text:
\section{Introduction}
\label{sec:intro}
Core-collapse supernovae (SNe) are explosive events that
occur at the final stage of the massive-star evolution. In the typical
scenario \citep[e.g.,][]{Janka2012b}, after the collapse of
the iron core of progenitor stars, a proto-neutron star (PNS) is
first formed.  Then, a shock wave is generated at the inner
core of the PNS and propagates outward sweeping the matter. However, because of the photo-dissociation of irons,
the shock is stalled in the middle of the propagation. Subsequently,
the heating by neutrinos emitted from the PNS is believed to play a key role
for supplying the energy to the stalled shock~\citep{Bethe1985a}. If
the neutrino heating timescale becomes shorter than that of the matter
infall from the outer envelop, the stalled shock is revived and
the explosion is driven by the neutrino
heating~\citep{Janka2001a}.  By contrast, if the neutrino
heating is not efficient enough, the stalled shock eventually goes
back to the PNS and a black hole (BH) is formed.  In particular, for
high-mass progenitor stars with the zero-age main-sequence (ZAMS) mass
of $M_{\rm ZAMS} \agt 40M_\odot$~\citep{Woosley2002a}, the naive expectation for the final fate is the formation of a BH without the shock revival.

As summarized above, the key quantity for the successful
explosion is the efficiency of the neutrino heating~\citep{Janka2001a}.
In fact, many sophisticated simulations for core-collapse SNe have shown that the
success of the SN explosion depends sensitively on the neutrino
luminosity and neutrino heating efficiency~\citep[for the latest numerical simulations in this field, see, e.g.,][]{Mueller2012,Burrows2019,Nakamura2019,Mezzacappa2020,Muller2020a,Stockinger2020,Kuroda2020,Harada2020,Obergaulinger2020,Bollig2020}.

In this paper, we propose a mechanism by which the neutrino luminosity of the central object is naturally enhanced for very high-mass rotating progenitor stars.
We consider a rotating progenitor core, which results in a PNS rapidly rotating with the rotational period of $\leq 1$\,ms and surrounded by a massive torus with the mass beyond $1M_\odot$. Due to the rapid rotation, the PNS with the rest mass $\agt 3M_\odot$ can survive for the equation of state (EOS) with which the maximum gravitational mass for
cold non-rotating neutron stars (NSs), $M_\mathrm{max}$, is larger than
$2M_\odot$. This appreciably increases the lifetime of the PNS. In
addition, due to the presence of a compact massive torus as well as
the high mass of the PNS, the total neutrino luminosity is enhanced during the evolution
of the system. Furthermore, because of the flattened
geometry of these central objects, the neutrino flux is
enhanced in the polar region. As a consequence, the
neutrino heating timescale of the stalled shock becomes shorter than
the timescale of the matter infall in the polar region,
leading to a bipolar explosion.

By performing numerical-relativity simulations, we will illustrate that
this mechanism can indeed work for a rapidly rotating progenitor of
$M_{\rm ZAMS}\approx
45$--$65M_\odot$, which corresponds to the range of He-core mass of $M_\mathrm{He}=20$--$32M_\odot$. For such high-mass rapidly-rotating progenitors,
the total mass of the PNS
and surrounding torus becomes also high, and hence, the neutrino luminosity
is enhanced as well. As a result, the bipolar outflow becomes more
energetic than the ordinary SNe.
Thus, this mechanism may produce a class of energetic SNe like
broad-line type-Ic SNe (see, e.g.,
\citet{Woosley2006a,Cano2017a} for reviews).

This article is organized as follows.
In \S~\ref{sec:method}, we
summarize the progenitor models employed as the initial condition for
numerical-relativity simulations together with a brief summary of our
method for the simulation.  The results for the successful explosion
are shown in \S~\ref{sec:results}.  Section~\ref{sec:summary} is
devoted to a summary and discussions.

\section{Models and Method} \label{sec:method}

\begin{table*}[t]
\caption{List of the models and the results.
$t_\mathrm{exp}$ and $t_\mathrm{BH}$ denote the post-bounce time at the onset of the explosion and that of the BH formation, respectively.
}
\begin{center}
\begin{tabular}{lccccccc}

\hline \hline

Model & $M_\mathrm{He}$ & $\Omega_0$ & $R_0$ & $(\chi_{5M_\odot},\chi_{10M_\odot}$) & $t_\mathrm{exp}$ & $t_\mathrm{BH}$ & $E_\mathrm{exp}$ \\
 & $(M_\odot)$ & (rad/s) & (km) &  & (s) & (s) & ($10^{51}$\,erg) \\
\hline
M20-0     & 20 &  0  & ---  & (0,0) & --- & 0.3 & --- \\
M20-S040  & 20 & 0.40& 6000 & (1.0, 0.34) & --- & 1.1 & --- \\
M20-S050  & 20 & 0.50& 6000 & (1.3, 0.43) & 3.3 & 4.3 & \addsf{4.2} \\
M20-S075  & 20 & 0.75& 6000 & (1.9, 0.65) & 4.8 & 7.2 & \addsf{4.5} \\
M20-S100  & 20 & 1.00& 6000 & (2.5, 0.87) & 5.9 & 9.8 & \addsf{3.6} \\
M20-L050  & 20 & 0.50& 8500 & (2.2, 1.1) & 7.4 & 9.1 & \addsf{1.2} \\
M20-S050N & 20 & 0.50& 6000 & (1.3, 0.43) & 3.5 & 4.3 & \addsf{1.7} \\
\hline
M32-0     & 32 & 0   & ---  & (0,0) & --- & 0.1 & ---  \\
M32-S050  & 32 & 0.50& 5800 & (1.1, 0.61) & --- & 1.0 & ---  \\
M32-S075  & 32 & 0.75& 5800 & (1.7, 0.92) & 2.7 & 4.3 & \addsf{52} \\
M32-S100  & 32 & 1.00& 5800 & (2.3, 1.2) & 3.2 & 5.1 & \addsf{26} \\
M32-S075DD2 & 32 & 0.75& 5800 & (1.7, 0.92) & 2.8 & 4.4 & \addsf{58} \\
M32-S075N   & 32 & 0.75& 5800 & (1.7, 0.92) & 3.0 & 4.3 & \addsf{11} \\
M32-S075-modE & 32 & 0.75& 5800 & (1.7, 0.92) & 2.6 & 4.3 & \addsf{66} \\

\hline
\end{tabular}
\end{center}
\label{tab:model}
\end{table*}

We employ the final state of high-mass stellar evolution models as the initial condition of our numerical-relativity simulations.
The stellar evolution of non-rotating He-star models with their initial mass of $M_{\rm He}=20$ and $32M_\odot$ is calculated using the code described in~\citet{Takahashi2018}.
For these models, $M_{\rm ZAMS}\approx 45$ and $65M_\odot$, respectively~\citep{Woosley2002a}. The evolution calculation is performed until the central temperature reaches $\approx 8 \times 10^9$ K. At this stage, the central density is $\approx 8 \times 10^8\,{\rm g/cm^3}$ for $M_{\rm He}=20M_\odot$  and $\approx 5 \times 10^8\,{\rm g/cm^3}$ for $M_{\rm He}=32M_\odot$.

Observationally, it is known that at least some broad-line type-Ic SNe are associated
with gamma-ray bursts \citep[GRBs;][]{Cano2017a}, and
theoretically, a broadly accepted candidate for the central engine of GRBs
is a system composed of a rapidly spinning BH and a dense accretion torus.
For the formation of the BH-torus system, a rapidly rotating
progenitor star is obviously necessary~\citep{Woosley1993,Macfadyen1999}.
Hence, we consider rapidly rotating massive stars as the progenitor of such energetic SNe.
Rapidly rotating progenitors may be formed via peculiar single-star evolution~\citep{Yoon2005,Woosley2006} or by binary merger~\citep[e.g.][]{Fryer2005}.
Recent stellar-evolution simulations predict that cores of the fastest rotating core-collapse progenitors may have $\approx 3 \times 10^{16}$\,cm$^2$\,s$^{-1}$ of the averaged specific angular momentum, or equivalently, $\approx 1.36$ of the spin parameters,  inside the enclosed mass of 5 $M_\odot$~\citep{Aguilera-Dena2018}.
These results should be interpreted with caution, however, as even the most advanced stellar-evolution simulations take into account the effects of angular-momentum transport via the convection, circulation, and magnetohydrodynamics (MHD) in a phenomenological manner.

The other point to be stressed is that during the long-term evolution of the PNS and the torus surrounding it, which are the typical outcomes for the rapidly rotating stellar core collapse, the angular momentum transport can play an important role for the evolution of the system, because the timescale of viscous angular momentum transport, which is likely to stem from MHD instabilities, is typically several hundred milliseconds \citep{fujibayashi2018a,Fujibayashi2020a,Fujibayashi2020b}, while we follow the evolution of the system for seconds.
It is also possible that MHD effects such as magnetic braking play an important role for the angular momentum redistribution. Thus, the specific angular momentum distribution of the progenitor star is likely to be significantly modified during the long-term evolution of the system. However, currently, it is not clear how efficiently such angular momentum redistribution proceeds.

Thus in this paper, as a first step toward a more detailed study, we add an ad-hoc, simple angular momentum profile to the final state of the evolved stars for the initial conditions, with which a system composed of a central object (either an NS or BH) surrounded by a massive torus is formed, even in the absence of the angular momentum
redistribution during the evolution of the collapse outcome (note that no angular momentum
transport effect is taken into account in this work).

