text:
\section{Introduction}\label{sec1}
Einstein~\cite{Einstein1916}, in 1916, opened up a new way to look at the universe through his General Theory of Relativity. The striking idea that matter and energy creates curvature in the spacetime was beyond the imagination before him. New branches of physics, known as
Astrophysics and Cosmology, were created on the basis of GTR. Still now this field attracts the researchers to solve the hidden mystery of universe, with the same force as in the initial day. In $1916$ Schwarzschild found out the solution of the Einstein field equations describing a star with uniform matter density. The exact solution of the Einstein field equations are very much relevant to describe the nature of a compact star. Though after that many scientists obtained new exact solutions but very few of them satisfied the physical conditions inside the stellar interior. A survey report, made by Delgaty and Lake~\cite{Delgaty1988}, showed that out of $127$ known solutions only $16$ solutions satisfied all the physical conditions.

A neutron star is the final stage of a gravitationally collapsing star. It stabilized by degenerate neutron pressure after exhausting all the thermo nuclear fuel inside it. A compact star is more compact than an ordinary neutron star. Some of the examples of such compact stars  are X-ray burster $4U 1820-30$, X-ray pulsar $Her X-1$, X-ray sources RX J $185635-3754$, Milisecond pulsar SAX J $1808.4-3658$, PSR $0943+10$ because their estimated compactness cannot be explained properly in terms of ordinary neutron star Equation of State (EOS)~\cite{Alcock1986,Haensel1986,Weber2005,Perez-Garcia2010,Rodrigues2011,Bordbar2011}. The theoretical modelling of neutron stars have improved considerably over the last few decades after much improvement of the understanding of high energy particle interactions~\cite{Shapiro1983}. Ruderman~\cite{Ruderman1972} had shown that matter densities of compact stars are to be of the order of $10^{15} gm/cc$ or higher. At this high density range all the nuclear interactions have to treat relativistically. So one can expect that anisotropy in pressure may occur and it can be decomposed into two parts namely radial pressure $p_r$ and tangential pressure $p_t$~\cite{Bowers1974,Sokolov1980}. At this high density range anisotropy may occur in various reasons, e.g., existence of a solid core, phase transition, presence of type {\it P}-superfluid, rotation, magnetic field, existence of external field, mixture of two fluids etc.

The renowned particle physists  Gell-Mann~\cite{Gell-Mann1964} and Zweig~\cite{Zweig1964} independently proposed that hadrons are composed even with more fundamental particles known as quarks. Though this quark model get support of experiment later on.
According to Witten~\cite{Witten1984} and Farhi et al.~\cite{Farhi1984} quark matter might be the true ground state of hadron. This idea gives birth of an entirely new class of stellar objects composed of deconfined  {\it u}, {\it d} and {\it s} quarks, known as `quark stars'. In  quantum chromodynamics (QCD) the quark confinement mechanism have been dealt with great details as they are not seen as free particles. According to QCD, for large exchange of momentum the quark interactions becomes weak. At very high temperature
or large density, or at both of the conditions, the quark interactions becomes very weak and as a result they become deconfined. At a high temperature ($\sim $180 Mev or above) deconfinement of quarks are shown in Heavy Ion Collider Experiment. But the temperature of the neutron stars are of the order of few keV. So for deconfinement of the quarks at the centre of the neutron star, an extremely large chemical potential is required. The quark star results if the neutron star matter get converted totally into quark matter. Theoretically it is possible, under some conditions, that some of the up and down quarks transformed into strange quarks. Since strange matter is the true ground state of matter so quark star gets the thrust to converted totally into a strange star if its core once converted into a strange matter. Therefore a neutron star gets converted into strange star.

The strange matter can be formed by the following two ways, as proposed by Witten~\cite{Witten1984} that (i) at ultrahigh density range neutron star converted into a strange star and (ii) as a result of quark-hadron phase transition in the early universe.
Actually the transition from the normal hadronic matter to strange matter occurs at very high densities or corresponding to low
temperatures. Cheng et al.~\cite{Cheng1998} proposed that, nearly equal number of up, down and strange quarks are present in the Beta-Equilibrated strange quark star matter. Though there is a slight deficit of the latter. Bodmer~\cite{Bodmer1971}
suggested that, beyond nuclear density a phase transition between hadronic and strange quark matter could occur
in the universe when a massive star explodes as a supernova. As a result the inner core of the neutron star consists
most likely strange quark matter. In general if the mass to size ratio of a superdense star exceeds
$0.3$ then it can be expected to be composed of strange matter~\cite{Tikekar2007}. According to Alford~\cite{Alford2001},
in the dense core of a neutron star there is sufficiently high density and corresponding low temperature to crush the hadrons into quark matter. According to MIT bag model the quark confinement is due to the universal pressure $B_g$, called the Bag Constant. This simple model describes successfully the observations in particle physics. It is actually the difference between energy density of the perturbative and non perturbative quantum chromodynamics vacuum. Farhi and Jaffe~\cite{Farhi1984} as well as Alcock et al.~\cite{Alcock1986} proposed that the value of the bag constant should be within the following range $55-75$ $Mev/{fm}^{3}$, for a stable strange quark matter. In the nucleonic EOSs BSk $19$, BSk $20$ and BSk $21$ Chamel et al.~\cite{Chamel2013} used the values of effective bag Constant to be $78.6$, $65.5$ and $56.7$ $Mev/{fm}^{3}$. The data set of CERN-SPS and RHIC~\cite{Burgio2002} shows that a wide range of bag constant are permissible.

Tolman in $1939$~\cite{Tolman1939} gave explicit analytic solution of the Einstein field equations by choosing eight different types of metric potentials. Literature survey shows that there are no research works available in the field of astrophysics with the Tolman $V$ metric potential. As anisotropy is the most general case to investigate strange star so such situation has motivated us to study anisotropic strange star with Tolman $V$ metric potential through MIT bag model.

The planning of this paper is as follows: in Sec.~\ref{sec2} we have written down the basic field equations with the help of MIT bag model and Tolman $V$ metric potential. In Sec.~\ref{sec3} we have obtained solutions to the Einstein field equations along with the expressions for the anisotropy and EOS parameter whereas in Sec.~\ref{sec4} from the boundary condition we have found out the values of the constants. Sec.~\ref{sec5} can be decomposed into many subsections~\ref{subsec5.1} to~\ref{subsec5.4} containing the energy conditions, generalized TOV equation, Herrera's cracking concept and adiabatic index respectively. The mass-radius relation of the star and redshift are considered in Sec.~\ref{sec6}. Finally some concluding remarks are provided in Sec.~\ref{sec7}.

\section{Basic field equations of Einstein's space-time}\label{sec2}
The static spherically symmetric spacetime can be described by the line element
\begin{equation}
{ds}^{2}=-{{e}^{\nu(r)}}{{dt}^{2}}+{{e}^{\lambda(r)}}{{dr}^{2}}+{r}^{2}({{d\theta}^{2}}+{{sin}^{2}}\theta{{d\phi}^{2}}),\label{2.1}
\end{equation}
where $\nu(r)$ and $\lambda(r)$ are the metric potentials and function of the radial coordinate only. These metric coefficients have much
significance which actually help us to realize the gravitational environment of the stellar system. Considering the requirement for our study
we have assumed the form of line element which is most general and spherically symmetric. Here basically $g_{00} = e^{\nu}$ and $g_{11} = e^{-\lambda}$ such that only the magnitudes of these metric coefficients can change completely the scenario of physical structure~\cite{Maurya2017}.

The most general energy-momentum tensor for anisotropic matter distribution is given by
\begin{eqnarray}
{T_{{\nu}}}^{\mu}= (+\rho, - p_r, - p_t, - p_t), \label{2.2}
\end{eqnarray}
where $\rho$ is the matter density, $p_r$ is the radial pressure and $p_t$ is the
tangential pressure of the fluid which is in the orthogonal direction to $p_r$.

One can obtain the Einstein field equations, assuming $G=1=c$, as follows
\begin{eqnarray}\label{2.3}
& \qquad{{\rm e}^{-\lambda}} \left( {\frac {{\lambda}^{\prime}}{r}}-\frac{1}{r^{2}} \right) +{\frac{1}{{r}^{2}}}=8\pi
\rho,\\ \label{2.4}
& \qquad {{\rm e}^{-\lambda}}\left({\frac{{\nu}^{\prime}}{r}+\frac {1}{r^{2}}}\right)-{\frac{1}{{r}^{2}}}=8\pi{p_r},\\ \label{2.4a}
& \qquad\hspace{-0.5cm} \frac{1}{2}{{\rm e}^{-\lambda}}\left[\frac{1}{2}{\left({\nu}^{\prime}\right)}^{2}+{\nu}^{\prime\prime}-
\frac{1}{2}{\lambda}^{\prime}{\nu}^{\prime}+\frac{1}{r}\left({\nu}^{\prime}-{\lambda}^{\prime}\right)\right]=8\pi{p_t},
\end{eqnarray}
where prime denotes differentiation with respect to the radial coordinate $r$.

As we have mentioned in the Introduction that we are dealing with strange star in this paper so the equation of state, according to MIT bag model, will be
\begin{equation}
p_r=\frac{1}{3}\left(\rho-4{B_g}\right),\label{2.5}
\end{equation}
where $B_g$ is bag constant.

We define the mass function $m(r)$ of the star as
\begin{equation}
m \left( r \right) =4\pi \int_{0}^{r}\rho \left( r \right) {r}^
{2}{dr}.\label{2.6}
\end{equation}

Now to solve the field equation we choose Tolman V~\cite{Tolman1939} potential
\begin{equation}
{{\rm e}^{\nu}}=K{r}^{2n}, \label{2.7}
\end{equation}
where $K$ is the constant and $n$ is a parameter whose numerical value as chosen by Tolman~\cite{Tolman1939} was $1/2$. The choice of the above Tolman $V$ type potential is not all arbitrary here. Actually we wanted to study the case of strange star for different values of $n$, so that we could fix up the range of the index parameter $n$. However, after performing several numerical values of $n$ we have found that the model is stable only for $n=1/2$.

Another metric potential, needed for the spherical symmetry, is given by
\begin{equation}
{{\rm e}^{-\lambda}}=1-{\frac {2m}{r}}, \label{2.8}
\end{equation}
and this will help us to calculate the compactification factor in further.

\section{Solution of the Einstein field equations}\label{sec3}
Now from Eqs.~(\ref{2.3}),~(\ref{2.4}),~(\ref{2.5}) and~(\ref{2.7}) we find
\begin{eqnarray}
& \qquad\hspace{-1cm} {{\rm e}^{\lambda}}=-{\frac {3{r}^{4} \left( 3{n}^{2}+5n+2
 \right) {r}^{6n}}{ \left[\left( 48{r}^{6}\pi B_{{g}}-6{r}^{
4} \right) n+32{r}^{6}\pi B_{{g}}-6{r}^{4} \right] {r}^{6n}+9c_{{1}} \left( n+1 \right)\left( n+\frac{2}{3}\right) }}, \nonumber \\ \label{2.9}
\end{eqnarray}
where $c_{1}$ is an integration constant whose value can be determined from the boundary condition. For any physically viable model the metric potentials should be finite and free from singulrities inside the stellar system. Our model satisfies these conditions as at the centre we get  ${e^{\nu}|_{r=0}}=0$ and ${e^{\lambda}}|_{r=0}>1$.

