text:
\section{Introduction}
The study about physics beyond 4-dimensional spacetime has made great progress in recent decades, a lot of interesting physics was obtained from either the phenomenological aspects or theoretical implications, such as M theory \cite{Horava:1995qa,Horava:1996ma}, Anti de-Sitter space/conformal field theory correspondence \cite{Maldacena:1997re,Witten:1998qj} (i.e. AdS/CFT), and brane world scenario in which our universe is viewed as a 3+1 dimensional brane embedded in a higher dimensional spacetime \cite{Randall:1998uk,Randall:1999ee,Randall:1999vf}. Actually, the original concept of brane could be traced back to the work of Rubakov and Shaposhnikov \cite{Rubakov:1983bb,Rubakov:1983bz}, it was also developed to show that the fundamental gravitional scale could be close to Tev sacle by introducing large extra spatial dimension transverse to the brane \cite{ArkaniHamed:1998rs,Antoniadis:1998ig,ArkaniHamed:1998nn}. Compared to the previous ones, an important variant of barne world scenario involves warped compactification, this idea was first considered by RS-I model \cite{Randall:1999ee} in order to solve the gauge hierarchy problem, which introduced a 5-dimensional AdS compactified extra dimension between two Minkowski branes with a exponential warp factor in metric solution. For implementing localization of 4D graviton and reproducing Newton's law on the visible brane, RS-II model was proposed, which has a noncompactified extra dimension. From perspective of phenomenology, unlike the ADD model, these warped models have less striking signature at colliders or in astrophysical processes, and concomitantly being less constrained. In cosmological applications of brane world, RS-II model has been most successful model since it provided the capability of modifying the structure of Einstein's field equations \cite{Shiromizu:1999wj,Bostock:2003cv}.

For applying brane world to cosmology, a time dependent solution need to be constructed. There exist two physical scenarios, one focus on finding time dependent bulk geometry as cosmological solution \cite{Kaloper:1999sm,Kanti:1999sz,Flanagan:1999cu,Kanti:2018ozd}, another one consider a alternative case in which the bulk remains to be static but the brane acquires a velocity, while the observers on the brane will feel cosmological expansion or contraction as the brane moves \cite{Chamblin:1999ya,Kraus:1999it,Creek:2006je}. Actually, some enriched physical phenomena will be uncovered when considering the movement of brane in AdS spacetime. More interesting, if one considers the AdS black hole as bulk spacetime for a motional brane, the physics of black hole, brane universe and holography could be connected together naturally in this way. Under the situation of a motional brane in spacetime of AdS-Schwarzchild black hole, associating with the AdS/CFT correspondence and black hole thermodynamics, \cite{Savonije:2001nd} generalize the Cardy formula \cite{Cardy:1986ie} to the arbitrary-dimensional spacetime. Inspired by this work, the generalized Cardy formula (called by Cardy-Verlinde formula) have been checked in various black holes bulk with AdS asymptotics \cite{Klemm:2001db, Cai:2001jc, Birmingham:2001vd, Youm:2001yq, Cai:2001ja, Youm:2001qr, Jing:2002aq, Cai:2002bn, Lee:2008yqa, Nojiri:2000pi, Nojiri:2001fa, Nojiri:2002hz, Lidsey:2002ah, Nojiri:2002td, Nojiri:2002vu, BravoGaete:2017dso}. Besides, \cite{Kawai:2015lja} constructs a holographic reheating model by considering the movement of a probe brane in AdS-Vaidya spacetime, and the formation process of AdS black hole dual to the thermalization process of brane universe. Recently, through constructing a model of moving brane in AdS-Schwarzchild black hole, the holographic complexity growth in a FLRW universe is considered by \cite{An:2019opz}.

As the low-energy effective theory of supergravity and string \cite{Gibbons:1987ps}, dilaton gravitation theories have attracted many attentions in recent decades. Inspired by AdS/CFT, many works devote to finding the asymptotically AdS black hole solution in dilaton gravity with various self-interacting potential of dilaton. Particularly, it is of great interest to consider Liouville-type dilaton potential which is originated from the supersymmetry breaking of a higher-dimensional supergravity model \cite{Gregory:1992kr,Horne:1992bi,Poletti:1994ff}. And \cite{Poletti:1994ff,Mignemi:1991wa} has proved that in models of one and two Liouville-type potential, there doesn't exist the asymptotically flat or asymptotically AdS black hole solution. By combining three different Liouville-type dilaton potentials, \cite{Gao:2004tu,Gao:2004tv,Gao:2005xv} obtains the asymptotically AdS black hole solution in Einstein-Maxwell-Dilaton theory. Basing on this black hole solution, many interesting physical phenomenology have been explored, like the black hole thermodynamics \cite{Sheykhi:2009pf,Sheykhi:2016syb}, holographic thermalization \cite{Zhang:2015dia}, black hole phase transition in extend phase space \cite{ Li:2017kkj}, and domain wall cosmology \cite{Xu:2019abl}.

In this paper, our purpose is to consider the movement of brane in the charged AdS dilaton black hole solved by \cite{Gao:2004tv,Gao:2005xv} and the relevant holographic effects when brane approaches the AdS boundary. As showed in \cite{Sheykhi:2009pf,Li:2017kkj}, a rich phases structure of black hole thermodynamics could be uncovered when adjusting the dilaton coupling constant. Meanwhile, when considering the motion of domain wall in this charged AdS dilaton black hole, \cite{Xu:2019abl} also observes enriched evolution modes of domain wall universe as varying the value of dilaton coupling constant. Hence, it seems that there exists a connection between the thermodynamics of AdS dilaton black hole in bulk spacetime and the evolution of FLRW universe on brane/wall. Basing on the idea proposed in \cite{Savonije:2001nd}, namely associating the black hole thermodynamics with AdS/CFT correspondence, \cite{Cai:2001jc} obtains a modified Cardy-Verlinde formula for a CFT living in the boundary of AdS-RN black hole spacetime. In term of the AdS dilaton black hole \cite{Gao:2004tv,Gao:2005xv}, when we make the dilaton coupling constant $\alpha=0$, this solution will reduce to the AdS-RN one accordingly. Thus, when brane approaches the AdS boundary, we naturally expect to give a similiar Cardy-Verlinde formula on brane like the one obtained by \cite{Cai:2001jc} but with some corrections of dilaton coupling constant $\alpha$. Note that the matter field confined on brane is a general quantum field theory (QFT) without conformal symmetry \cite{Boonstra:1998mp,Behrndt:1999mk,Cvetic:2000pn}. And we need to involve an appropriate surface counterterm to restore the conformal symmetry when brane approaches the boundary of AdS dilaton black hole. Besides, although \cite{Xu:2019abl} have considered the movement of brane/wall in AdS dilaton black hole \cite{Gao:2004tv,Gao:2005xv}, they ignore the self-gravitating effects of brane/wall. Thus, in their case, the evolution of brane/wall is controlled by Israel junction condition \cite{Israel:1966rt} only. However, in our scenario, we involve the gravity on brane by using the method provided in \cite{Shiromizu:1999wj}, and the evolution of brane is determined by the effective Einstein field equation on brane and Israel junction condition together.

Our work is organized as follows. In Sec.\ref{BHpart}, we briefly review the 5-dimensional asymptotically AdS black hole solution and relevant thermodynamics. Besides, we give a well-defined boundary stress-energy tensor and caculate the black hole mass  by adding an appropriate surfacte counterterms to the gravitational action. The movement of self-graviting brane in the background of the AdS dilaton black hole are considered in Sec.\ref{BranMotion}. In Sec.\ref{BranHolo}, the holographic effects on brane will be investigated as the brane approaches the AdS boundary. Finally, Sec.\ref{ConAndDis} will summarize our results and give a discussion.

\section{AdS dilaton black holes and relevant thermodynamical quantities \label{BHpart}}

\subsection{Dilaton black holes solution in asymptotically AdS spacetime}
A asymptotically AdS dilatonic black hole with charge will be considered as a background spacetime (i.e. bulk) for brane's motion, thus we will review this black hole solution in present section. We begin with the action of 5-dimensional Einstein-Maxwell-dilaton gravity (we use the convention $\kappa^2=8\pi G$)
\bea{EMD}
&&\hspace{-5mm}S_{EMD}=\frac{1}{2\kappa_{5}^{2}}\int_{M}d^{5}x\sqrt{-g}[\mathcal{R}-\frac{4}{3}g^{MN}\partial_{M}\phi\partial_{N}\phi
\\
&&\rule{15mm}{0pt}-V(\phi)-e^{-\frac{4}{3}\alpha\phi}F^{2}]
\nonumber
\end{eqnarray}
where $\mathcal{R}$ and $\phi$ are the usual Ricci scalar and dilaton field respectively, the latter has self-interaction $V(\phi)$ and non-minimally couples to the electromagnetic field of kinetic energies $F^2$. The physical constants $\alpha$ measures the strength of this coupling. Equation of motions following from this action have the form
\bea{feq}
\nonumber
&&\hspace{-5mm}\mathcal{R}_{MN}=\frac{1}{3}[4\partial_{M}\phi\partial_{N}\phi+g_{MN}V(\phi)]+2e^{-\frac{4\alpha\phi}{3}}[F^L _M F_{LN}
\\
&&\hspace{-5mm} \quad \quad \quad -\frac{1}{6}g_{MN}F^{2}]
\end{eqnarray}
\bea{seq}
&&\hspace{-11mm} \nabla^{2}\phi=\frac{\partial_{M}(\sqrt{-g}g^{MN}\partial_{N}\phi)}{\sqrt{-g}}=\frac{3}{8}\frac{\partial V}{\partial\phi}-\frac{\alpha}{2}e^{-\frac{4\alpha\phi}{3}}F^{2}
\end{eqnarray}
\bea{Maxwell}
&&\hspace{-11mm} \nabla_{N}(e^{-\frac{4\alpha\phi}{3}}F^{NM})=\partial_{N}(\sqrt{-g}e^{-\frac{4\alpha\phi}{3}}F^{NM})=0
\end{eqnarray}
We consider a static black hole solution with metric ansatz
\bea{Metric}
\nonumber
&& ds^2 =g_{AB}dx^Adx^B \\
\label{Ge5dBHAnsa}
&& \quad ~=-A(r)dt^2+B(r)dr^2+R(r)^2d\Omega ^2 _{k,3}
\end{eqnarray}
where $d\Omega ^2 _{k,3}$ is the line element of 3-dimensional hyper surface of constant curvature $6k$ with $k=\pm1, 0$ corresponding to spheric, hyperbolic and plane topology respectively. In the case of only static electric fields occcur in the system, the only nonzero components of $F_{M N}$ could be obtained from the maxwell equation \eqref{Maxwell}
\bea{solEM}
F_{tr} =\sqrt{A(r)B(r)}\frac{qe^{4\alpha\phi/3}}{R^{3}(r)}
\end{eqnarray}
Explicitly, substitute \eqref{Metric},\eqref{Maxwell} into \eqref{feq} and \eqref{seq}, it can be obtained that
\bea{}
\label{Eintt}
&&\hspace{-14mm}\frac{A''}{2B}+\frac{3A'R'}{2BR}-\frac{A'B'}{4B^{2}}-\frac{(A')^{2}}{4AB}=\frac{4e^{-4\alpha\phi/3}(F_{tr})^{2}}{3B}-\frac{1}{3}AV
\\
\label{Einrr}
&&\hspace{-14mm}\frac{A''}{2A}+\frac{3R''}{R}-\frac{3B'R'}{2BR}-\frac{A'B'}{4AB}-\frac{(A')^{2}}{4A^{2}}=-\frac{1}{3}BV-\frac{4}{3}(\phi')^{2}\\
\nonumber
&&\hspace{-4mm}\quad\quad\quad\quad\quad\quad\quad\quad\quad\quad\quad\quad\quad\quad +\frac{4(F_{tr})^{2}e^{-4\alpha\phi/3}}{3A}
\\
\label{Einxx}
&&\hspace{-14mm}\frac{RR''}{B}+\frac{2(R')^{2}}{B}-\frac{B'R'R}{2B^{2}}+\frac{A'R'R}{2AB}=-\frac{1}{3}R^{2}V
\\
\nonumber
&&\hspace{-4mm}\quad\quad\quad\quad\quad\quad\quad\quad\quad\quad\quad\quad\quad-\frac{2R^{2}(F_{tr})^{2}e^{-4\alpha\phi/3}}{3AB}
\\
\label{eqphi}
&&\hspace{-14mm}\frac{\phi''}{B}+\frac{3R'\phi'}{BR}-\frac{B'\phi'}{2B^{2}}+\frac{A'\phi'}{2AB}=\frac{3}{8}V'+\frac{\alpha(F_{tr})^{2}e^{-4\alpha\phi/3}}{AB}
\end{eqnarray}
where we have set $k=1$ with topology $S^3$, namely $d\Omega ^2 _3 =d\theta ^2 _1+\sin^2\theta_1 d\theta^2 _2+\sin^2\theta_1 \sin^2 \theta_2 d\varphi ^2$. For simplicity, we will consider only the spherical case in this paper. By adjusting the form of $V(\phi)$ appropriately, reference \cite{Gao:2004tv, Gao:2005xv} obtains asymptotically AdS black hole solutions of the system analytically,
\bea{}
\label{solDilaPon}
&&\hspace{-3mm}V(\phi)=\frac{\Lambda}{2(2+\alpha^{2})^{2}}(4\alpha^{2}(\alpha^{2}-1)\cdot e^{-\frac{8\phi}{3\alpha}}\\
\nonumber
&& \hspace{-3mm}\quad \quad ~ +4(4-\alpha^{2})\cdot e^{\frac{4\alpha\phi}{3}}+24\alpha^{2}\cdot e^{-\frac{2(2-\alpha^{2})\phi}{3\alpha}})
\\
\label{solA}
&&\hspace{-3mm}A(r)=-\frac{c^{2}}{r^{2}}(1-\frac{b^{2}}{r^{2}})^{1-\frac{2\alpha^{2}}{2+\alpha^{2}}}-\frac{\Lambda r^{2}}{6}(1-\frac{b^{2}}{r^{2}})^{\frac{\alpha^{2}}{2+\alpha^{2}}}
\\
\label{solB}
&&\hspace{-3mm}B(r)=(1-\frac{b^{2}}{r^{2}})^{-\frac{\alpha^{2}}{2+\alpha^{2}}}/A(r)
\\
\label{solR}
&&\hspace{-3mm}R(r)=(1-\frac{b^{2}}{r^{2}})^{\frac{\alpha^{2}}{2(2+\alpha^{2})}}r
\\
\label{solPhi}
&& \hspace{-3mm}\phi(r)=\frac{3\alpha}{2(2+\alpha^{2})}\ln(1-\frac{b^{2}}{r^{2}})
\end{eqnarray}
Besides, the following relation is also implied by Einstein field equations,
\bea{}
\label{ElectriWithbc}
q^{2}=\frac{6}{(2+\alpha^{2})}b^{2}c^{2}
\end{eqnarray}
Here $b$ and $c$ are integration constants with dimension of length, as we show later, they are also related with the mass $M$. Reference \cite{Sheykhi:2009pf} shows that for this black hole solution, the Kretschmann scalar $R^{\mu \nu \alpha \beta} R_{\mu \nu \alpha \beta}$ and the Ricci scalar R both diverge at $r =b$, thus $r =b$ is the location of curvature singularity. Furthermore, as shown in Fig.\ref{figAdShorizon}, for AdS black hole solution, there only exists one horizon whatever the value of dilaton coupling constant $\alpha$.
\begin{figure}[ht]
	\begin{center}
		\includegraphics[scale=0.75]{figAdShorizon.eps}
		\caption{(color online). Plot the horizon function $A(r)$ of charged AdS dilaton black hole solution at fixed black hole mass and charge with different dilaton coupling constant..}
		\label{figAdShorizon}
	\end{center}
\end{figure}

