text:
\section{Introduction}

One of the most outstanding problems in gravitation theory is the evolution of
a collapsing massive star, after it has exhausted its nuclear fuel.
The problem of constructing physically realistic models for radiating collapsing
stars is one of the aims of the relativistic astrophysics.  However, in order to obtain
realistic models we need to solve complicated systems of nonlinear differential
equations.   In many cases we can simplify the problem considering some restrictions
in these equations and solve the system analytically.  Such models, although
simplified, are useful to construct simple exact solutions, which are at least
physically reasonable.  This allows a clearer analysis of the main physical
effects at play, and it can be very useful for checking of numerical procedures.

The majority of the previous works have considered
only shear-free motion of the fluid \cite{deOliveira85}\cite{Bonnor89}\cite{Wagh01}.
This simplification allows us to
obtain exact solutions of the Einstein's equations in some cases but it is
somewhat
unrealistic.  It is also unrealistic to consider heat flow without viscosity
but
if viscosity is introduced, it is desirable to allow shear in the fluid motion,
although we have not included the viscosity in this work.
Thus, it is interesting to study solutions that contains shear,
because it plays a very important role in the study
of gravitational collapse, as shown in \cite{Chan97, Chan98a, Chan98b, Chan00,
Chan01, Nogueira04, Pinheiro08, Pinheiro10} and in \cite{Joshi02}.
More recent studies on this subject with and without shear are also found in
\cite{Misthry08}-\cite{Sharif09}.

In the first paper\cite{Chan97}\cite{Chan98a} we have compared two collapsing
model: a shear-free and a shearing model.  We were interested in studying the
effect of the shearing motion in the evolution of the collapse.
It was shown
that the pressure of the star, at the beginning of the collapse, is isotropic
but due to the presence of the shear the pressure becomes more and more
anisotropic.
The anisotropy in self-gravitating systems has been reviewed and discussed the
causes for its appearance in \cite{Herrera97}.  As shown by
\cite{Chan97}\cite{Chan98a} the simplest cause of the presence of anisotropy in a
self-gravitating
body is the shearing motion of the fluid, because it appears without an
imposition ad-hoc \cite{Chan93}.

In the second paper \cite{Chan00} we have studied a model of a collapsing
radiating star consisting of an anisotropic fluid with initial homogeneous energy
density and shear viscosity undergoing
radial heat flow with outgoing radiation, but without bulk viscosity.

In the third paper \cite{Chan01} we have analyzed a model of a collapsing
radiating star consisting of an anisotropic fluid with initial homogeneous energy density
and bulk viscosity
undergoing radial heat flow with outgoing radiation, but without shear
viscosity.

The aim of this work is to generalize our previous models
by introducing initial inhomogeneous energy density, but without viscosity.

This work is organized as follows.  In Section 2 we present the Einstein's
field
equations.  In Section 3 we derive the junction conditions.
In Section 4
we present the proposed solution of the field equations.  In Section 5
we describe the model considered in this work for the initial configuration.
In Section 6 we present the energy conditions for an initial inhomogeneous energy
density fluid.
In Section 7 we show the time evolution of the total mass,
luminosity, the effective adiabatic index and
in Section 8 we summarize the main results obtained in this work.

\section{Field Equations}

We assume a spherically symmetric distribution of fluid undergoing dissipation
in the form of heat flow.  While the dissipative fluid collapses it produces
radiation.  The interior spacetime is described by the most
general spherically symmetric metric, using comoving coordinates,

\begin{equation}
ds^2_{-} = -A^2(r,t)dt^2+B^2(r,t)dr^2 + C^2(r,t)(d\theta^2+\sin^2 \theta d\phi^2).
\label{eq:dsi}
\end{equation}

The exterior spacetime is described by Vaidya's \cite{Vaidya53} metric, which represents
an outgoing radial flux of radiation,

\begin{equation}
ds^2_{+}=-\left[ 1- {\frac{2m(v)}{\bf r}} \right]dv^2-2dvd{\bf r}+{\bf r}^2
(d\theta^2+\sin^2 \theta d\phi^2),
\label{eq:dso}
\end{equation}
where $m(v)$ represents the mass of the system inside the boundary surface
$\Sigma$, function of the retarded time $v$.

We assume the interior energy-momentum tensor is given by

\begin{eqnarray}
G_{\alpha \beta}&=&\kappa T_{\alpha \beta}=\kappa \left[
(\mu+p_t)u_{\alpha}u_{\beta}+p_tg_{\alpha \beta}+
(p-p_t)X_{\alpha}X_{\beta} +\right. \nonumber \\
& & \left. +q_{\alpha}u_{\beta}+q_{\beta}u_{\alpha} \right],
\label{eq:tab}
\end{eqnarray}
where $\mu$ is the energy density of the fluid,
$p$ is the radial pressure,
$p_t$ is the tangential pressure,
$q^{\alpha}$ is the radial heat flux,
$X_{\alpha}$ is an unit four-vector along the radial direction,
$u^{\alpha}$ is the four-velocity,
which have to satisfy $u^{\alpha}q_{\alpha}=0$,
$X_{\alpha}X^{\alpha}=1$, $X_{\alpha}u^{\alpha}=0$ and $\kappa=8\pi$
(i.e., $c=G=1$).

The shearing tensor $\sigma_{\alpha \beta}$ is defined as
\begin{equation}
\sigma_{\alpha \beta}=u_{(\alpha;\beta)}+ \dot u_{(\alpha} u_{\beta)}-\frac{1}{3} \Theta (g_{\alpha \beta}+u_{\alpha}u_{\beta}),
\label{eq:sab}
\end{equation}
with
\begin{equation}
\dot u_{\alpha}=u_{\alpha;\beta}u^{\beta},
\label{eq:aab}
\end{equation}
\begin{equation}
\Theta=u^{\alpha}_{;\alpha},
\label{eq:theta}
\end{equation}
where $\Theta$ is the expansion scalar, the semicolon denotes a covariant
derivative and the parentheses in the indices mean symmetrizations.

Since we utilize comoving coordinates we have,

\begin{equation}
u^{\alpha}=A^{-1}\delta^{\alpha}_0,
\label{eq:u}
\end{equation}
and since the heat flux is radial
\begin{equation}
q^{\alpha}=q\delta^{\alpha}_1.
\label{eq:qa}
\end{equation}

Thus the non-zero components of the shearing tensor are given by
\begin{equation}
\sigma_{11}={2 \frac{B^2}{3A}}
\left( \frac{\dot B}{B} - \frac{\dot C}{C} \right),
\label{eq:sigma11}
\end{equation}
\begin{equation}
\sigma_{22}=-\frac{C^2}{3A}
\left( \frac{\dot B}{B} - \frac{\dot C}{C} \right),
\label{eq:sigma22}
\end{equation}
\begin{equation}
\sigma_{33}=\sigma_{22} \sin^2 \theta.
\label{eq:sigma33}
\end{equation}

A simple calculation shows that
\begin{equation}
\sigma_{\alpha \beta} \sigma^{\alpha \beta}=\frac{2}{3A^2}
 \left( {\dot B \over B} - {\dot C \over C} \right)^2.
\label{eq:sigma2}
\end{equation}

Thus, if we define the scalar $\sigma$ as
\begin{equation}
\sigma=-{1 \over {3A}}
 \left( {\dot B \over B} - {\dot C \over C} \right),
\label{eq:sigma}
\end{equation}
we can write that
\begin{equation}
\sigma_{11}=-{2 B^2 \sigma},
\label{eq:sigma11a}
\end{equation}
\begin{equation}
\sigma_{22}={C^2 \sigma},
\label{eq:sigma22a}
\end{equation}
\begin{equation}
\sigma_{33}={C^2 \sigma \sin^2 \theta}.
\label{eq:sigma33a}
\end{equation}

Using (\ref{eq:dsi}) and (\ref{eq:theta}), we can write that
\begin{equation}
\Theta={1 \over A}\left({{\dot B \over B} + 2 {\dot C \over C}}\right).
\label{eq:theta1}
\end{equation}

The non-vanishing components of the field equations, using (\ref{eq:dsi}),
(\ref{eq:tab}), (\ref{eq:u}), (\ref{eq:qa}) and
(\ref{eq:theta}), interior of the boundary
surface $\Sigma$ are

\begin{eqnarray}
G^{-}_{00} &=& -{ \left( A \over B \right) }^2 \left[ 2 {C'' \over C} +
{ \left( C' \over C \right) }^2 - 2{C' \over C}{B' \over B} \right]+ \nonumber \\
& & + {\left( A \over C \right)}^2 + {\dot C \over C}{ \left( {\dot C \over C}
+ 2{\dot B \over B} \right) } = \kappa A^2\mu,
\label{eq:g00}
\end{eqnarray}

\begin{eqnarray}
G^{-}_{11} &=& {C' \over C} { \left( {C' \over C} + 2{A' \over A} \right) }-
{ \left( B \over C \right) }^2 -\nonumber \\
& &- { \left( B \over A \right) }^2
\left[ 2{\ddot C \over C} + { \left( \dot C \over C \right) }^2 -
2{\dot A \over A} {\dot C \over C} \right] \nonumber \\
& &= \kappa B^2 p,
\label{eq:g11}
\end{eqnarray}

\begin{eqnarray}
G^{-}_{22} &=&
{ \left( {C \over B} \right) }^2 { \left[ {C'' \over C} + {A'' \over A}+
{C' \over C}{A' \over A} - {A' \over A}{B' \over B} - {B' \over B}{C' \over C}
\right] } +\nonumber \\
& & + { \left( C \over A \right) }^2 { \left[ -{\ddot B \over B} -
{\ddot C \over C} - {\dot C \over C}{\dot B \over B} + {\dot A \over A}
{\dot C \over C} + {\dot A \over A}{\dot B \over B} \right] } \nonumber \\
& &= \kappa C^2 p_t,
\label{eq:g22}
\end{eqnarray}

\begin{eqnarray}
G^{-}_{33} &=& {G^{-}_{22} \sin^2 \theta},
\label{eq:g33}
\end{eqnarray}

\begin{eqnarray}
G^{-}_{01} &=& -2{\dot C' \over C} + 2{C' \over C}{\dot B \over B}+
2{A' \over A}{\dot C \over C}= -\kappa A B^2 q.
\label{eq:g01}
\end{eqnarray}

The dot and the prime stand for differentiation with respect to $t$ and $r$,
respectively.