Using the Einstein field equations~(\ref{2.3})-(\ref{2.4a}) and Eqs.~(\ref{2.5})-(\ref{2.7}) and (\ref{2.9}) we find the following physical parameters which are given by
\begin{eqnarray}\label{4.1}
& \qquad\hspace{-0.5cm} \rho={\frac {\rho_{{1}}{r}^{-\left(4+6n\right)}+3{n}^{2}+ \left( 48B_{{g
}}\pi {r}^{2}+3 \right) n+32B_{{g}}\pi {r}^{2}}{ 8\left( 3{n}^{
2}+5n+2 \right) \pi {r}^{2}}},\\ \label{4.2}
& \qquad\hspace{-0.5cm} p_{{r}}={\frac {\rho_{{1}}{r}^{-\left(4+6n\right)} + \left(3 - 96B_{{g}}\pi
{r}^{2} \right) {n}^{2}+ \left(3 -112B_{{g}}\pi {r}^{2}
 \right) n-32B_{{g}}\pi {r}^{2}}{ 24\left( 3{n}^{2}+5n+2
 \right) \pi {r}^{2}}},  \label{4.3} \nonumber \\ \\
& \qquad\hspace{-0.5cm} p_{{t}}={\frac {-\rho_{{1}} \left( n+2 \right) {r}^{-4-6n}+p_{
{1}}-16B_{{g}}\pi {r}^{2} \left( 5n+2 \right) }{24 \left( 3{n}^{
2}+5n+2 \right) \pi {r}^{2}}}, \label{4.4}
\end{eqnarray}
where\\
$\rho_{{1}}=-36 \left( n+\frac{1}{2}\right)  \left[ \rho_{{2}}- \left( \frac{1}{2}
{n}^{2}+\frac{n}{2}\right) {R}^{6n+4}-\rho_{{3}} \right] $, \\
$\rho_{{2}}= M \left( n+1 \right) \left( n+\frac{2}{3}\right) {R}^{6n+3}$, \\
$\rho_{{3}}=\frac{8}{3}\left( n+\frac{2}{3} \right) B_{{g}}\pi {R}^{6n+6}$, \\
$p_{{1}}= \left( 6-48B_{{g}}\pi {r}^{2} \right) {n}^{3}+ \left( 6-80B_{{g}}\pi {r}^{2} \right) {n}^{2}$.

\begin{figure}[!htp]
\centering
    \includegraphics[width=6cm]{density}
        \caption{Variation of the density with the fractional radial coordinate $r/R$ for $LMC\,X-4$} \label{rho}
\end{figure}

\begin{figure}[!htp]
\centering
    \includegraphics[width=6cm]{rad_press}
    \includegraphics[width=6cm]{tan_press}
        \caption{Variation of the radial $p_r$ (left panel) and $p_t$ (right panel) with the fractional radial coordinate $r/R$ for $LMC\,X-4$} \label{pres}
\end{figure}

The variations of density and pressures are shown in Fig.~\ref{rho} and~\ref{pres}. From both the Figs.~\ref{rho} we see that the matter density, radial pressure and tangential pressure all decrease monotonically. In the case of density we note from Fig~\ref{rho} that $\rho(0)  \rightarrow \infty$ and $\rho(R) \rightarrow $ finite. Also from Fig.~\ref{pres} it is clear that for only $n=1/2$ we are getting positive value of the tangential pressure inside the stellar configuration and henceforth we shall consider only the $n=1/2$ case for further physical study.

The anisotropy of the system is calculated as follows
\begin{eqnarray}
& \qquad\hspace{-1cm} \Delta={\frac {-\rho_{{1}} \left( n+3 \right) {r}^{-(4+6n)}+
 \left( 96B_{{g}}\pi {r}^{2}-3 \right) {n}^{2}+ \left( 32B_{{g}}
\pi {r}^{2}-3 \right) n+p_{{1}}}{ 24\left( 3{n}^{2}+5n+2 \right)
\pi {r}^{2}}}. \nonumber \\\label{4.5}
\end{eqnarray}

\begin{figure}[!htp]
\centering
    \includegraphics[width=6cm]{anisotropy}
            \caption{Variation of the anisotropy with the fractional radial coordinate $r/R$ for $LMC\,X-4$} \label{aniso}
\end{figure}

The term $2\Delta/r$ is called anisotropic force, which will be directed outward (i.e. repulsive in nature) if $\Delta>0$
and directed inward (i.e. attractive in nature) if $\Delta<0$. The Fig.~\ref{aniso} tells us that $\Delta>0$ throughout the stellar distribution. So here $p_{t}>p_{r}$, i.e., $\Delta>0$ will helps to construct the more compact object according to Gokhroo and Mehra~\cite{Gokhroo1994}.

Now for a physically valid stellar model the radial pressure must vanish at the surface $(r=R)$, i.e., ${p_r}\left(R\right)=0$ and we have
\begin{eqnarray}
n={\frac {M}{R-2M}}.\label{4.6}
\end{eqnarray}

In the above Eq.~(\ref{4.6}) for finite value of the parameter $n$ we impose the condition $R \neq 2M$. However, it is interesting to note that at the radius $R$, if $R = 2M$, one can get $n \rightarrow \infty$. This therefore provides a limiting value of $n$ to avoid any unphysical situation. In the present study we have opted for the value of $n=1/2$ as other values do not yield physically viable results. This immediately suggests the radius of the present compact star as $R = 4M$ and can be written in the form $2M/R=0.5$. This fulfils the Buchdahl condition $2M/R<0.88$~\cite{Buchdahl1959} in connection to the mass-radius relationship which will be discussed later on in details.

Following Deb et al.~\cite{Deb2016} we maximize anisotropy at the surface and find the bag constant as
\begin{eqnarray}\label{4.7}
& \qquad\hspace{-0.5cm} B_{{g}}={\frac {12M{n}^{3}-6{n}^{3}R+54M{n}^{2}-23{n}^{2
}R+60Mn-14nR+18M}{16 \left( 2{n}^{2}+7n+3 \right) \pi {R}^{3
}}}.\nonumber \\
\end{eqnarray}

The radial~$\left({{\omega}_r}\right)$ and tangential~$\left({\omega}_t\right)$  EOS parameters for our system can be written in the following form as
\begin{eqnarray}\label{3.7}
& \qquad\hspace{-7.2cm} \omega_{{r}}=\frac{p_r}{\rho}\nonumber \\
& \qquad\hspace{-0.6cm}={\frac {\rho_{{1}}{r}^{-\left(4+6n\right)}+ \left(3-96B_{{g}}
\pi {r}^{2} \right) {n}^{2}+ \left(3-112B_{{g}}\pi {r}^{2}
 \right) n-32B_{{g}}\pi {r}^{2}}{3\rho_{{1}}{r}^{-\left(4+6n\right)}+3{n}^{2
}+ \left(48B_{{g}}\pi {r}^{2}+3 \right) n+32B_{{g}}\pi {r}^{2}}}, \nonumber \\
\end{eqnarray}

\begin{figure}[!htp]
\centering
    \includegraphics[width=6cm]{EOS}
           \caption{Variation of the radial and transverse EOS parameter with the fractional radial coordinate $r/R$ for $LMC\,X-4$} \label{eos}
\end{figure}

\begin{eqnarray}\label{3.8}
& \qquad\hspace{-7.2cm} \omega_{{t}}=\frac{p_t}{\rho}\nonumber \\
& \qquad\hspace{-0.6cm}={\frac {-\rho_{{1}} \left( n+2 \right) {r}^{-\left(4+6n\right)}-80
B_{{g}}\pi n{r}^{2}-32B_{{g}}\pi {r}^{2}+p_{{1}}}{3\rho_{{1}}{
r}^{-\left(4+6n\right)}+9{n}^{2}+ \left( 144B_{{g}}\pi {r}^{2}+9 \right) n+
96B_{{g}}\pi {r}^{2}}}.
\end{eqnarray}

From Fig.~\ref{eos}, we get $0 \leq (\omega_r, \omega_t) \leq 1/3$ where maximum value of EOS starts from the center and decreases to zero at the surface of the spherical stellar system. Moreover, we note that here $\omega_r < \omega_t$.

\section{Matching boundary conditions}\label{sec4}
Now we shall match our interior solutions to the exterior Schwarzschild metric at the boundary $r=R$, here $R$ being the total radius of the star, given as
\begin{eqnarray}    \label{3.1}
&\qquad\hspace{-1cm} ds^{2} =-\left(1-\frac{2M}{r} \right)\, dt^{2} + \frac{dr^{2}}{\left(1-\frac{2M}{r}\right)}+r^{2} (d\theta ^{2}+\sin ^{2} \theta \, d\phi ^{2} ),\nonumber \\
\end{eqnarray}

At the boundary the coefficients $g_{rr}$, $g_{tt}$ and $\frac{\partial g_{tt}}{\partial r}$ all are continuous and the continuity of $g_{rr}$, $g_{tt}$ gives us (vide Fig.~\ref{pot})
\begin{eqnarray}\label{3.2}
& \qquad\hspace{-4cm} {{\rm e}^{\nu \left( R \right) }}=K{R}^{2n}=1-{\frac {2M}{R}},\\ \label{3.3}
& \qquad {{\rm e}^{\lambda \left( R \right) }}=-{\frac {3{R}^{4} \left( 3{n
}^{2}+5n+2 \right) {R}^{6n}}{9c_{{1}} \left( n+1 \right)\left( n+\frac{2}{3} \right)+48{R}^{4} \left[ \pi B_{{g}}
 \left( n+\frac{2}{3} \right) {R}^{2}-\frac{n+1}{8}\right] {R}^{6n}}} \nonumber \\
& \qquad\hspace{-4cm} ={\left(1-{\frac {2M}{R}}\right)}^{-1}.
\end{eqnarray}
From the above two equations we will get the value of the constant $K$ and integration constant $c_{1}$ which are given by
\begin{eqnarray}\label{3.4}
& \qquad\hspace{-2cm} K= \frac{1}{R^{2n}}{\left(1-{\frac {2\,M}{R}}\right)},\\ \label{3.5}
& \qquad\hspace{-0.5cm} c_{{1}}={\frac {-48\, \left( n+\frac{2}{3}\right) B_{{g}}\pi {R}^{6n+6}-9
 \left( n+1 \right)  \left[ -2 \left( n+\frac{2}{3} \right) M{R}^{6n+3}+
{R}^{6n+4}n \right] }{9{n}^{2}+15n+6}}. \nonumber \\
\end{eqnarray}

We shall use numerical values of these constants to plot the graphs.

\begin{figure}[!htp]
\centering
    \includegraphics[width=6cm]{t_pot}
    \includegraphics[width=6cm]{r_pot}
        \caption{Variation of ${\rm e}^{\nu}$ (left panel) and ${\rm e}^{\lambda}$ (right panel) with the fractional radial coordinate $r/R$ for $LMC\,X-4$ for $n=1/2$} \label{pot}
\end{figure}

\section{Physical properties of the stellar model}\label{sec5}

\subsection{Energy conditions}\label{subsec5.1}
General relativity permits energy-momentum tensor $T^{ij}$ to describe the distribution of mass, momentum and stress due to matter and to any non-gravitational fields. Though Einstein's field equation not directly concern with what kind of states of matter or non-gravitational fields are admissible in the spacetime, the energy conditions allows all states of matter and all non-gravitational fields in GTR and ruled out many unphysical solutions. Therefore GTR allows the following energy conditions known as the Null Energy Condition (NEC), Weak Energy Condition (WEC), Strong Energy Condition (SEC) and
Dominant Energy condition (DEC).

 The energy conditions are satisfied if and only if the following inequalities hold simultaneously by every point inside the fluid sphere:
 \begin{eqnarray}\label{5.1.1}
& \qquad NEC: \rho \geq 0,\\ \label{5.1.2}
& \qquad {WEC_r}:\rho+{p_r} \geq 0, \rho\geq 0, \\ \label{5.1.3}
& \qquad {WEC_t}:\rho+{p_t} \geq 0, \rho\geq 0, \\ \label{5.1.4}
& \qquad {SEC}:  \rho+{p_r} \geq 0, \rho+{p_r}+2{p_t}> 0,\\ \label{5.1.5}
& \qquad {DEC_r}: \rho>|p_r|,~{DEC_t}: \rho>|p_t|. \label{5.1.6}
\end{eqnarray}

\begin{figure}[!htp]
\centering
    \includegraphics[width=7cm]{energy}
           \caption{Variation of the energy conditions with the fractional radial coordinate $r/R$ for $LMC\,X-4$} \label{energy}
\end{figure}

From Fig.~\ref{energy} it is observed very clearly that NEC, WEC, SEC and DEC are satisfied by our model.