\subsection{the mass of black holes}

When we consider the black hole thermodynamics through Euclidean path integral approach, there exists a unavoidable divergence on boundary of spacetime. In asymptotically AdS spacetime, a suitable surface counterterm could be found with feature of coordinate frame independence, after the renormalization procedure, a finite Euclidean action and a well-defined boundary stress-energy tensor will be obtained. According to the methods of Ref.\cite{Balasubramanian:1999re,Dayyani:2016gaa,Cai:1999xg}, we choose the surface counterterm as the following ansatz
\bea{}
\nonumber
&&\hspace{-2mm} S_{ct}	=	-\frac{1}{\kappa_{5}^{2}}\int_{\partial M}d^{4}x\sqrt{-\gamma}\bigg\{\frac{c_{0}}{l_{eff}(\phi)}(1+\frac{c_{\phi}}{c_{0}}\phi^{2})\\
\label{CounterAction}
&&\hspace{-2mm}\quad \quad \quad +c_{1}l_{eff}\mathcal{R}+c_2l_{eff}^{3}\big(\mathcal{R}^{2}+c_\beta \mathcal{R}^{ab}\mathcal{R}_{ab}\big)\bigg\} \\
\nonumber
\\
\nonumber
&& where\quad  \frac{1}{l_{eff}(\phi)}=\sqrt{-\frac{V(\phi)}{3(3+1)}}
\end{eqnarray}
the expression of $V(\phi)$ has shown in eqs.$\eqref{solDilaPon}$. Actually, $\mathcal{R}^{2}$ and $\mathcal{R}^{ab}\mathcal{R}_{ab}$ are similiar in magnitude, we will make $c_\beta=0$ for simplification in caculation. With inclusion of this counterterm, the quasilocal stress-energy tensor at the boundary $r=const$ with induced metric $\gamma_{ab}$ could be derived as
\bea{}
\nonumber
&&T_{ab}	=	\frac{1}{\kappa_{5}^{2}}\bigg\{ K_{ab}-K\gamma_{ab}+\frac{c_{0}}{l_{eff}}\big(1+c_{\phi}\phi^{2}\big)\gamma_{ab}\\
\nonumber
&&\quad \quad -2c_{1}l_{eff}\big(\mathcal{R}_{ab}-\frac{1}{2}\mathcal{R}\gamma_{ab}\big)+c_{2}l_{eff}^{3}\big(\gamma_{ab}\mathcal{R}^{2}\\
\label{GeneTab}
&&\quad \quad-4\mathcal{R}\mathcal{R}_{ab}+4\nabla_{a}\nabla_{b}\mathcal{R}-4\gamma_{ab}\nabla_{m}\nabla^{m}\mathcal{R}\big)\bigg\}
\end{eqnarray}
where the $\gamma_{ab}$ is the induced metric on the boundary $r=const$, which is defined as
\bea{}
\gamma_{ab}dx^adx^b=\lim_{r\to con} ds^2_5=-A(r)dt^2 +\big(R(r) \big) ^2d\Omega^2_3
\end{eqnarray}
The $K_{ab}$ is the extrinsic curvature on the boundary. Expand the $\eqref{GeneTab}$ explicitly, we give
\bea{}
\nonumber
&&T_{tt}=-3\frac{AR^{\prime}}{\sqrt{B}R}-\frac{c_{0}}{l_{eff}}A\big(1+c_{\phi}\phi^{2}\big)\\
\label{WithCouTtt}
&&\quad \quad -6\frac{c_{1}l_{eff}}{R^{2}}A-36\frac{c_{2}l_{eff}^{3}}{R^{4}}A\\
\nonumber
&&T_{ij}	=	\frac{h_{ij}}{R^{2}}\bigg(\frac{R^{2}A^{\prime}}{2A\sqrt{B}}+2\frac{RR^{\prime}}{\sqrt{B}}+c_{0}(1+\frac{c_{\alpha}}{c_{0}}\phi^{2})\frac{R^{2}}{l_{eff}}\\
\label{WithCouTij}
&& \quad \quad +2c_{1}l_{eff}-12c_{2}\frac{l_{eff}^{3}}{R^{2}}\bigg)
\end{eqnarray}
The mass of black hole is a conserved charge associated with a timelike killing vector, from the reference \cite{Balasubramanian:1999re}, it could be defined as
\bea{}
\label{DefiOfBHM}
M=\int _{r\to \infty} dx^3  \big(R(r) \big) ^3 \big( A(r) \big) ^{-\frac{1}{2}} T_{tt}
\end{eqnarray}
For getting a finite mass of black hole, we need to find a well-defined quasilocal stress-energy $T_{tt}$. Thus, we choose the undetermined coefficients in \eqref{CounterAction} as $c_0=-3, c_\phi=\frac{2}{9}, c_1=-\frac{1}{4}, c_2=\frac{1}{96}$. After substitute these coefficients and \eqref{solDilaPon}-\eqref{solPhi} into $\eqref{DefiOfBHM}$, we obtain
\bea{}
\label{FiExOf}
M=\frac{3\Omega_{3}}{2\kappa_{5}^{2}}\bigg(c^{2}+\big(\frac{2-\alpha^{2}}{2+\alpha^{2}}\big)b^{2}\bigg)
\end{eqnarray}

\subsection{the thermodynamical quantities of black hole}

In term of the general metric ansatz $\eqref{Ge5dBHAnsa}$, the Hawking temperature could be expressed as
\bea{}
\label{DefiTema}
T_{H}=\frac{\sqrt{A^{\prime}(B^{-1})^{\prime}}}{4\pi}\vert_{r=r_{+}}
\end{eqnarray}
Substitute \eqref{solA} and \eqref{solB} into \eqref{DefiTema}, we obtain
\bea{}
\nonumber
&&T_H=\frac{\big((2+\alpha^{2})r^{2}-3b^{2}\big)}{(\alpha^{2}+2)\pi L^{2}r_{+}}\big(1-\frac{b^{2}}{r_{+}^{2}}\big)^{\frac{\alpha^{2}-4}{2(2+\alpha^{2})}}\\
\label{ExpreTeam}
&&\quad\quad+\frac{1}{2\pi r_{+}}(1-\frac{b^{2}}{r_{+}^{2}})^{\frac{4-\alpha^{2}}{2(2+\alpha^{2})}}
\end{eqnarray}
in which we have used $A(r_+)=0$ to eliminate the parameter $c$, namely
\bea{}
\label{RepCWithHori}
c=(1+(1-\frac{b^{2}}{r_{+}^{2}})^{\frac{2\alpha^{2}-2}{2+\alpha^{2}}}\frac{r_{+}^{2}}{L^{2}})^{1/2}r_{+}
\end{eqnarray}
According to area laws, the entropy of system is
\bea{}
\label{BHentropy}
S=\frac{2\pi r_{+}^{3}\Omega_{3}}{\kappa_{5}^{2}}(1-\frac{b^{2}}{r_{+}^{2}})^{\frac{3\alpha^{2}}{2(2+\alpha^{2})}}
\end{eqnarray}
From the Gauss law, the electric charge is
\bea{}
\label{BHECharge}
Q=\frac{br_{+}\Omega_{3}}{4\pi}\sqrt{\frac{6}{2+\alpha^{2}}}\sqrt{1+\frac{r_{+}^{2}}{L^{2}}(1-\frac{b^{2}}{r_{+}^{2}})^{\frac{2\alpha^{2}-2}{2+\alpha^{2}}}}
\end{eqnarray}
in which we also use equality $A(r_+)=0$ to eliminate parameter $c$. Finally, the chemical potentials can be caculated as
\bea{}
U=A_{t}\vert_{r\to\infty}-A_{t}\vert_{r\to r_{+}}=-\frac{4\pi q}{\kappa_{5}^{2}r_{+}^{2}}
\end{eqnarray}
where the definition of $A_{t}$ is
\bea{}
A_{t}=-\int dr\frac{8\pi}{\kappa^{2}}F_{tr}=-\int dr\frac{8\pi q}{\kappa^{2}r^{3}}=\frac{8\pi}{2\kappa^{2}}\frac{q}{r^{2}}
\end{eqnarray}
Replace the parameter $c$ in \eqref{FiExOf} with the equality \eqref{RepCWithHori}, we give
\bea{}
M=\frac{3\Omega_{3}r_{+}^{2}}{2\kappa_{5}^{2}}\bigg(1+(1-\frac{b^{2}}{r_{+}^{2}})^{\frac{2\alpha^{2}-2}{2+\alpha^{2}}}\frac{r_{+}^{2}}{L^{2}}+(\frac{2-\alpha^{2}}{2+\alpha^{2}})\frac{b^{2}}{r_{+}^{2}}\bigg)
\end{eqnarray}
With thermodynamic quantities given above,  we can ensure the rightness of black hole mass \eqref{FiExOf} by cheking that the first law of black hole thermodynamics is holden. According to the link rule of differentiation \cite{Sheykhi:2009pf,Li:2017kkj}, we obtain
\bea{}
\label{PMPS}
&&\hspace{-15mm}\bigg(\frac{\partial M}{\partial S}\bigg)_{Q}=\bigg(\frac{\partial M}{\partial r_{+}}\frac{\partial r_{+}}{\partial b}+\frac{\partial M}{\partial b}\bigg)_{Q}\bigg/\bigg(\frac{\partial S}{\partial r_{+}}\frac{\partial r_{+}}{\partial b}+\frac{\partial S}{\partial b}\bigg)_{Q}\\
\label{MidPMPS}
&&\hspace{-15mm}\bigg(\frac{\partial r_{+}}{\partial b}\bigg)_{Q}=-\bigg(\frac{\partial Q}{\partial b}\bigg)\bigg/\bigg(\frac{\partial Q}{\partial r_{+}}\bigg)\\
\label{PMPQ}
&&\hspace{-15mm}\bigg(\frac{\partial M}{\partial Q}\bigg)_{S}=\bigg(\frac{\partial M}{\partial r_{+}}\frac{\partial r_{+}}{\partial b}+\frac{\partial M}{\partial b}\bigg)_{S}\bigg/\bigg(\frac{\partial Q}{\partial r_{+}}\frac{\partial r_{+}}{\partial b}+\frac{\partial Q}{\partial b}\bigg)_{S}\\
\label{MidPMPQ}
&&\hspace{-15mm}\bigg(\frac{\partial r_{+}}{\partial b}\bigg)_{S}=-\bigg(\frac{\partial S}{\partial b}\bigg)\bigg/\bigg(\frac{\partial S}{\partial r_{+}}\bigg)
\end{eqnarray}
note that the extra minus sign in \eqref{MidPMPS} and \eqref{MidPMPQ} are originated from the derivative of implicit functions $Q(b,r_+)=Q_0, S(b,r_+)=S_0$. After some tedious but straightforward caculations, it's easy to check that
\bea{}
\bigg( \frac{\partial M}{\partial S} \bigg)_Q =T, \quad \quad  \bigg( \frac{\partial M}{\partial Q} \bigg)_S =U
\end{eqnarray}
thus the above thermodynamics quantities indeed satisfy the first law of black hole thermodynamics,
\bea{}
dM=TdS+UdQ
\end{eqnarray}