\section{Junction Conditions}

We consider a spherical surface with its motion described by a time-like
three-space $\Sigma$, which divides spacetimes into interior and exterior
manifolds.  For the junction conditions we follow the approach given by
\cite{Israel66a}\cite{Israel66b}.  Hence we have to demand

\begin{equation}
(ds^2_{-})_{\Sigma}=(ds^2_{+})_{\Sigma},
\label{eq:dsidso}
\end{equation}

\begin{equation}
K^{-}_{ij}=K^{+}_{ij},
\label{eq:kijikijo}
\end{equation}
where $K^{\pm}_{ij}$ is the extrinsic curvature to $\Sigma$, given by

\begin{equation}
K^{\pm}_{ij}=-n^{\pm}_{\alpha}
{{\partial^2x^{\alpha}_{\pm}} \over {\partial \xi^i \partial \xi^j}}
-n^{\pm}_{\alpha}\Gamma^{\alpha}_{\beta \gamma}
{{\partial x^{\beta}_{\pm}}  \over {\partial \xi^i}}
{{\partial x^{\gamma}_{\pm}} \over {\partial \xi^j}},
\label{eq:kij}
\end{equation}
and where $\Gamma^{\alpha}_{\beta \gamma}$ are the Christoffel symbols,
$n^{\pm}_{\alpha}$ the unit normal vectors to $\Sigma$, $x^{\alpha}$ are
the coordinates of interior and exterior spacetimes and $\xi^i$ are the
coordinates that define the surface $\Sigma$.

From the junction conditions (\ref{eq:dsidso}) and (\ref{eq:kijikijo}) we obtain the following
results (see more details in \cite{Chan97}-\cite{Chan01})

\begin{equation}
m=\left\{ {C \over 2}\left[ 1 + {\left( \dot C \over A \right)}^2 -
{\left( C' \over B \right)}^2 \right] \right\}_{\Sigma},
\label{eq:ms}
\end{equation}
which is the total energy entrapped inside the surface $\Sigma$ \cite{Cahill70},

\begin{equation}
p=(qB)_{\Sigma},
\label{eq:pqbs}
\end{equation}
(This result is analogous to the one obtained by \cite{Chan97}\cite{Chan98a}\cite{Chan00}\cite{Chan01}
for a shearing fluid motion.)

\begin{equation}
L_{\infty}={\kappa \over 2}\left[ p C^2 { \left( {C' \over B} +
{\dot C \over A} \right) }^2 \right]_{\Sigma},
\label{eq:lsp}
\end{equation}
which is the total luminosity for an observer at rest at infinity
and

\begin{equation}
1+z_{\Sigma}=
{ \left( {C' \over B} + {\dot C \over A} \right)^{-1} }_{\Sigma}.
\label{eq:zs}
\end{equation}
which is the boundary redshift $z_{\Sigma}$.
The boundary redshift can be used to determine the time of formation of
the horizon.

\section{Solution of the Field Equations}

As in \cite{Chan97}\cite{Chan98a}\cite{Chan00}\cite{Chan01} we are proposing solutions of the field
equations (\ref{eq:g00})-(\ref{eq:g01})
with the form

\begin{equation}
A(r,t)=A_0(r),
\label{eq:art0}
\end{equation}

\begin{equation}
B(r,t)=B_0(r),
\label{eq:brt0}
\end{equation}

\begin{equation}
C(r,t)=rB_0(r)f(t),
\label{eq:crt0}
\end{equation}
where $A_0(r)$ and $B_0(r)$ are solutions of a static perfect fluid having
$\mu_0$ as the energy density and $p_0$ as the isotropic pressure.

We have chosen this separation of variables in the metric functions, in order
to have the following properties: when $f(t) \rightarrow 1$ the metric functions
represent the static solution of the initial star configuration and the
collapse takes place when $f(t) \rightarrow 0$.
We stress here that, following the junction condition, equation (\ref{eq:dsidso}),
the function
$C(r_{\Sigma},t)$ represents the luminosity radius of the body as seen by an
exterior observer.

Thus, the expansion scalar (\ref{eq:theta1}) can be written as
\begin{equation}
\Theta={2 \over {A_0}} \left( {{\dot f \over f}} \right),
\label{eq:thetaa}
\end{equation}
and the shear scalar (\ref{eq:sigma}) can be written as
\begin{equation}
\sigma={1 \over {3A_0}} \left({\dot f \over f}\right).
\label{eq:sigmaa}
\end{equation}

Now the equations (\ref{eq:g00})-(\ref{eq:g01}) can be written as

\begin{equation}
\kappa \mu = \kappa {\mu_0}+ {1 \over {A^2_0}}\left( \dot f \over f \right)^2+
{1 \over {r^2B^2_0}}\left( {1 \over f^2} - 1 \right)
\label{eq:mu}
\end{equation}

\begin{eqnarray}
\kappa p&=&\kappa{p_0} - {1 \over {A^2_0}}\left[ 2{\ddot f \over f}+
{\left( \dot f \over f \right)}^2 \right]-
{1 \over {r^2B^2_0}}\left( {1 \over f^2} - {1} \right),
\label{eq:p}
\end{eqnarray}

\begin{equation}
\kappa p_t=\kappa {p_0} - {1 \over {A_0^2}} \left( { \ddot f \over f} \right)
\label{eq:pt}
\end{equation}

\begin{equation}
\kappa q = {2 \over {A_0B^2_0}} \left[ \left( {\dot f \over f} \right)
\left( {B'_0 \over B_0} + {1 \over r} - {A'_0 \over A_0} \right) \right],
\label{eq:q}
\end{equation}
where

\begin{equation}
\kappa \mu_0 = -{1 \over {B^2_0}}\left[ 2{B''_0 \over B_0} -
{\left( B'_0 \over B_0 \right)}^2 + {4 \over r}{B'_0 \over B_0} \right],
\label{eq:mu0}
\end{equation}

\begin{equation}
\kappa p_0 = {1 \over {B^2_0}}\left[ {\left( B'_0 \over B_0 \right)}^2 +
{2 \over r}{B'_0 \over B_0} + 2{A'_0 \over A_0}{B'_0 \over B_0} +
{2 \over r}{A'_0 \over A_0} \right].
\label{eq:p0}
\end{equation}

We can see from equations (\ref{eq:mu})-(\ref{eq:q}) that when the function
$f(t)=1$ we obtain the static perfect fluid configuration.

Substituting equations (\ref{eq:p}), (\ref{eq:q}) and
(\ref{eq:thetaa})-(\ref{eq:sigmaa}) into
(\ref{eq:pqbs}), assuming also that $p_0(r_{\Sigma})=0$,
we obtain a second order differential equation in $f(t)$,

\begin{equation}
2{\ddot f \over f} + {\left( \dot f \over f \right)}^2
+a\left( {\dot f \over f} \right) +
b\left( {1 \over f^2} - {1} \right)=0,
\label{eq:pqbsigma}
\end{equation}
where

\begin{equation}
a = \left[ 2{\left(A_0 \over B_0 \right)}
\left( {B'_0 \over B_0} + {1 \over r} - {A'_0 \over A_0} \right)
\right]_{\Sigma},
\label{eq:as}
\end{equation}
and
\begin{equation}
b = \left( A^2_0 \over {r^2B^2_0} \right)_{\Sigma}.
\label{eq:bs}
\end{equation}

Now, we can write equation (\ref{eq:pqbsigma}) in the following way

\begin{equation}
2f\ddot f + {\dot f}^2 + a f \dot f + b(1-f^2)=0,
\label{eq:ft}
\end{equation}

\begin{figure}
\vspace{.2in}
\centerline{\psfig{figure=fig1_star.ps,width=3.3truein,height=3.0truein}\hskip
.25in \psfig{figure=fig1_old.ps,width=3.3truein,height=3.0truein}
\hskip .5in} \caption{Time behavior of the function $f(t)$ for the models with
homogeneous and initial inhomogeneous density.  The time is in units of second and
$f(t)$ is dimensionless.  The collapse for the initial homogeneous energy density model ($\mu = constant$)
is 3000 times faster than that one for the initial inhomogeneous energy density model ($\mu=\mu(r)$).}
\label{foft}
\end{figure}

This equation is identical to the one obtained in
\cite{Chan97}\cite{Chan98a}\cite{Chan00}\cite{Chan01}.  Thus, as before
it has to be solved numerically (figure \ref{foft}), assuming that at
$t\rightarrow-\infty$ represents the static configuration with
$\dot f (t\rightarrow-\infty)\rightarrow0$ and
$f(t\rightarrow-\infty)\rightarrow1$.  We also assume that $f(t\rightarrow 0)
\rightarrow 0$.
This means that the luminosity radius $C(r_{\Sigma},t)$ has the value
$r_{\Sigma}B_0(r_{\Sigma})$ at the beginning of the collapse and vanishing at
the end of the evolution.

