text:
\section{Introduction}

As examples of AdS/CFT correspondence \cite{ads-cft},
it is pointed out, e.g.\cite{hmns_cft_Ebh,csz,gg_rn_cft,chz,cs},
that the near-horizon dynamics of the charged (RN) black hole
is equivalent to that of the boundary CFT. For the extremal black hole,
the corresponding CFT is a chiral one \cite{hmns_cft_Ebh,csz,gg_rn_cft,cs}.
For the near-extremal black hole,
the corresponding CFT has two sectors (left and right)\cite{chz}.

Recently, new checks of AdS/CFT correspondences are suggested
by studying the decay rates of particles excited by some
star orbiting the black holes, see \cite{ps_kerr_cft,bgx_scalar_KN} etc.
In this paper, along this direction, we compute the decay rates of
the charged scalar particles in two kinds of RN/CFT correspondences
mentioned above \cite{hmns_cft_Ebh,csz,gg_rn_cft,chz,cs}. For these two kinds of
correspondences, on the gravity side, the four dimensional theory
is lifted to a five dimensional one with an extra compact direction
introduced. So, the
$U(1)$ gauge symmetry in the four dimensional theory becomes an isometry
of the five dimensional RN spacetime metric. It is interesting
to investigate how this geometrization of the 4D gauge symmetry appear
in the computation of the decay rates on the CFT sides.

In the section \ref{sect-nhern}, we consider the near-horizon extremal
RN/Chiral CFT correspondence (NHERN/$\chi$CFT).
In the section \ref{sect-nhnern}, we
consider the near-horizon near-extremal RN/CFT correspondence
(NHNERN/CFT).
For both kinds of correspondences, decay rates computed on the gravity side
match precisely to those computed on the CFT side, respectively.
We give some remarks on the difference of these two kinds of
correspondences in the final section
\ref{sect-discuss}.

\section{Near horizon extremal RN/$\chi$CFT}
\label{sect-nhern}

In this section, we will consider the correspondence between
the dynamics of the near-horizon extremal RN black hole and that of the
boundary chiral CFT. Decay rates of a charged scalar wave are computed
on both sides.

\subsection{Decay rate on the gravity side}

The extremal RN black hole is the vacuum solution of the Einstein-Maxwell
theory and is described by the following metric
and the gauge field strength,
\begin{equation} \begin{array}{l}
ds^2=-(1-Q/\hat r)^2d\hat t^2+(1-Q/\hat r)^{-2}d\hat r^2 +\hat r^2d\Omega_2^2
\\[10pt]
F=\dfrac{Q}{\hat r^2}d\hat t\wedge d\hat r
\label{Ern-sol}
\end{array}\end{equation}
where $d\Omega_2^2=d\theta^2+\sin^2\theta\, d\varphi^2$ is the round metric
of the two sphere, and one has set the Newton constant $G_N=1$,
the position of the event horizon is located at $\hat r=M=Q$.
To discuss the near horizon dynamics, taking the limiting process by defining
\cite{gg_rn_cft,csz},
\begin{eqnarray} \label{near-horizon-coord}
r={\hat r-Q\over\epsilon}\,,\qquad
t={\epsilon\over Q^2}\hat t
\end{eqnarray}
with $r, t$ fixed when $\epsilon\to 0$. In terms of this new coordinate system,
the metric of black hole and Maxwell field strength becomes,
\begin{eqnarray} \label{NHErn-sol}
ds^2&=&Q^2\left(-r^2dt^2+\dfrac{dr^2}{r^2} +d\Omega_2^2\right)
\\[10pt]
F&=&Qdt\wedge dr
\end{eqnarray}
which shows that the near-horizon geometry is $AdS_2\times S^2$ and the
isometry group is $SL(2,\mathbb{R})\times SO(3)$.
The gauge potential one-form can be chosen as
\begin{eqnarray}
A = -Qr dt
\end{eqnarray}
by taking a proper gauge.

Let us consider a star carrying electric charge $e_0$ with mass $\mu_0$,
which is moving around the black hole along an circular orbit
at the near horizon region. For the two Killing vectors,
$\xi_{(t)}=\partial_t$ and $\xi_{(\varphi)}$, there are two conserved quantities
\cite{mtw_gravitation},
\begin{eqnarray}
E_0&=&-g_{\alpha\beta}(u^\alpha+q_0A^\alpha)\xi_{(t)}^\beta
=-Q^2 r_*^2\left(\dot t_*+{q_0\over Qr_*}\right)
\\[5pt]
L_0&=&g_{\alpha\beta}(u^\alpha+q_0A^\alpha)\xi_{(\varphi)}^\beta
=Q^2\sin^2\theta_*\dot\varphi_*
\end{eqnarray}
where $E_0$ and $L_0$ are energy and angular momentum per unit mass of the star
respectively, $q_0=e_0/\mu_0$, constants $r_*$ and $\theta_*=\pi/2$
are radial and angular position of the star respectively.
$L_0$ and $E_0$ are constrained by the on-shell condition,
$-1=Q^2(-r_*^2\dot t_*^2+\sin^2\theta_*\,\dot\varphi_*^2)$. In the
following, without loss of generality, we will set $E_0=0$,  then one have
solution,
\begin{eqnarray}
\dot t_*=-{q_0\over Qr_*}\,,\qquad
\dot\varphi_*={L_0\over Q^2}
\end{eqnarray}
with $L_0=Q\sqrt{q_0^2-1}$. We will consider real angular momentum $L_0$,
i.e., $q_0>1$.