Specifically, the following cylindrical profile is imposed for the angular velocity:
\begin{align}
\Omega = \Omega_0 e^{-R^2/R_0^2}, \label{eq:Omega}
\end{align}
where $\Omega_0$ is the angular velocity along the rotation axis
($z$-axis), $R$ the cylindrical radius, and $R_0$ a cut-off radius.
This rotational profile is somewhat different from the one obtained in the
stellar-evolution simulations, in which the angular velocity is described as
a function of the radius in the spherical polar coordinates.
However, because the contribution of the matter along the rotation axis to the mass and angular momentum of the star is minor, the effect of the difference in the profile from spherically symmetric one is likely to be minor.

For $R_0$, we choose the radius at the edge of the Si layer (L model), at which the entropy profile becomes discontinuous, or 70\% of this radius (S model).
Equation~(\ref{eq:Omega}) implies that for $R \ll R_0$, the progenitor star is approximately rigidly rotating, while for the outer region,
stellar matter rotates slowly.
Such a state is reasonable if the efficiency of the angular momentum transport in the compact central region is sufficiently high.
The steep cut-off of the angular velocity is achieved during the stellar evolution in the presence of the convective layer associated with the shell burning, in which the angular momentum at the bottom of the layer is transported to a large radius.

Table~\ref{tab:model} lists the models considered in this work.
M20 and M32 denote the models with $M_{\rm He}=20$ and $32M_\odot$, respectively.
The letters ``S" and ``L" refer to the choice of $R_0$ and the following three-digit numbers denote the value of $\Omega_0$ in units of 0.01\,rad/s.
We also perform simulations omitting the neutrino pair-annihilation heating
(models M32-S075N and M20-S050N)
to show that this effect contributes substantially to increasing the explosion energy.
To indicate the rapidness of the stellar rotation,
in Table~\ref{tab:model}, we present a dimensionless spin parameter
defined by $\chi_M=cJ/GM^2$ where $J$ and $M$ are total angular momentum and
rest mass enclosed in mass shells at $M=5M_\odot$ and $10M_\odot$.
\addkt{We note that the values of $\chi_M$ are broadly comparable to the results of a state-of-the-art stellar evolution simulation \citep[e.g.,][]{Aguilera-Dena2018}.}

A finite-temperature EOS referred to as SFHo~\citep{steiner2013a} is employed in this work except for model M32-S075DD2, in which another EOS referred to as DD2 \citep{banik2014a} is employed for comparison.
With SFHo and DD2 EOSs, the maximum values of the gravitational mass for
the non-rotating cold NSs are $M_\mathrm{max} \approx 2.06$ and 2.42$M_\odot$, and the radii of the non-rotating NSs with mass $1.4M_\odot$ are 11.9 and 13.2\,km, respectively.
The SFHo EOS is relatively soft in the sense that the value of $M_\mathrm{max}$ is close to $2M_\odot$ and the radius is relatively small as $\alt 12$\,km.

With the setting listed in Table~\ref{tab:model}, the PNS formed after the collapse is rapidly
rotating and the resulting centrifugal force plays an important role
to allow the rest mass of the PNS beyond $3M_\odot$ (cf.~Fig.~\ref{fig:fig1}
in \S~\ref{sec:results}).
We note that several other simulations, for which we do not present the results
in this article, already confirmed the collapse to a BH without the shock revival for $\Omega_0 \leq 0.4\,\mathrm{rad/s}$ for $M_\mathrm{He}=20M_\odot$ and for $\Omega_0 \leq 0.5\,\mathrm{rad/s}$ for $M_\mathrm{He}=32M_\odot$.
We also note that, for non-rotating models, the PNS collapses into a BH approximately at 0.1\,s and 0.3\,s after bounce for $M_\mathrm{He}=32M_\odot$ and $20M_\odot$ models, respectively.

Numerical-relativity simulations are performed with our latest axisymmetric neutrino-radiation viscous-hydrodynamics code.
The details are described in~\citet{fujibayashi2017a,Fujibayashi2020b}.
In this work, we do not take the viscosity into account.

Einstein's equation is solved with the original version of the puncture-Baumgarte-Shapiro-Shibata-Nakamura formalism \citep{shibata1995a,baumgarte1999,marronetti2008} incorporating the Z4c prescription \citep{Hilditch2013a} for the constraint violation propagation.
We solve geometrical variables in Cartesian coordinates and employ the so-called cartoon method to impose axisymmetry to them \citep{Shibata2000a,Alcubierre2001a}. The spatial
interpolation necessary for the cartoon process is carried out using the
fourth-order accurate Lagrangian interpolation.

The radiation hydrodynamics equations are solved with a version of the leakage scheme together with a moment transport scheme.
The detailed description of the schemes is found in \cite{sekiguchi2010a} and \cite{fujibayashi2017a}.
In this method, the emitted neutrinos are divided into ``trapped" and ``streaming" components.
The trapped neutrinos are assumed to be thermalized with the fluid, and treated as a part
of the fluid. In our numerical scheme,
they are diffused out to the streaming component in the diffusion timescale.

The streaming neutrinos are solved using energy-integrated truncated-moment formalism \citep{shibata2011a} with the so-called M1-closure relation to estimate the higher moments.\footnote{It is well-known that the crossing multiple beams cannot be appropriately solved with moment-based schemes, and it can be a source of the systematic error on the neutrino distribution and heating rate in the system with a non-spherical hydrodynamical profile.
In~\citet{Sumiyoshi2021}, the Eddington tensor is evaluated with a Boltzmann neutrino transfer code and compared with that by an M1-closure relation for a system composed of a massive NS and a torus formed in a binary NS merger.
It is found that the deviation of the Eddington tensor from that derived with the M1-closure is at most 10\% in the edge of the NS and torus, and in the polar region the deviation is smaller.
The system that we consider in this work has a similar profile to the one investigated in~\citet{Sumiyoshi2021}, and hence, we expect that the systematic error associated with the moment-based scheme could not be significant, although for more quantitative studies a better radiation transfer scheme such as those in \citet{Harada2020} and \citet{Foucart2020} is obviously required.
}
The heating due to neutrino absorption and pair-annihilation is included in an approximate manner~\citep{fujibayashi2017a}.

The free parameters of our leakage scheme \citep[see][for the parameters]{sekiguchi2010a} are phenomenologically determined. Specifically, we performed simulations for the collapse of a 15\,$M_\odot$ solar-metallicity progenitor \citep{Woosley2002a} and compared the neutrino luminosity at the core bounce with those  in~\cite{Liebendoerfer2003a} and \cite{Janka2012b}.
We then employ the parameters by which their neutrino luminosity curves are approximately reproduced.
The heating of the matter by streaming neutrinos is conservatively incorporated in this work: specifically, the heating term is reduced by a factor of $\exp(-2\tau_i)$ with the optical depth of $i$-th species of neutrinos $\tau_i$ (i.e., this factor is multiplied to the opacity).
Thus, only for sufficiently outside the neutrino spheres, the heating is efficient.

In energy-integrated neutrino transfer schemes, the heating rate due to the neutrino-matter interaction depends on the method for estimating neutrino energy distribution through the energy dependence of the neutrino cross section \citep[see, e.g., ][]{Foucart2016b}.
To illustrate this dependence, we perform an additional simulation with the same setup as M32-S075, but with a different method for its estimation (see Appendix~\ref{app:energy} for the detail and results).

For numerical simulations, we employ the same nonuniform grid as that in our previous work \citep{Fujibayashi2020b}.
In the inner region with $z<15$\,km and $R<15$\,km, the uniform grid is prepared with the grid spacing of 150\,m.
In the outer region, the nonuniform grid is prepared with the increase rate of the grid spacing of 1.01.
The computational domain is $ 0 \leq x \leq L$ and $ 0 \leq z \leq L$ with $L\approx 3\times 10^4$\,km.

\section{Simulations Results} \label{sec:results}

\begin{figure}[t]
\includegraphics[width=0.48\textwidth]{Mass_den2_1e-3.pdf}
\caption{Evolution of the rest mass of the PNS (solid curves) and that
in the optically thick region for neutrinos (dashed curves) for selected models.
\textbf{Note.} Due to the definition of it, the contribution from the torus is
included in the value of $M_\mathrm{PNS}$, and thus, it becomes
very large just prior to the collapse to the BH.
For the same reason, $M_\mathrm{PNS}$ has a finite value even after the BH formation for model M32-S100.
}
\label{fig:fig1}
\end{figure}

\begin{figure*}[t]
\includegraphics[width=\textwidth]{den_4panels_320.png}
\caption{
Snapshots of the rest-mass density at $t_\mathrm{pb}=0.05$, 1.40, 2.75, and 4.40\,s for model M32-S075.
The solid, dashed, and dotted curves denote the surfaces with the density of $\rho=10^{14}$\,g/cm$^3$, with the neutrino optical depth $\tau=1$, and at the stalled shock, respectively.
In the fourth panel, a BH is formed at the center (shaded region).
On all the panels, the arrows display the poloidal velocity field ($v^x,v^z$).
Their length is proportional logarithmically to the velocity.
See also an animation at
\url{http://www2.yukawa.kyoto-u.ac.jp/~sho.fujibayashi/share/anim_den_M32-S075.mp4}.}

\label{fig:fig2}
\end{figure*}

For all the simulations, a PNS is first formed after the stellar-core collapse.
Then, the baryon rest mass of the PNS increases to $M_\mathrm{PNS}= 2.0$--$2.5M_\odot$ in $t_\mathrm{pb}:=t-t_\mathrm{b} \sim 1$\,s
(see~Fig.~\ref{fig:fig1}).
Here $t_\mathrm{b}$ denotes the time at the core bounce and we defined $M_\mathrm{PNS}$ to be the total rest mass in the region of $\rho \geq 10^{14}\,\mathrm{g/cm^3}$
(we note that due to this definition, a part of the rest mass of the dense region of the
torus is included
in $M_\mathrm{PNS}$ just prior to the BH formation).
Subsequently, $M_\mathrm{PNS}$ exceeds $3M_\odot$ for all the rapidly rotating models listed in Table~\ref{tab:model}.
This mass exceeds the maximum rest mass of the non-rotating cold NSs, which is $\approx 2.42 M_\odot$ and $\approx 2.89M_\odot$ for the SFHo and DD2 EOSs, respectively.
Thus, the centrifugal force (and partly the thermal pressure) plays a key role for preventing the collapse of the PNS to a BH for seconds.
Along the rotation axis the rotational period becomes $\sim 0.5$\,ms in the late stage of the PNS.