\section{Model of the Initial Configuration}

We consider that the system at the beginning of the collapse has a static
configuration of a perfect fluid satisfying \cite{Goldman78}

\begin{equation}
A_0^2=d_0\left[ \frac{1+(\alpha+\beta)g(r)}{1+(\alpha-\beta)g(r)} \right]^{1/\beta},
\label{eq:a0}
\end{equation}

\begin{equation}
B_0^2=c_0\frac{g(r)^2}{a_0^2(1+2\alpha g(r) + 2g(r)^2)}
\left[ \frac{1+(\alpha-\beta)g(r)}{1+(\alpha+\beta)g(r)} \right]^{(\alpha+1)/\beta},
\label{eq:b0}
\end{equation}
where

\begin{equation}
g(r)=\frac{a_0}{1-r^2},
\label{eq:gr}
\end{equation}
\begin{equation}
\beta=\sqrt{\alpha^2 - 2},
\label{eq:beta}
\end{equation}
\begin{equation}
d_0=\left( \frac{2r_{\Sigma}-m_0}{2r_{\Sigma}+m_0} \right)^2
\left[ \frac{1+(\alpha-\beta)g(r_{\Sigma})}{1+(\alpha+\beta)g(r_{\Sigma})} \right]^{1/\beta},
\label{eq:dd}
\end{equation}
\begin{equation}
c_0=\frac{a_0^2}{g(r_{\Sigma})}\left( 1+ \frac{m_0}{2r_{\Sigma}} \right)^4
\left[ 1+2\alpha g(r_{\Sigma}) + 2g(r_{\Sigma})^2 \right]
\left[ \frac{1+(\alpha+\beta)g(r_{\Sigma})}{1+(\alpha-\beta)g(r_{\Sigma})} \right]^{(\alpha+1)/\beta},
\label{eq:cc}
\end{equation}
\begin{equation}
a_0=\frac{2r_{\Sigma}}{m_0} (1-r_{\Sigma}^2),
\label{eq:aa}
\end{equation}
\begin{equation}
\alpha=\frac{r_{\Sigma}^3}{m_0 (1-r_{\Sigma}^2)}-\frac{m_0}{4r_{\Sigma}(1-r_{\Sigma}^2)}-\frac{2r_{\Sigma}}{m_0},
\label{eq:alpha}
\end{equation}
and where $r_{\Sigma}$ is the initial coordinate radius of the star in comoving coordinates
and $m_0$ is the initial mass of the system.
Thus the static initial inhomogeneous energy density and static pressure are given by

\begin{eqnarray}
\kappa \mu_0 &=&\frac{1}{B_0^2\left[ (1-r^2)^2 + 2\alpha a_0 (1-r^2) + 2a_0^2 \right]^2}
\left[ -4(2r^2-3a_0+1+4\alpha a_0)(1-r^2)^2- \right. \nonumber \\
& & \left. 8(1-r^2)^3 -8(\alpha a_0 -3 r^2a_0 -3\alpha a_0^2 -r^2 \alpha a_0 + 2a_0^2)(1-r^2)- \right. \nonumber \\
& & \left. 4a_0^2(2-6a_0-4\alpha r^2-5r^2) \right],
\label{eq:mu0a}
\end{eqnarray}

\begin{eqnarray}
\kappa p_0 &=&\frac{1}{B_0^2\left[ (1-r^2)^2 + 2\alpha a_0 (1-r^2) + 2a_0^2 \right]^2} \times \nonumber \\
& & \left[ 4(1-r^2)^3+(4r^2+8\alpha a_0)(1-r^2)^2+8a_0^2(1-r^2)-4a_0^2r^2 \right].
\label{eq:p0a}
\end{eqnarray}
This solution shows that the pressure and the energy density are finite and positive
everywhere inside the star, the pressure and energy density decreases toward the
boundary and that the speed of sound is smaller than the speed of the light $c$
everywhere.

We consider the initial configuration as due to an helium core of a
presupernova with $m_0=6M_{\odot}$,
with $r_{\Sigma}=2.1232\times10^5$ km which corresponds
approximately the same geometrical radius
$r_{\Sigma}B_0(r_{\Sigma}$) = $2.1218\times10^5$ km \cite{Woosley88}.

With these
values we can solve numerically the differential equation (\ref{eq:ft}).
Since the equation (\ref{eq:a0}) gives us positive or negative values for
$A_0$, we have assumed that $A_0 < 0$.
Thus, we can see from (\ref{eq:q}), using (\ref{eq:a0})-(\ref{eq:cc}) and this
initial configuration, that
$[(B'_0/B_0+1/r-A'_0/A_0)/A_0]_{\Sigma} < 0$, $(B'_0/B_0+1/r)_{\Sigma} > 0$,
and by the fact that $q_{\Sigma} > 0$ then we conclude that $\dot f < 0$.

In the figure 1 we can note that the collapse for the initial homogeneous
energy density model ($\mu = constant$) is 3000 times faster than that one
for the initial inhomogeneous energy density model ($\mu=\mu(r)$).
This fact may be due to two reasons. Firstly, the geometrical radius of the
both models are not the same. Secondly, the metric functions $A_0(r)$ and
$B_0(r)$ are also different, in such way that in the present work we have
an initial monotonically decreasing energy density profile.  This issue is
also discussed in previous works \cite{Herrera98}\cite{Herrera99} in the
context of the Tolman mass.  These works have shown that a negative energy
density gradient increases the Tolman mass of the system, thus decreasing
the total collapse time. This result seems to agree with our present work.
Besides, since the initial inhomogeneous model collapses slower is also
related to the fact that in the present model the system ejects all its mass
(this result will be shown later below)
reducing drastically the gravitationally force term, unlike the initially
homogeneous case where only about 33\% of the mass is radiated.

In figure \ref{sigma} we show the time evolution of the shear scalar, for
different radii, for the two models (initial inhomogeneous and homogeneous
energy density).

In order to determine
the time of formation of the horizon $f_{\rm bh}$, we use the equations
(\ref{eq:zs}) and (\ref{eq:art0})-(\ref{eq:crt0}) and write

\begin{equation}
{\dot f_{\rm bh} \over f_{\rm bh}} = -\left[ {A_0 \over B_0}
\left( {B'_0 \over B_0} + {1 \over r} \right) \right]_{\Sigma}
\approx +1.4140.
\label{eq:fbh1}
\end{equation}

Using the numerical solution of $f(t)$ and equation (\ref{eq:fbh1}),
we can see from figure \ref{bh} that the horizon is never formed, because
the function $\dot f/f$ never reaches the value $+1.4140$.
At the first sight this fact could be interpreted as the formation of a
naked singularity.  However, this is not the case as we will see below in
the calculation of the total energy entrapped inside the hypersurface
$\Sigma$.

\begin{figure}
\vspace{.2in}
\centerline{\psfig{figure=fig2_star.ps,width=3.3truein,height=3.0truein}\hskip
.25in \psfig{figure=fig2_old.ps,width=3.3truein,height=3.0truein}
\hskip .5in} \caption{Time evolution of the shear scalar at different radii
for the initial inhomogeneous and homogeneous energy density model.  The radii
$r$, $r_{\Sigma}$ and the time are in units of seconds and the shear scalar
 is in units of sec$^{-1}$. }
\label{sigma}
\end{figure}

\begin{figure}
\vspace{.2in}
\centerline{\psfig{figure=fig3_star.ps,width=3.3truein,height=3.0truein}\hskip
.25in \psfig{figure=fig3_old.ps,width=3.3truein,height=3.0truein}
\hskip .5in} \caption{The function $\dot f/f$ as a function of the time
for the model with initial homogeneous and inhomogeneous energy density.
The time is in units of second.}
\label{bh}
\end{figure}

\begin{figure}
\vspace{.2in}
\centerline{\psfig{figure=fig4_star.ps,width=3.3truein,height=3.0truein}\hskip
.25in \psfig{figure=fig4_old.ps,width=3.3truein,height=3.0truein}
\hskip .5in} \caption{Density profiles for the model with initial homogeneous and
initial inhomogeneous energy density.  The radii $r$ and $r_{\Sigma}$ are in units of
seconds and the density is in units of sec$^{-2}$.}
\label{mu}
\end{figure}

\begin{figure}
\vspace{.2in}
\centerline{\psfig{figure=fig5_star.ps,width=3.3truein,height=3.0truein}\hskip
.25in \psfig{figure=fig5_old.ps,width=3.3truein,height=3.0truein}
\hskip .5in} \caption{Radial pressure profiles for the model with initial homogeneous and
initial inhomogeneous energy density.  The radii $r$ and $r_{\Sigma}$ are in units of
seconds and the radial pressure is in units of sec$^{-2}$.}
\label{pr}
\end{figure}

\begin{figure}
\vspace{.2in}
\centerline{\psfig{figure=fig6_star.ps,width=3.3truein,height=3.0truein}\hskip
.25in \psfig{figure=fig6_old.ps,width=3.3truein,height=3.0truein}
\hskip .5in} \caption{Tangential pressure profiles for the model with initial homogeneous and
initial inhomogeneous energy density.  The radii $r$ and $r_{\Sigma}$ are in units of
seconds and the tangential pressure is in units of sec$^{-2}$.}
\label{pt}
\end{figure}

\begin{figure}
\vspace{.2in}
\centerline{\psfig{figure=fig5_6_star.ps,width=3.3truein,height=3.0truein}\hskip
.25in \psfig{figure=fig5_6_old.ps,width=3.3truein,height=3.0truein}
\hskip .5in} \caption{The ratio of the radial and tangential pressure profiles
for the model with initial homogeneous and
initial inhomogeneous energy density.  The radii $r$ and $r_{\Sigma}$ are in units of
seconds and the radial and tangential pressures are in units of sec$^{-2}$.}
\label{prpt}
\end{figure}

\begin{figure}
\vspace{.2in}
\centerline{\psfig{figure=fig7_star.ps,width=3.3truein,height=3.0truein}\hskip
.25in \psfig{figure=fig7_old.ps,width=3.3truein,height=3.0truein}
\hskip .5in} \caption{Heat flux scalar profiles for the model with initial homogeneous and
initial inhomogeneous energy density.  The radii $r$ and $r_{\Sigma}$ are in units of
seconds and the heat flux scalar is in units of sec$^{-2}$.}
\label{qq}
\end{figure}

It is shown in figures \ref{mu} and \ref{qq} the radial profiles of the energy density
and the heat flux.