Assume that the coupling of the star with a charged scalar field $\Phi$ is defined by
the following action,
\begin{eqnarray}
S_\Phi &=& -\int d^4x\sqrt{-g}\,(\nabla_\mu+ieA_\mu)\Phi^*(\nabla^\mu-ieA^\mu)\Phi
\nonumber\\[5pt]&&
+\,4\pi\lambda\int d\tau\int d^4x\,\delta^4(x-x_*) \Phi^* + {\rm c.c.}
\end{eqnarray}
where $e$ is the electric charge of the scalar field, $\lambda$ is the
coupling constant, `c.c.' indicates complex conjugate of the previous term.
The equation of motion reads
\begin{eqnarray}
\sqrt{-g}\,(\nabla_\mu-ieA_\mu)(\nabla^\mu-ieA^\mu)\Phi
&=&-4\pi\lambda\int d\tau\, \delta^4(x-x_*)
\nonumber\\[5pt]
&=&-{4\pi\lambda r_*Q\over q_0}\,\delta\left(\varphi+{r_*L_0\over q_0Q}t\right)
\delta(\theta-\pi/2)\delta(r-r_*)
\nonumber
\end{eqnarray}
The source (star) respects the Killing symmetry,
$\chi=\partial_\varphi - {q_0Q\over r_*L_0}\partial_t$. The variable
separation respects this Killing symmetry is
\begin{eqnarray}
\Phi=\sum_{\ell, m} e^{im(\varphi+{r_*L_0\over q_0Q}t)}S_\ell^m(\theta)R_{\ell m}(r)
\equiv \sum_{\ell, m} e^{i(m\varphi-\omega t)}S_\ell^m(\theta)R_{\ell m}(r)
\end{eqnarray}
where, $m\in\mathbb{Z}$, $\omega=-m{r_*L_0\over q_0Q}$.
The equation of motion separates into radial equations:
\begin{eqnarray} \label{ern_req}
r^2R''_{\ell m}(r)  + 2r R'_{\ell m}(r)
+ \left({\omega^2\over r^2} - {2eQ\omega\over r}
+ e^2Q^2-\mu^2\right)R_{\ell m}(r) = -\tilde\lambda\delta(r-r_*)
\end{eqnarray}
where $\tilde\lambda={2\lambda r_*\over q_0Q}S_\ell^m({\pi\over 2})^*$,
$\mu^2=\ell(\ell-1)$ ($\ell=0,1,2,\dots$).
$S_\ell^m(\theta)=\sqrt{(2\ell+1)(\ell-m)!\over 2(\ell+m)!}P_\ell^m(\theta)$
is the normalized associated Legendre function of the first kind,
\begin{eqnarray} \label{spherical-eigen-eq}
{d^2\over d\theta^2}P_\ell^m(\theta)
+ \cot\theta\, {d\over d\theta}P_\ell^m(\theta)
- {m^2\over\sin^2\theta}P_\ell^m(\theta)=-\mu^2P_\ell^m(\theta)
\end{eqnarray}
and the orthonormal condition reads,
\begin{eqnarray}
\int d\theta \sin\theta\, S_{\ell'}^m(\theta)^*S_\ell^m(\theta)
=\delta_{\ell\ell'}
\end{eqnarray}
Two linearly independent solution of the homogeneous radial equation,
set $\lambda=0$ in (\ref{ern_req}), are given by Whittaker functions,
\begin{eqnarray}
R^{(1)}(r) &=& M(-ieQ,h-\hbox{${1\over 2}$}, -2i\omega/r)
\\[5pt]
R^{(2)}(r) &=& W(-ieQ,h-\hbox{${1\over 2}$}, -2i\omega/r)
\end{eqnarray}
where the weight $h$ is defined by
\begin{eqnarray}
h=\hbox{${1\over 2}$} +\hbox{${1\over 2}$}\sqrt{1+4\mu^2-4e^2Q^2}
\end{eqnarray}
Near the horizon,
\begin{eqnarray}
R^{(1)}(r\to 0)
&\sim& A e^{-i\omega/r} r^{-ieQ} + B e^{i\omega/r} r^{+ieQ}
\\[5pt]
R^{(2)}(r\to 0)
&\sim& (-2i\omega)^{-ieQ} e^{i\omega/r} r^{+ieQ}
\end{eqnarray}
which shows that $R^{(2)}$ is purely ingoing. Near the boundary,
\begin{eqnarray}
R^{(1)}(r\to \infty) &\sim& (-2i\omega)^h r^{-h}
\\[5pt]
R^{(2)}(r\to \infty) &\sim& C r^{-h} + D r^{h-1}
\end{eqnarray}
We will take $h>1/2$, so
$R^{(1)}$ satisfies purely Neumann boundary condition.
Constants $A, B, C, D$ are defined by
\begin{eqnarray}
A=(-2i\omega)^{+ieQ}{\Gamma(2h)\over\Gamma(h+ieQ)}\,,&&
B=(2i\omega)^{-ieQ}e^{i\pi h}{\Gamma(2h)\over\Gamma(h-ieQ)}
\\[5pt]
C=(-2i\omega)^h{\Gamma(1-2h)\over\Gamma(1-h+ieQ)}\,,&&
D=(-2i\omega)^{1-h}{\Gamma(2h-1)\over\Gamma(h+ieQ)}
\end{eqnarray}
Since we want to compute the ingoing flux near the horizon, we
need solution which is purely ingoing at the horizon and satisfies purely
Neumann boundary condition on the boundary. This kind of solution can be
constructed by \cite{ps_kerr_cft}
\begin{eqnarray}
R_{\ell m}(r) = \theta(r_*-r)C_2R^{(2)}(r) + \theta(r-r_*)C_1R^{(1)}(r)
\end{eqnarray}
Substituting into the equation of motion, the constants $C_{1,2}$
can be determined to be
\begin{eqnarray}
C_1={\tilde\lambda\over 2}{R^{(2)}(r_*)\over W}\,,\qquad
C_2={\tilde\lambda\over 2}{R^{(1)}(r_*)\over W}
\end{eqnarray}
where $W$ is $r$-independent Wronskian,
\begin{eqnarray}
W=r^2(R^{(1)}(r)R^{(2)}{}'(r)-R^{(1)}{}'(r)R^{(2)}(r))
=-2i\omega{\Gamma(2h)\over\Gamma(h+ieQ)}
\end{eqnarray}
Now we can compute the Klein-Gordon particle number flux per unit time,
\begin{eqnarray}  \label{kg-n-flux}
{\cal F} =-\int d\theta d\varphi\,\sqrt{-g}J^r
\end{eqnarray}
where the current is defined by
\begin{eqnarray} \label{scalar-flux-current}
J_\mu = {i\over 8\pi}(\Phi^*(\nabla_\mu-ieA_\mu)\Phi-h.c.)
=-{1\over 4\pi}{\rm Im}(\Phi^*(\nabla_\mu-ieA_\mu)\Phi)
\end{eqnarray}
Then the flux is
\begin{eqnarray}
{\cal F} = {Q^4r^2\over 2}\sum_{\ell m}{\rm Im}(R_{\ell m}^*(r)R_{\ell m}'(r))
\end{eqnarray}
Near the boundary,
\begin{eqnarray} \label{horizon-flux}
{\cal F}_{\ell m}(r\to 0) ={Q^4|\omega|\over 2}e^{-\pi eQ}|C_2|^2
\end{eqnarray}
for $m<0$, i.e., $\omega>0$. Near the boundary,
\begin{eqnarray}
{\cal F}_{\ell m}(r\to\infty) = 0
\end{eqnarray}
for real $h$.

\subsection{Decay rate on CFT side}

In this subsection, we will compute the decay rate in the CFT on the
boundary dual to the quantum gravity on the near-horizon region
of the extremal RN spacetime. This problem is studied in Refs.
\cite{hmns_cft_Ebh,gg_rn_cft,cs}. Before performing the
computation, let us review some facts here.

The symmetry of the near-horizon-extremal RN black hole includes the isometry
of the metric and the gauge symmetry,
\begin{eqnarray}
SL(2,R)\times SO(3)\times U(1)_{\rm em}
\end{eqnarray}
To find out the CFT dual, the four dimensional RN black hole
is lifted to five dimensions. Especially, the metric becomes,
\begin{eqnarray} \label{5d_4d_y}
ds_5^2=ds_{\rm 4D}^2+Q^2(dy+{\cal A})^2
\end{eqnarray}
where $ds_{\rm 4D}^2$ is the 4D RN metric (\ref{NHErn-sol}), the compact
coordinate has period $2\pi$, $y\approx y+2\pi$, ${\cal A}=A/Q$.
In the 5D language, the 4D $U(1)_{\rm em}$ gauge symmetry is geometrized
as the isometry of the $S^1$-fibration of 4D RN black hole.
That is, the 4D gauge symmetry transformation, $A\to A-d\alpha$, appears
in 5D as
\begin{eqnarray}  \label{5d-gauge-trans}
{\cal A}\to {\cal A}-{1\over Q}d\alpha\,,\qquad
y\to y+{1\over Q}\alpha\,,\qquad
\Phi\to e^{-ie\alpha}\Phi
\end{eqnarray}
where $\alpha$ is real function depends only on 4D coordinates.

In this 5D setting, the near horizon dynamics will be dual to a chiral 2D
CFT on the boundary: only left-movers are excited and
the right-movers are frozen to the ground state.
For these two sectors, their temperatures are
\begin{eqnarray}
T_L={1\over 2\pi}\,,\qquad T_R=0
\end{eqnarray}
Specifically, on the
gravity side, non-zero conserved charge of the generator $\partial_t$
will indicate the deviation of the extremal state, on the CFT side,
non-zero charge of $SL(2,\mathbb{R})_R$ indicate the excitation of the right-movers
\cite{bhss_superradiance_kerr_cft}.
So we have a correspondence: the time translation $\partial_t$ on gravity side
is mapped to the right-translation $\partial_{\sigma^-}$ on CFT side, or
\begin{eqnarray}
t = \sigma^-
\end{eqnarray}
On the other hand, the non-zero conserved charge (electric charge) of
the generator $\partial_y$ on the gravity side corresponds to the non-zero
$SL(2,\mathbb{R})_L$-charge, and $\partial_y$ is mapped to the
left-translation, $\partial_y\sim\partial_{\sigma^+}$, or
\begin{eqnarray}
y=-\sigma^+
\end{eqnarray}
where we have used the fact that both $y$ and $\sigma^+$ have period
$2\pi$, so we identify these two coordinate directly, the extra minus sign
is found to be necessary for the matching of the decay rates in
NHERN/$\chi$CFT.

Now, adding an orbiting star into the 4D RN black hole will, on the CFT
side, lead to perturbation of the CFT. Assume that the perturbed action is
\begin{eqnarray}
S_{\rm CFT}^{\rm int}
= \sum_\ell \int d\sigma^+ d\sigma^- J_\ell(\sigma^+,\sigma^-)
{\cal O}_\ell(\sigma^+,\sigma^-)
\end{eqnarray}
The source $J_\ell$ should be determined by the asymptotic behavior of the
scalar field near the boundary, since only scalar field is assumed to be coupled
to the orbiting star. The conformal weight of ${\cal O}$ can also be read off
from the asymptotic behavior of the scalar field, $h_L=h_R=h$.

