprise.
OpenText EnCase eDiscovery
https://www.opentext.com/products-and-solutions/products/discovery/encase
OpenText EnCase eDiscovery provides 360-degree visibility across all endpoints, devices, and networks to enable discreet, forensically-sound data collection for litigation and investigations. EnCase eDiscovery is the industry gold standard for data collection and preservation.
https://www.opentext.com/products-and-solutions/products/discovery/axcelerate
OpenText Axcelerate is a complete, award-winning platform for legal discovery and investigations with proprietary advanced analytics, world class services and support, and the industry's best predictive coding. With Axcelerate, legal teams can identify and understand the facts that matter for litigation, compliance and governance.
OpenText ECM in the Cloud
https://www.opentext.com/products-and-solutions/products/enterprise-content-mana...
OpenText offers a wide variety of adaptable ECM cloud-based options, from managed services (available for virtually all Content Suite products and solutions) to cloud packaged managed services solutions to SaaS based solutions. Flexible cloud models for public, private, or hybrid deployments enable your organization to manage, protect and, most importantly, effectively use information within the very same governance framework used by the most bulletproof on-premises systems.
OpenText Core
https://www.opentext.com/products-and-solutions/products/opentext-core
OpenText Core is a simple yet secure way for users to share and collaborate on enterprise content in the cloud.
OpenText Snap
https://snap.opentext.com/
OpenText Snap is a lightweight document capture application. Snap has enterprise-grade development, test, production, template, and configuration features.
OpenText Captiva
https://documentum.opentext.com/captiva/
OpenText Captiva Intelligent Enterprise Capture Solutions transform paper from a liability into business advantage by converting your paper, faxes, and other content into application-ready information.
OpenText Documentum xCP
https://documentum.opentext.com/documentum-xcp/
OpenText Documentum xCP is a flexible development platform for automating complex, information-intensive processes to drive better business decisions and get more consistent quality and faster cycle times.
OpenText eDOCS
https://www.opentext.com/products-and-solutions/products/specialty-technologies/...
OpenText™ eDOCS is a light-footprint, cost-effective and highly-flexible enterprise content management (ECM) solution for legal, public sector and professional service organizations. eDOCS ensures sensitive work product is managed and secure throughout the content lifecycle, while remaining easily accessible for day-to-day operations, enabling users to deliver exceptional enterprise content services to their clients.
eDOCS DM is the platform module for the eDOCS Suite and a key component of a wider Enterprise Content Management (ECM) software offering. eDOCS DM supports a wide range of companion solutions for enhanced e-mail management, records management, workflow, business process management, SharePoint integration, mobile access, enterprise search, and much more.
OpenText Brava! for Content Suite
OpenText Brava! for Content Suite allows you to securely view, annotate, and redact virtually any type of file.
OpenText Archive Center
OpenText Archive Center is a highly scalable, multi-tenant archive helping organizations manage the explosion of unstructured data (e.g., e-mail and files) while ensuring it is cost effectively and securely stored in the cloud, on premise, or as a hybrid. End users access data from anywhere—online, offline or mobile—and it's completely stub-free and transparent. Business administration features provides a broad set of archive and retention management capabilities along with system reporting, legal hold and export.
OpenText InfoArchive
https://documentum.opentext.com/infoarchive/
OpenText InfoArchive is a compliant enterprise archiving platform for preserving both structured and unstructured data sources, irrespective of the archive method. InfoArchive allows data and content to be archived, managed in accordance with compliance policies and remain accessible to users.
Retire or decommission any application, recouping costs associated with software, maintenance and infrastructure.
Provide verifiable audit trails and set and enforce retention policies.
Encrypt and mask data selectively to secure privacy and satisfy regulations.
Enable controlled, compliant analytics.
OpenText Enterprise Information Archiving
OpenText™ Enterprise Information Archiving solutions deliver highly scalable, proven solutions for archiving and managing the enterprise information lifecycle for a broad range of structured and unstructured information, including e-mail, files, Microsoft SharePoint data, ERP data (e.g., SAP, Oracle), instant messaging, web and social content—all within one easily managed repository. Coupled with industry-leading records management and auto-classification software, OpenText Archiving solutions support rich capabilities to drive compliant retention and disposition policies. As such, organizations can deploy a defensible, long-term archiving strategy to comply with information governance requirements, meet legal obligations, and reduce the overall costs associated with archiving past-era content.
OpenText Hightail
https://www.hightail.com/
OpenText Hightail streamlines the creative process by easily sharing multimedia content between internal and external teams, collecting precise feedback on visual assets, assigning to-dos, tracking progress, and routing approvals, all in one solution.
OpenText Extended ECM Platform
With OpenText Extended ECM Platform, content is transparently integrated with other leading applications such as SAP S/4HANA, SAP SuccessFactors, Salesforce, Microsoft Office 365, or any other enterprise software. With integrations, the content services platform bridges content silos and business processes to allow information to flow effortlessly across applications. Extended ECM Platform leverages an organization's investment in its enterprise content management software and other applications.
OpenText Tempo Box
OpenText Tempo Box provides secure file sync and share for the enterprise.