\subsection{Generalized TOV equation}\label{subsec5.2}
To search equilibrium situation of this anisotropic star under different forces, the generalized Tolman-Oppeheimer-Volkoff (TOV) equation
can be written as~\cite{Varela2010}
\begin{equation}
-\frac{M_G(\rho+p_r)}{r^{2}}e^{\frac{\lambda-\nu}{2}}-\frac{dp_r}{dr}+\frac{2}{r}(p_t-p_r)=0,\label{5.2.1}
\end{equation}
where $M_G=M_G(r)$ is the effective gravitational mass inside a sphere of radius $r$ which can be derived from the modified
Tolman-Whittaker formula~\cite{Devitt1989} as
\begin{equation}
M_G(r)=\frac{1}{2}r^{2}e^{\frac{\nu-\lambda}{2}}\nu'.\label{5.2.2}
\end{equation}
substituting this value in Eq.~(\ref{5.2.1}) we get the following form of TOV equation
\begin{equation}
-\frac{\nu'(\rho+p_r)}{2}-\frac{dp_r}{dr}+\frac{2}{r}(p_t-p_r)=0,\label{5.2.3}
\end{equation}
which can be written in the following form as
\begin{equation}
F_g+F_h+F_a=0,\label{5.2.4}
\end{equation}
where $F_g$, $F_h$ and $F_a$ represents respectively gravitational force, hydrostatic force and anisotropic force.

From our model we get the following expressions of the above mentioned terms
\begin{eqnarray}\label{5.2.5}
&\qquad\hspace{-7cm} {F_g}=-\frac{\nu'}{2}(\rho+p_r)\nonumber \\
&\qquad\hspace{-1cm}=-{\frac { \left( -24B_{{g}}\pi {n}^{2}{r}^{2}+8B_{{g}}\pi
n{r}^{2}+16B_{{g}}\pi {r}^{2}+\rho_{{1}}{r}^{-(4+6n)}+3{n}^{2}
+3n \right) n}{6{r}^{3} \left( 3{n}^{2}+5n+2 \right) \pi }}\nonumber \\ \\\label{5.2.6}
&\qquad\hspace{-5.6cm} {F_h}=-\frac{dp_r}{dr}={\frac {n+\rho_{{1}}{r}^{-\left(4+6n\right)}}{4\pi \left( 3n+2 \right) {
r}^{3}}}\\\label{5.2.7}
&\qquad\hspace{-7.2cm} {F_a}=\frac{2}{r}(p_t-p_r)\nonumber \\
&\qquad\hspace{-0.9cm}={\frac {-\rho_{{1}} \left( n+3 \right) {r}^{-(4+6n)}+ \left( 96
B_{{g}}\pi {r}^{2}-3 \right) {n}^{2}+ \left( 32B_{{g}}\pi {r}^
{2}-3 \right) n+p_{{1}}}{12{r}^{3} \left( 3{n}^{2}+5n+2 \right) \pi}} \nonumber \\
\end{eqnarray}

\begin{figure}[!htp]
\centering
    \includegraphics[width=6cm]{forces}
           \caption{Variation of different forces with the fractional radial coordinate $r/R$ for $LMC\,X-4$} \label{forces}
\end{figure}

From Fig.~\ref{forces} it is obvious that the combined effect of the hydrostatic force and anisotropic force is balanced by the gravitational
force. This figure indicates that our stellar model is in equilibrium under these forces. However, here the anisotropic force is very small with respect to the other two forces. This implies that the radial and tangential pressures do differ in very small amount. Here to achieve stability for the system the hydrodynamic force is taking a major role to counter balance the gravitational force. But still there is a role of anisotropic force which is also balancing the gravitational force.

\subsection{Herrera cracking concept}\label{subsec5.3}
For a physically realistic model the speed of sound should follow the condition $0\leq{v_{rs}^{2}}\leq1$ and $0\leq{v_{ts}^{2}}\leq1$, which can be termed as causality condition. Also for the stability checking there is an another technique for anisotropic matter distribution, which is known as cracking concept of Herrera~\cite{Herrera1992}. According to this concept the region for which transverse speed of sound is smaller than the radial speed of sound is a potentially stable region~\cite{Herrera1979,Herrera1992,Chan1993,Abreu2007}. The square of radial~$\left({v}_{\it rs}^2\right)$ and tangential~$\left({v}_{\it ts}^2\right)$ sound speed for our system are given as
\begin{eqnarray}\label{5.3.1}
&\qquad\hspace{-6.5cm} {{v}_{\it rs}^2}=\frac{dp_r}{d\rho}=\frac{1}{3},\\ \label{5.3.2}
&\qquad\hspace{-0.5cm} {{v}_{\it ts}^2}=\frac{dp_t}{d\rho}={\frac {-v_{{1}} \left( n+2 \right) +v_{{3}}{R}^{
6n+4}+v_{{2}} \left( n+2 \right) -2{n}^{2}{r}^{6n+4}}{3v_{{1}}
+ \left( -54{n}^{3}-81{n}^{2}-27n \right) {R}^{6n+4}-3v_{{2}
}-3{r}^{6n+4}n}}, \nonumber \\
\end{eqnarray}
where \\
$v_{{1}}=36M \left( n+1 \right)  \left( n+ \frac{1}{2}\right)  \left( n+ \frac{2}{3}\right) {R}^{6n+3}$, \\
$v_{{2}}=96B_{{g}}\pi \left( n+\frac{1}{2} \right)  \left( n+\frac{2}{3} \right) {R}^{6n+6}$, \\
$v_{{3}}=18{n}^{4}+63{n}^{3}+63{n}^{2}+18n$.

\begin{figure}[!htp]
\centering
    \includegraphics[width=6cm]{vel}
    \includegraphics[width=6cm]{vel_diff}
           \caption{Variation of radial speed of sound, transverse speed of sound (left panel) and velocity difference (right panel) with the fractional radial coordinate $r/R$ for $LMC\,X-4$} \label{vel}
\end{figure}

From Fig.~\ref{vel} it is very clear that through out the stellar structure causality condition and Herrera's cracking condition holds simultaneously. So our model gives a stable configuration.

\subsection{Adiabatic Index}\label{subsec5.4}
For a Newtonian isotropic fluid sphere the condition for stability is given by $\Gamma>\frac{4}{3}$. For a relativistic isotropic sphere it changes and for an anisotropic general relativistic sphere $\Gamma$, known as adiabatic index, can be written as $\Gamma_r$ and
$\Gamma_t$~\cite{Bondi1964}.

For a relativistic anisotropic fluid sphere the stability condition is given by
\begin{eqnarray}
&\qquad \Gamma_r>\frac{4}{3}, \\
&\qquad \Gamma_t > \frac{4}{3}+\left[\frac{4(p_{t0}-p_{r0})}{3|p_{r0}^{'}r|}+\frac{8\pi r \rho_0 p_{r0}}{3|p_{r0}^{'}|}\right],\label{5.4.1}
\end{eqnarray}
where $p_{r0}$, $p_{t0}$ and $\rho_0$ are the initial radial pressure, tangential pressure and energy density in static equilibrium
satisfying TOV. The first and the last term inside the square bracket respectively the anisotropic and relativistic correction respectively.
These are being positive quantities, increases the unstable range of the adiabatic index~\cite{Herrera1979,Chan1993}. Using the above relation we shall get the following expressions from our model as
\begin{eqnarray}\label{5.4.2}
&\qquad\hspace{-7cm} \Gamma _{{r}}=\frac{\rho+{p_r}}{p_r}\frac{dp_r}{d\rho}, \nonumber \\
&\qquad\hspace{-0.8cm} ={\frac {96 \left( n-1 \right) B_{{g}} \left( n+ \frac{2}{3}
 \right) \pi {r}^{6n+6}+ \left( -12\,{n}^{2}-12n \right) {r}^{6
n+4}-4\rho_{{1}}}{288 \left( n+\frac{2}{3} \right) B_{{g}}\pi \left(
n+ \frac{1}{2} \right) {r}^{6n+6}+ \left( -9{n}^{2}-9\,n \right) {r}^{6n+
4}-3\rho_{{1}}}}, \nonumber \\ \\ \label{5.4.3}
&\qquad\hspace{-7cm} \Gamma _{{t}}=\frac{\rho+{p_t}}{p_t}\frac{dp_t}{d\rho}\nonumber \\
&\qquad\hspace{-0.2cm} ={\frac {2 \left( \Gamma _{{1}}-\frac{1}{2}v_{{3}}{R}^{6n
+4}+{n}^{2}{r}^{6n+4} \right)  \left[ \rho_{{1}} \left( n-1 \right)
{r}^{-\left(4+6n\right)}+\Gamma _{{2}}-64B_{{g}}\pi {r}^{2}-p_{{1}} \right]
}{3 \left( \Gamma _{{3}}+{r}^{6n+4}n \right)  \left( \rho_{{1}}
 \left( n+2 \right) {r}^{-\left(4+6n\right)}+\Gamma _{{4}} \right) }},  \nonumber \\
\end{eqnarray}
where \\
$\Gamma _{{1}}=\frac{1}{2} \left( v_{{1}}-v_{{2}} \right)  \left( n+2 \right) $,\\
 $\Gamma _{{2}}=-9{n}^{2}+ \left( -64B_{{g}}\pi {r}^{2}-9 \right)n$,\\ $\Gamma _{{3}}= \left( 18{n}^{3}+27{n}^{2}+9n \right) {R}^{6n+4}-v_{{1}}+v_{{2}}$,\\ $\Gamma _{{4}}=80{r}^{2} \left( n+2/5 \right) B_{{g}}\pi -p_{{1}}$.

\begin{figure}[!htp]
\centering
    \includegraphics[width=6cm]{adia}
 \caption{Variation of adiabatic index with the fractional radial coordinate $r/R$ for $LMC\,X-4$}\label{adia}
\end{figure}

To see the behaviour of the adiabatic index we have plotted $\Gamma_r$, $\Gamma_t$ with the fractional radial coordinate $\frac{r}{R}$ in Fig.~\ref{adia}. The figure shows that both $\Gamma_r,\Gamma_t > \frac{4}{3}$ everywhere within the stellar interior. This graphical representation indicates the stable model.

\section{Mass-radius relation and redshift}\label{sec6}
Buchdahl~\cite{Buchdahl1959} derived an upper limit for maximum allowed mass to radius ratio for a static spherically symmetric perfect fluid star, as $\frac{2M}{R}<\frac{8}{9}$. Later on Mak et al.~\cite{Mak2001} generalized it for a charged sphere. The mass of the star is given by
\begin{eqnarray}\label{6.1}
& \qquad m \left( r \right) =\frac{9r \left[ c_{{2}}{r}^{-\left(4+6n\right)}+{n}^{2}+ \left( \frac{16}{3}B_{{g}}\pi {r
}^{2}+1 \right) n+{\frac {32}{9}}B_{{g}}\pi {r}^{2} \right]}{18{n}^{2}+30n+12},\nonumber \\
\end{eqnarray}
where $c_{2}= \left( n+1 \right)  \left( n+ \frac{2}{3}\right) c_{1}$. This turns out to be $c_{2}= (7/4) c_{1}$ for our prescription of $n=1/2$. From Eq.~(\ref{4.6}) we immediately get the radius of the present compact star as $R = 4M$. This can be written in the form $2M/R=0.5$ which is well bellow the Buchdahl condition $2M/R<0.88$~\cite{Buchdahl1959} and thus provides the stability of the present model in terms of the mass-radius ratio.