\section{Brane's motion in spacetime of black hole \label{BranMotion}}

\subsection{Motion of brane in a static bulk with one extra dimension}

We assume $\mathcal{M}$ is a 5-dimensional manifold containing a brane $\Sigma$ with two sides (denoted by $\Sigma_\pm$ respectively), which splits M into two parts, i.e. $\mathcal{M}_{\pm}$, with a $Z_2$ symmetry. For describing the bulk-brane system clearly, we need to introduce some physical quantities before giving formula expression. We use $X^A$ to denote bulk coordinates and $x^\mu$ to denote internal coordinates of the brane world sheet. If we consider the motion of brane in bulk with one extra dimension, one can then embed brane into bulk with trajectory $X^A(x^\mu)$ (see Table.\ref{EmbedBrane} for more detail), while construct the vielbein as $e^A _\mu =\frac{\partial X^A}{\partial x^\mu}$.
\begin{table}[!ht]
	\begin{center}
		\begin{tabular}{|c|c|c|c|}
			\hline
			Bulk & $t$ & $r$ & $\vec{X}_3$ \\
			\hline
			brane & $t_{b}$ & $\times$ & $\vec{x}_3$ \\
			\hline
			embeded brane & $t(t_b)$ & $r(t_b)$ & $\vec{x}_3=\vec{X}_3$\\
			\hline
		\end{tabular}
		\caption{This table shows how embed brane into bulk in each component of coordinates.}
		\label{EmbedBrane}
	\end{center}
\end{table}
According to the static gauge, the $t_b$ could be chosen as proper time $\tau$ of bulk coordinates. We will set $t_b=\tau$ in the following contents.

We consider a static bulk spacetime with the ansatz \eqref{Ge5dBHAnsa}.
The velocity of the brane could be written as $u^M=(\dot{T}(\tau),\dot{r}(\tau),0,0,0)$, normalization $u^M u_M=-1$ gives $\dot{T}(\tau)=\sqrt{(1+B\dot{r}^{2})/A}$. Let $n_M$ be the unit normal pointint into $M_\pm$, according to orthogonal condition $u^M n_M =0, n^M n_M=1$, we obtain $n_{M}=(\sqrt{AB}\dot{r},-\sqrt{B(1+B\dot{r}^{2})},0,0,0)$. The induced metric on $\Sigma_\pm$ is defined by $h_{\mu\nu}=e^M _\mu e^N _\mu g_{AB}$, explicitly
\begin{align}
\label{induceBrane}
ds^2=-d\tau^2 +R\big( r(\tau) \big)^2 d\Omega ^2 _3
\end{align}

The physics of bulk-brane system could be described by action
\bea{}
\label{BhBraneAct}
&&S=S_{EMD}+S_{brane}\\
\label{BraneAct}
&&S_{brane}=\int dx^{4}\sqrt{-h}\big\{\frac{\mathcal{K}}{\kappa_{5}^{2}}+\lambda(\phi)+\mathcal{L}_{matter}\big\}
\end{eqnarray}
where $\lambda$ is a undetermined function of $\phi$, which represents the effective brane tension. And the $\mathcal{K}$ is the trace of extrinsic curvature tensor \cite{Gibbons:1976ue}. Varying $\eqref{BhBraneAct}$ with respect to metric tensor. Besides getting a standard Einstein equation in bulk spacetime, we also obtain a Israel junction condition on brane \cite{Israel:1966rt,Chamblin:1999ya},
\bea{}
\label{OriIsrael}
\big\{\mathcal{K}_{\mu\nu}-\mathcal{K}h_{\mu\nu}\big\}\vert_{\Sigma_{+}}-\big\{\mathcal{K}_{\mu\nu}-\mathcal{K}h_{\mu\nu}\big\}\vert_{\Sigma_{-}}=\kappa_{5}^{2}S_{\mu\nu}
\end{eqnarray}
where $S_{\mu \nu}$ is the energy-momentum tensor of matters which are confined on brane, and the $\mathcal{K}_{\mu \nu}$ is defined as
\bea{}
\label{ExtrinCurva}
\mathcal{K}_{\mu \nu}=\frac{1}{2} e^M_{\mu} e^N_{\nu} \big( \nabla_M n_N +\nabla_N n_M  \big)
\end{eqnarray}
We will involve a $Z_2$ symmetry in two sides of brane, namely $\big\{\mathcal{K}_{\mu\nu}\big\}\vert_{\Sigma_{-}}=-\big\{\mathcal{K}_{\mu\nu}\big\}\vert_{\Sigma_{+}}$. In this way, the junction condition $\eqref{OriIsrael}$ could be further simplified as
\bea{}
\label{z2juncon}
\mathcal{K}_{\mu\nu}-\mathcal{K}h_{\mu\nu}=\frac{\kappa_{5}^2}{2} \mathcal{S}_{\mu\nu}
\end{eqnarray}
for clearness in expression, we omit the subscript $\Sigma_{+}$. Alternatively, \eqref{z2juncon} could also be written as
\bea{}
\label{alterz2juncon}
\mathcal{K}_{\mu\nu}=-\frac{\kappa^2_5}{2} \big( S_{\mu\nu}-\frac{1}{3}Sh_{\mu\nu} \big)
\end{eqnarray}
For general ansatz of 5-dimensional static black hole \eqref{Ge5dBHAnsa}, the nonvanishing components of $\mathcal{K}_{\mu \nu}$ are given by
\bea{}
\label{ExtKij}
&&\mathcal{K}_{ij}=-\frac{R^{\prime}}{R}\frac{\sqrt{1+B\dot{r}^{2}}}{\sqrt{B}}h_{ij}\\
\label{ExtKtautau}
&&\mathcal{K}_{\tau\tau}=\frac{\sqrt{\big(1+B\dot{r}^{2}\big)}}{2A\sqrt{B}}\bigg(A^{\prime}+\big(AB^{\prime}-A^{\prime}B\big)\dot{r}^{2}\bigg)
\end{eqnarray}
in which $\dot{r}=dr(\tau)/d\tau$, and we will also use dot to denote the derivative with respect to $\tau$ in following contents. Varying \eqref{BhBraneAct} with respect to dilaton field. Besides giving the equation of motions \eqref{eqphi} in bulk, we also obtain a boundary condition of dilaton field on brane,
\bea{}
\label{JunScalar}
\frac{4}{3\kappa_{5}^{2}}n^{M}\partial_{M}\phi=\frac{\partial\lambda}{\partial\phi}
\end{eqnarray}
Expanding the \eqref{JunScalar} yields
\bea{}
\label{DetaJunScalar}
-\frac{\sqrt{(1+B\dot{r}^{2})}}{\sqrt{B}}\partial_{r}\phi=\frac{3\kappa_{5}^{2}}{4}\frac{\partial\lambda}{\partial\phi}
\end{eqnarray}
Besides, if we set the energy-momentum tensor of matters on brane as simple ideal fluid types, namely
\bea{}
\label{Exoidealfluid}
\mathcal{S}^\mu _\nu=Diag\{-\rho,P,P,P \}
\end{eqnarray}
then by combining $\eqref{Exoidealfluid}$ with $\eqref{BraneAct}$, we will obtain the two independent components of the Israel junction condition as
\bea{}
\nonumber
&&\hspace{-19mm}\frac{\sqrt{(1+B\dot{r}^{2})}}{2A\sqrt{B}}\big(A^{\prime}+(AB^{\prime}-A^{\prime}B)\dot{r}^{2}\big)+\frac{2R^{\prime}\sqrt{1+B\dot{r}^{2}}}{R\sqrt{B}}\\
 \label{ExpIsrael1}
&&\quad \quad \quad \quad \quad \quad \quad \quad \quad \quad=\frac{\kappa_{5}^{2}}{2}(\lambda+P)\\
 \nonumber
 \\
 \label{ExpIsrael2}
&&\quad\frac{R^{\prime}}{R}\frac{\sqrt{1+B\dot{r}^{2}}}{\sqrt{B}}=\frac{\kappa_{5}^{2}}{6}(\lambda-\rho)
\end{eqnarray}

\subsection{Effective Einstein field equations on  brane}

As shown in \cite{Shiromizu:1999wj}, the effective Einstein field equation on brane is
\bea{}
\nonumber
&&\hspace{-4mm}\frac{3}{2}\bigg(\mathcal{R}_{\mu\nu}-\frac{1}{6}h_{\mu\nu}\mathcal{R}\bigg)+\frac{3}{2}E_{\mu\nu}-\frac{3}{2}\mathcal{K}\mathcal{K}_{\mu\nu}+\frac{3}{2}\mathcal{K}_{\mu\rho}\mathcal{K}_{\nu}^{\rho}+\frac{1}{4}h_{\mu\nu}\mathcal{K}^{2}\\
\label{effEinOnbrane}
&&\hspace{-4mm}-\frac{1}{4}h_{\mu\nu}\mathcal{K}_{\alpha\beta}\mathcal{K}^{\alpha\beta}=\kappa_{5}^{2}\bigg(\mathcal{T}_{MN}h_{\mu}^{M}h_{\nu}^{N}-\frac{1}{4}h_{\mu\nu}\mathcal{T}\bigg)
\end{eqnarray}
in which $R_{\mu\nu}$ and $R$ is the Ricci tensor and Ricci scalar of the induced metric $h_{\mu \nu}$, while the $E_{\mu \nu}$ is defined as
\bea{}
\label{tidaltensor}
E_{\mu \nu}=\mathcal{C}_{MNAB} n^M  n^A e^N _\mu e^B _\nu
\end{eqnarray}
where the $\mathcal{C}$ is the Weyl curvature tensor,
\bea{}
\nonumber
\mathcal{C}_{MNAB}=R_{MNAB}-\frac{2}{3}(g_{MA}R_{BN}-g_{NA}R_{BM})+\frac{1}{6}g_{MA}g_{BN}R
\end{eqnarray}
substitute $\eqref{induceBrane},\eqref{z2juncon}$ into $\eqref{effEinOnbrane}$ and expand it explicitly, we give two equations as following
\bea{}
\nonumber
&&\frac{3A^{\prime}}{2AB}\frac{R^{\prime}}{R}+\frac{3A^{\prime}}{2A}\frac{R^{\prime}}{R}\dot{r}^{2}+\frac{3B^{\prime}}{2B}\frac{R^{\prime}}{R}\dot{r}^{2}-\frac{3}{2B}\frac{(R^{\prime})^{2}}{R^{2}}-\frac{3}{2}\frac{(R^{\prime})^{2}}{R^{2}}\\
\label{EffEinOnbrane1}
&&+3\frac{R^{\prime}}{R}\ddot{r}=\frac{\kappa_{5}^{4}\lambda}{4}P+\frac{\kappa_{5}^{4}\lambda^{2}}{24}-\frac{\kappa_{5}^{4}}{4}P\rho+\frac{\kappa_{5}^{4}\lambda}{6}\rho-\frac{5\kappa_{5}^{4}}{24}\rho^{2}\\
\label{EffEinOnbrane2}
&&\frac{3}{2B}\frac{(R^{\prime})^{2}}{R^{2}}\big(1+B\dot{r}^{2}\big)=\frac{\kappa_{5}^{4}\lambda^{2}}{24}-\frac{\kappa_{5}^{4}\lambda}{12}\rho+\frac{\kappa_{5}^{4}}{24}\rho^{2}
\end{eqnarray}
Note that the $R$ represents the solution \eqref{solR}, which is the function of $r$ in metric \eqref{Metric} rather than the Ricci scalar. It's easy to see that the $\eqref{EffEinOnbrane2}$ is same with $\eqref{ExpIsrael2}$. Thus the bulk-brane system is described by 4 independent equations $\eqref{DetaJunScalar},\eqref{ExpIsrael1},\eqref{ExpIsrael2},\eqref{EffEinOnbrane1}$. When combining with the Einstein field equation in bulk $\eqref{Eintt}$-$\eqref{Einxx}$  and Israel junction condition $\eqref{ExpIsrael1}$-$\eqref{ExpIsrael2}$, the $\eqref{EffEinOnbrane1}$ could be further simplified as
\bea{}
\label{DeterEvort}
\ddot{r}+\frac{A^{\prime}}{2A}\dot{r}^{2}+\frac{A^{\prime}B}{2A}\dot{r}^{4}-\frac{1}{2}B^{\prime}\dot{r}^{4}=0
\end{eqnarray}
After substituting $\eqref{solA}$, $\eqref{solB}$ into $\eqref{DeterEvort}$ and solving this differential equation numerically at fixed parameters $M$ and $Q$ with different $\alpha$. We display the variation of brane's position $r(\tau)$ and corresponding velocity $\dot{r}(\tau)$ in top-left and top-right panel of Fig.\ref{Solrtau}. Note that for the observer confined on the brane universe, the scale factor is $R(r(\tau))$ according to the induced metric $\eqref{induceBrane}$, thus we also show the variation trend of $R(r(\tau))$ and corresponding Hubble constant $H=\frac{\dot{R}}{R}=\frac{R^\prime (r(\tau))}{R}\dot{r}$ in Fig.\ref{Solrtau}.
\begin{figure}[ht]
	\begin{center}
		\includegraphics[scale=0.29]{fig2rtVarya.eps}
		\includegraphics[scale=0.29]{fig2drtVarya.eps}\\
		\includegraphics[scale=0.29]{fig2RRtVarya.eps}
		\includegraphics[scale=0.29]{fig2HtVarya.eps}
		\caption{(color online). The upper part displays the location $r(\tau)$ and velocity $\frac{dr(\tau)}{d\tau}$ of brane in bulk coordinates as the increase of proper time. The bottom part plots the evolution of effective scale factor $R(r(\tau))$ and Hubble constant $H=\frac{dR/d\tau}{R}$ for the observer confined on brane universe. The red, green, blue, and black curves correspond the $\alpha=3,\alpha=1,\alpha=\sqrt{3}/3,\alpha=0$ respectively, meanwhile all of these curves correspond the same black hole mass and charge. Both the AdS radius and $\kappa$ are set to be 1.}
		\label{Solrtau}
	\end{center}
\end{figure}