Together with the PNS, a massive torus is formed around it.
Here, we define the torus mass by $M_\mathrm{torus}:=M_{\tau>1}-M_\mathrm{PNS}$, where $M_{\tau>1}$ is the total rest mass in a region with the average optical depth of electron neutrinos and antineutrinos ($\tau\equiv (\tau_{\nu_\mathrm{e}}+\tau_{\bar{\nu}_\mathrm{e}})/2$) larger than unity.
We find that the torus mass increases by the matter infall and eventually far exceeds $1M_\odot$.
For $M_\mathrm{He}=32M_\odot$ models, this mass becomes very large in a short post-bounce time.
The torus initially has a radius of $\sim 200$\,km on the equatorial plane (see the second panel of Fig.~\ref{fig:fig2} for M32-S075; the dashed curve).
During the growth of the torus, a standing accretion shock with a donuts shape is formed surrounding the PNS and torus (the second panel of Fig.~\ref{fig:fig2}; the dotted curve),  and this shock expands gradually with time due to the shock heating induced by the matter infall.
Because of our choice of the initial angular-velocity profile, the matter that accretes onto the PNS and torus at late times has smaller specific angular momenta.
Because of its high mass and less specific centrifugal force at late times, the torus shrinks (its density increases; the third panel of Fig.~\ref{fig:fig2}), and as a result, the value of $M_\mathrm{PNS}$ steeply increases prior to the formation of a BH (see the upper panel of Fig~\ref{fig:fig1}). For the larger value of $R_0$ for which the specific angular
momentum of the matter in the outer region is larger, the mass accretion timescale is longer.

The shrink of the torus enhances the neutrino luminosity (see Fig.~\ref{fig:fig3} for the increase of it in late stages), in particular from the torus.
The maximum neutrino luminosity is higher for the higher values of $M_\mathrm{He}$ and could be close to $10^{54}\,$erg/s as found in~\citet{Sekiguchi2011}.
Because the ram pressure by the infalling matter decreases with time, such huge neutrino heating naturally leads to the shock revival.
The explosion occurs in particular toward the polar direction for which the matter density and associated ram pressure are relatively small (see Fig.~\ref{fig:fig25}).
The explosion occurs qualitatively in the same manner for all the rapidly rotating models listed in Table~\ref{tab:model}.

Table~\ref{tab:model} lists the diagnostic explosion energy, $E_\mathrm{exp}$.
Here, this explosion energy is evaluated in the computational region of $\alt 30000$\,km by integrating the positive binding energy of the matter as in \citet{Mueller2012} (see Appendix A for our formulation to it).
For the present explosion models, $E_\mathrm{exp}$ eventually exceeds $10^{51}\,{\rm erg}$, and for $M_\mathrm{He}=32M_\odot$ models, it becomes higher than $10^{52}$\,erg, i.e., appreciably higher than the kinetic energy of typical SNe.
This is the reflection of the neutrino luminosity by one order of magnitude higher than in the typical SNe \citep[on the relation between the neutrino luminosity and explosion energy, see, e.g.,][]{Yamamoto2013}.
\addsf{
The explosion energy for models without the neutrino-antineutrino pair annihilation process (M20-S050N and M32-S075N) is 2.5--4 times smaller than that for corresponding models with the process (see Table~\ref{tab:model}).
This indicates that the pair-annihilation of neutrinos is the dominant process of the energy injection.
}

This lager neutrino-driven energy injection could be a substantial fraction of the energy injection for broad-line type-Ic SNe with a bipolar outflow~\citep{Maeda2002a,Maeda2003a,Mazzali2005a,Maeda2008a}.
We note that the energy deposition rate to the outflow is $\gtrsim 10^{52}$\,erg/s for $M_\mathrm{He}=32M_\odot$ models.
Thus, $^{56}$Ni with mass of $10^{-2}$--$10^{-1}M_\odot$ may be synthesized in the ejecta~\citep[][Wanajo et al.~in preparation]{Tominaga2007}.

For model M32-S075DD2, the explosion energy is slightly higher than that for M32-S075, but the difference is not significant.
This is because the lifetime of the PNS and the duration of the energy injection through the neutrino heating are only slightly different between the two models with different EOSs due to the rapid increase of $M_\mathrm{PNS}$ to the critical mass for the gravitational collapse to a BH.

\begin{figure}[t]
\includegraphics[width=0.48\textwidth]{Luminosity_total_1e-3.pdf}
\includegraphics[width=0.48\textwidth]{Eexp_ejecta_1e-3_28854.pdf}
\caption{Top: Total neutrino luminosity as a function of post-bounce time. Bottom: Diagnostic explosion energy as a function of $t-t_\mathrm{exp}$, where $t_\mathrm{exp}$ is the explosion time defined as the time at which the explosion energy exceeds $10^{50}$\,erg.
The filled circle on each curve denotes the BH formation time for each model.
}
\label{fig:fig3}
\end{figure}

\begin{figure}[t]
\includegraphics[width=0.48\textwidth]{4panel_zfull_30000_000000.png}
\caption{Snapshots of the rest-mass density (top-left), entropy per baryon (top-right), temperature (bottom-left), and electron fraction (bottom-right) at $t_\mathrm{pb}=3.80$\,s for model M32-S075. \addms{$k_{\rm B}$ denotes the Boltzmann's constant.}
The arrows display the poloidal velocity field ($v^x,v^z$). Their length is proportional logarithmically to the velocity. See also an animation at
\url{http://www2.yukawa.kyoto-u.ac.jp/~sho.fujibayashi/share/anim_4_M32-S075_30000.mp4}.
}
\label{fig:fig25}
\end{figure}

\addms{For the larger value of $R_0$, the explosion is delayed and the explosion energy is smaller (compare the results of M20-S050 and M20-L050). The reason for this is that for the larger value of $R_0$ (for a given value of $\Omega_0$), the increase of the torus mass is delayed due to the larger centrifugal force, and the specific neutrino emissivity is decreased in the late time at which the explosion is driven (i.e., the formation timescale of the torus is as long as or longer than the neutrino cooling one).
This suggests that the angular momentum distribution is the key for controlling the explosion energy.}

We also note that for model M32-S100, the massive torus remains, maintaining a high neutrino luminosity ($\gtrsim 10^{52}$\,erg/s), after the BH formation (see Figs.~\ref{fig:fig1} and \ref{fig:fig3}).
As a result, the neutrino-driven outflow is still present after the BH formation.
However, the neutrino luminosity is not enhanced significantly and the explosion energy is relatively low for this model, in spite of the formation of a massive torus.
The reason for this is, \addms{again}, that the formation timescale of the torus is as long as or longer than its neutrino cooling one in this model.
Hence, to enhance the neutrino luminosity far beyond $10^{53}$\,erg/s, the torus has to be formed before the sufficient neutrino cooling occurs.
For achieving such a physical state, a pre-collapse progenitor with a compact core, which
has angular momentum sufficiently large in its inner region with a steep cut-off at a
radius, is likely to be necessary.

For the high-mass progenitors employed in this work,
a BH is eventually formed due to the continuous
matter accretion onto the PNS, in particular from the equatorial direction.
Since the central object gains a large amount of the angular momentum from the rotating progenitor, the BH at the formation is rapidly spinning with the dimensionless spin $\gtrsim 0.9$ irrespective of the models.
The rest-mass density in the vicinity of the rotation axis becomes low as $\alt 10^3\,{\rm g/cm^3}$ after the BH formation (see the fourth panel of Fig.~\ref{fig:fig2}).
The eventual total rest mass in the funnel region of
$R \leq 50$\,km and $|z| \leq 10^4$\,km is
$\alt 10^{-7}M_\odot$.

\section{Summary and Discussions} \label{sec:summary}
This article proposes a new mechanism for driving energetic SNe like broad-line type-Ic SNe by the neutrino heating.  The
model supposes that the progenitor stars of the SNe have high mass and
rotation rapid enough to form a rapidly rotating PNS surrounded by a
high-mass torus. The resulting PNS can survive for seconds due to the
strong centrifugal-force support, and in addition, due to the presence of a
high-mass torus surrounding it, the total neutrino luminosity can be
quite high at several seconds after the core bounce. Then, the
neutrino heating drives a high-energy SNe, in particular toward the polar direction.  In the successful explosion, the total rest mass of the central object becomes high enough (i.e.,
$\agt 3M_\odot$) and the explosion is significantly delayed, typically
for seconds, after the core bounce (thus to study this model, we need a long-term
general relativistic simulation, only by which the criterion for the
formation of the BH is accurately taken into account). In this case, the explosion occurs
in a bipolar manner via the neutrino heating.
The explosion energy is beyond the typical explosion energy of SNe $\sim 10^{51}\,{\rm erg/s}$, and even larger than $10^{52}$\,erg for high-mass progenitor models.
Thus, this mechanism could provide (at least a part of) energy-injection for energetic SNe like broad-line type-Ic SNe.

Furthermore, a rapidly spinning BH is eventually formed.
Since the polar outflow found in this paper produces a low-density funnel along
the rotation axis, the remnant looks suitable for launching an ultra-relativistic jet, i.e., GRB~\citep[][]{Woosley1993,MacFadyen2001,Woosley2006a,Cano2017a}, in the presence of
an energy injection.
We here note that the mechanism for launching the ultra-relativistic jet is not necessarily the same as that for inducing the bipolar outflow; e.g., an MHD
process may be the source for GRBs; see, e.g.,~\citet{Piran2004}.
If the formed BH is surrounded by a magnetized massive torus, such a system could drive a relativistic jet by subtracting the rotational kinetic energy of the BH~\citep{Blandford1977}.
The relativistic jet could not only drive a GRB but also be the additional energy injection for the SN explosion. Thus, this model provides a scenario for the association of broad-line type-Ic SNe and GRBs.

