text:
\section{Introduction}
\label{sec:introduction}

In the limit of low-frequency magnetohydrodynamic (MHD) fluctuations,
charged relativistic particles
are accelerated by mirror forces resulting from magnetic
compressions \citep{Achterberg1981},
\begin{equation}
  \label{eq:mirrorForce}
  \frac{d p_\parallel}{dt} = \frac{p_\perp v_\perp}{2B}
  \nabla_\parallel \mid\boldsymbol{B} \mid,
\end{equation}
where  $\parallel$ and $\perp$ denote directions relative to the local magnetic field.
In MHD, magnetic compressions are caused by slow modes and fast
modes, with slow modes containing most of the compressive energy in
subsonic turbulence. Because slow modes
propagate approximately along the magnetic field in most regimes, a
pure linear resonance with relativistic particles requires
$\omega \simeq k_\parallel v_p = k_\parallel v_\parallel$, or
equivalently $v_p \simeq
c$, where $v_p$ is the parallel phase velocity of slow modes. Thus
linear theory predicts no acceleration of
high-energy particles by MHD-scale slow modes, because the resonance condition
cannot be satisfied.   As a result, fast modes have traditionally been
believed to be the dominant source of relativistic particle
acceleration by MHD-scale turbulent fluctuations
\citep{Achterberg1981,Miller1996}.   However,  subsonic
turbulence does not contain significant fast mode energy (see, e.g., \citealt{Yao2011a, Howes2012} for empirical constraints on the fast and slow mode energy in the solar wind).   This appears
to significantly limit the efficiency of relativistic particle
acceleration by MHD turbulence in many astrophysical environments.

In strong MHD turbulence, the waves comprising MHD turbulence are not
long-lived but instead have a decay time comparable
to their linear period.  In this case,
the linear resonance is not the appropriate condition for
wave-particle interaction. Instead, the
resonance is nonlinearly broadened
\citep{Bieber1994a,Gruzinov1999b,Shalchi2004,Shalchi2004a,Qin2006,Yan2008a,Lynn2012}.
Resonance broadening allows waves to interact with
relativistic particles when $\omega_{\rm nl} \gtrsim k_\parallel
c$, where $\omega_{\rm nl}^{-1}$ is the non-linear correlation time of
the turbulence.   In this paper, we estimate the resulting
particle acceleration analytically (\S
\ref{sec:transportProperties}) and numerically using simulations of
relativistic test particles interacting with MHD turbulence (\S
\ref{sec:numericalMethods} \& \ref{sec:numericalResults}).   Our
results are potentially relevant to a wide range of astrophysical
plasmas; in \S \ref{sec:conclusions} we briefly assess the
implications of our results for non-thermal emission from accretion
disks around black holes.

\section{Relativistic momentum diffusion by low-frequency MHD
  turbulence}
\label{sec:transportProperties}

We first provide an order of magnitude estimate of the momentum
diffusion coefficient for relativistic particles interacting with magnetic field compressions associated with slow modes (the case of fast modes is considered separately). The diffusion coefficient for a particle with reduced momentum
$\overline{p} \equiv p/mc$ may be estimated as
$D_{\overline{p}, \boldsymbol{k}} \sim f^2
\delta t / c^2$ where $f \sim \overline{p}
c^2 k_\parallel \delta B_\parallel(\boldsymbol{k}) / B_0$ is the force felt by a particle
interacting with a given spatial scale labeled by $\boldsymbol{k}$,
$\delta
t \sim  \omega_{\rm nl}^{-1}$ refers to the timescale over which
wave-particle interactions are correlated, and $\delta B_\parallel(\boldsymbol{k})$ is the rms fluctuation in magnetic compressions on scale $\boldsymbol{k}$.   For a given $k_\perp$,
the total acceleration will be determined by the
average of $k_\parallel^2 \delta B_\parallel(\boldsymbol{k})^2$ over $k_\parallel$,
limited to those
$k_\parallel$ that satisfy the broadened resonance condition
$k_\parallel \lesssim \omega_{\rm nl} /c $. Provided that $\delta
B_\parallel(\boldsymbol{k})^2$ does not scale too steeply with $k_\parallel$,
parallel wavenumbers near $k_\parallel \sim \omega_{\rm nl} /c$ will dominate, resulting in a
diffusion coefficient at fixed $k_\perp$ of order
\begin{equation}
  \label{eq:approxDiffusion}
  D_{\overline{p}, k_\perp} \sim {\overline{p}^2}  \, \frac{v_A}{c} \, \frac{\omega_{\rm nl} \, \delta B_\parallel(\boldsymbol{k_\perp})^2.}{B_0^2}
\end{equation}
where we have used the fact that  most of the turbulent energy in anisotropic MHD turbulence has $k_\parallel \lesssim \omega_{\rm nl}/v_A$ and that only a fraction $v_A/c$ of the energy in magnetic compressions satisfies the conditions required for efficient particle acceleration, namely $k_\parallel \lesssim \omega_{\rm nl} /c$ {\bf (this follows formally from the magnetic field power spectrum in eq. \ref{eq:gsTurbulence} below, which implies a parallel energy spectrum of $dE/d \ln k_\parallel \propto k_\parallel$).}   Equation \ref{eq:approxDiffusion} shows that the scaling of
$\omega_{\rm nl} \delta B_\parallel(\boldsymbol{k_\perp})^2$ with $k_\perp$
determines which $k_\perp$ dominates. For the strong MHD power
spectrum of \citet{Goldreich1995}, $\omega_{\rm nl} \propto
k_\perp^{2/3}$ and $\delta B(\boldsymbol{k_\perp}) \propto
k_\perp^{-1/3}$, so that all scales contribute equally, provided that
they can satisfy $k_\parallel \lesssim \omega_{\rm nl} / c$ (which
favors long-wavelength fluctuations).