From the $\eqref{DetaJunScalar}$, we obtain the mathmatical expression of brane tension $\lambda$ as the integrate function of $\tau$,
\bea{}
\label{InteFofLamtau}
&&\lambda=\lambda_{0}-\frac{4}{3\kappa_{5}^{2}}\int\frac{\sqrt{(1+B\dot{r}^{2})}}{\sqrt{B}}(\phi^{\prime})^{2}\dot{r}d\tau
\end{eqnarray}
Basing on $\eqref{InteFofLamtau}$, we give the variation trend of $\lambda$ with respect to $\tau$ in Fig.\ref{SolLamtau}.
\begin{figure}[ht]
	\begin{center}
		\includegraphics[scale=0.43]{fig3LamtVarya.eps}
		\caption{(color online). According to the equation \eqref{InteFofLamtau}, we plot the evolution of effective brane tension $\lambda$ as the function of proper time $\tau$. The initial brane's tension is set as $\lambda_0=6.5$. Both the AdS radius and $\kappa$ are set to be 1.}
		\label{SolLamtau}
	\end{center}
\end{figure}
Combining the equations \eqref{ExpIsrael1} and \eqref{ExpIsrael2} with the numerical solutions $r(\tau)$ and $\lambda(\tau)$, we can also plot the  evolution of energy density $\rho$ and pressure $P$ of the matters confined on brane as follows
\begin{figure}[ht]
	\begin{center}
		\includegraphics[scale=0.29]{fig4RhotSLVa.eps}
		\includegraphics[scale=0.29]{fig4RhotLLVa.eps}\\
		\includegraphics[scale=0.29]{fig4PtSLVa.eps}
		\includegraphics[scale=0.29]{fig4PtLLVa.eps}
		\caption{(color online). The evolution of energy density $\rho$ and preessure $P$ for the matters confined on brane, at fixed black hole mass $M$ and charge $Q$ with different dilaton coupling constant $\alpha$ and initial brane tension $\lambda_0$. Both the AdS radius and $\kappa$ are set to be 1.}
		\label{RhotPt}
	\end{center}
\end{figure}

\section{Holographic effects on  brane \label{BranHolo}}

\subsection{A renormalization procedure inspired by AdS/CFT}

As indicated in \cite{Witten:1998qj}, the energy, entropy and temperature of the CFT on boundary spacetime at high temperatures could be identified with the mass, Bekenstein-Hawking entropy, and Hawking temperature of AdS black hole. Thus, the matters on brane will have the CFT's feature when brane approaches the AdS boundary. In bulk spacetime, the total energy is just the black hole mass\eqref{FiExOf}, namely $E=M$. In case of large $r(\tau)$, the matter's energy on brane is given by
\bea{}
\label{EonBatLr}
E=M\dot{t} \approx ~\frac{3\Omega_{3}}{2\kappa_{5}^{2}}(c^{2}+\frac{2-\alpha^{2}}{2+\alpha^{2}}b^{2})~ \frac{L}{r}
\end{eqnarray}
Note that the $E=M$ is obtained by using the bulk's time coordinate $t$. Nevertheless an observer on brane measures the total energy by using the time coordinate $\tau$, thus we need to scale $E$ by $\dot{t}$. And the energy density is given by
\bea{}
\label{rhoCFT}
\rho=\frac{E}{V}=\frac{3}{2\kappa_{5}^{2}}(c^{2}+\frac{2-\alpha^{2}}{2+\alpha^{2}}b^{2})\frac{L}{r^{4}}
\end{eqnarray}
where the $V=(R(r(\tau)))^3 \Omega_3$ is just the spatial volume of the brane, from \eqref{solPhi} we know that $R(r(\tau)) = r(\tau)$ in the large $r(\tau)$ limit. Meanwhile, we use the $r$ to denote $r(\tau)$ in \eqref{EonBatLr}, \eqref{rhoCFT} for convenience, and this convention will still be used in this and next section. Namely, without pointing out explicitly, the $r$ will always represent the $r(\tau)$ in Sec\ref{BranHolo}. According to the first law of thermodynamics,
\bea{}
\label{FirstTher}
TdS+UdQ=dE+PdV
\end{eqnarray}
the pressure is obtained as
\bea{}
\label{pressCFT}
P=-\frac{\partial E}{\partial V}=\frac{L}{2\kappa_{5}^{2}r^{4}}\big(c^{2}+\frac{2-\alpha^{2}}{2+\alpha^{2}}b^{2}\big)
\end{eqnarray}
It's easy to check that $P=\frac{1}{3}\rho$. However, from the Fig.\ref{RhotPt}, we observe that $P=-\rho$ in region of large $r$.

Actually, from the scenario of brane-bulk geometry, there exists a motional brane which has cut off the bulk spacetime. Translate the scenario of geometry into the word of quantum field theory, it means that the matter field confined on brane is a symmetry broken effective field theory of CFT on AdS boundary at lower energies. Namely, in the case of $r(\tau) \ll \infty$, the Israel junction could be re-expressed as
\bea{}
\mathcal{K}_{\mu \nu} -\mathcal{K}h_{\mu \nu}=\frac{\kappa^2_5}{2}\big(\langle S^{CFT}_{\mu \nu}\rangle+\langle S^{IR}_{\mu \nu} \rangle+\lambda h_{\mu\nu} \big)
\end{eqnarray}
When the brane approaches the AdS boundary, namrly $r(\tau)\to \infty$, we need add a counterterms to subtract the infrared(IR) divergences and restore the conformal symmetry, finally the modified Israel junction condition becomes
\bea{}
\label{ModiIsrael}
\mathcal{K}_{\mu\nu}-\mathcal{K}h_{\mu\nu}-\frac{\kappa_{5}^{2}}{2}S_{\mu\nu}^{ct}=\frac{\kappa_{5}^{2}}{2}\big(\langle S_{\mu\nu}^{CFT}\rangle+\lambda h_{\mu\nu}\big)
\end{eqnarray}
As considered in \cite{deHaro:2000wj, Gubser:1999vj, Anchordoqui}, the action of countermterms could be involved as the Ricci scalar $R$ and higher order curvature terms respect to brane's induced metric $h_{\mu\nu}$. To be consistent with \eqref{CounterAction}, we choose the counterterm as the following ansatz
\bea{}
\label{ctBraneLr}
&&\hspace{-8mm}S_{ct}=-\frac{1}{\kappa_{5}^{2}}\int_{\Sigma}d^{4}x\sqrt{-h}\big\{ b_{1}l_{eff}\mathcal{R}+b_{2}l_{eff}^{3}\mathcal{R}^{2} \big\}
\end{eqnarray}
where $l_{eff}(\phi)=\sqrt{-\frac{3(3+1)}{V(\phi)}}$. Similarly, we have ignored the $\mathcal{R}^{\mu\nu} \mathcal{R}_{\mu\nu}$ term for simplification in caculation, without loss of generality. From $\eqref{ctBraneLr}$, the corresponding $S^{ct}_{\mu\nu}$ could be caculated as
\bea{}
\nonumber
&&S^{ct}_{\mu\nu}=-\frac{2c_{1}l_{eff}}{\kappa_{5}^{2}}\bigg(\mathcal{R}_{\mu\nu}-\frac{1}{2}\mathcal{R}h_{\mu\nu}\bigg)+\frac{c_{2}}{\kappa_{5}^{2}}l_{eff}^{3}\bigg\{h_{\mu\nu}\mathcal{R}^{2}\\
\label{ctTenBrane}
&&\quad\quad-4\mathcal{R}\mathcal{R}_{\mu\nu}+4\nabla_{\nu}\nabla_{\mu}\mathcal{R}-4h_{\nu\mu}\nabla_{\alpha}\nabla^{\alpha}\mathcal{R}\bigg\}
\end{eqnarray}
Meanwhile, we assume the $\lambda(\phi)$ has the following mathmatical form in case of large $r(\tau)$
\bea{}
\label{AsymLam}
\lambda(\phi)=\frac{1}{\kappa_{5}^{2}}\frac{b_{0}}{l_{eff}(\phi)}\big(1+\frac{b_{\alpha}}{b_{0}}\phi^{2}\big)
\end{eqnarray}
 the coefficients $b_0, b_\alpha, b_1, b_2$ will be decided later.

 Substitute $\eqref{AsymLam}$ and $\eqref{ctTenBrane}$ into the modified Israel junction condition $\eqref{ModiIsrael}$, and expand $\rho, P$ in the case of large $r(\tau)$, we obtain
 \bea{}
 \nonumber
 &&\hspace{-3mm}\kappa^2_5\rho=\frac{(b_{0}-6)}{L}-\frac{3L(1-2b_{1})}{r^{2}}+\frac{3}{4L(2+\alpha^{2})^{2}r^{4}}\big\{\\
\nonumber
&&\hspace{-3mm}\quad\quad~\alpha^{2}b^{4}(3b_{\alpha}-8)+(2+\alpha^{2})^{2}L^{2}\big(4c^{2}+(1+48b_{2})L^{2}\big) \\
 \label{HoloModRho}
&&\hspace{-3mm}\quad\quad~+8(2+\alpha^{2})\big(1+(b_{1}-1)\alpha^{2}\big)b^{2}L^{2}\big\}+O(\frac{1}{r^{6}})\\
\nonumber
\\
\nonumber
&&\hspace{-3mm} \kappa^2_5P=\frac{(b_{0}-6)}{L}+\frac{(1-2b_{1})L}{r^{2}}+\frac{1}{4L^{2}(2+\alpha^{2})^{2}r^{4}}\big\{\\
\nonumber
&&\hspace{-3mm}\quad\quad~3\alpha^{2}b^{4}L(8-3b_{\alpha})+(2+\alpha^{2})^{2}L^{3}(4c^{2}+(1+48b_{2})L^{2})\\
\label{HoloModP}
&&\hspace{-3mm}\quad\quad~-8(2+\alpha^{2})(b_{1}\alpha^{2}-1)b^{2}L^{3}\big\}+O(\frac{1}{r^{6}})
 \end{eqnarray}
Note that the equation $\eqref{DeterEvort}$ is invariant, although the Israel junction condition is changed from $\eqref{OriIsrael}$ to $\eqref{ModiIsrael}$. So, the evolution of $r(\tau)$ is still controlled by the equation $\eqref{DeterEvort}$. It's easy to observe from fig.\ref{Solrtau} that the $\dot{r}$ and higher order derivatives will approaches 0 when $r(\tau)\to \infty$, thus we have ignored all $O(\frac{1}{r^2}), O(\frac{1}{r^4})$ terms which include the derivatives of $r(\tau)$. Finally, by comparing the \eqref{HoloModRho} and \eqref{HoloModP} with the expected results \eqref{rhoCFT} and \eqref{pressCFT}, we can give these undetermined coefficients as $b_0=6,~b_1=\frac{1}{2},~b_\alpha=\frac{8}{3},~b_2=-\frac{1}{48}$.