In figures \ref{pr} and \ref{pt} we plot the radial profiles of the radial and
tangential pressures.

In figure \ref{prpt} is shown the radial profiles of the radial and tangential
pressure ratio.
In this figure we can see that the star is isotropic
at the beginning of the collapse ($f = 1$) but becoming more and more
anisotropic at later times.

\section{Energy Conditions for an Initial Inhomogeneous Energy Density Fluid}

All known forms of matter obey the weak, dominant and strong energy conditions.
For this reason a star model based on some fluid which violates these
conditions cannot be seriously considered as physically relevant.

Thus, in order to find the energy conditions, we have
followed the same procedure used in Kolassis, Santos \& Tsoubelis (1988) and
have generalized the energy conditions for an anisotropic fluid. See more
details in \cite{Chan00}\cite{Chan01}.
These conditions are fulfilled if the following inequalities are satisfied:

\begin{equation}
(i)~~~~~~ |\mu+p|-2|\bar q| \ge 0,
\label{eq:gcr1}
\end{equation}

\begin{equation}
(ii)~~~~~ \mu-p+2p_t+\Delta \ge 0,
\label{eq:gcr3}
\end{equation}

\noindent and besides,
\bigskip

\noindent a) for the weak energy conditions

\begin{equation}
(iii)~~~~ \mu-p+\Delta \ge 0,
\label{eq:wcr1}
\end{equation}

\noindent b) for the dominant energy conditions

\begin{equation}
(iv)~ \mu-p \ge 0,
\label{eq:dcr1}
\end{equation}

\begin{equation}
(v)~~~~~~ \mu-p-2p_t+\Delta \ge 0,
\label{eq:dcr2}
\end{equation}

\noindent c) for the strong energy conditions

\begin{equation}
(vi)~~~~~ 2p_t+\Delta \ge 0,
\label{eq:scr1}
\end{equation}
where $\Delta=\sqrt{(\mu+p)^2-4\bar q^2}$.

From figure \ref{i-vi}(i)-(vi) ($\mu=\mu(r)$) we can note that the
conditions (\ref{eq:gcr1})-(\ref{eq:scr1}) are always satisfied for all radii and times.
However, in contrast, from the figure \ref{i-vi}(i)-(vi) ($\mu=constant$) we can conclude that
the conditions $(i)$ and $(vi)$ are not satisfied during all
the collapse and for any radius.  These inequalities are not satisfied for the
innermost radii ($r \le 0.2r_{\Sigma}$) and for the latest stages of the
collapse.

\begin{figure}
\vspace{.2in}
\centerline{\psfig{figure=fig8_star.ps,width=3.3truein,height=3.0truein}\hskip
.25in \psfig{figure=fig8_old.ps,width=3.3truein,height=3.0truein}
\hskip .5in} \caption{The energy conditions (\ref{eq:gcr1})-(\ref{eq:wcr1}), for
the model with initial inhomogeneous and homogeneous energy density.
The time is in units of seconds and all the
others quantities are in units of sec$^{-2}$.}
\label{i-vi}
\end{figure}

\section{Physical Results}

As in \cite{Chan97}\cite{Chan98a}\cite{Chan00}\cite{Chan01},
we have calculated several physical quantities,
as the total energy entrapped
inside the $\Sigma$ surface, the total luminosity perceived by an observer
at rest at infinity and the effective adiabatic index, and we have compared
them to the respective initial homogeneous ones.

\begin{figure}
\vspace{.2in}
\centerline{\psfig{figure=fig9_star.ps,width=3.3truein,height=3.0truein}\hskip
.25in \psfig{figure=fig9_old.ps,width=3.3truein,height=3.0truein}
\hskip .5in} \caption{Time behavior of the total energy entrapped inside
the surface $\Sigma$ for the models with initial inhomogeneous and homogeneous energy density.
The time, $m$ and $m_0$ are in units of seconds.}
\label{mass}
\end{figure}

From equation (\ref{eq:ms}) we can write using (\ref{eq:art0})-(\ref{eq:crt0})
that

\begin{equation}
m=\left[ {{r^3B^3_0} \over {2A^2_0}}f{\dot f}^2 + {rB_0 \over 2}
f(1 - f^2) + m_0f^3 \right]_{\Sigma},
\label{eq:mf}
\end{equation}
where

\begin{equation}
m_0=-\left[ {r^2B'_0} + {r^3B'^2_0 \over {2B_0}} \right]_{\Sigma}.
\label{eq:m0}
\end{equation}
We can observe from figure \ref{mass} that the mass inside $\Sigma$ is
different for both models, initial inhomogeneous and homogeneous energy density ones.
The initial inhomogeneous star model radiates all its mass during the evolution, in
contrast to the initial homogeneous star model where the star radiates about 33\% of
its total mass.

\begin{figure}
\vspace{.2in}
\centerline{\psfig{figure=fig10_star.ps,width=3.3truein,height=3.0truein}\hskip
.25in \psfig{figure=fig10_old.ps,width=3.3truein,height=3.0truein}
\hskip .5in} \caption{Time behavior of the luminosity perceived by an
observer at rest at infinity for the models with initial inhomogeneous and homogeneous energy density.
The time is in units of second and the luminosity is dimensionless.}
\label{lumin}
\end{figure}

Using the equations (\ref{eq:lsp}) and (\ref{eq:art0})-(\ref{eq:crt0}) we can
write the luminosity of the star as

\begin{eqnarray}
L_{\infty}&=&{\kappa \over 2}\left\{ p r^2B^2_0f^2 \times \right. \nonumber \\
& & \left. \times \left[ \left( r {B'_0 \over B_0} +1 \right)f +
\left( rB_0 \over A_0 \right) {\dot f} \right]^2 \right\}_{\Sigma}.
\label{eq:lf}
\end{eqnarray}

The effective adiabatic index can be calculated using the equations
(\ref{eq:mu})-(\ref{eq:p}), (\ref{eq:ft}) and
(\ref{eq:a0})-(\ref{eq:p0a}). Thus, we can write that

\begin{eqnarray}
\Gamma_{\rm eff}=
\left[ {\partial (\ln p)} \over {\partial (\ln \mu)} \right]_{r=const}
= \left( {\dot p} \over p \right) \left( \mu \over {\dot \mu} \right) & = &\nonumber \\
\frac{aB_0^2f \left[ -a f \dot f  - b(1-f^2) -3 \dot f^2 \right] - 4(b B_0^2 - A_0^2/r^2) \dot f}
{f^2 A_0^2 B_0^2 \kappa p_0 + a B_0^2 f \dot f + (B_0^2 b - A_0^2/r^2)(1- f^2)} \times \nonumber \\
\frac{f^2 A_0^2 B_0^2 \kappa \mu_0 + B_0^2 \dot f^2 + A_0^2(1-f^2)/r^2}
{2B_0^2 \dot f \left[ -a f \dot f - b(1-f^2) - 3 \dot f^2 \right] -4 \dot f/A_0^2}.
\label{eq:gamaf}
\end{eqnarray}

\begin{figure}
\vspace{.2in}
\centerline{\psfig{figure=fig11_star.ps,width=3.3truein,height=3.0truein}\hskip
.25in \psfig{figure=fig11_old.ps,width=3.3truein,height=3.0truein}
\hskip .5in} \caption{Time behavior of the effective adiabatic index
for the models with initial inhomogeneous and homogeneous energy density.
The time is in units of second and $\Gamma_{\rm eff}$ is dimensionless.}
\label{gama}
\end{figure}

Comparing the figures for $\Gamma_{\rm eff}$ ($\mu = \mu(r)$ and $\mu = constant$)
we notice that the time
evolution of the effective adiabatic indices are very different graphically.
We can note in figure \ref{gama} ($\mu = constant$) that shortly before the
peak of luminosity (see figure \ref{lumin}) there is a large discontinuity
in $\Gamma_{\rm eff}$, in contrast to the initial inhomogeneous star model where there
is no discontinuity in $\Gamma_{\rm eff}$.

\section{Conclusions}

A new model is proposed to a collapsing star consisting of an
initial inhomogeneous energy density fluid, radial heat flow and outgoing
radiation.  In previous papers \cite{Chan97}-\cite{Chan01} one of us has
introduced a collapse model of an initial homogeneous energy density.
In this work we have generalized
this previous model by introducing an initial inhomogeneous energy
density and we have compared it to the initial homogeneous one.