Let us now define the compactification factor of the compact stellar system as
\begin{eqnarray}\label{6.2}
& \qquad u\left(r\right)=\frac{m}{r} =\frac{9 \left[ c_{{2}}{r}^{-\left(4+6n\right)}+{n}^{2}+ \left( \frac{16}{3}B_{{g}}\pi {r
}^{2}+1 \right) n+{\frac {32}{9}}B_{{g}}\pi {r}^{2} \right]}{18{n}^{2}+30n+12}.\nonumber \\
\end{eqnarray}

Therefore the gravitational redshift is defined as
\begin{equation}\label{6.3}
\qquad Z=(1-2u)^{-\frac{1}{2}}-1.
\end{equation}

\begin{figure}[!htp]
\centering
    \includegraphics[width=6cm]{compact}
    \includegraphics[width=6cm]{redshift}
               \caption{Variation of compactification factor (left panel) and redshift (right panel) with the fractional radial coordinate $r/R$ for $LMC\,X-4$} \label{redshift}
\end{figure}

Fig.~\ref{redshift} shows that the compactification factor increases non-linearly with the fractional radial coordinate and it satisfied Buchdahl limit. Also, the variation of redshift with respect to the fractional radial coordinate is featured in Fig.~\ref{redshift}.

\section{Discussion and conclusion}\label{sec7}
In this paper we have studied different features of a strange star through Tolman $V$ metric potential. With this potential and MIT bag EOS we have presented many interesting physical features of the strange stars and featured variation of the different physical parameters with the radial coordinate graphically.

However, the most important result of the present model is that with the help of this model we can predict exact values of radius of the different strange stars and bag constant, which are featured in Table~\ref{Table1}. We find from this table that the surface density of different stars are much higher than the normal nuclear density $2.3\times{{10}^{14}}$~$gm/{cm}^3$ and such high density confirms the presence of quark matter inside the discussed stars. Also, we have derived a wide range of values of the bag constant. It have been shown by some authors~\cite{Farhi1984,Alcock1986} that the bag constant should be $55-75 Mev/(fm)^3$. But recent experimental results of CERN-SPS and RHIC confirms the possibility of a wide range of values of the bag constant. This is possible for a density dependent bag model~\cite{Burgio2002}. From the table it is very clear that the value of the bag constant increases with the increasing values of the density of the stellar systems. A density dependent bag constant have employed by Bordbar et al.~\cite{Bordbar2012} to model magnetized strange quark stars and obtained similar results as in the present model.

\begin{table}[!htp]
	\centering
\caption{Predicted Physical parameters where $1~{{M}_{\odot}}$=1.475~km for $G=c=1$. The complete data set is valid for $n=\frac{1}{2}$}\resizebox{\columnwidth}{!}{
\begin{tabular}{cccccccccccc}
 \hline Strange & Observed  & Predicted & \hspace{0.5cm}${\rho}_{s}$  & \hspace{0.3cm}${{B_g}}$  \\
Stars  & Mass $({{M}_{\odot}})$ & Radius (km) & (${gm/cm}^3$) & \hspace{-0.2cm}($MeV/{fm}^3$) \\
\hline $PSR~J~1614-2230$ & $1.97 \pm 0.04$ \cite{Demorest2010} & $11.623 \pm 0.236$  & $2.546 \times {10}^{14} $ & $ 35.704$\\
\hline $Vela~X-1$  & $1.77 \pm 0.08$\cite{Dey2013} &  $10.443 \pm 0.472$  & $ 3.152 \times 10^{14} $ & $44.204$\\
\hline $PSR~J~1903+327$ & $1.667 \pm 0.021$\cite{Dey2013} &  $ 9.835 \pm 0.120$ & $3.556 \times 10^{14}$ & $49.872$  \\
\hline $Cen~X-3$ & $1.49 \pm 0.08$\cite{Dey2013} &  $8.791 \pm 0.472$ & $4.459 \times 10^{14}$ & $62.528$  \\
\hline $LMC~X-4$ & $1.29 \pm 0.05$\cite{Dey2013} &  $7.611 \pm 0.292$ & $5.954 \times 10^{14}$ & $83.497$  \\
\hline $4U~1538-52$ & $0.87 \pm 0.07$\cite{Dey2013} &  $5.133 \pm 0.412$ & $13.08 \times 10^{14}$ & $183.429$  \\
\hline $SMC~X-1$ & $1.04 \pm 0.09$ \cite{Dey2013} &  $6.136 \pm 0.532$ & $9.146 \times 10^{14}$ & $128.268$  \\
\hline $Her~X-1$ & $0.85 \pm 0.15$\cite{Dey2013} &  $5.015 \pm 0.884$ & $13.70 \times 10^{14}$ & $192.119$  \\
\hline $4U~1820-30$ & $1.58 \pm 0.06$\cite{Guver2010b} &  $9.322 \pm 0.356$ & $3.960 \times 10^{14}$ & $55.539$\\
\hline $4U~1608-52$ & $1.74 \pm 0.14$\cite{Guver2010a} &  $10.266 \pm 0.828$ & $3.260 \times 10^{14}$ & $45.716$\\
\hline \label{Table1}
\end{tabular}}
\end{table}

Some other salient features from our study can be discussed as follows:

(i) We have studied our model for different values of $n$ as $n=1/2$, $n=3/5$, $n=4/5$ and $1$ but we find  physically valid solution for $n=1/2$ only which is the same as assumed by Tolman~\cite{Tolman1939}.

(ii) We know that for a physically acceptable stellar model the metric potentials should be free from singularities inside the stellar structure. Our model satisfies this condition as at the centre metric potentials are giving finite values as ${e^{\nu}|_{r=0}}=0$  and ${e^{\lambda}}|_{r=0}>1$.

(iii) Though the parameters, like density and pressures, are singular at the origin, but if we take the ratio of the density with radial and tangential pressure separately, the singularity does not appear at the limit $r \rightarrow 0$. In this case we can have a linear relation between the pressures  with the density  at the centre as $ p_r=\rho$. Moreover, this is not geometrical singularity as the metric potentials are finite at the center. So the main reason of appearing the singularity is that the EOS is inadequate at the center. The highly ultra dense fluid at the center is not even compatible with the MIT bag EOS. Hence this issue can be resolved considering a core at the center of the stellar system where fluid distribution follows different EOS, for example $p_r=\rho$, a stiff fluid EOS as discussed earlier. The variation of the EOS parameters  are shown in Fig~\ref{eos}.

(iv) Through out the stellar distribution anisotropic force is positive (i.e., $p_t>p_r$) which helps to construct a more massive stellar structure.

(v) Our model satisfies all the energy conditions. The graphical representation of TOV equation shows that the stellar structure is in equilibrium under gravitational, anisotropic and hydrostatic forces. For our model causality condition and Herrera's cracking condition holds simultaneously representing a stable configuration. Also variation of adiabatic index is in expected region.

(vi) In the present study we have opted for the value of $n=1/2$ as other values do not yield physically viable results. Therefore, from Eq.~(\ref{4.6}) we get the radius of the present compact star as $R = 4M$. This can be written in the form $2M/R=0.5$ which fulfils the Buchdahl condition $2M/R<0.88$~\cite{Buchdahl1959} in connection to the mass-radius relationship. For the ultradense strange star $LMC~X-4$ we find the value of compactness as $0.25$ which also satisfies the Buchdahl limit. The surface redshift in this case is $0.41$.

Overall, by using Tolman $V$ metric potential we have represented a stable anisotropic and compact stellar configuration which satisfies all the physical conditions and gives exact numerical values of some of the physical parameters.

\section*{Acknowledgments}
SR is thankful to the authority of the Inter-University Centre for Astronomy and Astrophysics, Pune, India and Institute of
Mathematical Sciences, Chennai, India for providing Visiting Associateship under which a part of this work was carried out.
DS is also grateful to the authority of IUCAA for the hospitality during the visit.

redpajama_set_name: RedPajamaArXiv


Hey there PCPP! Here's my 5th build and the first one I've felt comfortable posting here. There's probably a lot to improve, but for now it works well.
Building this was a dizzying mix of extreme frustration, stress, and relief. Originally, I started with a Gskill 16 GB DDR4 3200 kit which was not on the QVL list, but was Samsung B-die. The board refused to post, and continued to not post even after each dimm was cycled through the 4 slots on the board. This was before I had the case and I had the board on a cardboard box. I then tried resetting CMOS and doing the same thing at least 4 times. After that, I tried resetting CMOS, reseating the CPU, and cycling the RAM through. Still no POST. I then added moving the GPU to the mix. Again, no POST. Eventually, I realized the board was throwing a keyboard error and storage error, so I plugged in a keyboard and my SSD. The board still refused to POST. Finally, I disassembled everything and reassembled it, repeating the process above with a keyboard and SSD plugged in. It refused to POST, again. Cables were checked and re-checked, and everything was connected correctly. A couple months later, I get the RAM kit you see in the list now, which was on the QVL list. It refused to POST, even after repeating the full troubleshooting process. I asked around and nobody knew what the problem was. I eventually gave up, until my friend came over a week later to diagnose issues and complete the build. We moved the test build into another room and set the motherboard on a cutting board. Miraculously, it managed to post for no apparent reason. And from there, the build began.
The Thermaltake View 71 TG was a great case to build in. Lots of room and great aesthetic. My only problem is it's extremely heavy, so portability is not in the cards for this PC. But no matter, my next build should fix that problem.
This build was meant to conquer video editing, 1440p gaming, and streaming. It's done well so far, and I have yet to work out how to make the AIO work just right. After that gets fixed, I should be able to attempt overclocks. RAM is stable at 3200 MHz XMP.
Overall, I'm happy with the build so far and can't wait to make improvements.
Edit 8/7/18: Been having a lot of fun with Ryzen Master and Afterburner. CPU is stable at 4.2 GHz (1.3625 volts) on all cores and GPU is stable at 2088 MHz on the core and 5090 on the memory. Scores have been great so far.
Great value and great performance. Shreds any game and video editing project I throw at it.
Great value and great performance. Has kept CPU cool so far, but not the easiest to figure out.
This board is great, but in my experience it has been frustratingly inconsistent. Buy at your own risk.
Great value and great performance. Have not been able to get up to 3466 just yet, but sitting comfortably at 3200 MHz.
240 GB of solid state for $50? Yes please.
Not worth the extra price you'd normally pay for it, but like most WD drives has been fast and dependable.
Good for the price, but has been a little inconsistent. Originally didn't detect, but after messing with it for a while it started to work ok.
Pushes insane frame rates at 1440p Ultra and was definitely worth the money. I for sure don't regret selling my 1070.
Case is extremely heavy, but worth the price and extra heft. It's just gorgeous, with tempered glass all around and RGB fans. Lots of room for AIOs and stuff as well. Highly recommend it.
Good price and lots of flexibility. Love this PSU so far.
It's not an IPS display, but has worked great so far. Experience has been very smooth and visuals have been awesome.
A little bit on the expensive side in my opinion as it's just the Strafe with RGB LEDs, but other than that it's very well made and Cherry MX Red speaks for itself.
Love the customization available with this thing. Very comfortable and love the weights.
Not too bad, but it's fairly evident that this was meant to be a budget product. The mic is not very good and the headset feels cheap, but the audio is fairly good.
Thanks! Overclocks don't like to stick, and weird errors occasionally happen. It also took me 3 months of on and off troubleshooting before it magically POSTed out of nowhere.
Thanks for the answer. Are you on the latest BIOS?
As far as I know I am. I'll have to check when I get a chance, but I know I at least updated the bios once or twice since I built it.
After reading your review on the MB, I'm on the fence about buying it. After the initial issues with posting, have you had any major problems with it? I'm deciding between downgrading my card to a 1070ti and upgrading the board to the crosshair Hero because of it. Do you think it would be worth it to stay with the board?
I think it just might be an AsRock thing. Their boards can be very finicky. It's really up to you. I don't like Asus' customer service, so you best hope that if you go to the Hero, it works without any issues. They're both pretty good boards, I would just be wary and do a massive amount of research into the Ultimate before buying.
It has been a great mouse for me. Takes some getting used to but still a great mouse, and you can add weight to it.