However, in the angular-velocity profiles chosen in this paper,
the matter initially located in large radii has small angular momenta.
Thus, except for M20-L050, the torus mass is not very large after the BH formation, and hence,
in the present models,
it is unlikely to subsequently cause long-term energetic phenomena powered by the accretion of the torus matter onto a BH.
By contrast, if the matter in the outer region initially has larger specific angular momenta than that in the central region, which may be a reasonable assumption considering more realistic stellar evolution, a massive accretion torus can be formed after the BH formation.
In such a case, a further activity of the system is expected.
Exploring this possibility is interesting future work.

The above speculation suggests that the presence or absence of the activity after the bipolar explosion may depend on the angular momentum distribution of the progenitor stars, and this may explain a variety of the activity
duration of the central engine and
a variety of the high-energy events associated with the
broad-line type Ic SNe~\citep{Woosley2006,Margutti2014,Lazzati2012} (see also~\citet{Nakar2015} on the importance of the density profile of the pre-collapse progenitor).
Our numerical results also match with the speculation that
the rapidly rotating massive stars are likely to be
the progenitors for the energetic type-Ic SNe and GRBs~\citep{Yoon2005,Fryer2005,Woosley2006,Aguilera-Dena2018}.

Recent radiation-MHD simulations (in non-relativistic gravity) by \citet{Obergaulinger2017,Obergaulinger2020,Obergaulinger2021,Aloy2021a} also have shown that in the presence of a rapid rotation, a high-mass progenitor star can explode by the combination of the neutrino heating, rotation, and magnetic-field effects.
Our result is similar to theirs, but our work shows that an energetic explosion can occur purely by the neutrino heating effect even in the absence of magnetorotational effects, for the progenitor stars more massive than that employed in \citet{Obergaulinger2017,Obergaulinger2020,Obergaulinger2021,Aloy2021a}.
The only required condition for our case is the presence of sufficiently rapid rotation
inside the stellar core.

In this paper, we present only models that show the explosion.
For low angular-momentum models, the PNS collapses to a BH before the explosion.
Thus, for the explosion, the progenitor stars need to have a sufficient angular momentum.
The details on the non-explosion models and approximate criterion for the explosion should be systematically studied.

There are several issues to quantitatively improve the present work.
First, our treatment for the neutrino-radiation transfer is currently based on a gray leakage scheme. Obviously, simulations with a better radiation transfer code are needed.

The present work is based on axisymmetric simulations. Because the torus is massive,
non-axisymmetric deformation is likely to take place in reality \citep[e.g.,][] {Shibata2005,Shibagaki2020}. This may cause an
angular momentum transport in the torus and the accretion onto the PNS
may be enhanced leading to earlier collapse to a BH. The
angular momentum transport can also be enhanced by
MHD effects such as the magneto-rotational
instability~\citep{Moesta2014} and magnetic braking.
Alternatively, MHD effects may help earlier explosion if
the magnetic field is amplified significantly by MHD instabilities~\citep{Obergaulinger2020,Obergaulinger2021}.
All these possibilities suggest that we need more sophisticated simulations.
Thus, we plan to investigate the MHD effects using a radiation-MHD
code recently developed~\citep{Shibata2021a}.

The non-axisymmetric deformation of the massive torus could also lead to the
burst emission of gravitational waves. Our latest study shows that if an
one-armed spiral deformation mode grows in a dynamical timescale comparable
to the typical rotational period of the torus, the degree of the
non-axisymmetric density fluctuation can be 10--20\% of the torus mass~\citep{Shibata2021}.
In such deformation, the maximum amplitude of burst-type gravitational waves
at the hypothetical distance to the source of 100\,Mpc can be
$\sim 10^{-22}$ with the typical frequency of 0.7--0.8\,kHz for
$M_\mathrm{PNS}\approx 3M_\odot$ with the comparable torus mass~\citep{Shibata2021}.
Such gravitational waves are the interesting sources for the third-generation
gravitational-wave detectors such as Einstein Telescope \citep{Punturo2010} and Cosmic Explorer \citep{Abbott2017}.
Thus, in the future, high-energy supernovae with the bipolar outflow may be
explored not only by electromagnetic telescopes but also by the
gravitational-wave detectors.

\acknowledgments

We thank T. Kuroda, K. Maeda, N. Tominaga, and S. Wanajo for useful discussions.
This work was in part supported by Grant-in-Aid for Scientific
Research (Grant Nos.~JP20H00158) of Japanese MEXT/JSPS.  Numerical
computations were performed on Sakura and Cobra at Max Planck
Computing and Data Facility and XC50 at National Astronomical Observatory of Japan.

redpajama_set_name: RedPajamaArXiv


Former Chief Prosecutor. Former State District Court Judge. Now providing his experience for violation of probation charges.
Have you been accused of violating probation? Since probation is granted as an alternative to prison or jail time, breaching the terms can lead to serious consequences. During these risky situations, hiring an experienced attorney can help you avoid further problems.
The founding attorney at Turnbull Legal Group, E.R. (Ned) Turnbull, served as a former Chief Prosecutor and as a State District Court Judge, bringing the experience and insight you need to secure a favorable outcome in your case.
Call us now at 832-314-3232 for a free consultation with an aggressive Houston criminal defense lawyer. We have offices in Houston, Bryan and Conroe and serve clients across the State of Texas and Oklahoma.
Different actions can be considered a violation of probation, so being accused does not automatically mean you are facing prison or jail time. Take action early to avoid suffering potential consequences. Trust an experienced professional to help you make the right move.
(2) Judicial Community supervision (aka "straight probation").
Some Defendants are offered what is known as Deferred Adjudication Community Supervision, or Deferred Probation. If you accept deferred adjudication through a plea bargain, you must plead guilty to your criminal charge; however, although a judge will make an express finding that there was sufficient evidence to find you guilty, the Judge will defer a finding of guilt (conviction) and place you on community supervision for a certain period of time.
Deferred Adjudication has many advantages, particularly that if you successfully complete the deferred adjudication probation, you will ultimately receive a dismissal from the Court. At this point, you may be eligible to petition the court for an Order of Non-Disclosure, which can seal your criminal record and prevent government agencies from releasing your information to third parties.
If in the unfortunate event that the State feels that you violated any of the terms outlined in your deferred adjudication probation, the State will automatically file a document known as a "Motion to Adjudicate Guilt", which allows the court to apply the full range of punishment for the defendant's particular criminal offense and a final conviction on your permanent record.
Other Defendants are placed on what is known as Community Supervision, or Straight Probation. Straight Probation is much like deferred adjudication with respect to the terms and conditions. However, a major difference is that a defendant is found guilty of the crime charged and a definitive sentence is imposed. That sentence, however, is suspended, and the Defendant is then placed on probation for a specified period of time. Straight probation is a way to avoid jail time.
As with deferred adjudication, any violation of the terms and conditions outlined in your probation will jeopardize your future. In these situations, the State will automatically file a document known as a "Motion to Revoke Probation." Should the Court find that you violated the terms and conditions of probation, and find that your probation should be revoked, the Court is limited to that definitive sentence previously imposed, which may include significant jail or prison time. While a judge may decide to give less time for the probation violation, he or she cannot exceed that original sentence. Straight probation is a way to avoid jail time.
When you are placed on probation, you are advised of the conditions of that supervision. Violating any of the terms or conditions of probation, whether intentionally or by accident, could subject you to having your probation revoked. A judge will be asked to sign a warrant for your arrest and you may be kept in the County Jail pending the results of the violation hearing without bond. A judge has the authority to set bond, but the judge is not required to set a bond. Turnbull Legal Group can work with the court to either get a bond posted for a client or have the amount reduced if one is already in place.
1. Continue probation without punishment for the violation.
2. Modify the conditions of probation or extend the period of probation.
3. Revoke probation and sentence the defendant on the underlying offense.
WARNING: If you recently violated the terms and conditions of your probation, chances are a warrant has already been issued for your arrest. For this reason, and the reasons listed above, you must contact Turnbull Legal Group today. We have the resources and skills to assist you and to determine whether a warrant has been issued. Since probation is considered a privilege, courts take violations very seriously. You can rely on Turnbull Legal Group probation violation lawyers to represent your best interests and aggressively defend your rights.
Trust an experienced professional to help you make the right move.
You can rely on our Houston probation violation lawyers to represent your best interests and aggressively defend your rights. Contact us today to put a former Chief Prosecutor and State District Court Judge on your defense team.