The behavior of the energy density, pressure, mass, luminosity and the
effective adiabatic index was analyzed. We have also compared to the case
of a collapsing fluid with initial homogeneous energy density of another previous model \cite{Chan97}\cite{Chan98a},
for a star with 6 $M_{\odot}$.

As we have shown the black hole is never formed
because the apparent horizon formation condition is never satisfied.
This could be interpreted as the formation of a naked singularity, as
Joshi, Dadhich and Maartens \cite{Joshi02} have suggested.  However
this is not the case because the star radiates all its mass before it
reaches the singularity at $r=0$ and $t=0$.  Not even a marginally naked
singularity is formed by the same reason, since in this case the apparent
horizon should coincide with the singularity at $r=0$ and $t=0$.

The pressure has negative values although physically this
could be considered unreasonable.  However, due to the heat flow (the term
$\Delta$) the energy conditions are always satisfied.

The pressure of the star, at the beginning of the collapse, is isotropic but
due to the presence of the shear the pressure becomes more and more
anisotropic.

The star radiates all its mass during the collapse and this explains
why the apparent horizon never forms.
In contrast of the result of this work, the
former model radiates about 33\% of the total mass of the star, before the
formation of the black hole.

An observer at infinity will see a radial point source radiating
exponentially until reaches the time of maximum luminosity and
suddenly the star turns off because there is no more mass in order to be
radiated.
In contrast of the former model with initial homogeneous energy density \cite{Chan97}-\cite{Chan01}
where the luminosity also increases exponentially, reaching a maximum and after
it decreases until the formation of the black hole.

The effective adiabatic index, in the initial inhomogeneous energy density model,
is always positive without any discontinuity in contrast of the former model
where there is a discontinuity around the time of maximum luminosity.
In the case of initial homogeneous energy density,
the effective adiabatic index has a very unusual behavior because we have
a non-adiabatic regime in the fluid due to the heat flow.  The index becomes
negative since the hydrodynamic pressure and the energy density may become negative.
Besides, in this case, neither the energy density is the measure of the
total energy density of a given piece of matter nor the hydrodynamic
pressure the only opposing contraction \cite{Barreto92}.

\bigskip
\bigskip

\noindent{\bf ACKNOWLEDGMENTS}

The author (RC) acknowledges the financial
support from FAPERJ (no. E-26/171.754/2000, E-26/171.533/2002 and
E-26/170.951/2006) and from
Conselho Nacional de Desenvolvimento Cient\'{\i}fico e Tecnol\'ogico - CNPq -
Brazil.
The author (GP) also acknowledges the financial support from CAPES.

\bigskip

redpajama_set_name: RedPajamaArXiv


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text:
Femise > Publications > Policy brief > FEMISE MED BRIEF no11 : "External and internal imbalances in South Mediterranean countries"
FEMISE MED BRIEF no11 : "External and internal imbalances in South Mediterranean countries"
The FEMISE Policy Brief series MED BRIEF aspires to provide Forward Thinking for the EuroMediterranean region. The briefs contain succinct, policy-oriented analysis of relevant EuroMed issues, presenting the views of FEMISE researchers and collaborators to policy-makers.
The eleventh issue of MED BRIEF "External and internal imbalances in South Mediterranean countries" is available by clicking here.
Dr Doaa Salman (MSA, Egypt) and Dr Vassilis Monastiriotis (LSE, UK)
This MED brief provides insights on the medium and the long term consequences of the external and internal imbalances in the South Mediterranean (South Med) countries over the period of the last twenty years, trying to identify the main areas of macroeconomic imbalance in these countries and the key aggregates which seem to drive wider developments in their macroeconomic and fiscal positions.
The list of FEMISE MED BRIEFS is available here.
The policy brief has been produced with the financial assistance of the European Union within the context of the FEMISE program. The contents of this document are the sole responsibility of the authors and can under no circumstances be regarded as reflecting the position of the European Union.

redpajama_set_name: RedPajamaCommonCrawl


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text:
See how we are responding to the COVID-19 outbreak.
CBILS
Business Support Directory
Maven opens Nottingham office to manage £40m MEIF Maven Debt Finance
Investment team will support growth SMEs across the East and South-East Midlands, as part of the Midlands Engine Investment Fund (MEIF), supported by the European Regional Development Fund.
Maven has opened its eleventh regional office in Nottingham city centre and appointed David Tindsley and Sajid Sabir to its growing investment team to support SMEs in the East and South-East Midlands.
The new office will add to Maven's strong presence across the Midlands enabling it to provide the necessary support to local companies, both in terms of the initial investment process and ongoing support as those businesses grow.
(L-R) David Tindsley, Investment Manager, Sajid Sabir, Investment Associate and Jonathan Lowe, Investment Director of Maven
David and Sajid have responsibility for new MEIF investments across the East and South-East Midlands, as well as managing portfolio investments across the region. David joins Maven following a 35-year career with two high street banks, primarily in the SME commercial and corporate banking sectors. Most of his banking career has been in the East Midlands region. Before joining Maven, David also ran his own business advisory company, offering support and guidance on a variety of banking issues to SME clients. Sajid joined Maven at the start of January 2018, having previously worked within the Corporate Finance team at Grant Thornton and, prior to that, Orbis Partners. During his Corporate Finance career Sajid has worked on transactions across Technology, Manufacturing and the Food & Beverage sectors.
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Funding opportunities for SMEs in Nottingham and D2N2 LEP
Keep up-to-date with our latest deals, events and business support blog.
The MEIF Maven Finance fund is backed by
Copyright © Maven Capital Partners UK LLP 2021.
MAVEN CAPITAL and MAVEN logo are the registered trade marks of Maven Capital Partners.
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As usual, not that immediate to find a proper answer on the 'Net, hence I'm providing one here.
While in Snow Leopard was quite easy to see your ext2/ext3 formatted disks via MacFuse and ext2-fuse, in Lion you need to install another fuse fork and select a special option. That new fork is OSXFUSE, which latest release at the time of this post if from December 2011.


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Porus malayalam dubbed version coming on surya tv.
chandrakumari serial started on sun network channels, it's malayalam dubbed version airing on surya tv.
zee keralam serial alliyambal getting good reviews, channel earned 76 points.
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Vanambadi – it's listed in top 1 for the last few weeks, official malayalam remake of potol kumar gaanwala (bengali tv series). sai kiran ram, gouri krishna , sana jelin , suchithra nair , seema g nair, uma devi nair, pria menon, chippy renjith , indira thampi , balu menon are in the star cast of vanambadi asianet serial. it's online videos at hotstar application is also getting record views. Mouna ragam is the tamil version on star vijay, which is also getting decent trp ratings.
Asianet planning to launch star singer season 8, audition will start very soon.
2019 sabarimala makaravilakku live coverage will be available on dd4 (doordarshan malayalam)channel, 14th january 2019 at 4.00 p.m.
Disclaimer – This post is made with the recent barc trp data, changes may happen in future and we are not streaming or embedding any videos here.


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text:
Report: 18-year-old shot, killed in Detroit over Cartier glasses
Micah Walker
Detroit police are searching for a man who shot and killed an 18-year-old man after stealing his Cartier glasses, WXYZ-TV reported.
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The alleged gunman is described as a male between the ages of 20 and 25, about 175 pounds with a slim build. He was last seen wearing a gray hooded sweatshirt, gray sweatpants and white shoes, and armed with a handgun.
More:Police: At least 7 people shot overnight in Detroit
More:Video: Detroit police seeking these 2 men after fatal shooting