text:
the world classic pictures
Viva la France! Stephan Cohen Shocks World as the New Predator World 14.1 Champion
photos courtesy Jerry Tarantola
Cohen made history as France's first World Pool Champion Stephan's Cohen name will be inscribed as the 69th Champion of the World 14.1 Tournament
Ortmann #1 : USA's Deuel & Williams Surprise Top Seeds at Predator World 14.1 Championship
photo courtesy Jerry Tarantola
Deuel will enter the next stage of the event as #2 seed, and the top seeded American
Parsippany, New Jersey- Oliver Ortmann's dominance of Group 2 has been unparelled compared to the previous years of the Predator World 14.1 as he utterly blitzkreiged his opponents. Ortmann held all of his opponents to 10 points or less, with two matches where he ran perfect 100's . Surprisingly is USA's Corey Deuel and Charlie Williams who not only went undefeated in their groups, but edged out the Europeans to take the #2 and #3 spots in the stage 2 cut of the Predator 69th World 14.1 Championship presented by Ozone Billiards. The Dragon Promotions revived event is in its 4th consecutive year alive with help of industry giants such as Predator, Ozone Billiards, Brunswick Billiards, Simonis Cloth, Master Chalk, Aramith Balls, Accu-Stats and the Laser Rack. Comet Billiards will host this year's event which will start play on August 24, 2009 and end August 29. The greatest straight pool players from around the world will arrive on USA's east coast again to New Jersey, and attend this prestigious event to play for the coveted title of World Straight Pool Champion.
3Cushion / Features
2009 USBA TOUR Dion Nelin From Denmark Wins the Carom Cafe International Open
Preliminaries: 5 groups of 8 players each/round robin/25 points
Top 4 from each group advance to the semi-finals (20 players)
2 auction & 2 lottery winners = 24 players
Semi-Finals: 3 groups of 8 players each/round robin/30 points
Top 4 from each group advance to Finals (12 players)
Finals: 2 groups of 6 players each/round robin/40 points
Top 2 finishers from each group advance to the final matches: single elimination to 40 points to determine 1st through 4th place.
Women & Americans at Predator World Straight Pool Championship: Complete Schedule
The players of the 69th World Straight Pool Tournament- photo courtesy Tom Flowers
Parsippany, New Jersey- Day 1 is in the books of the 69th World 14.1 Championship. Of course the favorites, the Europeans, made it through relatively easy, such as Hohmann's 92 and out against Jonathan Smith,Ortmann's dominating play over Steve Lipsky, and France's Stefan Cohen's 91 and out against Earl Herring. But the USA is looking good and so are the ladies,as they made their niches, too. The Predator World Straight Pool Championship is presented by Ozone Billiards. The Dragon Promotions revived event is in its 4th consecutive year alive with help of industry giants such as Predator, Ozone Billiards, Brunswick Billiards, Simonis Cloth, Master Chalk, Aramith Balls, Accu-Stats and the Laser Rack. Comet Billiards will host this year's event which will start play on August 24, 2009 and end August 29. The greatest straight pool players from around the world will arrive on USA's east coast again to New Jersey, and attend this prestigious event to play for the coveted title of World Straight Pool Champion
Galveston World Classic Reaches Agreement with Versus
(Houston TX, August 21)—Taylor Road Productions today announced five one-hour shows featuring the Galveston World Classic billiards tournament will air on VERSUS, the nation's fastest growing sports cable network now in more than 75 million homes, beginning Wednesday, November 11, at 6 p.m. ET.
The tournament, which will take place September 11-20 at Moody Gardens in Galveston, Texas, brings together top billiard professionals and thousands of amateur players as they compete in eleven events for a chance to win $1,000,000 in prizes. Top professional players who will be competing include Efren Reyes, Earl Strickland, Francisco Bustamante, Johnny Archer, Nick Varner, Jeremy Jones, Gabe Owen and Charlie Bryant.
Features / Press Releases
U.S Bar Table Championships Adds New Divisions
Entering its 17th year, The U.S Bar Table Championships is expanding. The popular and long standing $24,500 added event is including two new divisions starting with the February 22-28, 2010 tournament.
Produced by CueSports International (CSI) and hosted by the Terrible's Sands Regency Hotel & Casino in Reno, Nevada the always competitive tournament has traditionally featured three divisions: open 8-Ball, open 9-Ball and open 10-Ball. A special cash "All Around" bonus is awarded every year to the top three men and women shooters who enter all three open events.
Accu-Stats Live Coverage of Predator World Straight Pool Championship! Groups Announced
Parsippany, New Jersey- For the first time ever, Accu-Stats will be filming the 69th Predator World 14.1 Championship! Now fans from around the world can watch the biggest and best straight pool event in the world live online and also keep to own forever on DVDs. The Predator World Straight Pool Championship is presented by Ozone Billiards. The Dragon Promotions revived event is in its 4th consecutive year alive with help of industry giants such as Predator, Ozone Billiards, Brunswick Billiards, Simonis Cloth, Master Chalk, Aramith Balls, Accu-Stats and the Laser Rack. Comet Billiards will host this year's event which will start play on August 24, 2009 and end August 29. The greatest straight pool players from around the world will arrive on USA's east coast again to New Jersey, and attend this prestigious event to play for the coveted title of World Straight Pool Champion.
Advance tickets are now on sale online for the 2009 Billiard Congress of America Hall of Fame Banquet,
Advance tickets are now on sale online for the 2009 Billiard Congress of America Hall of Fame Banquet, the United States Billiard Media Association (USBMA) announced today. The dinner banquet, at which pool greats Johnny Archer and Allison Fisher will be formally inducted into the BCA Hall of Fame, will take place Thursday, Oct. 22, at the Marriott Chesapeake Hotel, Chesapeake, Va., in conjunction with the 2009 U.S. Open 9-Ball Championships.
The banquet, honoring Archer and Fisher as the 54th and 55th inductees into the sport's hallowed shrine, will also be attended by previous inductees and will feature testimonials celebrating the pair's illustrious careers. Cocktails (cash bar) will be served from 5:00 pm – 6:00 pm, with dinner and the formal induction ceremony running from 6:00pm – 7:45 pm.
Ortmann, Hohmann, & Immonen are Heavy Bids & Make Heavy Words about the Predator 69th World Straight Pool Championship
Ortmann Gunning for 2nd World 14.1 Championship
Parsippany, New Jersey- Europe's iron grip on straight pool this millennium doesn't seem easy to shake even this year with 2007 World 14.1 Champion Oliver Ortmann, 2006 World 14.1 Champion Thorsten Hohmann, and World #1 Mika Immonen all aiming for the crown. The Dragon Promotions revived event is in its 4th consecutive year alive with help of industry giants such as Predator, Ozone Billiards, Brunswick Billiards, Simonis Cloth, Master Chalk, Aramith Balls, Accu-Stats and the Laser Rack. Comet Billiards will host this year's event which will start play on August 24, 2009 and end August 29. The greatest straight pool players from around the world will arrive on USA's east coast again to New Jersey, and attend this prestigious event to play for the coveted title of World Straight Pool Champion.
Premiere Brand Integration Firm, Brand In Entertainment, Gets In "Pool, Poker and Pains" Corner
Premiere Brand Integration Firm, Brand In Entertainment, Gets In "Pool, Poker and Pain's" Corner Los Angeles CA, August 20th, 2009: Premier LA-based brand integration firm,...
Mike Dechaine Wins New England 9 ball Series Season Finale
At Busters Billiards in Somersworth NH.
Story by Marc Dionne
64 players come out from all of New England for a chance at the $ 5,100.00 in prize money. The format was Race to your handicap: (D Level Players Race to 4) (C Level Players race to 5) (B Level Players race to 6) (A Level player's race to 7) (Open Level player players race to 8) (Pro players race to 10.)
The tournament had 16 players from each Level group, The Tournament Director Marc Dionne was Very happy about this. Here is a list of the Notables that attended. Mike Dechaine, Nelson Olivera, Luis Rios, Jay Hutchins, Nick Kafalas, PJ Kafalas, Kevin Guimond, Roy Morgridge, Harry Nathan, Cletion Rocha, Tim Perry,
Mike Barbagallo, Randy Labonte, Robert Lewis, Billy Lanna, Tom McGongale.
This was the strongest Tournament the tour has had to date.
Chicago,New York City, Philadelphia Qualifier Winners for the Predator 69th World Straight Pool Championship
Israel's Zion Zvi will be an interesting addition to the 2009 Predator World 14.1 Championship
Parsippany, New Jersey- Qualifier winners from Chicago, Philadelphia, and New York City will be heading to Parsippany, New Jersey for the 69th Annual Predator World 14.1 Championship presented by Ozone Billiards. Bob Chamberlain, Michael Frank, Jeffrey Mohl, Richard Michalec, Jonathan Smith, and Jude Rosenstock will go up against the world's best 14.1ers!
JORDANIAN CHAMPION ZAID THWEIB REINS IN "THE HILLBILLY" ON THE LONE STAR BILLIARDS TOUR!
The Lone Star Billiards Tour held its Bogies Houston Classic IV this weekend, August 15th-16th a whopping 90-player field! Saturday morning Bogies Billiards & Games was packed with talent including Louisiana's own Gary Abood and Derrick Fontenot, Mississippi's Jerry Slivka, and Texas' favorites Sylver Ochoa, Lanny Herrin, Dennis Strickland, Nick Hood, Rene Rendon and Billy Sharp. Pro Players included Charlie Bryant, Zaid Thweib, and Cliff Joyner.