text:
Multi-State Tobacco Suits
Lieff Cabraser represented the Attorneys' General of Massachusetts, Illinois, Louisiana, Indiana, Rhode Island, Maine, and New Hampshire, and 18 cities and counties in California, including the City and County of San Francisco, the City of Los Angeles, and the City of San Jose, in litigation against Philip Morris, R.J. Reynolds, and other cigarette manufacturers.
The lawsuits were resolved as part of the landmark $206 billion Master Settlement Agreement ("MSA") announced in November 1998 between the tobacco industry and the states' attorney generals. Under the MSA, our clients recieved $42 billion to be paid over 25 years.
Marketing Restrictions Under the Master Settlement Agreement
The states, cities and counties sought both to recover the public costs of treating smoking-related diseases and to require the tobacco industry to undertake extensive modifications of its marketing and promotion activities in order to reduce teenage smoking. The marketing curbs, part of the MSA, consist of bans on billboards, transit ads, cartoon characters, targeting of minors, youth access to free samples, and paid-for product placement in movies, TV shows, plays and concerts. Tobacco brand-name sponsorships are also limited.
Commenting one year after approval of the settlement, Owen Clements, Chief of Special Litigation for the San Francisco City Attorneys' Office, observed, "Just a few years ago, you'd see a dozen tobacco billboards en route to any airport, not to mention cigarette t-shirts and all sorts of products. Now they're vanishing. They're not a part of the cultural landscape anymore."
Following the signing of the MSA, tobacco usage in California dropped significantly, by 60% from 2000 to 2002. Californians consume less than half the tobacco compared to the national average, and only 16% of Californians smoke.
Government Lawsuits Under the MSA
On June 6, 2002, in a lawsuit filed by California Attorney General Bill Lockyer against R.J. Reynolds Tobacco Company for violating the MSA, California Superior Court Judge Ronald Prager found that R.J. Reynolds had sought to avoid losing market share through an aggressive ad campaign that exposed teens to its advertising to the same degree as adult smokers. The Court ordered R.J. Reynolds to change its marketing practices and fined the company $20 million. Read a copy of this Order (in Adobe Acrobat format).
Project SCUM Marketing Campaign
In 1997 in the California tobacco litigation, Lieff Cabraser served document requests on R.J. Reynolds seeking their current marketing data for Red Kamel. After months of litigation and following an order compelling production, R.J. Reynolds finally produced the documents. Inside the scores of boxes of documents produced and reviewed was the Project SCUM document.
The document showed that R.J. Reynolds targeted San Francisco area gay and homeless communities for special marketing efforts in the mid-1990s. The plan was labeled "Project SCUM" for "Subculture Urban Marketing."
Project SCUM was highly offensive not only because of how it characterized homeless and gay communities, but also because R.J. Reynolds sought to market to the so-called 'rebellious' and 'Generation X' population in San Francisco. Project SCUM highlighted how the tobacco industry in the late 1990s was still targeting young adults for a lifetime of nicotine addiction.
Read a copy of the Project SCUM document (in Adobe Acrobat format).
Lieff Cabraser Sues Alkermes Over Death of Man Who Overdosed After Taking Vivitrol
Vaping Illness Tracker: 2,290 Cases and 47 Deaths
A.M.A. Urges Ban on Vaping Products as Juul Is Sued by More States
How much money will it take to undo the damage from opioids?
Veterans sue 3M, claim faulty ear plugs caused hearing damage
Fox News Tampa Bay
Personal Injury Law Brochure
Answers to Frequently Asked Questions About Personal Injury Cases
Meet Our Legal Team for Injury Cases
PERSONAL INJURY TESTIMONIALS
"Outstanding work. You went to work and got us maximum offer plus additional compensation. I would highly recommend anyone to Lieff Cabraser Heimann & Bernstein law firm. Extremely organized, professional, detail oriented and extremely knowledgeable in personal injury cases."
Maurice in New York
"You were responsive to my questions and concerns at all times. The quality of representation was excellent."
Jill in Indiana
"I couldn't be more pleased with how the case resolved. What stands out is your professionalism, personal attention, and concern. This has been a long road, and I am so grateful."
Cheryl in Utah
Read more client testimonials

redpajama_set_name: RedPajamaCommonCrawl


Team Trump's military junta of Iraq War criminals posing as 'revolutionaries' is apparently considering appointing Rex Tillerman who is currently the CEO Of Exxon Mobil as their U.S. Secretary of State with John Bolton as his Deputy.
The 'Kurdish' canard has always been waved around by NATO and Russia because that is what is used to try and 'gloss' over the illegality of the Iraq War where they have all signed fraudulent contracts with Barzani.
As we have always pointed out unlike unprecedented public opposition to the Iraq War, most governments were not really opposed to the Iraq War because it suits OPEC to keep Iraq in chaos because abiotic oil is not running out anytime soon.
There is a quite extraordinary arrogance towards human life from crony 'capitalism'.
The only possible real purpose of the fraudulent oil contracts with Barzani was always to try and illegally impose military control over Iraq to rip off Iraqis.
The draft dodging septuagenarian Trump can obviously never claim he was ever even opposed to the Iraq War with his line-up of Iraq War criminals.
The dirty backstory is Rex Tillerson connived with the U.S. government and their fixer Ali Khedery hiding behind Dragoman Ventures to circumvent Baghdad too and sign illegal oil contracts with what they call 'Kurdistan', after the UK and US illegally imposed a sectarian 'Constitution' on Iraq.
Ali Khedery who claimed he signed up to go to Baghdad for the U.S after 9/11 which had nothing to do with Iraq was the EXXON MOBIL mouthpiece who falsely claimed that there was no reason the company could not invent and impose whatever contracts they wanted in Iraq.
Exxon Mobil did their dodgy deal with Barzani on October 18th 2011.
Nathaniel Rothschild and Tony Buckingham and the City of London's MI6 mercenary recruiter Macer Gifford have all been peddling the same 'Kurdish' propaganda stealing oil with Qatar too.
Russia's Rosneft has also signed fraudulent contracts with Barzani.
[The UN Security Council disinfo machine also covers up we BEAT the global multi-billion dollar free speech ban etc etc etc that Moscow et al copied.
There has never been anything lawful about what Stake-knife Corbyn & Co have been up to, while working with the Tories and Moscow.
Westminster and Moscow are very obviously trying to undermine Baghdad to rip off all Iraqi people with the fraudulent oil contracts.
When Baghdad brought a legal challenge over the fraud that involved Iraqi oil being stolen through Barzani, Murdoch [& Medyan Daireh] launched the a) 'Islamic State' moniker and b) Mosul was held hostage c) MI6 Haider Al-Abadi was installed in Baghdad.
The big Brexit scam is "the biggest mis-selling fraud since the Iraq War" because it was invented by Blair because it is all about trying to launder the illegal Iraq War.
The UN Security Council really need to be reformed.


Admittedly, we're still getting the kinks worked out on memePDX, the new podcast featuring Cami Kaos and me that covers all the tech news that we can wedge into 20 minutes. This week, we introduce a whole new feature: tricaster green screen magic. So even if Cami and I are boring, Dr. Normal will find something with which to entertain you.
This week on memePDX we talk about PhoneGap, Urban Airship, Portland on Fire, Apple Snow Leopard, the rumored Apple Cougar OS, and the equally rumored Apple Tablet. And then we throw in a little Skype and Marvel + Disney for good measure.
So without further ado, here's the video.
And, as always, your feedback and guidance is both encouraged and greatly appreciated.
Next: Next post: Geomena: Could this be the Wikipedia of geolocation data?


On Wednesday, a motion was passed by the Sheffield City Council committing to divest from fossil fuels. With this, Sheffield becomes the the largest of nine UK councils to pass divestment policy.
"We're over the moon that Sheffield City Council has taken this bold step to divest. Sheffield is now the first city in the world to have commitments from both the council and its universities.
Sheffield is now the first city in the world to have commitments from both the council and its universities.
The motion from the city council follows similar policy being adopted at both the University of Sheffield and Sheffield Hallam University – making Sheffield the first in the UK to rack up commitments across all the city's major public institutions.
In September 2015, South Yorkshire Pension Fund – in which the council is a major employer – released a climate change policy, including divesting from some coal and tar sands companies. The £5.5 billion fund has yet to commit to full divestment.
"We know that to stop catastrophic climate change we have to keep fossil fuels in the ground and transition quickly towards a clean renewable economy. The fossil fuel industry has spent decades spreading lies about the climate to protect their profits at the expense of people and planet, but now the tide is turning against them.
The movement for fossil fuel divestment campaign is a global campaign calling on public institutions to rid themselves of fossil fuel investments for ethical and financial reasons. Globally, over 600 institutions worth $3.4 trillion dollars have made divestment commitments.


Yesh Atid MK Mickey Levy said the two-year budget is bad for the Israeli market and economy, and the motivation for passing it is purely political.
The next state budget will be a two-year budget, for 2017-2018, after the Knesset approved legislation making the change in a final vote Tuesday.
The temporary amendment to Basic Law: State Budget, requires the government to submit a report to the Knesset Finance Committee by the end of 2017 on its economic forecasts for the next year. Any changes to the budget must be brought to the committee for oversight.
If no report is brought to the Finance Committee by the end of the year, the government will have to submit a new budget by the end of January 2018, and if there is no budget by the end of March, the Knesset will be dispersed and an election will be called.
"A two-year budget requires forecasts for 32 months, as opposed to a regular budget, which includes forecasts for 20 months. The longer the period for which the forecasts are made, the greater the chance it will be mistaken," the bill reads, explaining the need for oversight at the end of 2017.
Finance Committee chairman Moshe Gafni (United Torah Judaism) said that while there will be a vote on one budget, the 2017 and 2018 budgets will actually be separate because of the way his panel changed the bill.
The advantage of the two-year budget, Gafni said, is that it creates political stability, which also helps the economy.
Opposition MKs spent the entire afternoon criticizing the two-year budget.
MK Manuel Trajtenberg (Zionist Union), former chairman of the National Economic Council, recounted that Israel adopted the two-year budget in 2009 because it was an election year and the government had been working without a budget for months.
"The necessity turned into a method. At the time, the prime minister didn't like the idea, because he understood, and maybe he still understands economics. Over time, it became a tool that the prime minister thinks has political benefits, even though in Israel no government has fallen because of a budget not passing," he said.
Trajtenberg expressed concern that two-year budgets will become a permanent fixture, and wondered why Finance Minister Moshe Kahlon did not insist on a one-year budget.
Kahlon, like Gafni, opposed a two-year budget, but allowed it to go forward because of coalition agreements.