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Programme and Operations Co-ordinator – West Africa Operations
Organization: Danish Refugee Council
Division for Africa and Americas – West Africa Operations
HQ, International Department, Operations
The position requires full proficiency in English and French.
You need to have the right to work in Denmark (through nationality or existing work visa) to be considered for this role).
The Danish Refugee Council (DRC) is looking for an experienced Programme and Operations Co-ordinator (POC) within for the Division of Africa and Americas in International Department to focus on programme support, grants management, operational compliance and risk management for 3-4 Country Operations in the West Africa region.
DRC offers a challenging position in an international and dynamic work environment to experienced and dedicated professionals committed to continue his/her career with a leading international humanitarian organisation committed to the protection of forced displaced people in conflict zones world-wide.
Who is Danish Refugee Council
DRC is Denmark's largest international non-governmental organisation. We work with humanitarian and development activities to ensure a dignified life for refugees, the displaced, and displacement-affected people and communities in more than 35 countries.
We focus our assistance on the entire displacement process: From the moment a crisis first emerges and displaces people in their home countries or across borders, to these people's life in camps, to their arrival in a foreign country, and ultimately to the process of rebuilding a normal life, either through voluntary return, local integration or resettlement.
Main tasks and responsibilities
The POC is overall responsible for providing and mobilising HQ support to country operations and regional office hosted within the Division in general and to West Africa region in particular. The POC operates under the raison d'etre of the Operational Divisions by which he/she support the Head of Division to provide management and leadership to the DRC & DDG operations globally, and in particular to promote and ensure operational compliance and development, and to promote a global execution of new policies and standards.
The POC takes a proactive and supporting approach in helping to ensure that the programmes operate in compliance with standards, guidelines and commitments, and that relevant priorities and objectives are pursued.
Promote and help ensuring that communication with donors in particular related to grants is timely, compliant and characterised by high quality;
Organisational risks are systematically and comprehensively identified as well as properly managed;
Oversee the annual cycle and related processes and tools are applied in the local context;
Constitute the contextualising link between HQ and field that helps translate and apply global policies and procedures to the operational context of his/her geographical responsibility and visa versa.
Maintain overall knowledge as to what happens in the Country Operations of his/her focus allowing him/her to respond in general terms to internal and external country specific inquiries.
Engage in various workgroups and strategic initiatives at HQ levels and in particular where the operational and contextual perspective is required and/or Operations are lead or co-lead.
The successful candidate will be part of the Division for Africa and Americas consisting of 10 colleagues working with the 18 country operations and three regions in Africa as well as DRCs operation in Colombia. In addition to this, Operations has the lead on a number of strategic priorities especially within Financing. The POC will travel 3-5 time a year.
Profile and qualifications
You are a flexible and team-oriented colleague able to handle – at times – intense work pressure, tight deadlines and ad hoc demands. Towards the field, you have a service-minded approach and you are keen to build strong working relations, while at the same time being pro-active and persistent in our shared pursuit for a high level of quality and compliance. Your experience allows you to take initiative and operate with a high degree of independence.
Specific qualifications
Relevant and qualifying educational background.
At least 3 years of full-time employment applying tasks related to the above.
At least 5 years of experience within the international humanitarian sphere preferable from both HQ and field employments.
Experience in planning, co-ordinating and leading processes that include multiple stakeholder.
Familiarity with programming related to Danish Demining Group (mine action, security governance and conflict management) would be an advantage.
Strong writing credentials and experience in reviewing proposals and reports.
Full professional proficiency in English and French.
Experience in developing and applying tools and systems.
Systematic and analytical approach with a high degree of attention to details.
Good command and interest in reviewing financial data and compliance. A certain analytical capacity within Finance and risk management in general an advantage.
Fluency in Spanish is an advantage.
Salary terms are in accordance with the agreement between DRC and AC. DRC offer a permanent full-time contract with starting date 1 March 2019. Duty station in Copenhagen, Denmark. Right to work in Denmark is a precondition for applying.
For more information, please refer to the attached Terms of Reference and on DRCs homepage.
Please note that due to an organisational restructuring, changes to the assigned tasks might occur and a number of the specific roles and responsibilities are still to be developed and specified.
Further information about the position can be obtained by contacting POC, Clarine Lacroux 3373 5349 or Head of Division, Christian Jacob Hansen on +45 3373 5036.
Application and CV
Please apply online via HR Manager. www.drc.dk > Vacancies > Current vacancies > Programme and Operations Co-ordinator West Africa or click here. Please submit your application in English no later than January 23, 2019.
DRC's capacity to ensure the protection of and assistance to refugees, IDP's and other persons of concern depends on the ability of our staff to uphold and promote the highest standards of ethical and professional conduct in relation DRC's values and Code of Conduct, including safeguarding against sexual exploitation, abuse and harassment. DRC conducts thorough and comprehensive background checks as part of the recruitment process. Visit drc.ngo to read more about what we do to secure robust safeguarding mechanisms.
If you have questions or are facing problems with the online application process, please visit drc.ngo/jobsupport.
FRANCE - INTERNSHIP - ASSISTANT LOGISTIQUE (H / F) - PARIS / CLICHY
Polio Data Officer (Consultant), Multiple duty station.


Publishing has been revolutionised in the past 30 years, due to the technological and cultural challenges to traditional modes of scientific and professional communications. Learned Publishing has been at the heart of these changes, serving as a living record of the transformations in our industry. From the advent of digital publishing to disruptive new business models, LP has been with us through the years, featuring reports on innovations and new initiatives, original research and insights, and expert commentary, helping us all make evidence-based publishing decisions. The timeline below features some notable highlights captured in Learned Publishing's 30-year history.
Click "Expand all" to open all dates and the news tabs within them, then click on either General, LP news, ALPSP news or Most cited articles tabs to see the facts and news related to either Learned Publishing Journal, ALPSP Society news or the most cited articles from that year.
Where do ethical responsibilities in editing and publishing lie? By John Glen heralds the launch of the Committee on Publication Ethics in 1997.
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Shao, JF; Shen, HY The outflow of academic papers from China: why is it happening and can it be stemmed?
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A journal is only as good as each component part, and we would like to thank everyone who has contributed to its success during the last 30 years. To our authors, thank you for contributing your expertise, ensuring every issue is packed with actionable, interesting content. To our reviewers, thank you for your evaluative skills and tireless efforts to shape the rigor and value of each article. To everyone who has sat on the editorial board, thank you for your knowledgeable consultation and passionate advocacy for high-quality publishing. To ALPSP, thank you for supporting the journal so enthusiastically and allowing us to act as the global platform for discussion and debate within our industry. To Wiley, our publishers, thank you for your efficient and competent services and advice. And finally, thank you to our readers—many of whom return as authors, as it is your voices that have made the last 30 years of Learned Publishing so engaging and worthwhile and which will lead us into the next 30 years and beyond.


text:
Malta Island
Tal-Lembi
Tal-Lembi is a locality in Mellieħa. Tal-Lembi is situated nearby to Ix-Xifer, and close to Ta' Redusa.
Notable Places in the Area
St Paul's Island
St Paul's Island, also known as Selmunett, is a small island off Selmun near the north-east of the main island of Malta. Photo: Jeffrey Sciberras, CC BY 3.0.
Fort Campbell, also known locally as Il-Fortizza ta' Selmun, is a former fort in Mellieħa, Malta. Photo: Wikimedia, CC BY-SA 3.0.
Popeye Village
Popeye Village, also known as Sweethaven Village, is a purpose-built film set village that has been converted into a small attraction fun park, consisting of a collection of rustic and ramshackle wooden buildings. Popeye Village is situated 4 km west of Tal-Lembi. Photo: Wikimedia, Public domain.
Buġibba Temple
Buġibba Temple is a megalithic temple on the border of Buġibba and Qawra towns, limits of St. Paul's Bay, Malta. Buġibba Temple is situated 3 km east of Tal-Lembi. Photo: Wikimedia, CC BY-SA 3.0.
Mellieħa is a large village or small town in the Northern Region of Malta. Photo: Lifeboatsrule, CC BY-SA 3.0.
Xemxija is a suburb on the western part of St. Paul's Bay in the Northern Region, Malta. Photo: Felix Koenig, CC BY 3.0.
Saint Paul's Bay is a town in the Northern Region of Malta, sixteen kilometres northwest of the capital Valletta. Photo: Yarah, CC BY-SA 3.0.
Location: Mellieħa, Malta Island, Malta, Europe
35.9619° or 35° 57' 43" north
14.3836° or 14° 23' 1" east
8F7PX96M+QC
92 metres (302 feet)
Ix-XiferLocality
Ta' RedusaLocality
Il-ĠdidaLocality
Għajn ĦadidLocality
Selmun PalaceBuilding
Fortizza ta' CampbellFort
Il-Qala tal-MistraCove
Selmun BayCove
Selmun Palace HotelHotel
Selmun ChurchChurch
Wied tal-MistraWadi
Kalkara RavineRavine
HuachupampaLocality in Peru
Tres ChiflonesLocality in Los Ríos, Chile
Baza'i GonbadHamlet in Afghanistan
ConchitaLocality in Cuba
DoonaveeraghLocality in County Sligo, Ireland
KavančilišteLocality in Serbia
Popular Destinations in Malta Island
Valletta Mdina
Sliema St. Julian's
I travel not to go anywhere, but to go. I travel for travel's sake. The great affair is to move. - Robert Louis Stevenson
South KoreaEast Asia SydneyNew South Wales, Australia
Ambergris CayeBelize District, Belize YorkEngland, United Kingdom
About Mapcarta. Thanks to Mapbox for providing amazing maps. Text is available under the CC BY-SA 4.0 license, excluding photos, directions and the map. Photo: Lifeboatsrule, CC BY-SA 3.0.