redpajama_set_name: RedPajamaCommonCrawl


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text:
When something Dies…
I started the Ivie series last year when I got an opportunity to participate in a very elaborate and important cultural exhibition in the ancient city of Benin city Nigeria, which happens to be where I am from (both my parent are from Benin). So you can understand my excitement to be a part of this exhibition. Coincidentally, my twin sister was having her traditional wedding ceremony on the same day in Benin at our family home, so I couldn't be at the opening of the exhibition.
My Installation in Benin city, Igun street (home of bronze casting) Each measure 28x35.5cm
About Ivie…
I did include a short synopsis on my work which you can find here on its website but I think it is important for me to expand on the project here on my blog. It got me thinking recently and the project still continues to grow in my studio.
A few weeks ago, there was an incident here in Lagos about a kidnapping of 3 children by a nanny that was hired online story here. People went wild on social media about the irresponsibility of the parents but more specifically they blamed the mother, which is the case most times when it comes to children, the woman takes the blame. So I have been thinking, did she deserve the backlash she got from Nigerians at that time?
How does Ivie relate to this…
Ivie means "beads" in the bini language and it is a symbolic and very important ornament both in the palace and among the people of Benin and even with many other cultures across Nigeria. Today one can rarely find real coral beads, because plastics have begun to replace them, but this isn't my point, but rather to show the huge interest in beads especially by brides, as it is a compulsory necessity for almost every traditional wedding bride, whether it is real or fake.
But my story begins from the palace…
Everyone knows the FESTAC 77 mask
This image in particular is of the Queen Idia pendant is from the book above by Barbara Plakensteiner (Editor), O.J. Eboreime (Foreword)
This pendant is representative of "Iyoba", meaning queen mother or the mother of the king. The story goes that Queen Idia the only woman believed to have gone to war in ancient Benin had helped her son Oba Esigie defend his throne and kingdom and as a form of gratitude, he created the second most important and powerful title in the Benin Kingdom the "Iyoba of Benin". She is the only one after the Oba that has her own palace, and her own attending chiefs. She is basically the second most important person in Benin city. To this day Iyoba Idia is still remembered especially because of the popularity of the pendant above and yes the title still exists today and is still is just as important and as powerful.
Just before this project I had met a woman priest through my mum (we didn't go for sacrifice oo, she is a family friend to my mum), I was pretty shocked to see her as women don't usually occupy such positions. She had her house and guards and her own throne and you must kneel to greet her.
Benin is not exactly a city where women are confirmed with such power and voice hence my later interest in the Iyoba title. The history of Benin is visible in its arts and it is quite obvious that women are absent in the sculptures of Benin not until the Iyoba title came about, then we started to see carvings of different queen mothers from different decades or centuries. Although at present the position has been empty and it may remain so even after a new king ascends the throne after the present king; long story! (I can address that another time).
Back to the Kidnapped kids…
Do women really belong at home? Iyoba Idia played this role too well hence her title. Should women work? What is the role of women in the 21st century?
In this Ivie project, the beads are symbolic of the title of "Woman", there is an absence or void left within the beads. It is a question, or an interest, a search for who will fill this title or position and how?
As we are confirmed with this title of "Woman", what is our role? What are our duties as daughters, mothers, wives, aunties, grandmothers etc.
It's a curiosity, I don't know if there's a right or wrong answer. The 21st century life is different and it may be unfair to compare Iyoba Idia with a 21st century woman but a woman is a woman and the genes remain.
My thoughts… Don't judge!
I like to think I'm old school and I am also Christian, so I PERSONALLY feel that (especially) when children are involved, a woman has an obligation and duty as a parent and as a mother to take care of her family and besides it's in our DNA to care and nurture and raise a child or children. Too many women have abandoned their "Woman" title, seeking other things and other titles. Priorities have become misplaced. As mothers, I think a child should be a priority and it isn't an impossible task to work and raise a child. Our mothers did it, at least mine did. She worked but she was home as well, never grew up with a nanny and my mum had 11 of us. Yes 11!! Oba Esigie's mother too, she was a warrior!
I have friends who do it and I know others who have made their families their priority and forsaken the white collar job. Are they wrong to do that? No.
Its a choice we must all make as women, but we must be aware of the consequences of our choices and be ready to face them.
As I make these markings with my pen that look like hair, I am imagining how I can fill this title as "Woman" and considering how much of it am I occupying at the moment.
The Ivie series will continue to pose such questions about the 21st century woman in Africa.
← Artist Talk	When something Dies… →
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Felipe Balbi March 20, 2014, 6:25 p.m.
> >>>>>try to acquire the same port lock again.
> >>>>>Looking at other line disciplines that looks like a bug in hci_ldisc.c.
> >>>>>wakeup the bottom half so we handle ->write() in another context ?
> >>>>>Is it legal to call tty->ops->write() from within ->write_wakeup() ?
> >>>you want this to be sorted out ?
> >>hci_uart_tx_wakeup() should perform the I/O as work.
> >>FWIW, this was reported by Huang Shijie back on Dec 6.
> >>I'd fix it but I have no way to test it.
> Where's the cancel_work_sync() on teardown?
the same port lock and we will deadlock.
> > >>>>>try to acquire the same port lock again.
> > >>>>>Looking at other line disciplines that looks like a bug in hci_ldisc.c.
> > >>>>>wakeup the bottom half so we handle ->write() in another context ?
> > >>>>>Is it legal to call tty->ops->write() from within ->write_wakeup() ?
> > >>>you want this to be sorted out ?
> > >>hci_uart_tx_wakeup() should perform the I/O as work.
> > >>FWIW, this was reported by Huang Shijie back on Dec 6.
> > >>I'd fix it but I have no way to test it.
> > Where's the cancel_work_sync() on teardown?
> the same port lock and we will deadlock.
>>>>>>> try to acquire the same port lock again.
>>>>>>> Looking at other line disciplines that looks like a bug in hci_ldisc.c.
>>>>>>> wakeup the bottom half so we handle ->write() in another context ?
>>>>>>> Is it legal to call tty->ops->write() from within ->write_wakeup() ?
>>>>> you want this to be sorted out ?
>>>> hci_uart_tx_wakeup() should perform the I/O as work.
>>>> FWIW, this was reported by Huang Shijie back on Dec 6.
>>>> I'd fix it but I have no way to test it.
>> Where's the cancel_work_sync() on teardown?
Thanks. Minor edits below but, strictly speaking, not necessary.
I know you found it independently but ?
> >>>>>>>try to acquire the same port lock again.
> >>>>>>>Looking at other line disciplines that looks like a bug in hci_ldisc.c.
> >>>>>>>wakeup the bottom half so we handle ->write() in another context ?
> >>>>>>>Is it legal to call tty->ops->write() from within ->write_wakeup() ?
> >>>>>you want this to be sorted out ?
> >>>>hci_uart_tx_wakeup() should perform the I/O as work.
> >>>>FWIW, this was reported by Huang Shijie back on Dec 6.
> >>>>I'd fix it but I have no way to test it.
> >>Where's the cancel_work_sync() on teardown?
> Thanks. Minor edits below but, strictly speaking, not necessary.
> >the same port lock and we will deadlock.
> I know you found it independently but ?
I will never add any *-by tags without seeing it in the mailing list.


Elastic yet durable, Cooley-Brite Lite is a lightweight, vinyl-coated polyester fabric that features excellent clarity in any backlit canopy, awning, or sign application. The white and eradicable colored substrates are easy to work with and simple to install.
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Nah champa!!! It's the only incense I will buy! I was introduced to it at the beginning of my travels and used it everywhere since, I only need to close my eyes when I light it up and I can take myself back to the most beautiful places I've been.


XDDD P-pirates! Ah, nothing exciting like that happened, besides the store owners who kept trying to call us over to buy food/whatnot.
Next year get a group of friends together a dress up like pirates. Then you can go around singing pirate songs. Makes it even funner!


text:
John Cotton Library at Rutgers University
Home » John Cotton Dana Library
John Cotton Dana Library – Newark, NJ
The John Cotton Dana Library is the physical and academic center of the Rutgers University – Newark campus. One of the guiding principles for the project was to promote easy access for faculty and students from the Student Center directly across the Norman Samuels Plaza. This first phase of the Library renewal creates a more welcoming, user-friendly facility by including an addition to the Library featuring a centralized stair and elevator tower, which allows for better access at each floor level. The addition infills between portions of the existing building to create light-filled spaces with a dynamic stair volume that extends out into the western quad.
A new elevator, stair, and library entry clad in Millennium Forms cupped metal tiles both inside and out creates a clear, unified, and comfortable way to access all building levels. The metal tiles were specified by Steinberg Hart, design architect for the project, for their visual impact, durability, and bold coloration in partnership with Clarke Caton Hintz, who served as the architect-of-record for the project. The burgundy mill LIC (light interference color) tiles bring in the Rutgers red branding and provide a wayfinding cue for students. The cupped profile of the tiles allows for beautiful shadow-play as the changing angle of the sun washes across the facade throughout the day. A visual counterpoint to the existing Library's precast concrete exterior, the exterior materials and forms serve as an accent on campus and within the building. While the curving curtainwall offers relief to the rectangular shapes of the existing building, the curve also echoes the elliptical wall in the newly renovated third floor of the Library.
Access into the Library from the tile-clad stair and elevator creates active, dynamic hubs at each level of the Library that connects users to seating areas and collections throughout the building. Small gathering spaces occur at the stair and elevator landings, encouraging impromptu meetings. The interior walls of the stair feature custom wallcovering with color-blocking that mimics the patterning of the metal tiles that enclose the exterior of the form. Overlooking the green plaza between the Dana Library and the Robeson Campus Center, the new addition provides expansive views to the outside and allows passersby to observe the life happening within the building.
Upon entering the third floor, the P3 Collaboratory for Pedagogy, Professional Development, and Publicly-Engaged Scholarship at Rutgers University-Newark is a dedicated space that brings together professors, Ph.D. candidates and graduate teaching assistants through the sharing of best practices. It provides mentoring to the next generation of scholars and encourages participation in publicly engaged scholarship. The desire for collaborative gathering and study spaces results in an open floor plan along the perimeter of the space, providing maximizing access to natural daylight. Flexible, easily configurable furniture allows groups to come together at the spur of the moment. Taking cues from the existing space with its concrete structural elements, the industrial ethos is retained by leaving infrastructure exposed, absorption added to the ceilings and walls ensures a suitable acoustic environment.
In contrast to the open space, program elements requiring enclosure such as office suites, meeting and consultation rooms for the P3 Collaboratory, Graduate School, and International Programming are located within a large ellipse. The elliptical wall, which defines the open floor plan from the partitioned spaces, is distinguished by its interactivity and connectivity. Integrated desking, benching, and seating allow users to directly interact with the wall and each other, while openings in the wall allow for visual porosity. The remaining floors of the Library will undergo a transformation in the next phase of renovation work, as the Dana Library responds to the 21st-century users' needs and expectations.
Architect-of-Record: Clarke Caton Hintz
Design Architect: Steinberg Hart
Product: Large Cupped Tile
Color/Finish: LIC Burgundy Mill
Photographer: Jeffrey Totaro Photography
By gcibon|2022-01-13T11:41:17-06:00January 13, 2022|0 Comments
By millenniumform|2021-12-20T15:18:03-06:00October 7, 2021|0 Comments
By gcibon|2022-01-13T11:41:17-06:00January 13, 2022|Project Spotlights|0 Comments
About the Author: gcibon