OpenText Content Suite Platform
OpenText Content Suite Platform, the foundation for OpenText Enterprise Information Management (EIM) offerings, is a comprehensive enterprise content management (ECM) system designed to manage the flow of information from capture through archiving and disposition. Content Suite Platform ensures agile information governance to address an increasingly complex and dynamic regulatory landscape and the rapid growth of business information. The Content Suite Platform reduces risk while allowing organizations to focus on using information to drive strategic growth and innovation.
OpenText TeamSite
https://www.opentext.com/products-and-solutions/products/customer-experience-man...
OpenText TeamSite is an enterprise web content management system developed by Interwoven. At present, it is owned, maintained, marketed by OpenText, a company that acquired it from Hewlett-Packard on May 1, 2016.
OpenText TeamSite provides a single, easy-to-use web content management (WCM) platform to help you create more personal, visually rich, two-way digital customer experiences – that are optimized for any device, digital channel, or context.
OpenText Web Content Management
OpenText web content management (WCM) solutions are open, flexible, and connected platforms to solve the next generation of digital experience challenges faced by marketers and business managers. OpenText WCM brings together content, process, and applications to create and deliver optimized and personalized multi-channel interactions across the full customer journey, from awareness to purchase to advocacy and recommendation.
OpenText MediaBin
OpenText MediaBin is a digital asset management solution, available on-premise and in the cloud, that helps even the largest organizations with globally distributed teams deliver a more engaging and consistent customer experience by effectively managing, distributing, and publishing thousands of customer-facing digital assets. MediaBin automatically extracts key concepts from audio, video, and image file content, analyzes and categorizes assets, removing the need for hours of reviewing and tagging images with automated meta-tagging and labeling. It recognizes sophisticated traits, such as color, to provide a highly detailed, time-encoded range of searchable data. This intelligence allows you to locate the right asset for your campaign without knowing exact keywords associated with the file, saving time and exposing a more accurate selection of files. Assets can also be viewed in context with other content within the extended enterprise, across social networks and web search.
OpenText Media Management
OpenText Media Management provides a "single source of truth" and consolidated asset repository for marketing, branding, commerce, video and global distribution. It's an integral part of an ecosystem with interconnected and interdependent contributors and production environments (such as agencies, photo, video, audio, graphics, layout) provisioning digital media content for the multi-channel digital supply chain, digital operations, marketing and brand management.
OpenText Digital Asset Management
OpenText™ Digital Asset Management (DAM) solutions serve as the centralized, secure and accessible repository - whether cloud-based or on-premises - to manage digital media, branding and video. OpenText's DAM solutions help people find, share and use digital media assets to deliver beautiful experiences. Scalable for the largest enterprises, their DAM solutions offer capabilities to manage the entire content lifecycle with workflows and features for creative production, collaboration, publishing and distribution of assets.
OpenText AppWorks Platform
https://www.opentext.com/products-and-solutions/products/digital-process-automat...
The OpenText AppWorks Platform provides the foundation for digital businesses. With intelligently automated, content-rich, connected processes that you can quickly build and easily modify, AppWorks gives you the power to deliver a variety of new digital experiences with a much lower IT workload.
Gain the power and flexibility to digitize, automate and unify processes
Automate routine work or optimize knowledge-driven work for better control over your customers' experience
Simplify interactions with structured and unstructured content residing in diverse business systems and content repositories
BPM in the Cloud with AppWorks
OpenText delivers BPM in the Cloud with AppWorks. AppWorks enables enterprises to take their business to the cloud; it helps service providers to differentiate their cloud services and Independent Software Vendors (ISVs) to build next generation Software-as-a-Service (SaaS) applications.
Uses a sophisticated workflow toolset with standard BPMN 2.0 process notation for building document-centric workflows allowing for both structured and ad hoc routing of documents for a variety of approval, review, and feedback processes.
Enables robust, multi-lingual metadata capabilities to address needs of global users.
Provides integrated reporting to retrieve information about content, permissions, attributes, users/groups, workflows, and many other content activities.
OpentText Enterprise Content Management (ECM) Software
OpenText enterprise content management (ECM) software products manage information flows across the organization—from capture through to archiving and disposition. OpenText's ECM software extends the reach of traditional ECM capabilities into previously isolated applications and information silos, such as ERP, CRM, SCM and HCM.
OpenText Documentum Platform
https://documentum.opentext.com/documentum-platform/
OpenText Documentum Platform offers an enterprise content management system with the essential capabilities to control all your information content. Documentum provides a robust, scalable, fault-tolerant, and extensible architecture to manage and control content.
OpenText Content Server
Content Server provides the core set of tools you need to capture, process and manage unstructured content across your organization including document management, workflow, search and information retrieval services, all tightly integrated into a platform that is easily customized and extended.