text:
/ People
/ History
/ Italian History: Biographies
/ Farnese, Alessandro
Farnese, Alessandro
Farnese, Alessandro älĕs-sän´drō färnā´zā [key], 1545–92, duke of Parma and Piacenza (1586–92), general and diplomat in the service of Philip II of Spain. He was the son of Duke Ottavio Farnese and Margaret of Parma and thus a nephew of Philip II and of John of Austria, under whom he distinguished himself at the battle of Lepanto (1571). In 1577, Farnese joined John in the Low Countries to fight the rebels against Spain. Appointed (1578) governor of the Netherlands, he took Tournai, Maastricht, Breda, Bruges, Ghent, and Antwerp from the rebels and secured continued possession of the southern part of the Netherlands for Spain (see Netherlands, Austrian and Spanish). In 1590 he was sent to France at the head of a Spanish army to assist the Catholic League against Henry IV of France. He relieved the siege of Paris (1590) and the siege of Rouen (1592), but was wounded soon afterward and retired to Arras, where he died. Farnese showed exceptional skill in military art and diplomacy.
See R. Solari, The House of Farnese (1968).
See more Encyclopedia articles on: Italian History: Biographies


Michael Cohen's personal attorney has just made a massive blunder that put his clients "case" against in Trump in a laughable new light.
Davis, who is a Clinton crony, admitted that there is no "new evidence" from his client Michael Cohen, who plead "guilty" to so-called campaign finance violations…..It's just his word against President Trumps.
So, a disgraced lawyer who secretly taped his client vs a man who is President of the United States.
However, as Trump supporters, we can't sit back. We must be vigilant because they will continue to come after President Trump. We must get registered and vote in the midterm elections.
It doesn't matter who is on the ballot. President Trump and his policies, and yes, impeachment, are all on the ballot.
Lanny Davis, the attorney for President Donald Trump's former lawyer Michael Cohen, told NBC's Chuck Todd on Meet the Press Daily on Wednesday that he is not aware of any additional evidence to corroborate Cohen's claims that Trump "directed" him to break campaign finance laws.
Todd pressed Davis about whether prosecutors had additional evidence, "more than just Michael Cohen's word," to corroborate Cohen's claims.
Davis merely said that Trump and his lawyers had admitted that money was paid and that evidence of the payment existed.
Todd: [D]o they have evidence on one specific charge, this idea that President Trump, then-candidate Trump, directed Michael Cohen to do this? Other than Michael Cohen's word that the president directed him to do this, do they have other physical evidence that the president directed Michael Cohen? I understand the physical evidence of the money transfers and all of that. But does he have evidence — is it more taped conversations? Is that the evidence?
Davis: Well, the prosecutors may have evidence they haven't revealed. All I've read is the criminal information in which they state that there are individuals from the Trump campaign and from the Trump Organization who were involved, and Mr. [Rudy] Giuliani said, yes, Mr. Trump knew that he had to reimburse Mr. Cohen for the advance made for this payment. Is there any independent evidence that Mr. Trump said to Mr. Cohen, "You need to do this, I don't want to do this?" That may come down to Mr. Cohen's word versus Mr. Trump's. And we'll have to just, now that there's a guilty plea, wait and see if Mr. Trump is willing under oath to say what Mr. Cohen said under oath, which is that he was directed to Mr. Trump to do this.
Davis also told Todd that the FBI had raided Cohen for "everything he ever possessed," which suggests that the government might have any additional evidence on Cohen's part, if it existed.
Among the charges to which Cohen pleaded guilty on Tuesday was a charge of bank fraud, which could be used to impeach Cohen's credibility in any subsequent judicial proceedings.
NEW YORK — Anatoli Samochornov, a Russian translator who was present at the infamous June 2016 meeting at Trump Tower with campaign officials, testified that he was previously an interpreter for Hillary Clinton, John Kerry and Barack Obama.
Samochornov also said that he held a "public trust" clearance from the U.S. government. The clearance provides a level of screening for individuals who do government work described as sensitive, but whose positions do not require a security clearance.
Samochornov was previously identified as being the Russian translator who was present at the meeting at which Russian attorney Natalia Veselnitskaya reportedly argued against the Magnitsky Act, which sanctions Russian officials. The meeting was set up with Donald Trump Jr., presented as being about information regarding Hillary Clinton. Veselnitskaya says she does not speak English and has given interviews to U.S. news media outlets through translators.
Breitbart News reported last year that, according to his LinkedIn profile, from 2005 until at least that year Samochornov was a project manager at the Meridian International Center, which describes itself as a "nonprofit, global leadership organization headquartered in Washington, DC." Meridian is a principal partner of the U.S. State Department.
The Breitbart News report noted at the time that Samochornov's LinkedIn profile further describes his work on behalf of the State Department, purportedly while he was at Meridian. The timeline of his work at Meridian included the period when Clinton was secretary of state.
Samochornov gave his testimony last November and it was recently made public. The 121 pages of transcript were reviewed by Breitbart News and have become newly relevant following renewed news media scrutiny of the Trump Tower confab.
Samochornov has other links to the Obama State Department. He was listed as the program administrator for the State Department's International Visitor Leadership Program, which is implemented by Meridian. Breitbart News found the draft program book for the March 4-12, 2013 leadership initiative, which listed a State Department email for Samochornov.
Samochornov was also listed as the "Program Officer" for the State Department's International Visitor Leadership Program in February 2010. The FBI's New York field office participated in that month's program.
Samochornov is not the only individual at the Trump Tower meeting with a personal tie to Clinton.
Email transcripts and other information disclosed in testimony released by the Senate Judiciary Committee reveal a significant relationship between Russian-born Washington lobbyist Rinat Akhmetshin, who was present at the Trump Tower meeting, and an associate of Clinton. Akhmetshin also claims a personal relationship with Clinton and describes meeting with a Clinton associate the same day as the Trump Tower meeting.
In his Senate testimony, Akhmetshin says that he "knows" Hillary Clinton and has a personal relationship with her that dates back to the late-1990s. Besides describing a direct connection to Clinton, Akhmetshin also testified that he "knew some people who worked on" Clinton's 2016 presidential campaign. Akhmetshin further revealed that the same day as the Trump Tower meeting he met with a Clinton associate after the confab and possibly also just before.
In his Senate testimony, Akhmetshin related a personal connection to Clinton via attorney Ed Lieberman, whose late wife Evelyn previously served as Clinton's chief of staff when she was First Lady. Evelyn Lieberman also served as Bill Clinton's deputy chief of staff, and famously transferred Monica Lewinsky out of the White House to the Defense Department.
In his Senate testimony, Akhmetshin described taking an Acela train to New York the day of the June 9, 2016 Trump Tower meeting and says that Lieberman "may" have been with him on the train.
During further questioning in Senate testimony, Akhmetshin admitted to possibly telling Clinton associate Lieberman about the Trump Tower meeting, but says he may have told him on another day and not the night they met the same day as the meeting.
Besides Akhmetshin's links to Lieberman, the Russian lobbyist is also reportedly tied to Fusion GPS and the controversial firm's co-founder, Glenn Simpson.
The Russia collusion conspiracy theory was sparked by the discredited dossier produced by Fusion GPS, which was paid for its anti-Trump work by Trump's primary political opponents, namely Clinton's 2016 presidential campaign and the Democratic National Committee (DNC) via the Perkins Coie law firm.
Russian lawyer Veselnitskaya also evidenced a relationship with Fusion GPS.
Akhmetshin's November 14, 2017 testimony before the Senate Judiciary Committee contained numerous sections that detail his past relationship with Fusion GPS and Simpson. Some of that relationship, which also involved Veselnitskaya, spanned the period just prior to the meeting with Trump Jr.
The email related to the Russian-linked Prevezon Holdings Ltd., a firm that had settled a case in the U.S. involving the purchase of real estate with allegedly laundered money, accusations that centered around the Magnitsky Act.
Veselnitskaya, who countered the Magnitsky Act along with Akhmetshin, was an attorney for Prevezon. Veselnitskaya was involved in the case since it investigated financier Bill Browder, who successfully lobbied Congress to pass the Magnitsky Act and was a witness in the Prevezon legal matter. Fusion GPS investigated Browder for another client and their findings were used in the Prevezon trial.
In his testimony, one Senate griller asked Akhmetshin about a December 2015 email from a Bloomberg News reporter that states he was told that Akhmetshin was "handling media calls" for Prevezon and its owner.
Another email read in the testimony described plans for a February 4, 2016 dinner meeting between Simpson, Akhmetshin and Veselnitskaya, with Akhmetshin confirming that he did have a meeting with Simpson and Veselnitskaya around that time, possibly dinner. This puts Simpson in person with two participants in the Trump Jr. meeting just four months before the June 2016 Trump Tower meet, although Akhmetshin described the meeting with Simpson as being about the Prevezon case.
Akhmetshin further describes pitching stories directly to Simpson while Simpson was a journalist prior to his co-founding of Fusion GPS. Simpson previously worked for the Wall Street Journal.
Akhmetshin also relates a previous working relationship with Simpson's wife, pitching her stories while she served at the Journal.
In yet another under-reported issue raising questions about the Trump Tower meeting, Akhmetshin admitted to being present at the same security conference in Canada where Sen. John McCain was reportedly first informed about the anti-Trump dossier.
Akhmetshin says he might have spoken to McCain and the senator's assistant David J. Kramer at the Halifax International Security Forum in 2016.
In his Senate testimony, Akhmetshin describes attending the Halifax security conference in 2016, but claimed he played no role in the contact where Wood connected with McCain and Kramer to inform them of the dossier's existence. Akhmetshin also claimed he was not aware of the dossier at the time.
Akhmetshin also stated that he had a previous relationship with McCain. "I knew Senator McCain when he was running years ago because I had friends who were — did advance work for him," Akmetshin said, referring to McCain's 2008 presidential campaign.