Now let us look at $J_\ell$. At first, since the star respect the symmetry
$\chi$, so
\begin{eqnarray}
J_{\ell}(\sigma^+,\sigma^-) \sim e^{im(\varphi+{r_*L\over q_0Q}t)}
\equiv e^{i(m\varphi-\omega t)}=e^{i(m\varphi-\omega \sigma^-)}
\end{eqnarray}
Secondly, the source $J_\ell$ should have the same gauge behavior as
the charged scalar field. Since a gauge transformation
is given by (\ref{5d-gauge-trans}), $\Phi\to e^{-ie\alpha}\Phi$,
we must require the source transform in the same way,
\begin{eqnarray}
J_\ell \to e^{-ie\alpha}J_\ell
\end{eqnarray}
and since $y$ is identified as $\sigma^+$ and under gauge transformation,
$y\to y+\alpha/Q$, the dependence of $J_\ell$ on the $y$-coordinate should be
\begin{eqnarray}
J_\ell(\sigma^+,\sigma^-) \sim e^{-ieQy}=e^{ieQ\sigma^+}
\end{eqnarray}
In all, we have expansion of the source as follows,
\begin{eqnarray}
J_{\ell}(\sigma^+,\sigma^-) =\sum_{m} e^{im\varphi-i\omega \sigma^- +ieQ\sigma^+}J_{\ell m}
\end{eqnarray}
where $J_{\ell m}$ are constants.
To determine $J_{\ell m}$, one can extend the solution $R_{\ell m}$ at the
near horizon region to the whole spacetime \cite{ps_kerr_cft},
\begin{eqnarray}
R_{\ell m}^{\rm ext}(r)=C_2 R^{(2)}(r)\,,\qquad 0<r<\infty
\end{eqnarray}
The asymptotic behavior of $R_{\ell m}^{\rm ext}(r)$ is
\begin{eqnarray}
R_{\ell m}^{\rm ext}(r\to\infty)\sim C_2 (C r^{-h} + D r^{h-1})
\end{eqnarray}
The coefficient $J_{\ell m}$ can be read off from the Dirichlet mode as,
\begin{eqnarray}
J_{\ell m} = C_2 D
\end{eqnarray}
The decay rate of vacuum-to-vacuum per unit time is
\cite{bhss_superradiance_kerr_cft},
\begin{eqnarray} \label{dr-nhern-ccft}
{\cal R}&=&2\pi\sum_{\ell m}|J_{\ell m}|^2\int d\sigma^+d\sigma^-\,
e^{i\omega \sigma^- -ieQ\sigma^+}\langle{\cal O}_\ell(\sigma^+,\sigma^-)
{\cal O}_\ell(0,0)\rangle
\nonumber\\[5pt]
&=&2\pi\sum_{\ell m}C_O^2|C_2|^2|D|^2
{(2\pi T_R)^{2h_R-1}\over\Gamma(2h_R)}e^{{\omega\over 2T_R}}
\left|\Gamma\left(h_R+i{\omega\over 2\pi T_R}\right)\right|^2
\nonumber\\[5pt]
&&
\times {(2\pi T_L)^{2h_L-1}\over\Gamma(2h_L)}e^{-{eQ\over 2T_L}}
\left|\Gamma\left(h_L+i{eQ\over 2\pi T_L}\right)\right|^2
\end{eqnarray}
Substituting $T_L={1\over 2\pi}$, $h_L=h_R=h$, and taking the limit,
$T_R\to 0$,
\begin{eqnarray}
{\cal R}_{\ell m}
= C_O^2{2^{5-2h}\pi^2\over Q^{2h+3}(2h-1)^2}{\cal F}_{\ell m}(r\to 0)
\end{eqnarray}
for $m<0$, i.e., $\omega>0$.
This decay rate is precisely equal to that computed
in the gravity side (\ref{horizon-flux})
if we take $C_O^2={Q^{2h+3}(2h-1)^2\over 2^{5-2h}\pi^2}$.

\section{Near horizon near-extremal RN/CFT}
\label{sect-nhnern}

There is a correspondence between the dynamics on
the near-horizon near-extremal RN black hole and a 2d CFT, e.g.\,\cite{chz,cs}.
In this section we will compute the decay rates of a charged scalar wave
from both sides, and compare the results.

\subsection{Decay rate on the gravity side}

Similar to the extremal RN case discussed in the previous section,
in this subsection, we will consider a charged scalar wave sourced by
a charged star which is orbiting the near-extremal RN black hole.

The non-extremal (general) RN black hole can be described by the metric
and gauge field,
\begin{eqnarray}
ds^2&=&-{(\hat r-r_+)(\hat r-r_-)\over \hat r^2}d\hat t^2
+{\hat r^2\over (\hat r-r_+)(\hat r-r_-)}d\hat r^2 +\hat r^2d\Omega_2^2\,,
\\[5pt]
\hat F&=&{Q\over\hat r^2}d\hat t\wedge d\hat r
\end{eqnarray}
Define new coordinates, \cite{chz}
\begin{eqnarray}
r={\hat r-Q\over\epsilon}\,,\qquad
t={\hat t\over Q^2}\epsilon\,,\qquad
r_0={\sqrt{2QE}\over\epsilon}
\end{eqnarray}
where $E=Q-M$ is the deviation from the extremality.
The near-horizon near-extremal limit can be obtained
by letting $\epsilon\to 0$ and keeping $r, t, r_0$ fixed.
In this new coordinate system, the metric and the gauge field become
\begin{eqnarray}
ds^2&=&Q^2\left[-(r^2-r_0^2) dt^2 + {dr^2\over r^2-r_0^2} +d\Omega_2^2\right]
\label{nhnern-met}
\\[5pt]
F&=& Qdt\wedge dr
\end{eqnarray}
where $r=r_0$ is the horizon position. The gauge potential can be chosen as
\begin{eqnarray}
A=-Qrdt
\label{nhnern-AF}
\end{eqnarray}
The Hawing temperature of the near-horizon spacetime (\ref{nhnern-met})
can be found to be
\begin{eqnarray} \label{nhnern-TH}
T_H = {r_0\over 2\pi}
\end{eqnarray}
It is different from the Hawking temperature corresponding to the original
coordinate with hats, $\hat T_H ={\epsilon\over Q^2}T_H$, which
vanishes under the limit $\epsilon\to 0$.