text:
Q: How to match the unique ids that I created in df1 to df2 based on two column values? I have two dataframes, and I am struggling to match the unique ids that I created in df1 to df2 based on 'name' and 'version' values. I need to add a column to df2, let's call it ['ID'], whose values match with the unique id values in df1. The condition is that both the 'name' and 'version' values in df2 must equal the same 'name' and 'version' in df1 in order to be assigned the correct ID value. DF2 has all the elements of DF1 but they are repeated.
df1 = pd.DataFrame(
    {
        'Unique ID': ['111', '222', '333', '444'],
        'Name': ['A', 'A' ,'B','C'],
        'Version': ['1.1', '1.2', '1.0', '1.1'],
        'x': ['...', '...', '...', '...']
    }
)

DF1
   | UNIQUE ID | NAME | VERSION |  X  |
  1|     111   |   A  |     1.1 | ... |
  2|     222   |   A  |     1.2 | ... |
  3|     333   |   B  |     1.0 | ... |
  4|     444   |   C  |     1.1 | ... |

df2 = pd.DataFrame(
    {
        'Name': ['A', 'A', 'A', 'A', 'B'],
        'Version': [ '1.1' ,'1.1', '1.1', '1.2', '1.0'],
        'x': ['...', '...', '...', '...','...'],
        'x': ['...', '...', '...', '...','...'],
    }
)

DF2
    | NAME | VERSION |  X  | X  |
  1 |  A   |  1.1    | ... |... |
  2 |  A   |  1.1    | ... |... |
  3 |  A   |  1.1    | ... |... |
  4 |  A   |  1.2    | ... |... |
  5 |  B   |  1.0    | ... |... |

Desired Output for DF2:
DF2
    | NAME | VERSION |   ID    | X  |  X |
  1 |  A   |  1.1    |   111   |... | ...|
  2 |  A   |  1.1    |   111   |... | ...|
  3 |  A   |  1.1    |   111   |... | ...|
  4 |  A   |  1.2    |   222   |... | ...|
  5 |  B   |  1.0    |   333   |... | ...|

Attempted code:

df2['ID'] = df1[df1['name' + '_' + 'version'].isin(df2['name' + '_' + 'version'])]['Unique ID'].values

A: A way which is a little bit dirty but works :
df2.merge(df1[['Unique ID','Name','Version']],left_on=['Name','Version'], right_on=['Name','Version'],
suffixes=('_left', '_right'))