They also happen to be outstanding broadcasters.
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Model is hand-crafted from hard wood with planks on frame construction and painted as the color of the real ship. There is no plastic used and our model is fully assembled and ready for display. Model comes with a display case and a brass nameplate.
Built in 1939, MS Achille Lauro was a cruise ship based in Naples, Italy. In 1947 changed to MS Willem Ruys, a passenger liner for the Rotterdamsche Lloyd, it was hijacked by members of the Palestine Liberation Front in 1985.
In 1994, the ship caught fire and sank in the Indian Ocean off Somalia.
Ordered in 1938 to replace the aging ships on the Dutch East Indies route, her keel was laid in 1939 at De Schelde shipyard in Vlissingen, Netherlands, for Rotterdamsche Lloyd (now Nedlloyd). Interrupted by World War II and two bombing raids, the ship was finally launched in July 1946, as the Willem Ruys. The ship was named after the grandson of the founder of the Rotterdamsche Lloyd who was taken hostage and shot during the war.
Willem Ruys was completed in late 1947. At that time, the Rotterdamsche Lloyd had been granted a royal prefix in honor of its services during the war. Willem Ruys was 192 metres (630 ft) in length, 25 metres (82 ft) in beam, had a draught of 8.9 metres (29.2 ft), and measured 21,119 gross register tons. Eight Sulzer engines drove two propellers. She could accommodate 900 passengers. She featured a superstructure very different from other liners of that era; Willem Ruys pioneered low-slung aluminium lifeboats, within the upper-works' flanks. The next ship to adopt this unique arrangement was the SS Canberra in 1961. Today, all cruise ships follow this layout.
As Willem Ruys, the ship began her maiden voyage on December 5, 1947. Together with her main competitor and running mate, the MS Oranje of the Netherlands Line, she became a popular fixture on the Dutch East Indies route. However, when the East Indies gained independence from The Netherlands in 1949, passengers numbers decreased.
The former Prime Minister of Singapore, Lee Kuan Yew had traveled aboard the Willem Ruys as a fresh graduate upon completing his studies in the United Kingdom.
On January 6, 1953, Willem Ruys collided in the Red Sea with running mate MS Oranje, heading in the opposite direction. At that time, it was common for passenger ships to pass each other at close range to entertain their passengers. During the (later heavily criticized) abrupt and fast approach of Oranje, Willem Ruys made an unexpected swing to the left, resulting in a collision. It was a near-miss disaster. Oranje badly damaged her bows. Due to the possibility that she would be impounded for safety reasons, she was unable to call at Colombo as scheduled, and went directly to Jakarta. Willem Ruys suffered less damage. There was no loss of life involved. Later, it was determined that miscommunication on both ships had caused the collision.
During 1957, the English diplomat, author and diarist Harold Nicholson, together with his wife, the author and poet, Vita Sackville-West toured the Far East for two months aboard the Willem Ruys. The voyage is fully documented in his published journal of the trip "Journey to Java" which provides a detailed account of First class travel on the vessel in the 1950s.
After repairs, Royal Rotterdam Lloyd decided to release the Willem Ruys on the North Atlantic run. First, she was placed on the New York service, and later Canada was included.
In 1958, the Royal Rotterdamsche Lloyd and the Netherlands Line signed a co-operative agreement to create a round-the-world passenger service. The joint fleet would sail under the banner of "The Royal Dutch Mail Ships". Together with the Oranje and the Johan van Oldenbarneveldt, the Willem Ruys underwent an extensive refit to prepare her for this new service. She made two charter trips to Montreal for the Europa-Canada service. Then, from September 20, 1958, until February 25, 1959, she underwent a major facelift at the Wilton-Fijenoord shipyard in Amsterdam, turning her from a passenger liner into a cruise ship. Her original four class distinctions became First and Tourist Class. A hundred new cabins were installed and air-conditioning was extended throughout all accommodations. The Javanese crew members were replaced by Europeans, who required upgraded crew accommodation. Externally, she was fitted with a new glazed in Tourist Class Wintergarden, her forward funnel was heightened and stabilizers were fitted. Willem Ruys was now able to accommodate 275 first class, and 770 tourist class passengers, although there were many interchangeable cabins which had additional berths fitted, which could increase the maximum passenger number to 1167. Her new specifications would see her tonnage increase from 21,119 to 23,114 gross register ton.
On March 7, 1959, Willem Ruys went off on her new world service to Australia and New Zealand. She departed from Rotterdam, sailing via Southampton, the Mediterranean, the Suez Canal, Fremantle, Melbourne, Sydney, New Zealand, returning via the Panama Canal. The Royal Dutch Mail Ships (Willem Ruys, Johan van Oldenbarnevelt and Oranje) became a popular alternative to the British liners.
At the end of 1964, due to a strong drop in passenger numbers, Willem Ruys was laid up in Rotterdam and put up for sale.
In 1965, she was sold to the Flotta Lauro Line, or Star Lauro, (now MSC Cruises) and renamed the Achille Lauro (after the company owner). Extensively rebuilt and modernized after an August 1965 onboard explosion, the Achille Lauro entered service in 1966 carrying passengers to Sydney, Australia. The ship played a role in evacuating the families of British servicemen caught up in the unrest in Aden, and then made one of the last northbound transits through the Suez Canal prior to its closure during the Six Day War.
The Achille Lauro was converted to a cruise ship in early 1972, during which time she suffered a disastrous fire. A 1975 collision with the cargo ship Youseff resulted in the sinking of the latter, and another onboard fire in 1981 took her out of service for a time. She was laid up in Tenerife when Lauro Lines went bankrupt in 1982. The Chandris Line took possession of her under a charter arrangement in 1985, shortly before the hijacking.
On October 7, 1985, four members of the Palestine Liberation Front (PLF) took control of the liner off Egypt as she was sailing from Alexandria to Port Said. Holding the passengers and crew hostage, they directed the vessel to sail to Tartus, Syria, and demanded the release of 50 Palestinians then in Israeli prisons. After being refused permission to dock at Tartus, the hijackers killed disabled Jewish-American passenger Leon Klinghoffer and then threw his body overboard.
The ship then headed back towards Port Said, and after two days of negotiations, the hijackers agreed to abandon the liner in exchange for safe conduct and were flown towards Tunisia aboard an Egyptian commercial airliner. This plane, however, was intercepted by US fighter aircraft and directed to land in Sicily, where the hijackers were arrested and later tried for murder.
The ship continued in service; she was reflagged in 1987 when the Lauro Line was taken over by the Mediterranean Shipping Company to become StarLauro. On November 30, 1994, she caught fire off the coast of Somalia while en route to South Africa. At that time, the cause of the fire was suggested by Italian officials to be a discarded cigarette. In reality, the fire started in the engine room with the explosion of one of the engines; due to the lack of supervision, the fire burned out of control before discovery. The crew attempted to battle the fire for several hours but were unsuccessful. Abandoned, the vessel sank on December 2, 1994.


Strollo PJ Jr, Gillespie MB, Soose RJ, Maurer JT, de Vries N, Cornelius J, Hanson RD, Padhya TA, Steward DL, Woodson BT, Verbraecken J, Vanderveken OM, Goetting MG, Feldman N, Chabolle F, Badr MS, Randerath W, Strohl KP; Stimulation Therapy for Apnea Reduction (STAR) Trial Group. Upper airway stimulation for obstructive sleep apnea: durability of the treatment effect at 18 months. Sleep. 2015 Oct 1;38(10):1593-8. doi: 10.5665/sleep.5054.
Kent DT, Rogers R, Soose RJ. Drug-induced sedation endoscopy in the evaluation of OSA patients with incomplete oral appliance therapy response. Otolaryngol Head and Neck Surg 2015; Aug;153(2):302-7.
Dedhia RC, Strollo PJ, Soose RJ. Upper airway stimulation therapy: past, present, and future. Sleep 2015; Jun;38(6):899-906.
Woodson BT, Gillespie MB, Soose RJ, Maurer JT, de Vries N, Steward DL, Baskin JZ, Padhya TA, Lin HS, Mickelson S, Badr SM, Strohl KP, Strollo PJ Jr; STAR Trial Investigators. Randomized controlled withdrawal study of upper airway stimulation on OSA: short-term and long-term effect. Otolaryngol Head Neck Surg 2014; Nov;151(5):880-7.
Stapleton AL, Chang YF, Soose RJ, Gillman GS. The impact of nasal surgery on sleep quality: a prospective outcomes study. Otolaryngol Head Neck Surg 2014; Nov;151(5):868-73.
Strollo PJ, Soose RJ, Maurer JT, de Vries N, Cornelius J, Froymovich O, Hanson RD, Padhya TA, Steward DL, Gillespie MB, Woodson BT, Van de Heyning PH, Goetting MG, Vanderveken OM, Feldman N, Knaack L, Strohl KP; STAR Trial Group. Upper airway stimulation for obstructive sleep apnea. N Engl J Med 2014; Jan;370:139-49.
Dedhia R, Rosen CA, Soose RJ. What is the role of the larynx in adult obstructive sleep apnea? Laryngoscope; 2014; Apr;124:1029-34.
View Dr. Soose's most current publications.
Dr. Soose is the Director of the UPMC Division of Sleep Medicine and Upper Airway Surgery and Assistant Professor in the Department of Otolaryngology at the University of Pittsburgh School of Medicine. He earned his undergraduate degree from the University of Notre Dame and completed medical and surgical training at UPMC.
Board-certified in both otolaryngology and sleep medicine, Dr. Soose specializes in the medical and surgical treatment of snoring and obstructive sleep apnea. He is an appointed member of the Sleep Disorders Committee of the American Academy of Otolaryngology – Head & Neck Surgery (AAO-HNS), and is an active member of the American Academy of Sleep Medicine (AASM) and the International Surgical Sleep Society (ISSS). Dr. Soose has a special interest in sedated endoscopy and neurostimulation therapy in the management of patients with sleep apnea.


The Roadie DAX inflates high pressure road tyres fast. Dual-Action (DA) doubles volume by inflating on both the push and pull strokes. Integrated dust cap keeps pump head clean and thumb lock lever insures air-tight seal.


Pour all ingredients in bottle. Shake well. Take a sip and swish in mouth for at least 20 seconds, then spit it out. It is recommended to not swallow the mouthwash. You can add a few more drops of essential oils for a heavier scent and concentrated blend. I get my essential oils from Mountain Rose Herbs. They truly have high quality organic ingredients. You should only use organic or 100% high grade and pure essential oils.
Have you tried making mouthwash before? Which essentials oils you like using that blends well together?


Hi I am Sol Hi guys I work part time as a waitress and own a dog. I recently became single and joined arousr In my spare time I like texting. I am ready to share some dirty little fantasies if you are.
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April 7, 2019, 9:41 a.m.
Sol is so Amazing!! She's the Best!!
April 3, 2019, 10:53 a.m.
March 15, 2019, 6:31 p.m.
Sol is the Best!! A Rockstar!!
March 12, 2019, 8:20 a.m.
Feb. 18, 2019, 9:20 a.m.
Sol is amazing!! She always knows exactly what you need!!
Dec. 13, 2018, 11:11 a.m.
Nov. 25, 2018, 11:54 a.m.


text:
Definition from Wiktionary, the free dictionary
1.1 Etymology
1.2 Pronunciation
1.3 Proper noun
English[edit]
From earlier Ossingsing, named for the nearby Sing Sing Kill, borrowed from Dutch Sintsing, Sintsinck, from Munsee *ăsúnchung (*ăsə́nčəng), *ăshúnshung (*ăšə́nšəng, "at the small stone"), ăsún (ăsə́n, "stone") + -ush (-əš, diminutive suffix) + -ung (-əng, locative suffix), from Proto-Algonquian *aʔsenya. The prison located on the site retains the older form of the name, Sing Sing.[1][2][3][4]
Pronunciation[edit]
IPA(key): /ˈɒsɨnɪŋ/
Proper noun[edit]
English Wikipedia has an article on:
A town in Westchester County, New York State.
A village, within this town; the site of Sing Sing prison.
^ John Thomas Scharf, History of Westchester County, New York, voume 2 (1886)
^ 1846 March 14, An Act to confirm the election and official acts of the town officers of the town of Ossinsing in the county of Westchester, and for other purposes, section 5, published in the compiled Laws of the State of New-York, passed at the Sixty-Ninth Session of the Legislature (1846; C van Benthuysen and Co., Albany, NY): "The name of the said town of Ossinsing is hereby changed to "Ossining," by which name the same shall hereafter be known and designated."
^ Henry Townsend Smith, Manual of Westchester County: Past and Present, volume 3, page 180 (1913)
^ Alanson B. Skinner, The pre-Iroquoian Algonkian Indians of central and western New York, in Indian notes and monographs, volume 2 (1919–1920)
Retrieved from "https://en.wiktionary.org/w/index.php?title=Ossining&oldid=51248305"
English terms borrowed from Dutch
English terms derived from Dutch
English terms derived from Munsee
English terms derived from Proto-Algonquian
English 3-syllable words
English terms with IPA pronunciation
English lemmas
English proper nouns
About Wiktionary


Indulging in Baja California's food scene is all the rage among adventurous foodies these days. But even with fewer concerns about violence in the region, and shorter wait times at the border thanks to additional traffic lanes, traveling to another country for an afternoon of culinary delights isn't for everyone. And that's OK.
The beauty of living in San Diego is that you don't have to leave the country for authentic, regional Mexican cuisine. Case in point is Chula Vista, where you can dig into the best lamb barbacoa at Aqui es Texcoco; Guadalajara-style sandwiches from El Gallito Tortas Ahogadas; and of course Tacos el Gordo, whose TJ-style tacos are something of legend in San Diego.
But there's more. In recent weeks I've spent a lot of time (and calories) exploring the best of what Chula Vista has to offer, and my research brought me to the following three restaurants, and I highly recommend that you get to know them for yourself.
you get a bowl of plump, citrus-cured shrimp, garnished with orange slices, red onion, cucumber and avocado, with tostadas on the side for shoveling it all into your mouth. On a spicy scale of 1-10, the halfway point will make beads of sweat drip off your brow, so best cool down with a gigantic michelada - served in glassware akin to a beer stein - for only $4.50. Between the fast, friendly service, super-fresh seafood and almost-too-good-to-be-true pricing, eating here kind of feels like robbery, so tip generously and tell your amigos about this refreshing (on many levels) mariscos joint. 217 Third Ave., (619) 816-5042.
First, choose from stewed beef (res) or goat (chivo) at this Mexican comfort food eatery; then, decide on a presentation. You can get birrieria packed tacos, quesadillas and menudo here, but there's nothing quite like the ultra juicy, cheesy ahogada (or drowned) version of the quesadilla that comes stuffed with cheese, tender, smoky meat, beans, cilantro and onions. Then, flavorful consommé is spooned over the whole thing, making for a stew and quesadilla in one. Warning: after one visit here, you'll be hooked. 560 Broadway, (619) 934-5135.