text:
Westinghouse defeats Steel Valley to advance to state championship game
Top stars, best performances in Pennsylvania high school football in state semifinals
From Wes Barnes of Southern Columbia to Kyle Williams, Jr. of Harrisburg, there were several big-time high school football performances across the state of Pennsylvania
Ryan Isley
Wes Barnes, Southern Columbia
In a 42-7 win over Trinity, Barnes carried the ball 18 times for 252 yards and scored three touchdowns.
Ronald Burnette, Steelton-Highspire
In a 28-21 win over Canton in the 1A semifinals, Burnette carried the ball 20 times for 112 yards and three touchdowns, including the game-winner from 10 yards out with 34 seconds remaining.
Mikal Davis, Imhotep Charter
In a 21-14 win over Upper Dublin in the 5A semifinals, Davis had eight carries for 70 yards and two touchdowns and threw for 154 yards and a score.
Alex Erby, Steelton-Highspire
Erby completed 25-of-34 passes for 226 yards and a touchdown in a 28-21 win over Canton.
Samaj Jones, St. Joseph's Prep
In a 48-7 win over Garnet Valley in the 6A semifinals, Jones threw for 155 yards and three touchdowns and ran for a 21-yard score.
Who are SBLive Sports' Florida Girls Basketball Top Performers of Jan. 23-28?
Braden Laux, Belle Vernon
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Ryan Palmieri, Pine-Richland
Palmieri completed all but one of his 10 pass attempts for 200 yards and three touchdowns and ran for 83 yards and a score in a 34-12 win over Cocalico in the 5A semifinals.
Stone Saunders, Bishop McDevitt
Saunders completed 19-of-24 passes for 200 yards and three scores in a 35-0 win over Crestwood in the 4A semifinals.
John Tracy, Aliquippa
In a 31-10 win over Allentown Central Catholic, Tracy had 129 yards rushing and a touchdown on 19 carries and grabbed two passes for 73 yards and a score.
Kyle Williams, Jr., Harrisburg
In a 27-7 win over State College in the 6A state semifinals, Williams, Jr. carried the ball 28 times for 263 yards and four touchdowns.
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text:
Usage
=====

======
Python
======

There are multiple ways to use dolphin. The first is with a basic if statement::

    from dolphin import flipper
    if flipper.is_active("flag_name"):
        do_something()
    else:
        do_something_else

There is also a decorator that allows redirects, other view functions to be called,
or just a 404 by default::

    @flipper.switch_is_active("flag_name")
    def view(request):
        return ...

    @flipper.switch_is_active("flag_name", redirect="/")
    def view2(request):
        return ...

    @flipper.switch_is_active("flag_name", alt=view1)
    def view3(request):
        return ...

========
Template
========

In a template::

    {% load dolphin_tags %}
    {% ifactive "flag_name" %}
        Active
    {% else %}
        Not active
    {% endifactive %}

There's also a template tag that will list active flags as a comma delimited list::

    {% active_flags %}

==========
Javascript
==========

For usage in javascript, there are a couple of convenience functions in dolphin.views
that can be added to your urls.py. As an example::

    url(r'^dolphin/js/$', 'dolphin.views.js'),
    url(r'^dolphin/json/$', 'dolphin.views.json'),

The js view provides a flipper object which has a function is_active that may
be used like the python is_active function::

    <script type="text/javascript" src="/dolphin/js/">
    <script type="text/javascript">
        if ( flipper.is_active("flag_name") ) {
            ...
        }
        else {
            ...
        }
    </script>

The flipper object also has the active flags in an array called flipper.active_flags.

The json function returns a structure as follows::

    {"active_flags": ["enabled", "ab_random", "max"]}

All processing is done in python with the javascript views. If any frontend caching would
cache this view, you may want to add never cache if you're utilizing geolocation, random,
max, or date based flags.

redpajama_set_name: RedPajamaGithub


text:
You are here: Home / International Arbitration / Interim Measures in International Arbitration: A Need for Irreparable Harm?
Interim Measures in International Arbitration: A Need for Irreparable Harm?
It is a well-established rule of international arbitration that arbitral tribunals have the power to grant interim or conservatory measures. This is explicitly provided in all major arbitration rules (see, e.g., Article 28 of the 2017 ICC Rules, Article 25.1 of the 2014 LCIA Rules, Article 26 of the 2010 UNCITRAL Rules, Rule 30 of 2016 SIAC Rules, Article 37 of 2017 SCC Rules, Article 47 of the ICSID Convention). The power to grant interim relief is also vested with so-called "emergency arbitrators", a common feature of major arbitration rules, allowing parties to request interim relief even before the arbitral tribunal has been constituted (see, e.g., Article 29 of the 2017 ICC Rules, Article 9B of 2014 LCIA Rules, Rule 30 and Schedule 1 of the 2016 SIAC Rules, Appendix II of the 2017 SCC Rules).
However, arbitral procedural rules do not generally set out the criteria for interim measures to be granted, often leaving the arbitrators with wide discretion to order "any interim measure they deem necessary or appropriate" in light of the circumstances of a particular case. Lack of uniform standards poses significant challenges in practice: for the parties, it leads to uncertainty as to whether their application will be accepted; for arbitrators, it leaves them without firm guidance on the criteria they should apply.
In practice, how arbitrators will exercise this discretion depends on a number of factors: the circumstances of each case, the applicable lex arbitri, the applicable procedural rules, and the arbitrators' interpretation of the criteria to be applied.
Absent strict criteria, many arbitrators look to Articles 17-17A of the UNCITRAL Model Law 2006 and Article 26(3) and (4) of the UNCITRAL Arbitration Rules for guidance. The UNCITRAL Arbitration Rules and UNCITRAL Model Law both provide the same definition of "interim measure":
"(2) An interim measure is any temporary measure, whether in the form of an award or in another form, by which, at any time prior to the issuance of the award by which the dispute is finally decided, the arbitral tribunal orders a party to:
(a) Maintain or restore the status quo pending determination of the dispute;
(b) Take action that would prevent, or refrain from taking action that is likely to cause, current or imminent harm or prejudice to the arbitral process itself;
(c) Provide a means of preserving assets out of which a subsequent award may be satisfied; or
(d) Preserve evidence that may be relevant and material to the resolution of the dispute."
Article 17A of the UNCITRAL Model Law further lists the following conditions for interim measures to be granted:
"Article 17 A. Conditions for granting interim measures
(1) The party requesting an interim measure under article 17(2)(a), (b) and(c) shall satisfy the arbitral tribunal that:
(a) Harm not adequately reparable by an award of damages is likely to result if the measure is not ordered, and such harm substantially outweighs the harm that is likely to result to the party against whom the measure is directed if the measure is granted; and
(b) There is a reasonable possibility that the requesting party will succeed on the merits of the claim. The determination on this possibility shall not affect the discretion of the arbitral tribunal in making any subsequent determination.
(2) With regard to a request for an interim measure under article 17(2)(d), the requirements in paragraphs (1)(a) and (b) of this article shall apply only to the extent the arbitral tribunal considers appropriate."
However, the criteria for granting interim measures listed in the UNCITRAL Model Law and the UNCITRAL Arbitration Rules are not black letter law for non-UNCITRAL arbitrations. While they frequently are used by tribunals as guidance, they should not be blindly followed by arbitrators and practitioners. As set forth by Gary Born, "Article 17A's formula is lacking in a number of respects. Among other things, Article 17A apparently makes no provision for parties' agreements on the standards of proof, omits any reference to urgency, unduly focuses 'irreparable' harm on monetary damages (as distinguished from non-monetary relief), imposes a single standard for different types of interim relief and omits reference to security for costs."[1]
Regarding the "urgency" criteria, while not explicitly mentioned in the UNCITRAL Model Law and UNCITRAL Arbitration Rules, "urgency" is considered by nearly all commentators to be inherent in a request for interim measures.[2] This means that the party requesting interim measures should show that the tribunal's intervention is so urgent that the decision on interim measures cannot await the issuance of a final award. In practice, the "urgency" criteria is usually analysed together with the "degree of harm", whereas applicants should establish, prima facie, that an imminent harm might be caused to the applicant, if the requested interim measure is not granted before such measure can be obtained from the arbitral tribunal.
The degree of seriousness of harm is the most controversial criteria. Arbitrators have applied a range of potential harms, sometimes referring to "irreparable", "serious" or "substantial" injury necessary for the provisional measures to be granted.[3] The emerging view appears to be that the controversial notion of "irreparable harm" or a "harm not adequately reparable by an award of damages", should be understood in an economic and not literal sense and must take account of the fact that it may not always be possible to compensate for actual losses suffered or sullied business reputation through damages.[4] Many recent authorities also suggest that it is unnecessary for the harm to be "irreparable", in its literal sense, but only "serious" or "substantial".[5] In practice, as stated by Gary Born, even though most decisions state that the harm must be "irreparable", they do not necessarily appear to apply this formula, but instead require that there is a material risk of serious damage to the plaintiff.[6] The reason for this is simple and practical – in commercial cases it is sometimes difficult, if not impossible, to demonstrate truly "irreparable" harm that cannot be compensated by money damages in a final award. Accordingly, if "irreparable harm" was understood in its literal sense, this requirement would limit provisional measures principally to cases where one party was effectively insolvent or where enforcement of a final award would be impossible.
Controversies involving the "irreparable harm" criteria are nothing new. Even the drafters of the UNCITRAL Model Law expressed similar concerns during the Working Group on UNCITRAL Model law, where the majority considered the term "irreparable harm" to be too narrow in the commercial context. Instead, it was widely felt that the provision should be based on a "balance of convenience" test under which the assessment of the degree of harm suffered by the applicant if the interim measure was not granted should be balanced against an evaluation of the harm suffered by the party opposing the measure if that measure was granted.[8] In addition, it was felt that the quantitative approach reflected in the words "a significant degree of harm" might create uncertainties as to how a degree of harm should be considered to be sufficiently "significant" to justify certain provisional measures.
This approach to "irreparable harm" is also reflected in the practice of the arbitral tribunals. For example, ICC arbitral tribunals have recently construed the risk of financial loss to be included within the definition of "harm not adequately reparable by an award of damages".[9] Certain investment tribunals have also taken the same approach. For example, in Burlington Resources Inc. v. Republic of Ecuador,the tribunal held that it was not essential for provisional measures to prevent irreparable harm, but that "the harm spared the petitioner by such measures must be significant and that it greatly exceeds the damage caused to the party affected thereby".[10] Furthermore, in PNG Sustainable Development Program Ltd. v. Independent State of Papua New Guinea, the degree of harm required was cited as "substantial" or "serious", as explained by the tribunal:[11]
"The degree of 'gravity' or 'seriousness' of the harm that is necessary for an order of provisional relief cannot be specified with precision, and depends in part on the circumstances of the case, the nature of the relief requested and the relative harm to be suffered by each party, suffice it to say that substantial, serious harm, even if not irreparable, is generally sufficient to satisfy this element of the standard for granting provisional measures."
There is no "one-size-fits all" solution, but the "degree of harm" has to be a flexible notion, wide enough so that it can adequately be analysed in light of the circumstances of each particular case. This has been pointed out by a number of commentators,[12] who also note that the criteria for granting interim measures are not necessarily the same for different types of interim measures – for example some of them require strong showings of serious injury, urgency and a prima facie case (e.g., maintaining or restoring the status quo, or ordering performance of a contract or other legal obligation), while other interim measures are unlikely to demand the same showings (e.g., preservation of evidence, or enforcement of confidentiality obligations).[13]
While it is not debatable that arbitral tribunals and emergency arbitrators have wide discretion to grant interim measures, the criteria for granting interim relief remain controversial. There is no "one-size-fits-all" criteria for the degree of harm, which needs to be analysed in light of the circumstances of each case and depending on the type of interim relief in question. The UNCITRAL Model Law and UNCITRAL Arbitration Rules provide guidance for international practitioners, but should not be expected to be followed blindly by arbitrators overseeing non-UNCITRAL proceedings.
[1] Gary Born, International Commercial Arbitration (Second Edition, 2014), p. 2466.
[2] Jan Paulsson and Georgios Petrochilos, UNCITRAL Arbitration (Kluwer Law International, 2017) UNCITRAL Arbitration Rules, Section III, Article 26, Interim measures, p. 219.
[3] Gary Born, International Commercial Arbitration, Chapter 17: Provisional Relief in International Arbitration (Kluwer International Law 2014), p. 2469.
[4] Julian D. M. Lew , Loukas A. Mistelis , et al., Comparative International Commercial Arbitration (Kluwer Law International; Kluwer Law International 2003), p. 604.
[7] Nathalie Voser, Interim Relief in International Arbitration: The Tendency Towards a More Business-Oriented Approach, Dispute Resolution International, Vol. 1, No. 2, December 2007, at 181-183.
[8] Howard M. Holtzmann, Joseph E. Neuhais et al., A Guide to the 2006 Amendments to the UNCITRAL Model law on International Commercial Arbitration: Legislative History and Commentary (Kluwer Law Internatonal 2015), pp. 238,273, 283, 312.
[9] Eric Schwartz, The Practice and Experiences of the ICC Court, Conservatory and Provisional Measures in International Arbitration, ICC Publishing, 1993, p. 45.
[10] Burlington Resources Inc. v. Republic of Ecuador, ICSID Case No. ARB/08/5, Procedural Order No. 1, 29 Jun. 2009, para. 81.
[11] PNG Sustainable Development Program Ltd. v. Independent State of Papua New Guinea, ICSID Case No. ARB/13/33, Decision on the Claimant's Request for Provisional Measures , 21 January 2015, para. 109.
[12] M. Savola, Interim Measures and Emergency Arbitrator Proceedings, Croat. Arbit. Yearb. Vol. 23 (2016).
[13] Gary Born, International Commercial Arbitration, Chapter 17: Provisional Relief in International Arbitration (Kluwer International Law 2014), p. 2468.
Filed Under: Arbitration Rules, International Arbitration, LCIA Arbitration, UNCITRAL Arbitration