Similar to the extremal case,
corresponding to the two Killing vectors, $\xi_{(t)}=\partial_t$
and $\xi_{(\phi)}$, we define conserved quantities,
\begin{eqnarray}
E_0&=&-g_{\alpha\beta}(u^\alpha+q_0A^\alpha)\xi_{(t)}^\beta
=Q^2 (r_*^2- r_0^2)\left(\dot t_*+{q_0r_*\over Q(r_*^2-r_0^2)}\right)
\\[5pt]
L_0&=&g_{\alpha\beta}(u^\alpha+q_0A^\alpha)\xi_{(\varphi)}^\beta
=Q^2\sin^2\theta_*\dot\varphi_*
\end{eqnarray}
where $x_*^{\mu}$ are coordinates of the orbiting star, and we will let
$r=r_*>r_0$ be constant and $\theta=\theta_*=\pi/2$ in the following.
The normalization condition is $-1=Q^2[-(r_*^2-r_0^2)\dot t_*^2+\dot\varphi_*^2]$.
For convenience, take $E_0=0$ and then $\dot t_*=-{q_0r_*\over Q(r_*^2-r_0^2)}$,
$\dot\varphi_*=L_0/Q^2$, or
\begin{eqnarray}
t_*=-{q_0r_*\over Q(r_*^2-r_0^2)}\tau\,,\qquad
\varphi_*={L_0\over Q^2}\tau
\end{eqnarray}
where the integral constants are set to zero. The equation of motion
of the scalar field is
\begin{eqnarray}
\sqrt{-g}\,(\nabla_\mu-ieA_\mu)(\nabla^\mu-ieA^\mu)\Phi
=-{4\pi\lambda\over |\dot t_*|}\,
\delta\left(\varphi-{\dot\varphi_*\over\dot t_*}t\right)
\delta(\theta-\pi/2)\delta(r-r_0)
\end{eqnarray}
The source (star) respects the Killing symmetry,
$\chi=\partial_\varphi+{\dot t_*\over\dot\varphi_*}\partial_t$. The variable
separation respects this Killing symmetry is
\begin{eqnarray}
\Phi=\sum_{\ell, m} e^{im(\varphi-{\dot\varphi_*\over\dot t_*}t)}
S_\ell^m(\theta)R_{\ell m}(r)
\equiv \sum_{\ell, m} e^{i(m\varphi-\omega t)}S_\ell^m(\theta)R_{\ell m}(r)
\end{eqnarray}
where $\omega=m{\dot\varphi_*/\dot t_*}$, $m\in\mathbb{Z}$.
In the following we will take $m>0$, i.e., $\omega<0$,
in the concrete calculation.
The equation of motion separates into radial equations:
\begin{eqnarray} \label{nern_req}
((r^2-r_0^2)R'_{\ell m})'
+ \left[{(\omega-eQr)^2\over r^2-r_0^2}-\mu^2\right]R_{\ell m}
= -\tilde\lambda\delta(r-r_*)
\end{eqnarray}
where $\mu^2=\ell(\ell-1)$ ($\ell=0,1,2,\dots$), $R_{\ell m}'=\partial_rR_{\ell m}$,
$\tilde\lambda={2\lambda\over|\dot t_*|Q^2}S_\ell^m({\pi\over 2})^*$.
$S_\ell^m(\theta)$ is defined in the previous section.
The two linearly independent solutions of the radial homogeneous equation
(when $\lambda=0$) are the following hyper-geometric functions,
\begin{eqnarray}  \label{hypergeometric-1}
R_{\ell m}^{(1)}=(r+r_0)^{-i\alpha}(r-r_0)^{i\beta}\,
{}_2F_1\left(1-h-i\alpha+i\beta, h-i\alpha+i\beta, 1-2i\alpha,
{r+r_0\over 2r_0}\right)
\\[5pt]  \label{hypergeometric-2}
R_{\ell m}^{(2)}=(r+r_0)^{i\alpha}(r-r_0)^{i\beta}\,
{}_2F_1\left(1-h+i\alpha+i\beta, h+i\alpha+i\beta, 1+2i\alpha,
{r+r_0\over 2r_0}\right)
\end{eqnarray}
where the constants are defined by
\begin{eqnarray} \label{parameter-def}
\alpha=\hbox{${1\over 2}|eQ+{\omega\over r_0}|$}\,,\quad
\beta=\hbox{${1\over 2}(eQ-{\omega\over r_0})$}\,,\quad
\hbox{$h={1\over 2}+{1\over 2}\sqrt{1-4e^2Q^2+4\mu^2}$}
\end{eqnarray}
The asymptotic behaviors near the boundary of $R^{(1,2)}$ are
\begin{eqnarray}
R_{\ell m}^{(1)}(r\to\infty)\sim A_\infty r^{h-1} + B_\infty r^{-h}
\\[5pt]
R_{\ell m}^{(2)}(r\to\infty)\sim C_\infty r^{h-1} + D_\infty r^{-h}
\end{eqnarray}
where the coefficient $A_\infty$ is defined by
\begin{eqnarray}
A_\infty=\frac{\Gamma (1-2 i \alpha ) \Gamma (2 h -1)
(-2r_0)^{-i \alpha +i \beta -h +1} }
{\Gamma (h-i\alpha -i\beta ) \Gamma (h -i \alpha +i \beta)}
\end{eqnarray}
and the other coefficients are related to $A_\infty$: $B_\infty=A_\infty(h\to 1-h)$,
$C_\infty=A_\infty(\alpha\to -\alpha)$ and
$D_\infty=A_\infty(h\to 1-h, \alpha\to -\alpha)$.
The near horizon behaviors are
\begin{eqnarray}
R_{\ell m}^{(1)}(r\to r_0)\sim A_0 (r-r_0)^{i\beta} + B_0 (r-r_0)^{-i\beta}
\\[5pt]
R_{\ell m}^{(2)}(r\to r_0)\sim C_0 (r-r_0)^{i\beta} + D_0 (r-r_0)^{-i\beta}
\end{eqnarray}
where the coefficient $A_0$ is defined by
\begin{eqnarray}
A_0={i \pi  (2r_0)^{-i \alpha }{\rm csch}(2 \pi  \beta ) \Gamma (1-2 i \alpha )
\over\Gamma (2 i \beta +1) \Gamma (1-h-i \alpha -i\beta)
\Gamma (h-i \alpha -i\beta)}
\end{eqnarray}
and the other coefficients are related to $A_0$:
$B_0=e^{2\pi\beta}(2r_0)^{2i\beta}A_0(\beta\to -\beta)$,
$C_0=A_0(\alpha\to -\alpha)$ and $D_0 = B_0(\alpha\to -\alpha)$.
From these results, one can see that the mode which is purely ingoing
near horizon (near region) can be constructed as
\begin{eqnarray}
R_{\ell m}^{(n)} = D_0 R_{\ell m}^{(1)} - B_0 R_{\ell m}^{(2)}
\end{eqnarray}
and the mode which is purely Neumann at infinity (far region) is
\begin{eqnarray}
R_{\ell m}^{(f)} = C_\infty R_{\ell m}^{(1)} - A_\infty R_{\ell m}^{(2)}
\end{eqnarray}
We have
\begin{eqnarray}
R_{\ell m}^{(n)}(r\to r_0)
&\sim& {\alpha\over\beta} (2r_0)^{2i\beta}e^{2\pi\beta}(r-r_0)^{i\beta}
\\[5pt]
R_{\ell m}^{(f)}(r\to\infty)
&\sim& {2i\alpha\over 1-2h}(2r_0)^{1+2i\beta}e^{2\pi\beta}r^{-h}
\end{eqnarray}
Now the solution of the inhomogeneous equation (\ref{ern_req}) is constructed
by the Green's method as
\begin{eqnarray}
R_{\ell m} = \theta(r_*-r)C_{(n)}R_{\ell m}^{(n)}
+\theta(r-r_*)C_{(f)}R_{\ell m}^{(f)}
\end{eqnarray}
where
\begin{eqnarray}
C_{(n)}={\tilde\lambda\over 2}{R^{(f)}(r_*)\over W}\,,\qquad
C_{(f)}={\tilde\lambda\over 2}{R^{(n)}(r_*)\over W}
\end{eqnarray}
where $W$ is $r$-independent Wronskian,
\begin{eqnarray}
W&=&(r^2-r_0^2)(R^{(n)}(r)R^{(f)}{}'(r)-R^{(n)}{}'(r)R^{(f)}(r))
\nonumber\\[5pt]
&=&2\pi i\alpha^2(2r_0)^{2-h+5i\beta}e^{2\pi\beta}
{(1+\coth\pi\beta)^2\tanh(\pi\beta)\Gamma(2h-1)
\over\Gamma(1-2i\beta)\Gamma(h-i\alpha+i\beta)\Gamma(h+i\alpha+i\beta)}
\end{eqnarray}
The Klein-Gordon particle number flux per unit time is still given by the equation
(\ref{kg-n-flux}) and for the mode with quantum numbers $\ell, m$,
\begin{eqnarray}
{\cal F}_{\ell m} = {Q^2\over 2}(r^2-r_0^2)\,{\rm Im}(R_{\ell m}^*(r)R_{\ell m}'(r))
\end{eqnarray}
At infinity, simple calculation shows that ${\cal F}_{\ell m}(r\to\infty)=0$.
Near the horizon,
\begin{eqnarray}
{\cal F}_{\ell m}(r\to r_0)={\alpha^2\over\beta}Q^2r_0 e^{4\pi\beta}|C_{(n)}|^2
\end{eqnarray}
Since the spacetime has non-zero temperature (\ref{nhnern-TH}), the decay rate
of the scalar particle into the horizon is
\begin{eqnarray}
{\cal R}_{\ell m}={1\over e^{\omega+e\Phi_H\over T_H}-1}{\cal F}_{\ell m}(r\to r_0)
\end{eqnarray}
where $\Phi_H=A_t(r=r_0)=-Qr_0$ is the gauge potential at the horizon (chemical
potential). Using the definition of $\beta$ in (\ref{parameter-def}), we have
\begin{eqnarray} \label{decay-rate-gravity-side}
{\cal R}_{\ell m}={1\over 1-e^{-4\pi\beta}}{\alpha^2\over\beta}Q^2r_0|C_{(n)}|^2
\end{eqnarray}
We will see that this Planck factor is important for the matching of the decay
rates in NHNERN/CFT correspondence.

\subsection{Decay rate on the CFT side}

Now turn to the computation from the CFT viewpoint. The analysis of the dictionary
in the near-horizon near-extremal RN/CFT correspondence is very similar
to the one in the near-horizon extremal RN/$\chi$CFT correspondence, which is
discussed in the previous section. For details, one can refer to the original
references, \cite{chz,cs} etal. In the following we will only sketch points
necessary in the computation.