text:
← Regency Ghost Story from Viscount Robert Stewart Castlereagh
Uppark, a National Trust Property, and Boyhood Home of H. G. Wells →
Charlecote Park, a National Trust Showplace
Posted on June 17, 2013 by reginajeffers
Charlecote Park is a grand 16th century country house, surrounded by its own deer park, on the banks of the River Avon near Wellesbourne, about 4 miles (6 km) east of Stratford-upon-Avon and 5.5 miles (9 km) south of Warwick, Warwickshire, England. It has been administered by the National Trust since 1946 and is open to the public. It is a Grade I listed building.
The Lucy family has owned the land since 1247. Charlecote Park was built in 1558 by Sir Thomas Lucy, and Queen Elizabeth I stayed in the room that is now the drawing room. Although the general outline of the Elizabethan house remains, nowadays it is in fact mostly Victorian. Successive generations of the Lucy family had modified Charlecote Park over the centuries, but in 1823, George Hammond Lucy (High Sheriff of Warwickshire in 1831) inherited the house and set about recreating the house in its original style.
In the middle of the 19th century the Fairfax Baronets inherited the property when the male line of the Lucy family failed on the death of Henry Spencer Lucy. The baronets changed their family name to Lucy to reflect the traditions of Charlecote.
The Great Hall has a barrel-vaulted ceiling made of plaster painted to look like timber and is a fine setting for the splendid collection of family portraits. Other rooms have richly coloured wallpaper, decorated plaster ceilings and wood panelling. There are magnificent pieces of furniture and fine works of art, including a contemporary painting of Queen Elizabeth I. The original two-storey Elizabethan gatehouse that guards the approach to the house remains unaltered.
Charlecote Park covers 185 acres (75 ha), backing on to the River Avon. William Shakespeare has been alleged to have poached rabbits and deer in the park as a young man and been brought before magistrates as a result. But it is unclear whether there were any deer in the park at that time. It was landscaped by Capability Brown in about 1760.
In the Tudor great hall, the 1680 painting Charlecote Park by Sir Godfrey Kneller, is said to be one of the earliest depictions of a black presence in the West Midlands. The painting, of Captain Thomas Lucy, shows a black boy in the background dressed in a blue livery coat and red stockings and wearing a gleaming, metal collar around his neck. The National Trust's Charlecote brochure describes the boy as a "black page boy." In 1735, a black child called Philip Lucy was baptised at Charlecote.
On display at the house is an original letter from Oliver Cromwell, dated 1654, summoning then owner Richard Lucy to the Barebone's Parliament. Also on display is a 1760 portrait of George Lucy by Thomas Gainsborough, which cost Lucy the sum of eight guineas.
A set of archives for the Lucy family at Charlecote is held by the National Archive. The house also has a display of carriages and a period laundry and brewroom.
In April 2012, Charlecote Park was featured as the venue for BBC1's Antiques Roadshow.
About reginajeffers
Regina Jeffers is the award-winning author of Austenesque, Regency and historical romantic suspense.
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This entry was posted in British history, buildings and structures, Georgian Era, Living in the Regency, real life tales, Regency era, Regency personalities and tagged Charlecote, Queen Elizabeth I, the National Trust, Warwickshire. Bookmark the permalink.
1 Response to Charlecote Park, a National Trust Showplace
carolcork says:
Regina, we used to live just north of Birmingham and frequently visited the historical country houses of Warwickshire including Charlecote Park. Warwickshire is rich in historical houses; Arbury Hall, Baddesley Clinton, Compton Verney House, Coughton Court, Farnborough Hall, Packwood House (one of my favourites), Upton House, Warwick Castle and Ragley Hall being the most famous ones.


Nelson Layag is a project director for CompassPoint. Nelson is responsible for the design and management of CompassPoint's public training program. In addition to leading the training program, he facilitates and teaches on topics including leadership and management, performance management, project management, and instructional design. Nelson's passion is working with staff and leaders of social change organizations. He appreciates and is motivated by the power individuals can have when they find a way to work effectively together as a team. He brings this excitement to his work in performance management, project management, and developing a training program that meets the needs of people working in the nonprofit sector.
As a student at Loyola University of Maryland, Nelson was instrumental in the early development of a campus volunteer center focused on social justice. A lifelong "islander," Nelson was born in the Philippines, grew up on Staten Island, and now lives in Alameda. He's a drummer in a garage band when he has spare time from being a father of three. He is on the steering committee for the nonprofit online magazine BlueAvocado. Nelson coaches youth football and basketball. He still sports the championship ring earned in 2000 when CompassPoint's team won the San Francisco Nonprofit Softball League title.
Customized In-house Trainings: Nelson regularly provides customized in-house training for nonprofit staff groups on a variety of topics, including coaching, performance management, and supervision. Recent organizations he has presented to include Catholic Charities Bay Area, Abode Services, and Mission Neighborhood Health Center.
CompassPoint Training Program: As training director at CompassPoint, Nelson is responsible for the management and instructional design of CompassPoint's workshops and learning programs. He has designed and co-written several of CompassPoint's workshop offerings including Supervision Parts 1 and 2. He also managed the Nonprofit Board Basics Online, a virtual learning center with instructional resources for nonprofit board members working in the corporate sector.
CompassPoint Nonprofit Conferences: Over the years, Nelson has designed and organized a variety of CompassPoint conferences—including Nonprofit Day—bringing nationally and internationally known speakers to CompassPoint's audience including Laura Van Dernoot Lipsky, Erica Williams, Kim Klein, Beth Kanter, and Jim Kouzes.
"My Reflections on Tuesday's Prop 8 Ruling"


This Mediterranean style home sits on 123 acres, perfect for the horse-lover and party-host.
Called Hummingbird Nest Ranch, the Los Angeles-area estate is currently listed for $49.5 million.
The house has six guest houses and 10 staff houses. The estate also has three equestrian arenas and two barns.
The largest house on the property is known as "The Sitting Bull Cottage." It alone is more than 3,000 square feet.
The main house is called "Sitting Bull"


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High-speed rail link to the North is wrong at every turn
Wednesday, 10 August, 2011
High-speed rail link to the North is wrong at every turn, Tories warn
A Conservative group says that Philip Hammond has abandoned the party's pre-election policy
The Transport Secretary's plans for a high-speed rail link from London to the Midlands and the North have been rubbished as "fundamentally flawed" by the Conservative Party's specialist transport group. The Conservative Transport Group says that the proposed link, known as HS2, is on the wrong route and ends up in the wrong places.
The group, a special-interest caucus of the party, has rejected almost all the details of the planned route. It has also criticised the political naivety of the proposals, given that the route travels through some of England's most beautiful countryside, represented in Parliament by a host of Conservative MPs and ministers.
The submission, a copy of which has been seen by The Times, says that the proposals will miss the chance to connect airline passengers, other rail users and motorists. It says that Heathrow — and not the previously unheralded Old Oak Common in Acton — should be the main London hub and interchange; that the link should follow the M40 through the Chilterns to minimise the environmental impact; and that the station arrangements in Birmingham should make Britain's second city not an HS2 terminal but a gateway to link the North to the Continent on trains that can pass on to HS1, the fast link from St Pancras to the Channel Tunnel.
"It is clear that, in broadly adopting the [last] Labour Government's proposals for HS2, the coalition has accepted a fundamentally flawed scheme that is the result of a similarly flawed brief," the submission states, adding that the proposals of Philip Hammond, the Transport Secretary, have abandoned pre-election Conservative policy.
It continued: "Only an HS2 alignment via a Heathrow interchange, located on the Great Western Main Line as close as possible to the airport, and providing direct connections between high-speed rail, classic rail, Crossrail, the motorway network and Heathrow, can provide the connectivity that the UK requires."
The group said the proposed route, which concentrated on the straightest line from London to Birmingham, took the link through the widest part of the Chiltern area of outstanding natural beauty. "It is difficult to imagine a more environmentally — and politically — destructive alignment for such a railway than that selected through the tranquil Misbourne Valley [in Buckinghamshire]," the submission states. It said that the proposals put forward "have been too obsessed with speed and benefit-to-cost ratio to take into account the political impact and acceptability of potential routes".
The comments came after the end of a consultation period on HS2. A final decision is expected at the end of the year. A spokesman for the Department for Transport said: "The Government believes a new high-speed rail network would present a once-in-a-lifetime opportunity to redraw Britain's economic map, bringing our major cities closer together and providing a rail network fit for the 21st century.
"Our proposals include a major new interchange station at Old Oak Common as part of the first phase of the project to provide direct connections between HS2, the Great Western Main Line, Heathrow Express and Crossrail — and subject to further consultation this would be followed in the second phase by the addition of a direct link to Heathrow.
"The Government is considering the responses to the consultation and will announce a decision on HS2 towards the end of the year."


Social outcasts and the unique are the subjects of Brooklyn photographer, Bruce Gilden. Using his camera to get up-close images, Gilden has snapped photographs in Coney Island and around the world which focus on people who are normally 'unphotographable.' Gilden has made these outcasts move inside as subjects of great art.
That's how Bruce Gilden describes his ever-developing photography style. Born in Brooklyn in 1946, the now 68-year-old artist is still exploring the people and places of the world, and presenting them to us in rich detail.
A local New Yorker, Gilden's most iconic images are those of the eclectic people that inhabit the city and surrounding areas. Not one to shy away from the odd and offbeat, Gilden began his career by photographing the crazy characters that we see every day. Up close and personal. His first collection comprised of those peculiar people that could be found out on Coney Island, during the 1960s.
The people he photographs are hardly models in the traditional sense. They are, however, amazing representations of the diversity of the human condition. Gilden's eye for these wonderful specimens is what started his career as an artist. His images can make you smile, laugh, gasp in surprise, or just stare in bewilderment. Everybody he photographs has a fascinating story. It's a great exercise for the viewer to try to decipher that story.
Gilden's signature simplicity derives itself from his basic equipment. Often armed with nothing more than a camera and a flashgun, Gilden is mobile and able to explore the wildest edges of the world. After beginning his career in New York, Gilden has since branched out across the globe. He's captured the decay of the once-great Detroit, the unpredictable and dangerous Yakuza mobsters of Japan, and the ferociously wild mobsters of rural Russia. Without Gilden's eye for the outliers, we would never get glimpses into these worlds.
Perhaps the most admirable quality about Bruce Gilden is his fearlessness. Not many would be comfortable on the same side of the street as some of his subjects, let alone being face-to- face. This is what makes his photographs so compelling. It allows the viewer, from a safe distance, to examine some of society's outsiders. The art gives us the opportunity to try to better understand those whom we might otherwise avoid or overlook. Gilden puts their humanity on full display.
Lucky for us Gilden has such fascinating friends. And because he has, we get to live with them, too.
Native Bostonian, philosophy major at Colgate University, and back-up vocalist/rhythm guitar player in an emerging Hootie and the Blowfish cover band, Tucker currently resides in Manhattan and is enjoying writing about his new city. He also enjoys light amounts of exercise, most appetizers, and Sunday night premium cable.