text:
Unusual India
Continental Food Recipes
Desserts and Sweets Recipes
Festival and Celebration Cuisines
Indian Chinese Cuisine
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Indian Pickles and Chutney Recipes
Indian Raita Recipes
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Bikes and SUV
Indian Restaurant Food Reviews
Food & More
Events | Travel
Amarnath Cave Story
Published on: June 15, 2013 | Updated on: February 15, 2017
By Ramandeep Kaur
'Ekam sat' means 'there is one Being'. It is the popular verse of Rigveda. As per this verse, God has three deities to carry on the tasks of the entire world. This is called Holy Trinity: Brahma is the creator, Vishnu is the perpetuator of life and Shiva is the destroyer of evil, purifier and harbringer of good. In Rig Veda, Lord Shiva has also been mentioned as Rudra. According to Yajurveda, Lord Shiva has been described as an ascetic warrior who wears deer skin's robe and carries a trishul in his hand. Lord Shiva is considered as a living God. He has three places of His residence – first and the foremost is Kailash Parvat, second one is Lohit Giri under which flows the Brahamputra and third one is Muzwan Parvat. Lord Shiva has been mentioned in the hymns of Rig Veda. Even in ancient India, Lord Shiva was worshiped and it is evident from the Mohinjodaro and Harappa findings.
Read: Amarnath Yatra 2016
One of the prominent religious destinations dedicated to Lord Shiva is the holy Amarnath Cave that is located in Jammu and Kashmir. Each year, lakhs of Hindu devotees visit the cave to pay obeisance to the ice Shiv lingam, a form of Lord Shiva that is formed inside the cave. Shiv lingam is formed when the water drips from the roof gets accumulated and start to freeze on the floor. According to Hindu religious belief, the size of Shiva lingam at Amarnath Cave increases and decreases with the different phases of the moon. But there is no scientific evidence to support this belief. Along with Shiva lingam, two more ice formations exist in the cave that are believed to be of Maa Parvati and their son Ganesha.
The Amarnath Cave has a special significance in the Hindu religion. As per legend, Lord Shiva had chosen this cave to describe the secrets of immortality and formation of the universe to Maa Parvati.
Once Maa Parvati asked Lord Shiva that when He started wearing the beads of heads. On this, Lord Shiva replied whenever you were born. Maa Parvati asked – why are you immortal and I keep on dying again and again? Lord Shiva said that this is due to the Amar Katha. Maa Parvati insisted to hear that Amar Katha and after convincing Lord for a long time, Lord Shiva decided to narrate that story to Maa Parvati.
To narrate the story, Lord Shiva started looking for an absolutely lonely place so that no living being can hear that Amar Katha except for Maa Parvati. He finally found the Amarnath Cave. To reach there, He left all his belonging on the way like His bull Nandi at Pahalgam, His Moon at Chandanwari, His snakes at the banks of Lake Sheshnag, His son Ganesha at Mahagunas Parvat and at Panjtarni, He left his Five Elements (Earth, Fire, Water, Air and Sky).
After this, Lord Shiva entered in this holy Amarnath Cave with Maa Parvati. Lord Shiva sat on the Deer Skin and took a samadhi. To further make sure that not even a single living being could hear the secret Amar Katha, He created a rudra named Kalagni and ordered him to set fire around the cave so that everything living around that place could be destroyed. He then started narrating the story of immortality to Maa Parvati. But in spite of all these efforts, one egg remained protected under the deer skin on which the Lord was sitting. But it was considered as non-living. A pair of pigeons was born out of that egg and supposedly became immortal. Pilgrims can still see the pigeon pair while going towards the Amarnath Cave.
Amarnath Yatra Route
Devotees visit Amarnath Cave close to the festival of Shravani Mela that is held between July-August.
From Pahalgam – A traditional route
To reach Amarnath Cave, one has to reach Pahalgam either from Jammu (315 Km) or from Srinagar (96km). Take a bus or taxi from Jammu to reach Pahalgam or reach Srinagar by air and from there take a car, bus or taxi. From Pahalgam, devotees have to reach Chandanwari (16 km)and this distance can also be covered by using road transport. Pilgrims can either camp at Pahalgam or Chandanwari.
From Chandanwari, pilgrims climb the height to reach Pissu Top that is believed to be formed by the dead bodies of Rakshas who were killed by Lord Shiva.
To reach at Sheshnag, pilgrims follow a steep incline. The entire route has untouched wild scenery with cascading stream on one side. The place got its name from the Seven Peaks. The shape of the peaks resemble that of the head of the mythical snake.
From Sheshnag one has to cover the steep height of 4.6 km to reach Panchtarni. This is the last camp to the Holy Amarnath Cave. Cold winds might lead to cracks on skin. Also at such an altitude one feels short of oxygen.
From Panchtarni, the Amarnath Cave is located at a distance of just 6 km. As there is no place to stay, so pilgrims have to start their journey early in the morning so that you can come back to the base camp on time. The entire route is very beautiful.
From Baltal – A new route
There is another route to Amarnath cave from Baltal that is located at 14 km from the Amarnath caves. The distance of Baltal from Jammu is 400 km that can be covered by taxi or bus. From there, pilgrims can either take ponies or travel by foot to cover the route from Baltal to Amarnath. Though this route is much narrower and steeper than from Pahalgam, it can be completed in one day with Baltal as base camp. If you want to complete the journey in one day then you can hire a helicopter from Pahalgam to Panchtarni.
All in all, Amarnath Yatra is an experience in itself and one must visit this holy place at least once during his or her lifetime.
!@#$%
Amarnath Yatra Map
Amarnath
Ramandeep Kaur
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SAMIR January 22, 2014 at 10:58 am
nice details…
om namah shivaya
Panja December 10, 2015 at 10:48 am
Thanks you for the info. I wish to visit this place soon. God Shiva please help to fulfill my request to visit you soon. OM NAMA SHIVAAYA.
roy February 9, 2014 at 12:49 am
Amazing story nice share
zaborilenta February 8, 2015 at 6:07 pm
I've read a few good stuff here. Certainly worth bookmarking for revisiting. I surprise how much effort you set to create this kind of fantastic informative website.
udai June 25, 2015 at 3:31 pm
Swati Kulkarni September 12, 2015 at 9:52 pm
NIRANKAR SHARMA July 10, 2016 at 9:09 am
Very Good information on AmarNath cave & accessible routes.
Till 1976 cave was accessible only via Pahalgam-Chandanwai track. In 1977, Geological Survey of India established its first Base Camp in BAL-Tal to take up the Glaciological Studies of Panch-Tarni (Neh-Nar) Glacier. I had been member of team for 2 years.
In the follow up years this route with one-day access has gained the present popularity.
Suraj kumar sahu September 21, 2016 at 1:49 pm
nice pls
Amarnath Yatra Attack – Bus Driver's Bravery Saved Many Lives
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The Erie County Industrial Development Agency, (ECIDA) is seeking Letters of Interest from qualified engineering firms licensed in the State of New York to rate railroad bridge structures, many of which have no drawing documents, to comply with all federal and state regulations on the Buffalo Southern Railroad line which runs 30 miles between Buffalo and Gowanda, NY. Interested firms should submit a one page "letter of intent" to ECIDA by April 9th, 2015. RFQ and support material will be mailed to all responders by April 14th.
Dates: A/E Firm awarded: May 12th, 2015.


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ALONE: Quarantine, the final book in the Alone trilogy, was written at cafes and at home, and a bit on the road while touring and traveling. I can write anywhere and almost any time, but what I need to sort out is my own headspace. Music helps, and for the entire trilogy I listened to a loop of all of Radiohead's music (both their own recordings and covers), usually on shuffle via iTunes.
I reorganise my office space when starting each new project, and by the end it's full of research notes, books, and unopened mail. I've written five adult thrillers and the 2nd and 3rd I did get into character and realised for the sake of my sanity and those around me it wasn't worth it.
My first novel I wrote at my parent's house, which is on the southern coast of Victoria. I'd moved out after high school, aged 17, to study architecture at RMIT. After a couple years I deferred a year to see if I could write the novel that'd been bugging me to be written, so I moved back home for the year. I managed to complete it (FOX HUNT) and enjoyed the process so much that I ditched architecture to focus on writing. The 2nd book was written in a rented apartment in the eastern 'burbs of Melbourne, an old terrace above a persian rug shop, where I had a windowless study. From book 3 to 10 novels later, the space has been the same: my study, in Richmond, in a space that I designed and built myself as a warehouse conversion.
My first 2 novels I had a day job at a newspaper and then university, so my writing was mostly done at night and weekends. The last five or so years it's been full-time novel writing, and I write in the morning and day, and only into the late night when deadlines approach (or pass by).
Being a young, full-time writer probably seems like a romantic existence, and I guess on some levels it is, but it's all about being disciplined. The curse is that you can't escape it – I write every day, because I cannot find the off switch. That means each day I have to trawl the depths of human experience and emotion, which can be wearisome and worrying. Yet to me it seems like the only way to live. Each moment I write I just want to get it right; I'm always trying to be accurate, to not cheat readers nor my characters.
I start each day over a couple coffees at a local cafe, reading through the previous day's work and then getting into typing the new stuff.
What settles my mind? Unfortunately, very little. Music helps with blanketing out the background clatter. Writing a good book feels like a good achievement, if only until page one is started on the next thing. Perhaps most settling are the two or three little moments of literary magic that seem to occur each day – when you write, and really put the effort in to get lost in the characters and story, connections are made and moments arise that are completely unforeseen and unknowable for the author. That's a fulfilling and settling, feeling; each day, after those moments, I feel some work of worth has been done.


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The answers were always inside me.
It's never too late to become the 'you' you're meant to be.
Understanding my Human Design has been life-changing.
I was introduced to Human Design later in life. After decades of influence, conditioning and behavior that didn't support my design … I began the process of rediscovering who I am. I knew that I had gotten lost somewhere, but until I discovered Human Design, I didn't have the correct tools for me to reclaim my individuality.
I started studying Human Design to understand myself, however, as I started to benefit from the process of "living my design" friends and co-workers starting asking what I was so passionate about. My genuine passion for this revolutionary system is contagious and I was encouraged to continue my studies as a Human Design practitioner.
Professional Certified Human Design Analyst (Foundation, Relationship, Cycles, and Incarnation Cross Readings).
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I'm a life-long student of the creative arts, including recording 2 children's music albums, participating in multiple stage and screen productions, and as playwright of 5 Murder Mysteries. I've lived across the US, including Alaska, and currently reside in SW Washington with my dog Lester.


text:
Yoo Jae-yong () (June 6, 1936 - December 29, 2009) was a South Korean novelist, known for his faithfulness to traditional forms and emphasis on steadfast characters.

Life
Yoo Jae-yong was born on July 6, 1936 in Cheorwon, Gangwon-do during the period of Japanese rule. He attended Hwanil High School but dropped out before his graduation. In 1965 he won a prize for a children's story, The Gangly Balloon, in the New Year's Literary Competition sponsored by Chosun Ilbo.

He died on December 29, 2009, due to an undisclosed chronic illness. He was 73.

Work
Yoo made his literary debut with the serial children's tale The Gangly Balloon (키다리 풍선), which was printed in the Chosun Ilbo in 1965. Thereafter he published novels including Sanctuary (성역, 1980), Gone into the Wind and Rain (비바람 속으로 떠나가다, 1982).