redpajama_set_name: RedPajamaStackExchange


A number of cities across the globe are exploring the idea of restricting chain stores from their high streets. Toronto is following in the footsteps of Nantucket, Jersey City and San Francisco to limit the number of chain stores that occupy commercial premises, in a bid to preserve the character of their respective cities. Over here in the UK, there are various planning regulations in place that prohibit retailers from setting up in large retail spaces. As convenient as chain stores are, they lack character and often customer service. If you're shopping for jewellery, you'll be pleased to hear that you can avoid the faceless high street names, and visit your local family-run business – Michael Frank Jewellers.
Based in Wickford, Michael Frank Jewellers was created by a family with a passion for beautiful jewellery. Michael had worked in the family business during his childhood, when his father passed down his knowledge and enthusiasm for both luxury design and jewels. Following a career in the army, Michael returned to the jewellery trade, this time with his wife Amanda, and together they set up Michael Frank Jewellers. What sets the business apart from the rest, is their dedication to creating high-quality pieces of jewellery, that will last a lifetime.
Whether you're looking for an engagement ring, wedding band or just an elegant bespoke piece to give to a loved one, you can find everything you need here. Ladies are well catered for with a choice of stunning bracelets, necklaces, rings and earrings. Those who are fond of a touch of nostalgia, will love the pre-owned collection which is made up of vintage brooches, pendants and much more.
Gentlemen too can indulge in some luxury purchases at this jeweller; as well as rings and bracelets, there are some stylish cufflinks and lapel pins to accessorise any outfit.
If you're looking for a new dream watch, or perhaps just wish to overhaul your existing timepiece, then Michael Frank is your one-stop shop for watch purchases. Luxury is the theme of the range on offer, with many models of Rolex and Cartier available.
If you'd love to afford one of these more expensive purchases, but are struggling to afford the price tag, you've got two options. You can either browse the high-end pre-owned range, or alternatively you can trade in an existing watch to offset the value against your new purchase. To do this, simply fill out a watch valuation form, send in your item which will be inspected by the in-house expert team, and then an offer will be made to you.
The beauty of independent jewellers is that the standard of customer care available is far superior to that you'll experience elsewhere on the high street. If you're in the market for some jewellery, your journey will begin with a completely free consultation, where you can take a look through the existing range or alternatively brainstorm some ideas for a bespoke design. But your relationship with Michael Frank Jewellers doesn't expire as soon as you've paid the bill and received your design. The team also offers comprehensive aftercare which includes having your jewellery cleaned, repaired or valued.
The next time you need to buy or repair some jewellery, why not pop in store at Michael Frank Jewellers at 11 The Broadway, Wickford SS11 7AD, just opposite Aldi?


We are excited to announce that Lion Capital is now a minority investor in Hatch Beauty!
This announcement marks a new and exciting phase allowing us to scale our ability to innovate in the health, wellness and beauty spaces.
A revolutionary hair volumizer from Orlando Pita Play. The formula features advanced polymers and a proprietary 5 protein complex, clinically proven to increase hair lift and hair diameter. The unique formula "recharges" hair volume the next day with the addition of heat.
We keep our fingers on the pulse of what-comes-next. Trend intelligence has always been the backbone of what we do. That is why beauty brands and retailers call on us to advise them through the development of new initiatives. HATCHBEAUTY is able to uniquely identify trends and whitespace opportunities in the beauty space which has translated to some of the industry's most exciting and profitable formulations, products, and brands.
We understand retail and are experts in every channel of distribution. We ensure our brand concepts resonate with the targeted customer with considerations of the retail environment, platform, and programs before we start development.
We believe in order to effectively market a brand, branding and product development must happen hand-in-hand. A singular vision is carried through from concept to formulation. There is magic in the makeup.
We like to complete the circle. We offer best-in-class innovation, product development, and branding coupled with vertically-integrated testing and manufacturing capabilities, all in the United States.
We influence, guide and advise some of the industry's most exciting and disruptive brands from small start ups to the well established, multi-billion dollar companies. Our clients include prestige brands, CPG companies, pharma companies, contract manufacturers, digital direct-to-consumer brands, and many of the country's largest retailers.
Introducing Bliss Ex"glow"sion Triple Oxygen Serum Foundation.
Born from the best-selling Ex"glow"sion Triple Oxygen Cream at the legendary New York City Bliss Spa, this traceless, fluid foundation utilizes innovative ingredients and exclusive oxygen technology to help revitalize skin for a healthy, glowing, youthful appearance.
HATCHBEAUTY truly embodies a full-service company that is knowledgeable from design to manufacturing to distribution. We wanted to work with a company that could relate and speak to all the facets of the industry in order to provide us with the best branding experience and outcome.
They have been instrumental in helping us think through the very large and complex beauty and skin care industry as DSC looks to make its mark there. With them you gain decades of experience, and all the handholding you need to take advantage of it.
HATCHBEAUTY has been unbelievably helpful throughout the development process. They have so many ideas and were able to understand how my vision would succeed at stores.
They helped us with the entire rebranding process, as well as all of our specific packaging choices. Our new look reflects the vision of our brand – we're thrilled with it.
HATCHBEAUTY is an exciting place to be.
Our office is an energetic, collaborative work space that allows people to turn passion and enthusiasm into products that tell stories.
Everyday at HATCHBEAUTY is different. We shift as trends change. We innovate to create diverse and compelling products.
We are a team comprised of amazingly talented people all sharing a single mission…to create brands that matter.