Vileplumegamer had the most liked content!
Anyone know how much a tamagotchi connection weighs?
sorry for the late reply! thank you!
i'm going to be shipping a purchase out and it's my first time shipping tamagotchis, i just need to know, how much do they weigh?
Vileplumegamer replied to Vileplumegamer's topic in What's On Your Mind?
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Please, i really need to know, christmas is coming and i wanna make sure i buy the right one with my money.
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In order to get the bonus though, you will need to sign up with someone's referral code so if you'd like to use my code, please click here to sign up.Uber does allow for retroactive referrals within 15 days of activation so if you didn't sign up with a referral code, e-mail me for more info.If you are having any issues with your account, a problem with a fare, or have questions that can't be found on Uber's support website (see below) then the best way to get support is by using Uber's In-App Support.
Some of the smaller Uber cities may not have their own support e-mail and in that case you should e-mail the closest Uber city.
My good buddies at Lyft on the other hand, sometimes take up to a week to get back to me.
And sometimes, drivers' e-mails get lost in a black hole somewhere up in San Francisco never to be seen again.
For most cities, Uber offers a bonus amount anywhere up to $1,000!
Uber doesn't have a published list of sign-up bonuses by city but you can always send an e-mail [email protected] verify the amount.
Some of the smaller Uber cities may not have their own support e-mail and in that case you should e-mail the closest Uber city.My good buddies at Lyft on the other hand, sometimes take up to a week to get back to me.And sometimes, drivers' e-mails get lost in a black hole somewhere up in San Francisco never to be seen again.For most cities, Uber offers a bonus amount anywhere up to $1,000!Uber doesn't have a published list of sign-up bonuses by city but you can always send an e-mail [email protected] verify the amount.
,000!Uber doesn't have a published list of sign-up bonuses by city but you can always send an e-mail [email protected] verify the amount.


Timber Tops Luxury Cabin Rentals gives guests an inside look at the newest Pigeon Forge moonshine distillery, Old Forge Distillery.
The newest Pigeon Forge moonshine distillery, the Old Forge Distillery, incorporates local ingredients and flavor into each of its products.
With Old Forge Distillery, we are most excited to see so much of the area's history come to life within their products.
On July 24, 2014, Timber Tops Luxury Cabin Rentals announced the opening of a brand new Pigeon Forge moonshine distillery.
The Old Forge Distillery is the first moonshine distillery to be opened in Pigeon Forge, and the owners plan to incorporate as much of the area's history as possible into the the items it sells.
The name Old Forge Distillery comes from the iron forge that was built in the early 1800's by Isaac Love, the son-in-law of Pigeon Forge founder, Mordecai Lewis. The iron forge stood where the new Pigeon Forge moonshine distillery does today.
In addition, the new Pigeon Forge moonshine distillery aims to incorporate as many locally-made and grown products as possible, including the corn used inside their debut flavor, 1830 Original. Not only was the corn harvested in Tennessee, but it was ground at the distillery's neighbor The Old Mill.
The custom moonshine jugs found at the Old Forge Distillery were also made by one of the company's neighbors, Pigeon Forge Pottery.
Old Forge Distillery is located at 170 Old Mill Avenue, Pigeon Forge, Tenn. 37863. The distillery is open for tours daily from 10 a.m.-9 p.m.
To learn more about new Pigeon Forge moonshine distilleries and Pigeon Forge attractions opening soon, be sure to follow Timber Tops Luxury Cabin Rentals' blog at http://www.yourcabin.com/blog.
Established in 1996, Timber Tops Luxury Cabin Rentals is an industry leader in professional property management in the Gatlinburg, Sevierville and Pigeon Forge area. Locally owned, the staff at Timber Tops strives to provide each guest with attentive, courteous, proactive and prompt service to ensure everyone who visits one of our luxurious cabins gets the most out of their vacation. Timber Tops Luxury Cabin Rentals' office is located at 1440 Upper Middle Creek Road, Sevierville, TN 37876. For additional information on our services, or to reserve your cabin today, contact us by calling 1 (800) 266-1066, by email at reservations(at)timbertops(dot)net, or visit our website at http://www.yourcabin.com. Our office is open 24 hours a day!
Old Forge Distillery, the new Pigeon Forge moonshine Distillery, is located next door to the most historic attraction in Pigeon Forge, The Old Mill.


text:
Iran is worried that Barbie, Shrek and Spiderman will corrupt young minds, but self flagellation, learning to hate Jews, Christians and Democracy are OK Sexual Cleansing in Irag as radicals go searching for gays to kill. This is a very frightening situation, and human rights groups must respond NOW
And yet ANOTHER financial debaucle defrauding "ethical investment takes place in Abu Dhabi!
On September 25, 2008 · In Abu Dhabi, Islam, Islamic Banking, Uncategorized
Police unearth Dh320m fraudulent savings fund scheme in Abu Dhabi
Published: September 24, 2008, 21:10
Abu Dhabi: A bogus multi-million dirham investment portfolio involving 1,300 investors, who were defrauded of their life savings, was uncovered in Abu Dhabi, police said on Wednesday.
An Emirati, S.A., sponsored a Sudanese, A.H., who reportedly duped 1,300 investors of Dh320 million, according to Colonel Maktoum Al Sharifi, director of the CID department.
"The accused claimed they were managing an Islamic portfolio that is based on the principle of Murabaha, where they share profits or losses with investors, who signed contracts preventing them from claiming their money in the case of losses," Al Sharifi said.
The accused promised their victims of 40 per cent monthly profits of their deposits, he added, adding Murabaha does not justify except partial losses of deposits but not all the deposits as claimed by the suspects.
continue reading at………………….. http://www.gulfnews.com/business/Banking_and_Finance/10247547.html