Yoo's characters were typically past-oriented and fail to adapt themselves or to appreciate the complexities of the world.  This is regarded by critics as a product of his intention to focus on the inner nature of the characters, rather than their interaction with external factors. In his fiction, Yoo frequently turns to lives of refugees from North Korea. A steady stream of works beginning with "Portrait of My Elder Sister" (누님의 초상, 1978) deal with Korea's division from the viewpoint of characters who idealize the past in order to compensate for the depraved reality of the post-war present. Moreover, they display traditional outlook on life, characterized by belief in fate and inability to adapt to changing ethos and structures of society. In more recent works, however, Yoo Jaeyong sought to explore the thread that connects the past to the present rather than contenting himself with retrospection. Notable works in this vein are "Shadows" (Geurimja, 1982), "My Father's River" (아버지의 강, 1986) and "Circle" (Hwan), all of which address the continuing legacy of Korean division manifested on the family. Yoo Jaeyong also wrote a number of stories with a distinct philosophical bent; such stories as "Relationship" (관계, 1980), "Another Man's Life" (Tainui saengae) and "The Wig" (가발) highlight the inherent absurdity of life by featuring characters who depart from ordinary routine and assume the role of another person.

Works in Korean (partial)
Short Stories
 "Shadows" (, 1982)
 "My Father's River" ()
 "Circle" (Hwan)
 "Relationship" (Gwangye)
 "Another Man's Life" ()
 "The Wig" (Gabal)
Collections
 Sanctuary (Seongyeok, 1980)
 Gone with the Rainstorm ()
 The Shade of the Evening Sun ()
 Land of Silence ()

Awards
Hyundai Munhak Literary Prize, 1980
Yi Sang Literary Award, 1980
Literature Prize of the Republic of Korea, 1982
Cho Yun-hyun Literary Award, 1985
Dong-in Literary Award, 1987

See also
List of Korean novelists
Korean literature
Korean poetry

References

External links
 Naver Encyclopedia entry

South Korean novelists
1936 births
2009 deaths
Yi Sang Literary Award

redpajama_set_name: RedPajamaWikipedia


text:
EXPLORE magazine
The Real Kendall County.
Kathleen Marie Wilson: Fire Drawing
Art, FEATURE, Featured
As kids, most of us loved to plop down in the grass, gaze up into the sky, and see how many images we could discover hiding among the swirls and swells of cotton-candy clouds. Just as we were really getting into it, some grown-up would holler, "Stop daydreaming and finish your chores!" Eventually, often rebelling all the way, we took on adult responsibilities and stopped looking for pictures in the clouds.
But Kathleen Marie Wilson figured out a way to make searching for images work for her—and became a nationally recognized, award-winning pyrographer in the process.
Pyrography actually means 'fire drawing': Kathleen selects a piece of wood that, to her practiced eye and exceptional ingenuity, will eventually become a vessel extraordinaire for stories and pictures. Once she has determined the tale her wood wants to express, Kathleen begins burning her visions into it with a delicate electric pen—always going with the grain, never against it—and occasionally applying color to the finished product. Her work is such a marvelous combination of imagination and hard physical labor that it's almost impossible to determine where her picture begins and the wood grain leaves off.
Kathleen prefers light-colored hardwoods with interesting grain patterns. She began using basswood (and still recommends it to beginners), then advanced to woods with more character: pecan, maple, poplar, sycamore and cypress, among others. One piece of wood in her workshop had a beautiful blue cloudy haze through it, perfect for her work, but the color comes from a disease caused by a pine beetle. It's perfect for her art, she says, but very bad for the Lodge Pole Pine.
"Pecan is another wonderful wood that I love to use," she explains, "but those distinct lines are caused by spalted pecan fungus. Some of my best pieces are created on spalted woods."
Kathleen started dabbling in the art of pyrography when she was just a child. Her mother, a Cub Scout leader, gave her an inexpensive wood-burning set, complete with a wedge-tipped tool similar to a soldering iron, like the one her scouts were learning to use.
"The kit came with a little pattern," Kathleen explains with a grin. "There was a little piece of plywood with a picture on it that you could burn in it with the iron, but I didn't like any of the pictures. So I turned it over and burned my own picture into the back. I just wanted to do it my way."
Encouraged by her family to follow her instincts, Kathleen Marie Wilson has always marched to the beat of her own drummer, as have her older brother and two younger sisters.
"My mother was very supportive," she explains. "We didn't have much money, but she always managed to scrape up enough to buy me some art supplies. And my grandmother used to save her old calendars so I could draw on the backs of the calendar pages. That gave me twelve pages of blank paper I could draw on. That kind of support is invaluable to a child."
When Kathleen was about seven years old, the family moved to the edge of Mount Vernon, Ohio, a wonderful little town she calls 'Dream Middle America.' Kathleen felt as if she was living out in the country because there was a wide open field across from her home bordered by woods that seemed to go on forever.
"I could go out in the woods any time I wanted to and sort of get away from…people," she says with a wry, rather embarrassed grin. "I climbed trees and stayed up there for hours. I liked observing the wildlife and how they behaved, and I studied the plants. I learned, too, that if I was still for five or ten minutes, all the animals would ignore me. All I had to do was stay quiet. Birds would land right next to me and do their thing like I wasn't even there. One time I was sitting in a really comfortable tree when a squirrel ran across the ground, up the trunk of the tree, and right across my lap. It was so cool."
She and her next-door neighbor, also a budding artist, became inseparable best friends.
"We'd go down in the basement and draw pictures together." Kathleen chuckles. "Come to think of it, that's probably where my love of western art started. We'd copy pictures from Remington—you know, cowboys and horses. We both loved horses so much."
When the family moved to Fairborn, Ohio, Kathleen felt as if she had been uprooted from the heart of the wilderness and dropped into the middle of a major metropolitan area. "I'm a country girl," she explains with a grin, "so even though Fairborn isn't a large city, it was way too big for me."
Maybe it was the woods of Mount Vernon, or the Remington pictures, or the Louis L'Amour westerns she had devoured as a kid, but Kathleen always knew she would one day move west. So, after college, Kathleen and her then-husband, Tom, headed for San Antonio—a seemingly fearless act Kathleen now says was based on the fearless stupidity of youth.
"It was just an adventure to us, even though we were completely broke and drove a 'Heap of the Week' car we bought for $180. We left Ohio in the middle of a blizzard with nothing but our camping gear, a few items of clothing, my dog and three pet mice. We didn't have sense enough to be afraid."
Over the years Kathleen has perfected not only the art of pyrography, but she's also become a skilled woodworker, metal worker and furniture-maker. It didn't make sense to her when people said that a woman couldn't work with wood or use a chain saw.
"What's that got to do with gender?" she asks indignantly. "If someone else can do something, there's no reason I can't do it, too."
Tall, slender, and utterly natural, Kathleen has never been afraid to take on unusual jobs in order to support her art career. She's bartended, stuffed fish for a taxidermist, and even scooped poop as a groom for a quarter horse training stable. "Unlike most artists, though, I've never been a waitress or a secretary," she says with a laugh. "I can't type."
Kathleen also worked in watercolor, acrylic, pencil, pastel, and pen-and-ink because those art forms seemed to sell better, but the procedures didn't inspire her. She built furniture, carved wood, and worked in metal, but her heart longed to return to wood-burning. She had fallen back into the old trap, she says now, of accepting other people's boundaries for her life and not listening to her own spirit. She realized she had to stop caring about whether or not her work would ever be accepted and simply return to doing what she loved.
"Wood-burning was my true passion and it didn't matter how difficult it was. I finally understood that success isn't how much money you make, but how much enthusiasm and energy you have to share with others."
Today, Kathleen's life is all about enthusiasm, energy, and passion. She and her husband, Jeff (an expert woodworker she met in an Austin lumberyard), reside on 15 acres near Pedernales Falls State Park outside of Johnson City, and their lifestyle is very 'green.' They heat their home with a wood stove, and cutting firewood is an annual chore. Their water comes from an elaborate rainwater-capturing system, they recycle so much they don't even need trash pick-up, and they're installing a 'solar-toilet' as part of an innovative Dream Shack they're building to illustrate how green living really works.
"I'm not saying this is the only way to live," Kathleen explains earnestly, "but it's the only way for me to live. I have to walk the talk because I care so much."
Since horses and natural living are so important to Kathleen, it stands to reason that one of her favorite charities is the Proud Spirit Horse Sanctuary, located in Mena, Arkansas; she does all she can to help them. These horses, formerly abused or neglected, will run free for the rest of their lives on 320 acres, making Proud Spirit the largest privately-run sanctuary in the country. (For more on this amazing sanctuary, visit www.horsesofproudspirit.com.)
Kathleen has won numerous awards over the years, and was inducted in 2004 into her hometown's Fairborn Schools Hall of Honor: Career Achievement, Community Service and High Standard of Character. She also belongs to a group of professional artists known throughout Texas as the Texas Wild Bunch, and has been profiled by CBS' Texas Country Reporter as well as several magazines.
Kathleen's work appears in The Black Spur Emporium (www.blackspuremporium.com) and The Silver K Café in Johnson City, as well as in other locations, and she especially enjoys receiving visitors at her workshop and gallery on her own property. Sharing the place that inspires her is one of the things she loves to do. To make an appointment for a private showing or for more information, visit www.kathleenmariestudio.com.
Tagged: art, artist, boerne, burning, fire, hill country, horses, wood
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