text:
For months I had hunted for something closer to the hub. In the far-reaches of Reservoir, I felt cut-off from the world, forever commuting to break the isolation. The unit in Brunswick was charming: a polished-floor, two-bedroom affair, awash with northerly light. Located at the rear of four cream-brick units, it was quiet. I liked the option of tucking myself away while still being at the centre of things. Being a 'boutique' complex – real-estate jargon for clusters of six or less – the new home I coveted was in high demand.
At auction I just scraped it in (note the ecstatic woman almost peeing her pants as she hugs and kisses total strangers). While you get less for your buck in sunny Brunny, I could no longer ignore the pull to be closer to friends and work.
There is no owner's corporation at Number 24. The agent who handled the sale spruiked this as a massive plus: no annual owner's-corporate fees, no need for consensus every time you fart. Sounded all right to me. I was also thrilled that the occupants of the other units were all women, hoping this might lead to a cosy community.
A few months in, I had settled nicely into my new home, mightily impressed by the solo-mum, Sally, in Unit B, who somehow managed to juggle a full-time midwifery degree yet still had energy to scoop up her two young boys and take them on frequent adventures.
'Hold still, guys,' she'd tell her sons, slip, slop, slapping the sunscreen. She would tug their hats firmly on their heads and set off: to the zoo, the National Gallery, Art Play or the Children's Garden. Having single-handedly raised two kids myself, I am familiar with this no-man's land. In Sally, I recognised a kindred spirit. She was resilient.
Now the problem with having no owner's corporation is that the garden at Number 24 was a shambles. Outside each unit were three feet deep garden-beds, plus a large slab along the front of the property: the spread of soil masquerading as garden – overrun with spider plants, scrappy geraniums, enough succulents to rival a desert scape, a monstrous tree that dropped noxious red berries, and a prunus plum that splattered fruit resembling squashed cockroaches onto the concrete.
I am not one to shirk a challenge. The garden screamed to be taken in hand. I thought the potential was huge. Native trees and shrubs would break the starkness. I have always loved gardens. They help make a place feel like home. But being the new kid, I needed to proceed with caution, try not to ruffle feathers. I have a habit of ruffling feathers.
I did the research. If all four owners agreed, the cost to each of us would be $600, including removal of several trees, a root-digger, weed mats, new flora and garden borders. Thanks to excellent contacts, a bargain.
At a rare meeting of the owners, I presented my plan, along with tea and biscuits. All four owners attended: Soula – the woman from Unit A who never opens her blinds, Hitomi – the officious landlord who rents to Sally, Rebecca – the no-nonsense cop from Unit C, and me.
'The garden is perfectly fine the way it is,' said Hitomi. If she sat up any straighter, I was sure her impeccable suit would snap.
'My sister helped me plant the succulents when I first moved in,' said Soula, seemingly on the verge of tears. I wondered if she was a widow, the way she always dressed in black.
'Julie's just trying to make the garden look nice,' said Rebecca. 'I'm sure we could keep some succulents.' I blessed all the cows in China that I had an ally.
'Of course,' I said. 'They can stay. It just needs more… variety.'
But Hitomi and Soula continued their assault, their volume increasing with every protest.
'In the forty years I have owned Unit B,' screeched Hitomi, 'other than rates and insurances… I have never had to spend a cent.' I didn't doubt it. A quick glance inside her original-condition unit, had already confirmed this.
Neither of my opponents were about to part with a brass razoo. I later Googled Hitomi's address and found that she lives at a property with an enormous garden in Kew. Lucky for some. The other owner, Soula, was simply broke. Fair enough. I get that. Visibly flustered, this woman of indeterminate age – at a guess I'd say late sixties – reeled off the list of repairs she can't afford inside her unit before she even considers the garden.
Here I was on new turf (okay, concrete) making waves again. Visions of forging community while instilling a touch of beauty to our dwellings, smashed like falling cards. It wasn't the first time I'd offended people. Stirred the pot. Or so they say. Like the time I unwittingly insulted an old writing friend: the flippant comment I made at a weekend writing workshop. How it forced her to turn the kaleidoscope lens just a smidge – enough to see me in a different light – one with dark edges. Melbourne's writing community is tight, and this careless moment spurred a knock-on effect. You'd think by now I would have learned to shut my mouth.
'I think it's a great idea,' said Rebecca, lamely, for without an owner's corporation we'd be fools to proceed without full consent.
'Well,' I said, not one to give up an idea lightly, 'what does everyone think about employing an owner's corporation? They'd help us deal with issues like this.'