Substitute $b_0=6,~b_\alpha=\frac{8}{3}$ into the \eqref{AsymLam}, we obtain a analytical expression for the effective brane tension as function of dilaton field
\bea{}
\label{AnaLamPhiLaTi}
\lambda(\phi)=\frac{1}{\kappa_{5}^{2}}\frac{6}{l_{eff}(\phi)}\big(1+\frac{4}{9}\phi^{2}\big)
\end{eqnarray}
Next, we check that the \eqref{AnaLamPhiLaTi} is indeed valid in large $r(\tau)$ case. Combine the \eqref{AnaLamPhiLaTi} with equation \eqref{eqphi} and the numerical solution of $r(\tau)$, we can plot the evolution of $\lambda$ with respect to the $\tau$ as shown by the dotted curves in Fig.\ref{efflamlati}. Meanwhile, the \eqref{InteFofLamtau} is also displayed in Fig.\ref{efflamlati} by the solid curves. It is obviously shown that by adjusting the parameter $\lambda_0$ appropriately, \eqref{AnaLamPhiLaTi} is consistent with the \eqref{InteFofLamtau} at late time. Besides the validity of \eqref{AnaLamPhiLaTi} in large $r(\tau)$ case, Fig.\ref{efflamlati} also reveals a physical fact that a fixed $\lambda_0$ is implied by the AdS/CFT correspondence.
\begin{figure}[ht]
	\begin{center}
		\includegraphics[scale=0.58]{fig5EffLamLar.eps}
		\caption{(color online). The dotted curves correspond to the approximate solution of effective brane tension $\lambda$ given by \eqref{AsymLam} which is valid in large $r(\tau)$ case (as shown in Fig.\ref{Solrtau}, the $r(\tau)$ is the monotonically increasing function of $\tau$, and hence the large $r(\tau)$ value also means the large $\tau$ value). The solid curves correspond to the  numerically exact solution of $\lambda$ given in \eqref{InteFofLamtau}. All these curves have the same parameter value $M=5,Q=0.125,L=1,\kappa=1$. The value of $\lambda_0$ set for the solid-red, solid-green, solid-blue curves are 6.0737, 6.02757, 6.01093 respectively.}
		\label{efflamlati}
	\end{center}
\end{figure}

\subsection{Cardy-Verlinde Formula}

The entropy of (1+1)-dimensional CFT system could be given by a very famous formula, namely the so-called Cardy formula \cite{Cardy:1986ie}. By using the combination of AdS/CFT correspondence and thermodynamics of AdS-Schwarzschild black holes, \cite{Verlinde:2000wg, Savonije:2001nd} has generalized the Cardy formula to the CFT system which lives in arbitrary-dimensional spacetime, this generalized Cardy formula is called as the Cardy-Verlinde formula. After that, the Cardy-Verlinde formula have been checked in various black holes with AdS asymptotics \cite{Klemm:2001db, Cai:2001jc, Birmingham:2001vd, Youm:2001yq, Cai:2001ja, Youm:2001qr, Jing:2002aq, Cai:2002bn, Lee:2008yqa, BravoGaete:2017dso}. In our case, as we have argued in last section, the matters confined on brane will behave as CFT system when brane approaches the AdS boundary. Thus, we naturally expect that the Cardy-Verlinde formula will hold in case of large $r(\tau)$.

In the limit of $r(\tau)\to\infty$, the temperature and chemical potential of the corresponding CFT on brane could be given as
\bea{}
\nonumber
&&T=T_{H}\dot{t}\approx\frac{L}{2\pi rr_{+}}(1-\frac{b^{2}}{r_{+}^{2}})^{\frac{4-\alpha^{2}}{2(2+\alpha^{2})}}\\
\label{TemaCFT}
&&\quad \quad \quad +\frac{\big((2+\alpha^{2})r_{+}^{2}-3b^{2}\big)}{(\alpha^{2}+2)\pi Lrr_{+}}\big(1-\frac{b^{2}}{r_{+}^{2}}\big)^{\frac{\alpha^{2}-4}{2(2+\alpha^{2})}}\\
\nonumber
\\
\nonumber
&&U=U\dot{t}\approx-\frac{4\sqrt{6}\pi bL}{\sqrt{2+\alpha^{2}}\kappa_{5}^{2}rr_{+}}\\
\label{UCFT}
&&\quad \quad \quad \quad \times\sqrt{1+\frac{r_{+}^{2}}{L^{2}}(1-\frac{b^{2}}{r_{+}^{2}})^{\frac{2\alpha^{2}-2}{2+\alpha^{2}}}}
\end{eqnarray}
The entropy and electric charge are given directly by \eqref{BHentropy} and \eqref{BHECharge}. And we obtain the entropic and electric density as
\bea{}
\label{CFTEntroDen}
&&s=\frac{S}{V}=\frac{2\pi r_{+}^{3}}{\kappa_{5}^{2}r^{3}}(1-\frac{b^{2}}{r_{+}^{2}})^{\frac{3\alpha^{2}}{2(2+\alpha^{2})}}\\
\nonumber
\\
\nonumber
&&\rho_e=\frac{Q}{V}=\frac{\sqrt{6}br_{+}}{4\pi\sqrt{2+\alpha^{2}}r^{3}}\\
\label{CFTElecDen}
&&\quad \quad ~ \times \sqrt{1+\frac{r_{+}^{2}}{L^{2}}(1-\frac{b^{2}}{r_{+}^{2}})^{\frac{2\alpha^{2}-2}{2+\alpha^{2}}}}
\end{eqnarray}
Using the symbol in \cite{Savonije:2001nd}, the $\gamma$ quantity which is relevant with the Casimir energy $E_c$ of CFT system on brane through the relation $E_c=(\frac{\gamma}{r^2})\cdot r^3 \Omega_3$, could be defined as
\bea{}
\nonumber
&&\frac{\gamma}{r^{2}}=3(\rho_{CFT}+P_{CFT}-\vert\rho_{e}U\vert-Ts)-\frac{\gamma_{proper}}{r^{2}}\\
\label{DefiGamma}
&&\quad ~ =3\frac{r_{+}^{2}}{\kappa_{5}^{2}r^{4}}L\bigg(1-\frac{b^{2}}{r_{+}^{2}}\bigg)
\end{eqnarray}
where
\bea{}
\label{GammaProper}
\frac{\gamma_{proper}}{r^{2}}=\frac{r_{+}^{2}}{\kappa_{5}^{2}r^{4}}\bigg(\frac{6}{2+\alpha^{2}}\frac{b^{2}}{r_{+}^{2}}L\bigg)
\end{eqnarray}
the $(\frac{\gamma_{proper}}{r^{2}}) \cdot r^3 \Omega_3$ has the physical meaning of proper internal energy which is viewed as the zero temperature energy of CFT \cite{Cai:2001jc}. Note also that the proper internal energy has no physical effects on the entropy, thus it needs to be subtracted from the total energy when considering the Cardy-Verlinde formula. Combine the physical quantity $\gamma, \gamma_{proper}$ with the energy density $\rho$ in $\eqref{rhoCFT}$, it's easy to find that the entropy density of brane universe in case of $r(\tau) \to \infty$ could be expressed as
\bea{}
\label{CarVerlinFormu}
\big(\frac{3}{2\pi}s\big)^{2}=\gamma \big(2(\rho_{CFT}-\frac{\gamma_{proper}}{r^{2}})-\frac{\gamma}{r^{2}}\big)
\end{eqnarray}
Compare with the original version of Cardy-Verlinde formula \cite{Savonije:2001nd}, our result $\eqref{CarVerlinFormu}$ has a extra physical quantity $\gamma_{proper}/r^2$. As explained in \cite{Cai:2001jc}, the $\gamma_{proper}/r^2$ is relevant with the proper internal energy which makes the contribution to the free energy of CFT system, but not to the entropy. Thus, the contribution of the proper internal energy must be subtracted when we consider the relationship between the entropy and energy of CFT system on brane. Besides, when $\alpha=0$, the $\eqref{CarVerlinFormu}$ will return the Cardy-Verlinde formula $(3.16)$ in \cite{Cai:2001jc}, which corresponds to the CFT system living on the boundary of AdS-RN black hole spacetime.

\section{Conclusion and Discussion \label{ConAndDis}}

In the background of charged AdS dilaton black hole solved by \cite{Gao:2004tu,Gao:2004tv,Gao:2005xv}, we study the movement of a self-graviting brane and holographic effects as the brane gets close to AdS boundary. Although the movement of brane/wall in this AdS dilaton black hole have been investigated by \cite{Xu:2019abl}, they ignore the self-gravitating effects of brane/wall. Specifically, they assume that there only exists matter field on brane, and the evolution of brane is controlled by the Israel junction condition only. But a more realistic case is that the effective gravitational field should also be localized on brane, thus the evolution of brane is determined by the effective Einstein field equation and Israel junction condition together. In our scenario, we derive the effective Einstein field equation on brane by using the method provided by \cite{Shiromizu:1999wj}, in which they localize the gravitational field by projecting the bulk's Riemann curvature and it's contractions (namely the Ricci tensor and scalar curvature) on brane spacetime. In results of \cite{Xu:2019abl}, they obtain the different evolution modes of brane/wall in various physical parameters, especially for $\omega=\frac{P}{\rho}$ and dilaton coupling constant $\alpha$. However, when taking inclusion of self-graviting effects of brane, we find that the evolution mode of brane is not so sensitive to the value of parameters $\alpha$ and $\omega$. Specifically, as shown in Fig.\ref{Solrtau}, we observe that the evolution of brane only in mode of decelerated expansion whatever the value of $\alpha$, while note that the velocity $\dot{r}$ of brane will tend to be zero as brane gets close to the AdS boundary. On the other hand, from the Fig.\ref{RhotPt}, it is obviously shown that the $\omega=\frac{P}{\rho}$ will approach a fixed vaule $-1$ as time increases.

Inspired by AdS/CFT correspondence, we expect to observe a connection between the brane universe and physical quantities of AdS dilaton black hole when the brane gets close to AdS boundary. Nevertheless, in our scenario of brane-bulk geometry, the AdS spacetime is cut off by a motional brane. And, the matter confined on brane is described by a general quantum field theory without conformal symmetry. Thus, as the brane move close to the boundary of AdS dilaton black hole, a renormalization procedure should be considered to cancel the IR divergences and restore the conformal symmetry. Note that the IR divergences on the gravitational side correspond to the UV divergence on the CFT side. Furthermore, as indicated in \cite{Savonije:2001nd}, when the brane approaches the AdS boundary, AdS/CFT correspondence implies that a radiation dominated FLRW-universe ($P=\frac{1}{3}\rho$) should be given. We add an appropriate surface counterterm to the gravitational action by using the method given in \cite{deHaro:2000wj, Gubser:1999vj, Anchordoqui}, after the inclusion of this counterterm, the correct energy density and pressure (namely $P=\frac{1}{3}\rho$) could be reproduced on brane in limit of $r(\tau)\to \infty$.  It's remarkable that this surface counterterm also plays a important role in caculating the black hole mass. What's more, basing on this holographic renormalization procedure, the evolution of brane's tension as the function of dilaton field could be given analytically in case of large $r(\tau)$.

By using a holographic method provided in \cite{Verlinde:2000wg}, the temperature, entropy, charge and chemical potential on brane could be given from the corresponding thermodynamic quantities of AdS dilaton black hole. With these thermodynamic quantities on brane, an extended Cardy-Verlinde formula is obtained in the large $r(\tau)$ limit. Meanwhile, our result has a similiar mathematical form with the one obtained in background of AdS-RN black hole \cite{Cai:2001jc}. This similarity is reasonable in physics, when making the dilaton coupling constant $\alpha=0$, the charged AdS dilaton black hole solution will return the AdS-RN one. Thus, when brane approaches the AdS boundary, we naturally obtain a similiar Cardy-Verlinde formula on brane like the one in \cite{Cai:2001jc} but with some corrections of dilaton field.