Similar to the extremal case discussed in the previous section,
we have the following matching of coordinates,
\begin{eqnarray}
t\leftrightarrow\sigma^-\,,\qquad y\leftrightarrow -\sigma^+
\end{eqnarray}
Corresponding to this identification, one can derive the left and right
temperatures of the boundary CFT as \cite{chz},
\begin{eqnarray}
T_L={1\over 2\pi}\,,\qquad T_R={r_0\over 2\pi}
\end{eqnarray}
Furthermore, the conformal weights of the operator corresponding to the
scalar field $\Phi$ is $(h_L,h_R)=(h,h)$.
Similar to the extremal case, the source $J_\ell$ depends on the compact
coordinate through
$J_{\ell}(\sigma^+,\sigma^-)
=\sum_{m} e^{im\varphi-i\omega \sigma^- +ieQ\sigma^+}J_{\ell m}$.
Now using the expression
(\ref{dr-nhern-ccft}) for the decay rate, for the mode with quantum numbers
$\ell, m$,
\begin{eqnarray}
{\cal R}_{\ell m}^{(\rm CFT)}
=2\pi e^{-2\pi\beta} \left({r_0\over Q}\right)^{2h-1}
{|\Gamma(h-i{\omega/r_0})|^2|\Gamma(h+ieQ)|^2
\over\Gamma(2h)^2}
C_O^2|J_{\ell m}|^2
\end{eqnarray}
The constant $J_{\ell m}$ is determined by the Dirichlet term of
$R_{\ell m}^{(n)}$ near infinity. That is, it is the coefficient of $r^{h-1}$ in
$c_{(n)}R_{\ell m}^{(n)}$ when $r\to\infty$,
\begin{eqnarray}
J_{\ell m} = {4\pi\alpha(2r_0)^{1-h+3i\beta}\over 1-e^{-4\pi\beta}}
{\Gamma(2h-1)
\over\Gamma(1-2i\beta)\Gamma(h-i\alpha+i\beta)\Gamma(h+i\alpha+i\beta)}
C_{(n)}
\end{eqnarray}
Substituting into the decay rate, we have
\begin{eqnarray}
{\cal R}_{\ell m}^{(\rm CFT)}
={1\over 1-e^{-4\pi\beta}}{\alpha^2\over\beta}
{2^{5-2h}\pi^2r_0Q^{1-2h}\over (2h-1)^2}C_O^2|C_{(n)}|^2
\end{eqnarray}
If we choose $C_O^2={Q^{2h+1}(2h-1)^2\over 2^{5-2h}\pi^2}$, this decay rate
is completely the same as that computed in the gravity side
(\ref{decay-rate-gravity-side}).

\section{Discussions}
\label{sect-discuss}

If we compare the computations of the decay rates in the previous
two sections, one will find that if the extremal limit, $E=M-Q\to 0$,
is taken before the near horizon limit, $\epsilon\to 0$, the near-extremal
case reduced to the extremal one ($r_0=0$). However, if the near horizon limit
is taken before the extremal limit, we will obtain the near-extremal
case ($r_0\neq 0$). It should be pointed out that one could not obtain
the results of the extremal case by taking the limit $r_0\to 0$ on the
results of the near-extremal case: $r_0=0$ is the essential singularity
of the hypergeometric functions (\ref{hypergeometric-1})
and (\ref{hypergeometric-2}).

\bigskip\bigskip

\noindent
{\bf Acknowledgments.}
R. L. is supported by National Natural Science Foundation of China
(Grant No. 11205048).
R. L. is also supported by the Foundation for Young Key Teacher of
Henan Normal University.


Dark Phoenix Events Game Master's aren't just GMs, they are also game designers . Andre Kruppa, well known in the Northeast for his theatrical style and immersive audio-visual game experiences, recently published the Lucid Dreams Roleplaying Engine. The following excerpt from the Playing the Game chapter is both a window into Lucid Dreams and a widely applicable essay on running RPGs in general.
There are a lot of factors important to running a role-playing game. The Game Master must organize play, facilitate sessions, and keep track of a myriad of factors with setting, characters, background and storytelling. It can be quite a challenge, but is also very exciting and fun!
The setting, period, and so forth can be developed out of whole cloth or taken from scenario books or supplements. When choosing a setting, it is a good idea to have a long chat with the rest of the Table and see what the players and co-GMs (if any) may desire in a game. For historically based fantasy, reading a concise history of the era is often a good idea and some of the most promising campaigns often incorporate details from the period, which helps keep the tone. A variety of published settings can be used and conversion from any Skill-based system is fairly straightforward.
There are many styles of play and no one style is best, but certainly folks often have a preference. Keeping distraction to a minimum and focusing the players on the scene in play is vital to a good session regardless of the methods employed. There are many ways to achieve this focus, from involving story bits for each Player Character to clear descriptive presentation of the environment and setting. Some folks prefer a strong narrative game with little along the lines of physical play aids, others may have well developed handouts that help give the flavor of the setting, and some may use miniatures and terrain.
Atmosphere can go a long way toward immersing the players in the game. Lighting and mood music have a strong impact, often subconscious, and can be quite helpful for those that are interested. Lighting might be as simple as turning off the lights and using flashlights, candles, glow sticks, or lanterns during some scenes, or using dimmable or intelligent lights. Some use period language and customs which help to create a feel for things as well.
Sound effects can also be effective as well, and sound boards on tablets and smart phones are beginning to be released more frequently and custom sound board apps can be used by the more enterprising gamer. Sound often helps create immersion and makes the setting come to life. One Table may have a strong preference for this, and another may wish to do without.
Description is vital to the game and the setting is framed almost wholly by the Game Master's description of the scene. It is important to inform all of the senses, most especially sight, hearing, and smell. A few details can really add to the impact and immersion of a scene, such as the dripping sound of water in a cave, the smell of mold, the sounds of insects, the way a stone wall is made, the nature of the path or road. Details can often convey vital information and also add to the experience of each player, helping to create the mind's eye picture.
Running a game is also often about pacing, which is an art in and of itself. Timing scenes and leaving campaign sessions with a feeling of anticipation through cliff hangers, twists, or otherwise on the brink of a vital coming scene can help when the GM can engineer it. One need not obsess over timing, but it is good to try and keep things flowing and make the tension of the plot strong and vibrant.
Every group has a sweet spot in terms of style and genre and it make take a bit of time for a group to hit its stride. When doing a new game, it is often wise to play a one-shot scenario or two to get the feel for things. Most games need cooperative effort and require a strong consensus to play smoothly and be enjoyable for everyone. Players should be encouraged to work together to create the story even when the Player Characters are not fully in alignment.
The Lucid Dreams Role-playing Engine available on both Amazon and RPGNow!