'It is not necessary,' Hitomi said sharply.
Soula gazed into her lap. I suspected that if Hitomi wasn't being so vehement, we might have had a different outcome.
'I've owned this unit since it wase built,' hissed Hitomi, daggers firing at me. 'We never had an issue like this before you came along.'
And there it was. Another queen wasn't welcome. But it was never my intention to rule the roost. I wanted to bring people together, not fight.
Rebecca dared raise the possibility of replacing the cracked concrete driveway with compressed gravel.
'Why don't we put a pool in while we're at it?' asked Hitomi.
Weeks slid past. A recluse at the best of times, Soula now worked hard to avoid me. I'd be punching out words on my laptop, and then notice her furtively glance outside her door before dashing madly to stuff rubbish in our side bins. I hated that I had upset her – though chances are the origins of her malaise pre-dated my arrival. At night I felt her anger seething through the mortar. It made it difficult to sleep. I have never found it easy being the source of someone's wrath. As a child I had been anxious, terrified by the prospect of stepping out of line.
In a bid to unplug the impasse, Rebecca suggested the two of us split the cost. Bizarrely, even this decision inspired ill-will from the other two.
'What about on-going maintenance?' I heard a hysterical note in Soula's voice. 'Gardeners, weed killer… that sort of thing.'
'We promise the garden won't cost you a thing,' assured Rebecca. 'Not now, not later.' And with that, we proceeded.
Now, I'm not flush. Divorcing young is akin to being stranded at base-camp, leaving miles to catch up. But the garden really mattered to me. I yearned for a space that felt pleasing to come home to – a place I could plant my roots and feel part of something greater. Since my grandmother died and it came to light that she had been adopted, I had a sense of being unmoored; unable to locate our kin, a little weightless. Roots would give me anchor.
Twenty months later the flowering gums in our garden are now as tall as the roof line. Bower wattles, wispy acacias, tee-trees and princess gums, the proteas with their golden orbs, all lush. Wattle birds wake me each morning with their wonderful cock-carock. The bees have come.
There is something lovely about watering, the reward of watching trees grow, the first buds and blossoms – like a few months ago in early spring when I uncurled the hose, looked up and discovered two little green gumnuts, twins sharing a spindly twig. Days later, a cluster of soft pink bristles peeked out, like tiny fairies, or demented cat's whiskers.
Over time, a kind of peace had settled between us ladies at Number 24. Even Soula was on speaking terms with me, conceding that the garden looked great. The block of units had begun to feel like home.
Now, at the rear of each unit is a sliver of land. You do with it what you can, which isn't much. Certainly not enough for Sally's active boys. Between the four units, we possess a total of three small cars, leaving plenty of space in the front concrete carpark for the kids to ride their scooters, chalk train tracks, construct tunnels, or splash in the plastic paddle pool. But it's hot out there.
I have six grandchildren, four of whom are five and under, and they often stay with me overnight. With this in mind as well as Sally's boys, a year ago I started creating a little sitting area on the concrete section where nobody parks. This, of course, with the consent of the other owners (no cost to them), and to the delight of Sally and her boys.
I sourced huge terracotta pots, filled them with black bamboo and yuccas – dragged home wooden bench seats. Soon, this lovely space complimented the new garden, while offsetting the ugliness of concrete. Sally and I often shared meals there, especially when my little ones stayed. We were proud of the festive space we had created, sprouted out of concrete. Our visitors enjoyed lounging with us there, too. And although we had welcomed the other two neighbours to join us – or to use the space at any time – neither had taken up the offer.
But recently the peace I was lulled into believing was the new status quo, banished with the arrival of a lengthy text – surprisingly from Rebecca: I am upset by the mess that has been created with the sitting area. Not least the new sunshade… (The sunshade: my recent bid to beat the radiant heat when the sun blasts the concrete.) I love children, but… and so on.
Sally and I were gutted. We loved this area. Still, I knew it was pointless arguing. There had been enough sleepless nights.
So with great sadness, one recent afternoon Sally and I dismantled the sunshade and drastically culled the communal space. It felt like dispensing with old friends.
I know I would miss our little oasis amid the sea of concrete, miss seeing this space come alive, when Sally's boys would water the potted plants or drive cars in the sandy clam shell. But soon, I will abandon my laptop, brew a coffee, ferry it outside to the newly-culled sitting area. I will listen to the night in our communal space – modified, not swept aside.
War Tales from Sunny Brunny appeared in the Victorian Writer print magazine 2016 Feb/March memoir edition.