As discussions, in light of this work, we point out that the following extensions are still worthwhile to explore. The first one is, investigate the holographic complexity growth in the FLRW brane and black hole system constructed in this paper. Besides, as indicate in \cite{Kawai:2015lja}, in frame of AdS/CFT correspondence, the reheating process in brane-universe could be dual to the collapse of a spherical shell and formation of a black hole in AdS bulk. Thus, a valuable work is to study the holographic reheating in current brane-bulk system. What's more, it is an interesting topic to consider the movement of brane in background of asymtotically (A)dS black hole with scalar and electromagnetic hair  \cite{Brihaye:2019gla,Ferreira:2017cta,Herdeiro:2016plq}, and check that how the Cardy-Verlinde formula is affected by the scalar charge. Finally, it is also worthwhile to explore the movement of brane in the inner spacetime of some non-singularity black hole solutions \cite{Zeng:2018pzk,Zeng:2018kbv,Zeng:2016epp,Glavan:2019inb}.
\\
\section{Acknowledgements}
AC is grateful for Lei-Hua Liu and Carlos Herdeiro of the fruitful discussions and comments for this research topic and manuscripts, and thanks Ru-Yong Li for her help in adjusting the physical parameters in a picture. This work is supported by NSFC grant no.11875082. Besides, this work is also supported by The Center for Research and Development in Mathematics and Applications (CIDMA) through the Portuguese
Foundation for Science and Technology (FCT - Fundação para a Ciência e a Tecnologia), references UIDB/04106/2020 and UIDP/04106/2020.

redpajama_set_name: RedPajamaArXiv


text:
The Insider Blu-ray Review
By Tom Bricker Reviews 2 Comments
The Insider tells the true story of two men, 60 Minutes producer Lowell Bergman, played by Al Pacino, and former Brown & Williamson R&D man Jeffrey Wigand, played by Russell Crowe. The film details their they work to uncover and bring to light the truth about nicotine's addictive properties and Big Tobacco's attempts at a cover-up while its CEOs testify before Congress. The film is adapted from from Marie Brenner's "The Man Who Knew Too Much" and based on an actual 60 Minutes interview from 1995 with a tobacco industry whistleblower. Wigand and Bergman fight the good fight as just about everyone stands in their way–from those associated with Big Tobacco to CBS executives.
The resulting film is an intense yet almost documentary-like accounting that is an excellent film. The film is provocative and character-driven, and despite the dense subject matter and quiet tone, always keeps the viewer on the edge of their seat.
The video looks great here, with wonderful clarity and cinematic noise retained as intended. Viewers will notice that there are significant shifts in tint and color balance from scene to scene–these are entirely intended and they look great in the Blu-ray release.
Audio is similarly well-done, but The Insider was never intended to be an auditory assault, so don't expect a ton here. Disney's DTS-HD Master Audio 5.1 surround track mostly focuses its attention on the front channels, but since the movie is dialogue-driven, this should be expected.
The Insider isn't exactly a film that will push your home theater system to its limits, but what Disney has done here with the transfer and audio is solid.
Here's where The Insider Blu-ray is a disappointment: there are only 2 extras. A throw-away production video and a trailer. It's incredibly disappointing that such a provocative film with real, rich history received such poor treatment in the extras department. I'm sure there could be a two-hour (or more) documentary that would be incredibly interesting, and yet…nothing.
Overall, The Insider is an excellent film. However, it's likely that if you're a huge fan of it, you already own it or don't need this review to tell you to buy it. If you're not a huge fan of it, this Blu-ray release probably isn't for you. For most people, despite its excellent quality, The Insider is simply not a film that will be watched over and over again.
2 Responses to "The Insider Blu-ray Review"
mitch March 4, 2013
Very cool that you reviewed this but it's definitely way outside your usual content! I guess since it was distributed by buena vista entertainment it counts as "disney"
Tom Bricker March 4, 2013
That's exactly why.

redpajama_set_name: RedPajamaCommonCrawl


Medsquare participates for the second time in the RSNA exhibition, organized by the Radiological Society of North America.
From 30 November to 4 December 2014, Medsquare is honored to be part of the French Pavilion in Chicago, McCormick Place.
An annual exhibition in medical imaging, RSNA is the place to meet with more than 60,000 healthcare professionals in the medical imaging field coming from 100 countries worldwide.
On the program: Presentation and demonstration of our RDM solution to healthcare professionals in medical imaging.
On Sunday, 30 November 2014, at the Intercontinental Hotel (Michigan Avenue), Dominique Gabriel, CEO Medsquare, participates in the meeting that is organized by the SNITEM (National Association of Medical Technologies Industry) with the delegations of CNEH (Centre Nationale d'Expertise Hospitalière) and AFIB (French Association of Biomedical Engineers) .


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text:
Soft market pain evident in Swiss Re results
4th August 2017 - Author: Artemis
Almost a year ago one of our interviewees said the pain was becoming real and at the time it was beginning to be reflected in the results of major reinsurers. In 2017 this soft market pain is becoming increasingly evident, something noted in Swiss Re's results this morning.
The reinsurance firm has reported a decline in performance, income and returns, as reported this morning over at our other publication, all to a backdrop of a shrinking book of business, as it pulls-back from reinsurance and insurance business that does not meet its requirements anymore.
Swiss Re's net income for the first-half of 2017 comes out as $1.2 billion, down 35% year-on-year from $1.86 billion and a 10% miss to analyst consensus, while its return on equity of 7% is down from 10.9% in H1 2016.
It's a pretty big decline over a single year, particularly while at the same time the company has reduced its gross premiums written by 8.3% to $18.1 billion, which while it puts this pull-back down to "disciplined underwriting and active portfolio management," does also suggest that the potential for a return to profit levels seen previously is likely seriously diminished by a smaller book.
Consecutive years of pull-back in reinsurance underwriting to protect results is the most sensible response in a softening and challenging market. Underwriting at any cost would very quickly be a problem at a company the size of Swiss Re, so it's disciplined approach has been welcomed by shareholders.
The problem is that the market is not getting any less competitive and so to return its reinsurance book to anything like the size it was in prior years is likely becoming more difficult with each year of soft market that passes.
Now this may not be a problem for Swiss Re, which has a diversified book across its units and a growing primary insurance focus, but for pure-reinsurers that have been pulling back the chances of recouping business lost, which lets face it a lot has been lost to more efficient ILS fund players, looks pretty unlikely at this stage.
In P&C reinsurance the effects of the soft market are very clear, with these charts from Swiss Re's financial report, published this morning, making the decline and the pain very clear.
Swiss Re H1 2017 P&C reinsurance results vs prior years
The steady decline in profitability over the last four first-half's is stark, and it has to be remembered that this is in an environment where major catastrophe losses remain relatively low.
The lower price quality of the overall book will be responsible for much of the decline in earnings and income. It's quite amazing how much this has declined across just four years.
In a soft market, of course, terms and conditions have generally been expanding over the last four years, which could be reflected in the increasing combined ratio as well, which has the effect of reducing margin.
Alongside the reduction in pure margin of the reinsurance business underwritten, it's no surprise to see net operating margin and return on equity so much lower, even though we are not seeing any particularly large uptick in losses.
If this much pain is being felt by Swiss Re in its P&C reinsurance business, how much are smaller more catastrophe focused reinsurers feeling?
It's likely significant and results of some of the Bermudians also show a steady decline in margin and profits over the same period, with an uptick in combined ratio, despite the relatively benign loss environment.
In recent weeks we've even had ILS fund managers explaining that the pain they feel in the reinsurance renewal process is greater this year.
It's often the way, that when people begin to get to grips with operating in a more pressured and challenged environment, the rhetoric quietens down and you can be fooled into thinking it's all ok. It's seemed this way in reinsurance, as companies reported more than adequate results repeatedly, but when you look back at just how profitable this business was in prior years the pain becomes increasingly evident.
Swiss Re CEO Christian Mumenthaler, commented on the results, saying; "In the first half of 2017, we reported a solid result – despite the challenging market environment and having paid significant claims in the aftermath of natural catastrophes. While in the short term these drivers, especially the pricing pressures, are concerning and are being addressed, we are steering our company with long-term value creation in mind."
Major cat losses were felt, with a $360 million hit from Cyclone Debbie in Australia and attrition due to losses across the United States, from severe storms. But these aren't particularly major, in the scheme of larger loss events seen over the last 10 years.
Perhaps making things even more challenging, the Corporate Solutions build-out is yet to return dividends, as the unit again reported a worsening underwriting loss this half.
In this unit Swiss Re has perhaps begun to come up against even more competition, as more reinsurers looks to commercial insurance lines and even some ILS capacity begins to back commercial property risks in the U.S.
This suggests that the pressure is not going to let up anytime soon, and it may be necessary for companies like Swiss Re to continue to make moves to address ongoing pricing pressure for some time to come.
Looking at the decline in earnings versus the decline in the size of the underwriting book, it is evident that the price per unit of risk underwritten has declined enormously, which also perhaps reflects the amount of risk taken on per dollar of balance-sheet capacity deployed having increased as well, with terms expansion included there.
How sustainable is such a large portfolio generating this level of returns, should pricing not rebound significantly over the next ten years. How much more contraction of the underwriting book will be necessary and where does a major reinsurer like Swiss Re generate its earnings if not from its underwriting?
Once again we have to ask whether reinsurers need to shift their focus to earning fees for their clear risk expertise, rather than being paid for the use of their balance-sheets. If a more efficient underwriting capacity pool can be created (third-party of course), allowing reinsurers to earn fees and profit shares, could that become a viable contributor alongside putting the balance-sheet to work in diversifying areas?
Or can the advent of InsurTech help reinsurers to become so much more efficient they can improve earnings by cutting waste and by making the connections between risk and their capacity so slick that there is little intermediary costs in the way?
Big questions remain for the leadership at a company like Swiss Re. Questions that need answers as, if the rate of decline shown in the charts above continues, what options will be left?
Mumenthaler closed out the results release, saying; "We acknowledge that the market environment remains difficult. At the same time, we take decisive measures addressing the industry challenges head on. We will continue to be selective in choosing the risks we underwrite, aiming to ensure future profitability. We are equally determined to put our knowledge and leadership position to work and collaborate with our clients. I am confident the long-term trends for our industry are positive as risk pools will continue to grow."
Another question is; who will be originating, analysing, structuring, pricing and underwriting these risk pools, and who will be backing them?
Or perhaps a better question is; what is the most efficient form of capital to back many of the world's peak risks and emerging risk pools and, if that's not always a traditional reinsurance balance-sheet anymore, how can a reinsurer like Swiss Re position itself to still earn margin from these opportunities?
Tagged as: Alternative reinsurance capital, capital markets, ILS funds, insurance, reinsurance, Reinsurance renewals news
← Older article Meteo Protect pays out on Spanish olive grower parametric covers
Meteo Protect pays out on Spanish olive grower parametric covers
The Agricultural Association of Young Farmers (ASAJA-JAEN), a Spanish olive growers' cooperative, has announced that 100% of its members that...


text:
Q: Intellij add standard attributes to html tag via plugin In IntelliJ,
when I type <in it auto suggests me the <input> -field. If I press tab/enter, I get what was proposed.
I am coming from atom for frontend stuff, where if you press enter there,
you get the input field with the basic attributes, like this:
<input type="" name="" value="">

Is there a plugin / setting for intellij to do the same?
I am already using live template/edit, this does not seem to do the trick.

A: Don't enter the opening angle bracket, just enter in, hit Ctrl+Space, then choose input Emmet live template from completion list. By default, it will expand to <input type="text">, but you can change the input live template in Settings | Editor | Live Templates, Zen HTML to add more predefined attributes to it, like:
<input type="$VAR0$" name="$NAME$" value="$VALUE$">