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How to Survive Summer in Austin, TX
by Cynthia Drake on July 3, 2017 July 6, 2017 Follow @@cynthiadrake
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Dry heat or not, with temps hovering near the 100-degree mark, Austin summers at some point just become seasons to endure. You flit from one air conditioned locale to the next trying your best not to melt on the pavement in the process.
There are, of course, some bright spots. Central Texans have long been creative in their pursuits of cooler temps, and there are plenty of options for splashing, spelunking and slurping your way to Chilltown, U.S.A.
Here are a few of our favorites:
Our shops are now selling Cilantro Lime, Horchata, and Chocolate Peanut Butter Brownie again! Yum!! pic.twitter.com/JlcxzJiN31
— Lick Ice Creams (@LickIceCreams) January 5, 2016
Let's start with a beverage, shall we? In Austin we make no secret of our enduring love for an effervescent Topo Chico, which goes down especially well in June, July and August. Another must-try: a raspado, or raspa — it's the Mexican take on a slushie, fresh fruit swirled with spices. The mangonada, a popular choice, includes mango, orange, chamoy and chile lime salt. If you're relatively new to Texas/The South, you might not be indoctrinated yet into the obsession here with shaved ice/sno cones/sno balls. A refreshing cup of ice crystals doused in sweet (or pickley, no judging) syrup is just so incredibly refreshing. Then, of course, there is the crème de la crème, as in ice cream. As with the other items on this list, everyone has their favorite purveyor. If your tastes run on the adventurous side, check out Lick, home of unusual yet surprisingly delicious flavors such as Goat Cheese, Thyme & Honey, and Roasted Beets & Fresh Mint (you can try before you buy). Amy's Ice Cream is another beloved local chain, with lots of delectable mix-ins to create the perfect chilled dessert.
Refreshing dips
The Ultimate Austin Tubing Guide https://t.co/rVmvx6mrUq pic.twitter.com/fOI1RNRS2F RT MySOdotCom — Marenda Taylor (@Marenda) July 7, 2016
Fortunately, Austin and Central Texas are home to several great natural swimming holes and lakes that are perfect for taking your core body temperature down a notch:
Barton Springs Pool, a three-acre spring-fed natural pool is located within Austin's sprawling downtown Zilker Park
Blue Hole in Wimberley used to be a local secret, but now is regularly named to lists of the top swimming holes in the state
Hamilton Pool & Preserve is a stunningly beautiful natural pool featuring water falling into a grotto, located about 23 miles west of Austin (paid reservations are required and are in high demand throughout the season).
Tubing is also hugely popular–check out the Comal River in New Braunfels or for a slightly more challenging run, try to the Guadalupe River.
Of course, there are several public swimming pool and waterpark options for your splashing pleasure, as well.
Deep Eddy Pool, Texas' oldest swimming pool, is unchlorinated with a zero-entry approach at one end. The original bathhouse, created during the Depression era as a Works Progress Administration project, has been renovated and still stands at the site.
Check out the area's newest renovated waterpark, Typhoon Texas in Pflugerville, which includes a Gully Washer play area for kids ages 3 to 10, several large slides and a lazy river.
Other cool places
Don't overlook the natural air conditioning of the area's caverns as a great way to find out some geological history while staying nice and cool in the average 70 degree year-round temperatures. Inner Space Cavern in Georgetown and Longhorn Caverns in Burnet are two great options.
If you want a little retail therapy on the side with your air conditioning, hit up one of the local malls. Barton Creek Square to the south and Lakeline Mall to the north are your best options for the total indoor mall experience.
For a little cinematic action, relax in one of the area's several full-service theaters (where you can enjoy a frosty beverage, too): Alamo Drafthouse, iPic Theaters and Moviehouse & Eatery, among others.
And get ya some culture, too, while beating the heat. Hit up Austin's several outstanding museums: the Bullock Museum, the Blanton Museum of Art and The Contemporary Austin, all located within a mile of each other downtown, are all perfectly worthy ways to spend an afternoon, regardless of weather.
About Cynthia Drake
Cynthia J. Drake is a travel/finance writer and Author of Budget Travel for the GENIUS.
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Achieving that peaceful and calm state of mind need not to be pricey. Here at VapeFuse we always look for ways and tips to share with you to experience healing the natural way. We believe this can be done through Aromatherapy and making the most out of your vaporizers.
Today, Nora will take you in a quick demonstration of how she uses Essential Oils to heal common illnesses like colds.
Essential Oils are extracts from plants. Its nature differs from plant to plant or from species to species. The delicate proportion of the aromatic components found in an essential oil is what makes it distinct and determines the health benefits it offers.
Now, with our surroundings and weather changes, we pick up viruses and bacteria that cause us illness. Getting common illnesses like colds, cough or headache shouldn't be a daunting experience. You can deal with it with a calm approach by utilizing these aromatic Essential Oils and be healed the natural way.
So without further ado, let's check out Nora's video below with how she used Eucalyptus oil to chase that cold away using the Arizer Extreme Q.
Learn more about how you can experience the healing benefits of Essential Oils. Just head over to our post here.
If you would like to learn more about Aromatherapy, we got you covered here as well.
Do you have aromatherapy tips that you can share with our vaping community? Let us know in the Comments section below. We'd love to hear from you!


text:
OIAF announces 2010 jury
By Mike Valiquette on August 31, 2010
INTERNATIONAL JURY FOR SHORT PROGRAM, STUDENT, AND COMMISSIONED ANIMATION
Munro Ferguson
Born in New York City in 1960, Ferguson took a very early interest in cartooning and made his first film, When I Get Older, at age 7. He studied painting and drawing at the Banff Centre and received a BA in philosophy from the University of Toronto. He continued to make films, becoming a core member of the Funnel Film Group in 1980. His science comic strip Eureka was syndicated in over 30 newspapers around the world. In 1994, he joined the NFB English Program's Animation Studio, where he wrote, directed and animated How Dinosaurs Learned to Fly (1995). In 1995, he began working for the legendary Roman Kroitor at IMAX Corporation, writing, animating and advising on the development of SANDDETM, a 3D stereoscopic animation technique. He returned to the NFB in 1998, and since then has been training other NFB animators in this innovative system. Ferguson has created two stereoscopic animations with SANDDETM: Falling in Love Again, winner of the 2004 Genie Award for Best Animated Short, and June, an elegy for his friend and mentor, artist Joyce June Wieland. In 2008 he was Animation Director for Facing Champlain a NFB production for the 400th anniversary of Quebec City. Currently, he is developing Neuropolis, a 3D film about the brain produced in collaboration with the Montreal Neurological Institute and the NFB.
Maya Yonesho
Born in Hyogo, Japan 1965. Yonesho studied Visual Design and Animation at Kyoto Saga University of Arts, which led her to work as an art teacher at a junior high school for 6 years. She returned to college to study Japanese painting and conceptual & media art at Kyoto City University of Arts, while also working as a clay animator for a children's TV program. While on exchange at the Royal College of Art, UK she made her first abstract animated short film, which synchronized 13 international languages under the theme "we can understand each other without understanding each language". She received her MA of fine art in 1998, and began making independent films including believe in it (1998), which won the Excellence prize from the Agency for Cultural Affairs of Japan that same year. She worked for the Eesti Joonisfilm Studio in Estonia from 2002-2003 under the Japanese Government Study Program for Promising Artists and Art Fellowships. Her films introspection(1998), believe in it(1998), learn to love(1999), countdown(2002), Üks Uks(2003), and Winer Wuast (2006) have been shown at numerous international festivals and museums around the world. She has also conducted animation workshops in Taiwan, Norway, Croatia, Israel and Poland, and has lectured at Kyoto Seika University since 2000.
Frances Leeming
Born in Toronto in 1951. Leeming's work as a media artist uses film to re-animate the image archives of 20th century popular culture. Her work has been presented across Canada, the U.S., Britain, Poland and Italy. Her collage animation, The Orientation Express (1987) has been screened internationally, including: Festival de Cine y Vídeo joven de La Habana, Cuba; Seattle Women's Film Festival; ASIFA Animation Festival; San Francisco International Animation Festival; and Women in the Director's Chair, Chicago. Her most recent collage animation Genetic Admiration (2005) won the Grand Prize at Images Festival, Toronto, and was nominated for Best Animation at the Syracuse International Film and Video Festival. The film was also recently featured in the symposium Animation/Automation, part of Screen Magazine's 50th Anniversary Celebration, Whitworth Gallery, Manchester UK. Genetic Admiration (chapter) appears in Jackie Stacey's The Cinematic Life of the Gene, (Duke University Press, 2010) and Jennifer Fisher's Technologies of Intuition, (YYZ/MAWA/DISPLAY CULT, 2006). Leeming's work has been purchased by The National Gallery of Canada, PBS, Channel Four UK, SBS Australia, The Women's Television Network and for numerous university archives throughout Canada and the U.S., and her contributions as a performance artist appear in Johanna Householder and Tanya Mars' book, Caught in the Act- An Anthology of Performance Art by Canadian Women (YYZ Books, 2004). She currently teaches experimental animation and media studies in the Department of Film and Media, Queen's University, Kingston, Ontario.
INTERNATIONAL JURY FOR ANIMATED FEATURE FILMS
Atsushi Wada
Atsushi Wada was born in 1980 in Hyogo Prefecture, Japan. He attended Osaka Kyoiku University, Liberal Arts School, where he began his study in animation. He graduated in 2004, and continued as a graduate student at the Image Forum Institute of the Moving Image (Tokyo) in 2005. His animated films have won awards and been seen at festivals all over the world: worm dance hand (2003) won the Grand Prize at the Tokyo Film Festival (2004); Day of Nose (2005) won the competition of the 52nd International Short Film Festival Oberhausen (Germany) and won for best short film at the Norwich International Animation Festival, Part 3 (UK); Well, That's Glasses took the 2007 best of festival award at the Ubusara 26th International Short Film Festival (Sweden), won the Jury Award for Best Young Animation at the Rio de Janeiro International Short Film Festival (Brazil), and won the competition at the International Short Film Festival Winterthur International Short Film Festival Winterthur (Switzerland) in 2008. In addition to his work in film, Wada's work for television has been broadcast since 2003. He continues to create animated works thanks to what he calls the power of inherent patience, which he credits to the love between the imagination and the bold will to achieve. Wada now works in the Animation Department of the Graduate School, Tokyo University of Arts.
Torill Kove
A Montréal animator and illustrator, Kove grew up in Norway and also spent some of her childhood in Nairobi, Kenya. She moved to Montréal in 1982 where she obtained a Bachelor of Arts at Concordia University and a Masters Degree in Urban Planning at McGill University. She has also studied architecture at Universitè De Montréal and animation at Concordia's Mel Hoppenheim School of Cinema. Torill began her animation career at the National Film Board working as an assistant on various animation and documentary projects. She has written and directed two animated shorts and written scripts for the TV series Dragon and for the animated short film Snails (), by Pjotr Sapegin. Torill's films have received numerous international awards. Her first film My Grandmother Ironed The Kings Shirts (1999) was nominated for an Academy Award, and her second film, The Danish Poet (2006), received a Genie and an Oscar in 2007. Torill has illustrated 6 picture books, two of which she also wrote, and she periodically teaches part-time at the Mel Hoppenheim School of Cinema.
Michaela Pavlatova
Michaela Pavlátová graduated from the Academy of Arts, Architecture and Design in Prague in 1987. Her short animation films have won numerous awards all over the world. She came to international prominence in 1991 when her short animation film "Words, Words, Words" was nominated for a U.S. Academy Award. In 1995, her animation short film "Repete" won a Golden Bear at the Berlinale. Since 1995, she has been blending live-action with her animation. From 1998 to 2001, she divided her time between Prague and San Francisco, where she worked as art director for the Wildbrain, Inc. In 2003 she directed her first all live-action film, the feature "Faithless Games", winner of a Special Jury Mention in the New Director's Prize competition at San Sebastian IFF. In 2008 she directed another feature Deti noci / Night Owls which was awarded a Best Actor and a Best Actress at Karlovy Vary International Film Festival.