text:
Q: Append Anchor tags to span in Jquery I created a span tag and I want to append anchor tags to it
var span = "";
// docs are fetched from Dynamics 365
$(docs).each(function(i, value) {
  var doc = value.Attributes;
  var blob = b64ToBlob(doc.documentbody, doc.mimetype);
  var a = $("");
  a.prop("href", URL.createObjectURL(blob));
  a.prop("download", doc.filename);
  a.prop("target", "_parent");
  a.html(doc.subject);

  $(span).append(a);
});

// render span as " ... "

I want to render the span as a long string since I'm using it inside a datatable.
But nothing gets appended to the span tag. What could be the problem with this piece of code?

A: You can use .attr()
Example:
$("#id").attr("href", URL.createObjectURL(blob));


As most of our reader knows, I really like logo design because this is the creative person's ultimate test. If you are able to deliver the message using a simple static message, then you are good. Good logos are like paintings: you can stare them for hours and you won't get bored, and that's why I always try to find and show the most interesting designs. In this article I have collected 20 superb examples of straight lines used in logo design.


text:
Home > Properties
22 Montpellier Walk, Cheltenham
By Bethany Winter
The property comprises a three storey Grade II* listed period building with a basement. The premises provide a ground floor sales area and ancillary basement accommodation.
Accessed via a separate entrance off Montpellier Street, the first and second floors provide a two-bedroom duplex apartment. Period features are found throughout the property including high ceilings, decorative coving, and sash windows.
EPC: The building is listed and therefore believed to be exempt.
Montpellier is a district of Cheltenham situated at the top of Promenade on the south side of the town centre. Originally developed in the 1830's, it is now known for its bars, cafes, restaurants and a range of specialist shops.
The subject premises is prominently situated on Montpellier Walk with dual frontage to Montpellier Street. Other nearby traders include Neal's Yard Remedies, Tom Howley, Dubarry, Blushes Hair Salon, All Bar One and The Ivy.
The approximate dimensions and Net Internal Areas (NIA) are as follows:
Internal Width: 4.49 m
Shop Depth: 13.73 m
Ground Floor: 52.41 sq m (563 sq ft)
Basement: 36.42 sq m (392 sq ft)
Total: 88.83 sq m (955 sq ft)
There is a two-bedroom apartment over the first and second floors, accessed separately via a door directly from Montpellier Street. Maximum dimensions are as follows:
First Floor Living / Dining Room 9.05 m x 4.34 m
Kitchen 4.48 m x 3.82 m
Second Floor Bedroom 1 8.29 m x 4.51 m with en-suite shower room (no WC)
Bedroom 2 4.55 m x 3.45 m with en-suite bathroom
Separate WC with wash hand basin.
The property currently has two assessments. Ground and Basement Rateable Value: £25,750 Apartment council tax band: B The above information was obtained from the Valuation Office and Council Tax website.
Interested parties should make their own enquiries of the billing authority (Cheltenham Borough Council) to verify the current rates payable.
Guide price £800,000, subject to vacant possession.
VAT may be payable on the price or any other charges or payments detailed.
All figures quoted are exclusive of VAT and intending purchasers must satisfy themselves as to the VAT position by taking appropriate professional advice.
Legal costs:
Each party to bear its own legal costs incurred in the transaction.
KBW Property Consultants
enquiries@kbw.co.uk
First Floor, 12 Royal Crescent, Cheltenham
12 Royal Crescent provides serviced office accommodation, and the subject office is location on the first-floor level with views to the front and rear of the building.
Unit 4 Pegasus Centre, Gloucester Business Park
Unit 4 is situated in the Pegasus Centre, within the industrial sector at the eastern end of the Park and comprises a modern mid terrace industrial/warehouse building of steel frame construction.
Refurbished offices - Beckford Silk, Ashton Road, Beckford, Tewkesbury
The property was built in 1998 and is of brick construction under a pitched slate roof with a combination of dormer and velux windows within the roofline and sash windows at ground floor level.
Manufacturing office facility, Oldends Lane, Stonehouse
The property comprises a substantial industrial/office complex set in a self-contained site with an electronically operated gated entrance.