redpajama_set_name: RedPajamaStackExchange


text:
Courier & Press High School Sports Blog
Memorial's Sullivan receives three more scholarship offers
April 30, 2015 Gordon Engelhardt	Leave a comment
The offers continue to pour in for Emily Sullivan, Memorial's 6-foot-4 junior center. Minnesota, St. John's and Miami (Ohio) are the latest group of schools to join the battle for her services. They all offered her a scholarship on Thursday, hiking the overall total to 11 schools.
She has also received offers from IUPUI, Boston University, the University of Evansville, Cal State Bakersfield, Indiana State, Valparaiso, Arkansas and Iowa State.
Sullivan, a member of the Indiana South Junior All-Stars, averaged 13.9 points, 12.0 rebounds and a school-record 6.0 blocks in leading the Tigers to a 19-6 record.
The Indiana Junior Stars will play the Indiana (senior) All-Stars on June 8 at Richmond and June 10 at Columbus North.
South Spencer, Jasper climb IHSBCA poll
April 27, 2015 Pat Hickey	Leave a comment
The Indiana High School Baseball Coaches Association Top 10 poll after week four. Records are through games of Saturday, April 25, with total votes in parentheses and the team's previous week ranking (NR-RV: not ranked-received votes).
1. Indianapolis Cathedral 12-0 (180) 2
2. Floyd Central 12-1 (156) 1
3. LaPorte 14-1 (132) 6
4. Lake Central 6-1 (96) 3
5. Lawrence North 12-0 (90) 9
6. Columbus North (74) 8
6. Zionsville 6-1 (74) 5
8. McCutcheon 9-2 (32) NR-RV
9. Bedford North Lawrence 9-3 (30) 4
10. Harrison (West Lafayette) 10-3 (26) 10
Dropped out: Castle (7).
Received votes (alphabetically): Avon, Brownsburg, Carroll (Fort Wayne), Castle, Center Grove, Evansville North, Homestead, Lawrence Central, Mishawaka, Munster, Terre Haute South.
1. Crawfordsville 13-0 (98) 1
2. Hanover Central 12-0 (92) 2
3. Jasper 11-0 (72) 5
4. Andrean 11-2 (60) 4
5. Silver Creek 12-1 (54) 3
6. Yorktown 8-2 (26) 10
6. Norwell 7-2 (26) 6
8. Peru 6-1 (24) NR-RV
8. North Harrison 10-2 (24) 9
10. Charlestown 8-3 (16) 7
Dropped out: Lebanon (8).
Received votes: Fort Wayne Dwenger, Griffith, Lebanon, Leo, Maconaquah, Mitchell.
1. Knightstown 8-0 (110) 2
2. South Spencer 10-2 (88) 3
3. Alexandria 9-2 (82) 1
4. Wapahani 10-3 (80) 4
5. Lafayette Central Catholic 10-4 (70) 5
6. Fort Wayne Canterbury 6-1 (44) 6
7. Sullivan 10-2 (36) 7
8. Lapel 9-1 (26) NR-RV
8. Cass (Lewis-Cass) 3-0 (26) 10
10. Austin 7-1 (18) NR-RV
Dropped out: Centerville (8), Eastern (Greene) (9).
Received votes: Centerville, Churubusco, Eastern (Greene), North Newton, Shenandoah, Woodlan.
1. Orleans 8-0 (110) 2
2. South Central (Elizabeth) 9-3 (108) 1
3. Rockville 8-1 (98) 3
4. Pioneer 7-1 (76) 4
5. Shakamak 1-2 (48) 5
6. Frontier 9-4 (46) 6
7. Fort Wayne Blackhawk Christian 0-3 (32) 10
8. Rising Sun 7-2 (30) NR-RV
8. Barr-Reeve 2-2 (30) 8
10. Hauser 6-4 (28) 7
Dropped out: Daleville (9).
Received votes: Caston, Daleville, Jac-Cen-Del, Morgan Township, North White, Northeast Dubois, Tecumseh.
Reitz sixth man Barnes headed to Lincoln Trail College
Mario Barnes, a senior guard who helped lead Reitz High School to a berth in the Class 4A state championship game, has committed to Lincoln Trail, a junior college in Robinson, Illinois. The Panthers' sixth man most of his senior year, he averaged 7.2 points after averaging 10.5 as a sophomore and 10.2 as a junior. His career mark was 8.9.
Lincoln Trail should be a good fit for the speedy Barnes, who becomes the fifth Reitz senior to announce he will go on to play college basketball. Jaelan Sanford is headed for the University of Toledo. Nate Hansen to Vincennes U., and Alex Stein and Jacob Norman to the University of Southern Indiana.
Dru Smith, an Indiana South Junior All-Star, is getting looks from Indiana State, among others. If he continues to improve, junior guard Blake Ruckman could also go on to play college ball.
South Spencer's 7-run 7th stuns Titans
Hannah Epperson's two-run double highlighted a seven-run seventh as visiting South Spencer snapped a scoreless tie to beat Pocket Athletic Conference rival Gibson Southern, 7-0, in a regular season softball showdown of epic proportions on Thursday night.
"We faced a really good pitcher (Jaime Nurrenbern) and it took a while to make adjustments," said Rebels coach Tara Compton. "We saw her a couple of times and were finally able to get something rolling toward the end of the game."
Kaylea Horn fired a three-hitter for Class 2A No. 1-ranked South Spencer (10-0, 3-0). The Rebels avenged a 3-2 9-inning loss to Gibson Southern last year. The 3A No. 2-ranked Titans are 11-3, 2-2.
Gibson Southern went on to win the PAC title last season and finished as 3A state runners-up. South Spencer went on to win the 2A state championship.
Memorial's Stachowski to attend Wabash College
Memorial senior Ben Stachowski announced that he will play baseball and basketball next season for Wabash College, a NCAA Division III member.
A 6-foot-3 guard, Stachowski averaged 13.5 points in 15 games in helping lead the Tigers to an 18-7 record in basketball. He battled a variety of injuries in both sports, but once he became healthy last winter Memorial's basketball team took off, winning eight in a row before losing to Vincennes Lincoln in the Class 3A regional finals.
"Wabash is a D-III school with a good mix of academics and sports," said Dave Stachowski, Ben's father.
Pendleton transfers to Minnesota State-Mankato
Bosse High School graduate Jalen Pendleton has announced that he is transferring from Southern Illinois University to Minnesota State-Mankato. Since he is transferring from a NCAA Division I school to a Division II school, he will not have to sit out next season.
Pendleton, a 6-foot-2, 205-pound guard, will have one year of eligibility remaining. He averaged 9.1 points as a sophomore for the Salukis and was named to the Missouri Valley Conference All-Bench Team. But his scoring average dipped to 6.6 as a junior, even though he started 14 games. He also averaged 2.9 rebounds.
Minnesota State-Mankato finished 24-8 last season, advancing to the Division II tournament. Pendleton is one of five former Salukis who elected to transfer at the conclusion of the 2014-15 season. He lifted Bosse to the Class 3A semistate in 2012.
SIU finished 12-21 this past season.
Jasper trending up in latest IHSBCA poll
Jasper's Cal Krueger delivers a pitch to a Castle batter in the second inning of their game at Castle High School Thursday evening. DENNY SIMMONS / COURIER & PRESS
The Indiana High School Baseball Coaches Association Top 10 poll after week three. Records are through games of Saturday, April 18, with total votes in parentheses and the team's previous week ranking (NR-RV: not ranked-received votes).
2. Indpls. Cathedral 10-0 (126) 2
4. Bedford N. Lawrence 9-1 (80) 8
6. LaPorte 10-1 (54) NR
7. Castle 8-3 (50) T4
8. Columbus North (48) T4
9. Lawrence North 10-0 (42) NR-RV
10. Harrison (West Lafayette) 9-1 (26) NR-RV
Dropped out: Noblesville (T4), Hobart (9), Munster (10).
Receiving votes (alphabetically): Evans. North, Hamilton Southeastern, Hobart, McCutcheon, Mishawaka, Munster, Noblesville, Terre Haute South.
2. Hanover Central 9-0 (76) 5
3. Silver Creek 9-1 (74) 2
4. Andrean 3-1 (72) 1
5. Jasper 8-0 (46) NR-RV
7. Charlestown 6-3 (32) 10
8. Lebanon 5-2 (28) 4
9. North Harrison 9-1 (24) NR
10. Yorktown 6-2 (20) 6
Dropped out: Griffith (3), Batesville (9).
Received votes: Fort Wayne Dwenger, Griffith, New Palestine, Peru, West Vigo.
1. Alexandria 6-0 (100) 2
2. Knightstown 5-0 (78) 5
3. South Spencer 5-2 (68) 3
4. Wapahani 6-3 (62) 1
5. Lafayette Central Catholic 7-4 (56) 6
7. Sullivan 8-1 (38) NR
8. Centerville 6-3 (22) 10
9. Eastern (Greentown) 5-1 (20) NR
10. Cass (Lewis-Cass) 2-0 (18) NR-RV
Dropped out: Mater Dei (4), Indpls. Cardinal Ritter (8), Forest Park (9).
Received votes: Austin, Evans. Mater Dei, Lapel, Lewis Cass, North Knox, Providence, Woodlan.
6. Frontier 7-3 (66) T5
7. Hauser 6-2 (58) 10
9. Daleville 4-2 (26) T5
10. Fort Wayne Blackhawk Christian 0-1 (26) 9
Dropped out: None.
Received votes: Jac-Cen-Del, North Daviess, North White, Northeast Dubois, Rising Sun, South Newton.
Memorial's Sullivan gets offer from IUPUI
Emily Sullivan, a 6-foot-4 junior center from Memorial High School, has been offered a scholarship by IUPUI.
She was previously offered by Boston University, the University of Evansville, Cal State Bakersfield, Indiana State, Valparaiso, Arkansas and Iowa State. Northwestern head coach Joe McKeown has made an in-house visit to Sullivan.
She averaged 13.9 points, 12.0 rebounds and a school-record 6.0 blocks last season and is a member of the Indiana Junior South All-Stars.
Pierce sets Castle school record
Castle High School senior Quentin Pierce set a new school record with a time of 4:16.1 on Friday at the "Miracle Mile" at Franklin Central. He placed fourth among 60 runners. David Goodman held the old mark of 4:18.1 in 1995.
Pierce, who signed with Indiana State University, placed 10th in the 1,600 meters at the 2014 state track meet in Bloomington. He was a school-record best 11th at the state cross country meet last fall.
Chezem moves from Covington to Loogootee
Kent Chezem, who guided Covington High School to the No. 1 ranking in Class A at the conclusion of this past regular season, was named Loogootee's new boys' basketball coach at a school board meeting Friday.
During his tenure at Covington, his teams posted a record of 152-94 in 11 seasons, including 52-14 the past three years. The Trojans won three sectional championships and advanced to the final eight in postseason in 2005 and 2010.
He will inherit three starters from last season's Loogootee team that finished 8-15 under interim coach Michael Hopkins.
"The tradition at Loogootee and their love of basketball is second to none," said Chezem, 46. "Everybody in the state of Indiana and beyond knows about what coach Jack Butcher has done there. It was a once in a lifetime opportunity for me to have a chance to lead the program."
Hopkins stepped into the breach when former coach Mike Wagoner abruptly resigned in September to become an assistant at South Knox. Wagoner guided Loogootee to a 90-44 record in six seasons, including the Class A state championship in 2012.
Loogootee's gym is named Jack Butcher Arena, after the legendary figure who is Indiana's all-time winningest coach with a 860-250 record in 45 years. Butcher, who retired following the 2002 season, guided the Lions to a berth in the single-class 1975 state championship game.
SIAC, Big 8, Pocket, Blue Chip, Patoka Lake and Southwest Conferences
SIAC Standings
SIAC Leaders
Big Eight Standings
Big Eight Leaders
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Pocket Leaders
C&P HS Sports Articles
Engelhardt's AP boys' basketball ballot
Baseball regional pairings, possible contingency plans
Reitz at Castle softball ppd. to Friday
Cheaney was No. 7 on Harrison's career scoring list
IHSAA regional boys' basketball pairings


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Q: Difference between proto link and Object.create I want to know the difference between __proto__  and Object.create method. Take this example:
var ob1 = {a:1};
var ob2 = Object.create(ob1);

ob2.__proto__ === ob1; // TRUE

This implies Object.create method creates a new object and sets __proto__ link to the object received as parameter.
Why don't we directly use __proto__ link instead of using create method ?

A:
Why don't we directly use proto link instead of using create method ?

Because __proto__ is a non-standard  property and therefore not necessarily available in every browser.
However it seemed to be considered for ES.next. More info: MDN - __proto__.

A: __proto__ is nonstandard and won't be supported everywhere.  Object.create is part of the official spec and should be supported by every environment going forward.
It also is implemented differently in different places.
From Effective Javascript:

Environments differ for example, on the treatment of objects with a
  null prototype.  In some environments, __proto__ is inherited from
  Object.prototype, so an object with a null prototype has no special
  __proto__ property

Moving forward the accepted way  to create objects and implement inheritance is the Object.create function, and if you do need to access the prototype, you'll want to use Object.getPrototypeOf  These functions are standardized and should work the same in all modern environments


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China criticizes US, German embassies for 'interference'
BEIJING — China's foreign ministry accused the American and German embassies on Thursday of interfering in its affairs after they objected to the prosecutions of an activist and a lawyer who handled sensitive cases.
Ministry spokeswoman Hua Chunying told reporters a joint statement by the embassies calling for Wu Gan's release and for lawyer Xie Yang to be allowed to return to work was irresponsible.
Wu, who criticized Chinese officials online, was sentenced Tuesday to eight years in prison on subversion charges. Xie was convicted of inciting subversion but spared a prison term after he admitted committing the offence.
"The embassies of those two countries are diplomatic missions, which have no right to point the fingers at China's internal affairs and judicial sovereignty," Hua said. "We hope the relevant embassies can have a clear understanding of their duties and do something to help improve mutual trust, mutual understanding and co-operation, not the opposite."
The embassies' statement criticized the "serious mistreatment" of Wu and Xie in detention.
"We urge Chinese authorities to view lawyers and rights defenders as partners in strengthening Chinese society through development of the rule of law," the statement said.
Wu, who called himself the "Ultra Vulgar Butcher," was among the first activists and lawyers caught up in a government crackdown that began in 2015. His one-day trial was held in August.
The court said Wu made comments online that "attacked state power."
Activists such as Wu focused on individual cases instead of challenging Communist Party policy at the national level, making them a greater headache for local officials than for Beijing. But their ability to organize people apparently made authorities nervous.
Statement from embassies: http://bit.ly/2pPM7dS