Chicagoan Flea — SOCIAL CHICAGOAN.
The Flea is a monthly Flea Market featuring local artist, creators and dreamers!
We love supporting local shakers and doers to get their products in front of the people in Chicago. Oh and you don't have to ask us twice if we like to boogie!! For The Flea, we team up with other party people who will keep you boozin' n groovin' while you shop. Come jive with us!
Our third Chicagoan Flea vendor applications are now open! Please be sure to select the market you'd be most interested in participating in!
If you're a local creator or dreamer interested in being a vendor at The Flea please submit your information here.
If you're a local musician or entertainer that is interested in performing at The Flea please submit your information here.
If you're a local artist that is interested in being the featured artist at The Flea please submit your information here.


Avatar Fan Fic! Death of a Movie Star.
I was messing around with perspectives, and I wrote up this. I decided I should share it with you guys. It's very short and simple. Again, I was only playing with perspectives.
Yep, short and simple. Kinda neat though how what he was supposed to act out really happened to him.
Yeah, glad it worked out ok.


text:
Q: How do I dynamically update a C++ ListView? I'm looking to insert data into a Listview on an event (e.g. new message received) rather than through a button click. This means that throughout the runtime of the software, rows will be continually added and deleted.
How do I go about doing this? I can add rows when I create the ListView e.g.
LVITEM lvi;
lvi.mask = LVIF_TEXT;
lvi.iItem = 0;
lvi.iSubItem = 0;
lvi.pszText = bob;

ListView_InsertItem(list, &lvi);

But I don't know which windows message handler I would need to put this in if I wanted to update on-the-fly. E.g. does it go in WM_PAINT? WM_NOTIFY? Etc.
I'm using the Win32 listview without MFC.
Thanks in advance!

A: You are over thinking this. Simply modify the list whenever your timer fires (or some other event). The rest list view control knows it needs to be re-painted and so will invalidate itself. This will provoke a paint cycle and the list view window will therefore get asked to paint itself.

redpajama_set_name: RedPajamaStackExchange


I went there to see if he bought guns. He said "maybe, depends". So I brought in a browning 22 rifle with a large scope on it, and I said what I thought it was worth, and he said yes but offered 1/2 of that ! Never going back !
Lisa is cool..been going there for years, however, the vaping hardware is way to damn expensive. Nice variety though.
I went to E-Z Pawn looking for a blu-ray player. Having never owned one, I didn't know what features to look for and whether it was worth buying over a DVD player. Lisa came out to the floor and assisted me with every question and was honest about the pros and cons of blu-ray vs DVD. She also helped me find the blu-ray player that was best suited for what I would need. The entire staff was very friendly and helpful. Some of the most helpful I've experienced in a long while. Rather than try to push me into buying, they offered me many options and let me decide what or even if I wanted to buy something. I was so impressed with their help and recommendations that I returned a few weeks later to buy movies from them as well. I will happily recommend this business to my friends.
Family owned and operated with great atmosphere. By far the best Cajun cooking I've ever had and a menu that will continue to bring you back again and again.
Randy Qualls works well with every one of his customers. He does all he can to ensure that ever customer leaves his business with a smile on his face. I would recommend his business to anyone and everyone!
I went there today looking for a Retro video game piece.# that I lovewithout even asking "may i help you" ...he said, " I'm not interested" ...I didn't even ask, "if he were."and rudely cut me off! assuming ...I wanted him to pay me for something . I suppose?? HOW RUDE! This was my first time there and I will never go back or recommended it to anyone ...I sincerely wish him the worst of luck!


text:
The Drama Desk Award for Outstanding Book of a Musical is an annual award presented by Drama Desk in recognition of achievements in the theatre among Broadway, Off Broadway and Off-Off Broadway productions. For two years, in addition to the award for Outstanding Book, an award was presented to the writers of the Most Promising Book. Recipients of this honor were Melvin Van Peebles for Ain't Supposed to Die a Natural Death in 1972 and Ron House and Diz White for El Grande de Coco-Cola in 1973.

Winners and nominees

1970s

1980s

1990s

2000s

2010s

2020s

Multiple wins

 3 wins
 James Lapine
 Thomas Meehan
 Hugh Wheeler

 2 wins
 Rupert Holmes

Multiple nominations

 5 nominations
Terrence McNally

 4 nominations
James Lapine
Thomas Meehan

 3 nominations
Joe DiPietro
Michael John LaChiusa
Dick Scanlan
John Weidman
Hugh Wheeler
Alfred Uhry

 2 nominations
Douglas Carter Beane
Chad Beguelin
Scott Brown
Harvey Fierstein
John Guare
Rupert Holmes
Anthony King
Jonathan Larson
Warren Leight
Jim Lewis
Bob Martin
Marsha Norman
Lynn Nottage
Peter Stone
Jeff Whitty
Doug Wright

See also

 Tony Award for Best Book of a Musical

References

External links
 Drama Desk official website

Musical Book

redpajama_set_name: RedPajamaWikipedia


text:
Q: Merging data points in NLTK's ConditionalFreqDist I have a Prussian newspaper corpus covering the years from 1863 to 1894 and want to plot the word usage over time. The corpus consits of roughly 2400 xml files, one file for each issue. If I would plot the ConditionalFreqDist I would get a graph with 2400 data points on the x-axis, which renders the graph unreadable.
How can I merge the information concerning the same year, displaying the average usage of each word in my search list u_input? E.g: I have 3 files for the year 1863, looking for the word 'König' - king (among other search terms), the first file contains 1 mention, the 2nd file 3 and the 3rd file 2. I would like the graph to only have one data point '1863' with the value '2'.
The plotting function:
def _plot_input():
    cfd = nltk.ConditionalFreqDist(
        (target, fileid[:-4])  # takes first 4 characters as lable names = year
        for fileid in reader.fileids()  # for all files in directory
        for w in reader.words(fileid)  # for all words in each file
        for target in u_input
        if w.lower().startswith(target) # includes words like 'könliglich' if search term was 'König'
    )
    cfd.plot(title='Word usage over time in Prussian Newspapers')

u_input is a list containing the words I'm analyzing, reader is my corpusreader object, files are named like this yyyy-mm-dd.xml, e.g. "1867-03-06.xml".
Thanks in advance.
Edit:
The quick fix would be to loop over all files, read all files beginning with the same year and write the contents into one single new file for each year.

A: To extract the year from the filename you must write fileid[:4], not fileid[:-4]. Once you do that, you'll have only as many x positions as there are distinct years in your corpus. This is exactly equivalent to the "quick fix" you suggest.
However, the y values will be totals for the year, not per-file averages within each year as you ask. If this is really what you needed, edit your question to clarify. (I suspect that what you really need is an average over the total number of words in a year; anything else is nonsense, unless all your files are exactly the same size.)


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text:
Q: Why requestAnimFrame need bind(this) Why does window.requestAnimFrame must be called like this: window.requestAnimFrame(this.__proto__.animate.bind(this)); and not like window.requestAnimFrame(this.__proto__.animate);.
My js-class looks like:
Game = function (moduleConfig, gameConfig) {
    this.moduleConfig = moduleConfig;
    this.gameConfig = gameConfig;

    // Game-Commands
    this.keyCommands = {
        moveLeft: false,
        moveRight: false
    };

    // Some init stuff

    requestAnimFrame(this.animate.bind(this));

    return this;
}

/**
 * Init the game system
 * @param {moduleConfig} moduleCongif - Module-Config instance
 */
Game.prototype = {

    // General member
    self: null,
    moduleConfig: null,
    gameConfig: null,

    // Game member
    renderer: null,
    catcher: null,
    stage: null,

    // Nested 'static' objects
    keyCommands: {
        moveLeft: false,
        moveRight: false
    },

    // Some more stuff

    /**
     * Main loop
     */
    animate: function () {
        window.requestAnimFrame(this.__proto__.animate.bind(this));

        // Some more things to do
    }
}

If i do not use bind, i get the following error message: Failed to execute 'requestAnimationFrame' on 'Window': The callback provided as parameter 1 is not a function..
Thank you!