I share my truth to break generational cycles. I share my truth to be obedient. I share my truth to help others heal. For me, I continue to be healed through Christ as others are healed and become set free.
I invite you to join me on this healing journey; it is not easy and requires an intentional level of commitment, but it is well worth it.


The Fearless Farm Frau: Can You Hear Me (Growing) Now?
After the heat and drought last year, I was really hoping for a bumper crop this year. It looks, at least so far, like I'm going to get my wish.
When we moved out here, I heard that Harry and Margie were getting over 100 lbs of asparagus a year. Folks, that's a LOT of asparagus. I was really disappointed when, after tallying up our last year's yield, we only got 75 lbs. This year, we might actually outpace them.
Not only did my wonderful hubby buy me (and plant for me too!) some 2 year old purple asparagus crowns, he's got the watering system figured out AND fertilized with horse manure. We had a few fronds come up a few days ago. I picked them and ate them as I walked since they were so tiny.
The other day we got a few keepers. Barb and Ralph (our sainted neighbors) said that we could have theirs too. Still, it's early in the season, right? There won't be much. YEAH RIGHT.
The first few days, we averaged close to a pound a day. Today, however, we came pretty dang close to 5 pounds. And that's with me not picking anything under 6 inches tall. We've already filled a huge tupperware bucket in the fridge and the season's just starting. I swear I can hear the stalks growing. It's kind of a quiet thing, but you can hear them straining out of the earth.
So, it's not easy peeing green, LOL. What we don't sell fresh, we'll pickle (and if you've never had pickled asparagus, you're missing something!), freeze, or dehydrate. Dehydrated asparagus is an awesome addition to soups or stews, and still tastes great on its own. I sure am glad that we've taught the kids to love their veggies.
Meanwhile, the potatoes are coming up nicely. The carrots, lettuce (leaf and romaine), and onions are doing great. I think some radishes, beets, and peas are making their presence known. After even a mild winter, it sure does feel good being surrounded by an ocean of green leaves and blossoms.
The chickens are outdoing themselves. Every single hen laid today, with the exception of Beautiful Sweet the Silkie who is sitting on some Phoenix eggs. I love to go hang out with them and "egg" them on, haha.
I love spring. The smell of lilacs perfumes my house. My chickies are happy. My horses are finding more of their own forage. The kids can go out and play until they wear themselves out (without driving me nuts in the house). Here's to a bumper crop year!


Our semi-open impeller vertical HNC pumps have steep curves and no submerged bearings and bigger shafts.
The exciting, semi-open impeller, vertical HNC is a steep curved, versatile contender in any industrial setting. Heavy-duty bearings and oversized shaft with no submerged bearings or seals. Ability to move up to 3000 GPM and up to 240 TDH.


The second collection of ten tiny house drawings, compiled into a pocket-sized book. The houses are inspired by buildings from all around the world, charmingly immortalised in watercolour and ink.
Buy the other one here.
Watch me make the original drawings here.
Zines are packaged in sturdy envelopes to ensure they reach you in the best condition.
Got a question about your order, shipping, payment etc.??? CLICK HERE.