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Yet another Sunday night show to set the tone for the week. If last night's show is any indication of how this week will go, I think I can go ahead and expect a fairly laid back and chill week. After last week being an insane week full of shows all over town and all over the place as far as genre is concerned, I think a chill week sounds pretty freaking amazing.
North Carolina based Jenny Besetzt opened up the show starting promptly at 8PM. I was instantly struck by singer John Wollaber's voice. It was unlike anything I had ever heard before and, whether I liked it or not, it caught my attention. His voice was dark and boomy. Honestly, if there was ever a genre entitled "doom indie" he would be the king of it. Even with the dark lowness of his voice, there was an undeniable sense of elegance behind it. After doing a bit of research this morning, it only makes sense that he had been born to an opera singer. You can hear the classical training but it's as if John has taken that and made it his own leaving fans with a completely new and different experience.
John's voice along with the tasteful instrumentation that came from the other three band members on stage had the sold out First Avenue crowd lost in a wave of music. It was layers on top of layers and, although there wasn't much movement on stage, you could see the movement in the music. The layers would come into the audience like waves, at some points the waves were heavier than others and you were left with an almost dark feeling inside you but, in just a couple of notes, a lighter wave would hit you lifting you right back up. It's quite amazing when a band has a live show that can have this kind of effect on you. Regardless if the music is what you listen to or not, you can't leave when experiencing something like this. It's truly just that– an experience and one that should not be overlooked.
I may never know why the band name is Jenny Besetzt as there is nobody name Jenny in the group but, let's be honest, what's in a name? Judging by their Facebook and other social media accounts, this group is still a wee baby in the scene but, after this tour and past tours with other huge bands, it's clear to see that they will be taking off sooner rather than later. I just hope that, with new found fame, they keep the raw power and emotion alive through their live show. That'll be what keeps me coming back.
Synthpop/ post-wave darlings Future Islands closed out the quick show with a powerful performance that had me begging for more. I'll be the first to admit (if you can't already tell) that last night wasn't a show I would typically go to. Honestly, I had the night off and was itching for some live music after skipping out on Saturday night's show due to exhaustion and pure laziness. I went into the show without any expectations other than some live music and catching up with my friend and fellow blogger/ photographer. Jenny Besetzt was fine but I found myself spending more time socializing during their set than actually paying attention. That's not to say that I didn't like the music or the soundscapes they were creating, because I did. There just wan't really anything to watch beyond the band members standing on stage and swaying with the music. Future Islands was the complete opposite and exactly what I needed to end my Sunday night and start my week off right.
Although Future Islands is from Baltimore, Maryland, they have a very exotic sound about them that makes you think they are from another planet. Much like John from Jenny Besetzt, Future Island singer Samuel Herring has an unnaturally low voice that seems to transport you to a faraway place with ease. His low and almost sinister voice didn't quite match the upbeat pop music being played behind him but neither did his dark and melancholy lyrics. This complete set of clashing words, sounds and music had me instantly sold on Future Islands. Beyond the mind-fucking music and lyrics was Samuel's pure fury on stage.
Sure, Future Islands' music isn't metal. Nothing about it is metal. That being said, I would love to see Samuel front a metal band. The amount of energy this guy showed on stage had my jaw on the floor within the first song. He seemed to attack every word he sang with a punch and, in turn, he would punch at the air or crouch down low and give the sold out crowd a sinister smile. It was quite amazing to see this one man completely control the older crowd the way he did. It was all eyes on him and, to help, the two other members of the band stayed a couple feet behind him and in the darkness as to just highlight Samuel's talent and passion.
The older crowd stood there with mouths open and beers in their hands as Future Islands powered through their set. Other than the occasional nodder and toe tapper, there really wasn't much movement coming from the audience but there was really none needed. The energy that Samuel had was more than enough to fill the entire First Avenue Mainroom and then some.
Future Islands has been around since 2006 and, with five full length albums out, have clearly already made their mark on the scene. With such a history and so many iconic albums out, choosing a set list for a band like this must be tough but, judging by the reaction of the crowd, Future Islands did the best they could. With an eighteen song set followed by a four song encore, the band did their best to keep everyone in the crowd happy.
You caught me, I'm not going to start listening to Future Islands on a daily basis as their music just doesn't get me going like some good old-fashioned pop punk does. That being said, as soon as they announce another show in town, I'll be snagging a ticket. Never judge a band based on their music– judge them on their live show. Sometimes passion and conviction can outweight the music and have you falling in love with a band that you would have never given the time of day to. Thank you Future Islands for having such a powerful show. See you next time!
Jenny Besetzt
Future Islands
Venue: First Avenue
Sausage Fest Meter- 7 out of 10
Average Age of the Crowd- 38
Crowd Surfers- 0
Stage Divers- 0
Broken Bones- 0
Spotted Flying Through The Air- Nothing
Fights-0
Pukers- 0
Drunkards Taken Out By Security- 0
Celebrity Sightings- None
Overall Score- 7 out of 10
Show on Deck- Pho/ Black Market Brass
concert review, Concert Reviews, first avenue, Future Islands, Jenny Besetzt, live music, minneapolis, minnesota, music, music review, twin cities


Michael G. Ruppert is the president of Ruppert & Schaefer, P.C., located in Indianapolis, Indiana. He, and all of the attorneys in the firm, devote their law practices solely to advising and representing people throughout Indiana who are confronted with legal matters involving practically any aspect of family law. He practices before all Indiana trial and appellate courts; is board certified as a family law specialist by the Family Law Certification Board of the Indiana State Bar Association; and, possesses a wealth of legal knowledge gained prior to specializing in family law by performing a wide variety of legal services for individuals and businesses.
Although a tenacious courtroom advocate, Mr. Ruppert is just as skillful at the resolution of family law disputes--whether the division of marital property, the determination of child custody and support or the need for spousal maintenance--through negotiation, mediation and arbitration. He has received training to serve as a family law Mediator and Arbitrator. In addition to preparing property settlement agreements, parenting time agreements and Qualified Domestic Relations Orders ("QDROs") in dissolution of marriage (divorce) cases, he has counselled many clients about protection of their assets before marriage and prepared prenuptial (i.e., premarital) agreements to suit their particular needs. The full range of services provided by Mr. Ruppert and his firm includes handling appeals of trial court decisions in family law cases. He has represented family law litigants in the Indiana Courts of Appeal and Supreme Court, resulting in favorable published and unpublished decisions.
In addition to delivering numerous oral and written presentations on family law topics for Continuing Legal Education courses, he is a graduate of the National Institute of Trial Lawyers, wrote the family law materials and taught for the IBA Bar Examination Review Course and has authored a number of articles concerning family law topics published in the Indiana Law Review.
Mr. Ruppert received a Bachelor of Arts degree from Indiana University at Bloomington; and, was awarded a Juris Doctorate degree from Cleveland-Marshall College of Law, where he was the editor-in-chief of the law school's newspaper, The Gavel. Mr. Ruppert is an active participant in the Indianapolis Bar Association, Hamilton County Bar Association and other legal organizations.


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FAQs about Bishops
Below you will find some responses to common (and not so common) questions about bishops and their role in The Episcopal Church. We encourage you to also read the Rite for the Ordination of a Bishop beginning on page 512 of the Book of Common Prayer.
As we explore, we invite you to follow the pattern of the ordination service which invites us to begin by offering our prayers to God.
O God of unchangeable power and eternal light: Look favorably on your whole Church, that wonderful and sacred mystery; by the effectual working of your providence, carry out in tranquillity the plan of salvation; let the whole world see and know that things which were cast down are being raised up, and things which had grown old are being made new, and that all things are being brought to their perfection by him through whom all things were made, your Son Jesus Christ our Lord; who lives and reigns with you, in the unity of the Holy Spirit, one God, for ever and ever. Amen.
Book of Common Prayer: Ordination of a Bishop (p. 515)
What is a bishop?
A bishop is one of the three orders of ordained ministers in the church, the other two being deacons and priests. In the Rite for the Ordination of a Bishop in the Book of Common Prayer, a bishop is called to "guard the faith, to provide for the sacramental life of the Church, to ordain, to be a pastor, and to exemplify the Christian life."
What does a bishop "do?"
Bishops "do" a lot; and not all of it is easily categorized. One of a bishop's primary responsibilities, as it is for all Christians, is to proclaim the Good News of Christ's life, death, and resurrection in their life and work. Bishops provide spiritual leadership to the community; calling, developing, and encouraging both lay and ordained to engage more deeply in God's mission of love, justice, reconciliation, and restoration in our local context, our country, and across the world. They encourage us to follow the leadings of the Holy Spirit, with scripture, tradition, and reason as our guides. They also ensure we are living into our agreed upon way of being together as gathered community by upholding the Constitution and Canons of The Episcopal Church and The Episcopal Church in Connecticut.
Is a bishop a CEO?
No. The church is not a business, and thus our leadership does not follow the pattern of a business. A bishop is a member of the gathered community and a bishop's role grows out of that particular community, not apart from it. Bishops anchor us to the past, continuing the line of apostolic succession dating back to the first apostles. They also call us into the future, inviting us to discern together where God is moving and how we are invited to participate in God's mission. Bishops also serve as the bridge between communities of faith locally, nationally, and internationally as part of their role as leaders in the Church.
What do we look for in a bishop?
While there are gifts a successful bishop may possess, the most important characteristics of a bishop are the same as those of every Christ-follower; a life rooted in Christ, formed by Word and Sacrament, and sustained by prayer.
Are there different kinds of bishops?
Kind of. Bishops within a particular diocese may hold different titles and function in slightly different ways, as we experience here in Connecticut. Our own Bishop Laura J. Ahrens is a Bishop Suffragan. While bishops may have different titles, all are ordained utilizing the same service from the Book of Common Prayer and their primary responsibility is always to serve as apostles, pastors, and leaders in the Church.
Diocesan Bishop: the primary bishop of a diocese; sometimes referred to as "The Diocesan."
Bishop Coadjutor: A bishop elected to succeed the Diocesan Bishop. An ordained person consecrated to become the next bishop of a diocese when the diocesan bishop retires or resigns.
Bishop Suffragan: A bishop elected to assist the Diocesan Bishop and to serve under the Diocesan's direction. A working co-bishop in a diocese but without inherent right of succession when the diocesan bishop retires or resigns.
Assistant Bishop: A bishop appointed by the Diocesan Bishop with the consent of the Standing Committee to assist the Diocesan and to serve under the Diocesan's direction, creation of the post having been approved by the Diocesan Convention. A specially ordained or otherwise specially designated person who has the spiritual and liturgical authority of a bishop and who usually assists the Bishop of a diocese; some retired diocesan bishops become assistants to other bishops; some assistant bishops are specially ordained for their work. Assistant Bishops can perform most functions performed by other bishops.
Assisting Bishop: A bishop appointed by the Diocesan Bishop to provide short-term assistance with episcopal duties in the Diocese.
What's up with the hat and the stick?
Two symbols have long been associated with a bishop: the "hat," also known as a mitre and the "shepherd's crook," also known as a crozier. The mitre is a pointed, shield-shaped hat with two lappets (flaps) which hang down. The lappets are said to symbolize the tongues of fire which landed on the apostles at Pentecost. The crozier represents a bishop's role as shepherd of the flock.
Learn more about Bishops
"Task Force on the Episcopacy" from The Protestant Episcopal Church.
"The Ordination of a Bishop" from the Book of Common Prayer


PORT OF SPAIN Trinidad, CMC – On Sunday, Trinidad and Tobago's Prime Minister Dr. Keith Rowley announced he would be traveling to the United States on Tuesday to undergo medical cardiac related tests.
"I should have gone back to do these tests last year September, but that was the budget time and so on and so on and I put it off," he said, adding that after the budget, he had to deal with the revamping of the state-owned oil company, PETROTRIN that had been losing billions of dollars annually (One TT dollar=US$0.37 cents).
"So, I really should have done that last year, so when I look back and realize it is a year and a half, I really did not take the advice that I got in 2017. So, I am going to take it now," he said, adding that he would be out of the country "for a couple of days".


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30th Anniversary of Patti Smith's Proto-Punk Masterpiece, 'Horses,' Celebrated With Release of 'Horses Horses' on Arista/Columbia/Legacy
Two-Disc Legacy Special Edition Features Newly Remastered 'Horses' Album + 'Horses' 30th Anniversary Performance Recorded Live at 2005 Meltdown Festival
'Horses Horses' In Stores November 8
November 2005 marks the 30th anniversary of the release of Patti Smith's debut album, Horses, a groundbreaking rock & roll masterpiece which continues its unparalleled influence on rock music, style and culture. Arista/Columbia/Legacy Recordings will celebrate this musical milestone with the release of Horses Horses, a two-disc Legacy Special Edition of Patti Smith's debut album, on Tuesday, November 8.
Disc One of Horses Horses features the original album, in its entirety, along with the bonus track, Patti's interpretation of the Who's classic "My Generation." Initially released as the B-side to "Gloria," the first single from Horses, in 1975, "My Generation" features John Cale, the album's producer, on bass. The Legacy Special Edition of Horses has been remastered by Greg Calbi producing superior sound to previous editions of the album.
The second disc of Horses Horses showcases Patti Smith and her Band -- Lenny Kaye (guitar), Jay Dee Daugherty (drums), Tony Shanahan (bass), Tom Verlaine (guitar) and featuring Flea from the Red Hot Chili Peppers -- performing the complete Horses album live, with a "My Generation" encore, at the Royal Festival Hall in London on June 25, 2005. This historic performance of Horses was the culminating concert at the 2005 Meltdown Festival, which was curated by Patti Smith. (Lenny Kaye and Jay Dee Daugherty were both members of the ensemble that played on the original Horses while Tom Verlaine was a guest artist on the 1975 album).
Horses Horses comes packaged with a deluxe booklet featuring rare archival photographs, ephemera, lyrics and documentation of the 2005 concert as well as Paul Williams' provocative essay on "Gloria."
http://www.pattismith.net/
http://www.columbiarecords.com/
SOURCE: Columbia Records
CONTACT: Benny Tarantini of Columbia Records, +1-212-833-5858,
Benny.Tarantini@sonybmg.com
Web site: http://www.columbiarecords.com/