A: Because your animate is Game's method and since its a recursive function it need a context to be able to call the next animate.
Now i've already told you that(or maybe it was someone) else but .bind is really bad to use for many reason - for you the main reason its extremely slow and you are making a render functionality that need to run extremely fast
to avoid the use of bind i would do:
animate: function () {
    var self = this
    window.requestAnimFrame(function(){
        self.animate();
    });

    // Some more things to do
}

A: window.requestAnimFrame may call the window.requestAnimationFrame which will call the parameter function every second.Without 'bind(this)','this.proto.animate' will call window.proto.animate.With 'bind(this)',it will call the Game's animate function and that will be correct.'bind(this)' just pass the Game context to this.


text:
Алекса́ндр Ива́нович Ло́сь (род. , Днепропетровск) — советский, украинский и молдавский автогонщик, 4-х кратный чемпион СССР по автокроссу в классе "багги", многократный чемпион УССР, МССР и независимой Молдовы.

Автоспортом занялся в 1976 году в секции картинга автозавода Коммунар. В 1977 году автокросс на багги получил статус чемпионата СССР, и Лось, изготовив свой первый спортивно-кроссовый автомобиль, принял в нём участие. На этих соревнования он занял 7-е место, также выполнив норматив КМС.

Становился чемпионом СССР в 1979 (класс II), 1982 (класс I), 1983 (класс I) и 1986 гг.
Серебряный призёр Спартакиады народов СССР 1986 года.
Бронзовый призёр Чемпионата СССР 1987 года.
Чемпион Прибалтики 1979 и 1980 годов.

Спортивную карьеру завершил в 1998 году.

В 1999 году был избран Президентом Федерации Автоспорта Республики Молдова и переизбирался до 2003 года.

Ссылки
 Профиль на сайте baggycross.com.ua

Персоналии по алфавиту
Автогонщики СССР
Автогонщики Украины
Чемпионы СССР по автоспорту


Description "30 [age] ; Carpenter ; 300 [value of real estate owned] ; 100 [value of personal estate] ; Mississippi [place of birth]."
Source Includes data from the 1870 Census Population Schedules, Not Stated, Titus County, Texas, Series: M593, Roll: 1606, p. 113 (stamped), entry 1421.
Artisan or Artist Neal, Callumbus.


Anyone who knows me can tell you that I LOVE my sweets. I consider myself a former sweet addict (thank you Shakeology and 21 Day Fix), but the struggle is real! There are days/times where I need to have something different than my normal sweet fix go to's (apple and almond butter, yogurt and fruit, smoothies, shakes, etc). For those moments I have found a solution. This is what I like to call the "healthy" version of my favorite snack as a kid —> pudding!!
One of the easiest, quickest treats I have ever made!
Place Shakeology, avocado, banana and almond milk in blender; cover. Blend until smooth (if too thick, add additional almond milk – I did not have to do this).
I bet your kids would not even know that you used Shakeology (the healthiest meal of the day) to make this yummy treat! Try it out and let me know what you and your family think!


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text:
Q: How do i establish two way encrypted server-client-connection in python? For a project, I need a server and a client. Not a problem so far. The difficulty is for me, that the connection must be encrypted since sensible information will be sent. You could use RSA encryption. I just don't know yet how to exchange the keys so nobody could intercept them or get any other chance to reach them.
Since I don't know, how to do it in general, I did not try anything so far.

A: Here is a TLS connection implementation in Python. All key exchanging and encrypting data is done within the protocol.
import socket
import ssl

def main():
  #Define Host Name And Port (Port 443 Is Typical Encrypted Web Connection Port)
  host_name = "www.google.com"
  host_port = 443

  #Create Unencrypted Connection And Then Encrypted It By Wrapping It
  unencrypted_socket = socket.socket(socket.AF_INET,socket.SOCK_STREAM)
  unencrypted_socket.settimeout(10)
  encrypted_socket = ssl.wrap_socket(unencrypted_socket,ssl_version=ssl.PROTOCOL_TLSv1) #Optional Ciphers Spec Parameter Too

  #Connect To The Host, Send Data And Wait To Recieve Data
  encrypted_socket.connect((host_name,host_port))
  encrypted_socket.send(b"Hello")
  response = encrypted_socket.recv(512)

  #Close The Connection
  encrypted_socket.close()

main()

Note: I am using Python 3.6, and I think that a newer version of TLS is available to use as of Python 3.7.


text:
Home » Lifestyle » Kaitlyn Bristowe & Jason Tartick Are Having Fun For A Good Cause In These Vacation Photos
Kaitlyn Bristowe & Jason Tartick Are Having Fun For A Good Cause In These Vacation Photos
12/05/2019 Comments Off on Kaitlyn Bristowe & Jason Tartick Are Having Fun For A Good Cause In These Vacation Photos
Ahead of the new season of The Bachelorette, one former lead continues to live out her own fairy tale. Kaitlyn Bristowe and Jason Tartick's relationship is stronger than ever, as evidenced by their recent Mexico vacation. On Saturday, the pair headed to Cancun from Kaitlyn's home base of Nashville, and it looks like they're having a blast spending quality time together.
Jason and Kaitlyn have been doing long-distance (he's based in Seattle) since going official with their Bachelor Nation romance in January. The couple initially connected on an episode of Kaitlyn's podcast, Off the Vine. Some flirty Instagram comments and a friendship followed, and now the couple is jetting off on a Cancun getaway. Jason and Kaitlyn have been documenting their trip on the 'gram, with Jason even sweetly buying Kaitlyn a bouquet of "airport flowers." "It's the thought that counts," she can be heard saying in another video. "I love them."
Kaitlyn revealed in an Instagram post that she and Jason were in Mexico not only to have some fun in the sun, but to support a charitable cause. "Tatted up and flexing for FA," Kaitlyn captioned a photo of her and Jason in their swimwear and sunnies. "@jason_tartick and I are lending some muscle from Mexico to show support and raise awareness of Friedreich's Ataxia, a degenerative neuromuscular disease." Kaitlyn went on to explain, "LUSM encourages you to run, walk, jog, swim, (we're about to do that), cycle, jog, box, jump — anything to get your heart pumping. In doing so, we're supporting research to hopefully #CureFA for my best friend's 8-year-old nephew and others worldwide diagnosed with this rare genetic disease."
Jason, who was a finalist on Becca Kufrin's season of The Bachelorette, posted a photo to his Instagram Stories of him and Kaitlyn poolside with the caption, "Whole ocean in front of us and we're at the swim up bar."
Kaitlyn and Jason are clearly moving full-stream ahead with their budding relationship. Kaitlyn and Shawn announced their split in November 2018, but the way the former reality star sees it, that relationship led her directly to her new love. Kaitlyn told Bustle in April that while her breakup was "really tough," she is now in a relationship where she feels fully supported in all of her endeavors. "He just is my biggest cheerleader," she said to Bustle. "Like he is such a hype man and, he always tells me, 'Oh, you have so much impact on people and you're just so empowering and I'm just so proud of you.'"
Fans are clearly invested in their relationship, which Kaitlyn talked about on last week's Bachelorette reunion special. And she says she can feel the love from Bachelor Nation. "I feel so much support from everybody," Kaitlyn told Bustle. "I mean I know everyone looks happy on Instagram, but I feel like people can really genuinely see my happiness." She admits she felt "a little worried" about "how much to share and I didn't want to be insensitive to my last relationship," but she can't deny that she's an open book. "Whether that's happiness or tough times or whatever I'm going through, I can't hide being so happy."
If Kaitlyn and Jason's latest 'gram PDA is any indication, they continue to be totally in love.
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v. t. 1. To vamp again; hence, to patch up; to reconstruct.
Verb 1. revamp - to patch up or renovate; repair or restore; "They revamped their old house before selling it"
2. revamp - provide (a shoe) with a new vamp; "revamp my old boots"


Motorists have experienced heavy traffic congestion in Boston town centre today as a six-week period of works to install a new cycle path begins.
One lane of John Adams Way is to be shut in each direction around Haven Bridge between 9.30am and 3pm.
The closure comes to allow a new cycle path to be installed between South Square and the crossing where High Street meets John Adams Way.
High Street is also shut between the John Adams Way junction and Nelson Way for the duration of the works.
The lane closure could last up to six weeks, although John Adams Way will operate with both lanes outside the 9.30am-3pm time slot.