More formally,  the
resonance-broadened diffusion coefficient for the reduced momentum is
given by \citep{Dupree1966,Weinstock1969}
\begin{equation}
  \label{eq:broadenedDiffusion}
  D_{\overline{p}_\parallel} = \frac{\overline{p}_\perp^2 v_\perp^2}{4 B_0^2} \int
  d^3k k_\parallel^2 I_B(\boldsymbol{k}) R(\boldsymbol{k}),
\end{equation}
where $\overline{p}_\perp$ is the perpendicular component of the
dimensionless momentum, $I_B(\boldsymbol{k})$ is
the 3D power spectrum of magnetic field
fluctuations, and $R(\boldsymbol{k})$ is a resonance function that
describes the time-averaged interaction of a test particle with waves
at a given $\boldsymbol{k}$.  Quantitatively, $R(\boldsymbol{k}) = \Re \int_0^\infty dt
\exp{[\imath (\omega(\boldsymbol{k}) - v_\parallel k_\parallel) t]} \,
f(t)$, where $f(t)$ is the time correlation function for wave-particle
interactions. $R(\boldsymbol{k})$ is necessarily
phenomenological, as it in principle depends on the momentum diffusion
coefficient itself.   Standard models in the literature assume that
waves decay as an exponential or Gaussian in time due to non-linear
interactions; e.g,  $f(t) = e^{-\omega_{\rm nl}^2 t^2}$ (a Gaussian
decay model), with a nonlinear decay frequency $\omega_{\rm nl}$.   We
focus on a Gaussian decay model favored by our previous test particle
simulations \citep{Lynn2012}.
These assumptions lead to \begin{equation}
  \label{eq:gaussianResonance}
  R(\boldsymbol{k}) = \frac{\sqrt{\pi}}{2 \omega_{\rm nl}}
  \exp{\left[-\frac{k_\parallel^2 (v_\parallel-v_p)^2}{4 \omega_{\rm nl}^2}\right]}.
\end{equation}
where we have assumed for simplicity that the waves have a dispersion
relation $\omega = k_\parallel v_p$, a reasonable approximation for
anisotropic slow modes with $k_\perp \gg k_\parallel$.   Physically, equation \ref{eq:gaussianResonance} implies that for the particles to couple to the turbulent fluctuations, the frequency that the particles feel as they pass through a wave, $k_\parallel (v_\parallel - v_p)$, must be of order (or less than) the
nonlinear frequency.

To perform the calculation in Equation \ref{eq:broadenedDiffusion}, we
assume that the magnetic power spectrum of slow modes is given by
strong anisotropic turbulence,
\begin{equation}
  \label{eq:gsTurbulence}
  I(\boldsymbol{k}) \equiv \frac{\delta B_S^2 L^3}{12 \pi} (k_\perp L)^{-10/3}
  g\left(\frac{k_\parallel L^{1/3}}{k_\perp^{2/3}}\right),
\end{equation}
where $L$ is the outer scale of the cascade, $\delta B_S^2$ is the
total energy in slow mode magnetic fluctuations,  and $g(x) \simeq 1$ for $x \lesssim 1$ and falls off sharply to zero for $x \gtrsim 1$.    The cutoff $g(x)$ in equation \ref{eq:gsTurbulence}
represents the lack of power outside the
anisotropic Goldreich-Sridhar cone \citep{Goldreich1995} in weakly
compressible MHD turbulence,\footnote{{\bf \citet{Cho2002a} show using numerical simulations that $g(x) \propto \exp[-x]$.  Our results are insensitive to the precise functional form of g(x).}}  and the power spectrum normalization is
chosen so that
$\int d^3k I(\boldsymbol{k}) \equiv \delta B_S^2 / 2$.
The nonlinear frequency in such turbulence is given by $\omega_{\rm nl} \simeq (v_A/L) (k_\perp
L)^{2/3}$, which is of order the eddy turnover time on a given scale.

Finally, to simplify the resulting estimate, we  assume that the particles are
relativistic ($\overline{p}_\perp \sim
\overline{p}_\parallel \gg 1$), and that wave speeds are
nonrelativistic.  To emphasize the net particle acceleration efficiency, we also present our results in terms of the total momentum diffusion coefficient, rather than the parallel momentum diffusion coefficient.   This implicitly assumes that modest pitch angle scattering isotropizes the distribution function (see \S \ref{sec:numericalResults}).  Under these approximations, the diffusion coefficient becomes
\begin{align}
  \label{eq:slowModeIntermediateIntegral}
 &  D_{\overline{p}} = \frac{\sqrt{\pi} \overline{p}_\perp^2 v_\perp^2}{48 v_A}
   \frac{\delta B_S^2}{B_0^2}  \left(\frac{v_\parallel}{v}\right)^2  \times \\ & \int
  dk_\parallel dk_\perp \frac{k_\parallel^2}{k_\perp^3} g\left(\frac{k_\parallel
  L^{1/3}}{k_\perp^{2/3}}\right)  \nonumber \exp{\left(-\frac{k_\parallel^2 L^2 v_\parallel^2}{4 (k_\perp L)^{4/3} v_A^2}\right)}.
\end{align}
Both the exponential and
the $g(x)$ term in equation
\ref{eq:slowModeIntermediateIntegral}
have the effect of cutting off the interaction at
high $k_\parallel$ for a given $k_\perp$.   When $v_A \ll v_\parallel$, the
exponential cutoff will always be more constraining and requires
$k_\parallel \lesssim L^{-1} v_A/c (k_\perp L)^{2/3}$. Given this, we
find
\begin{equation}
  \label{eq:slowModeDiffusion}
  {D_{\overline{p}}}= {\overline p^2} \frac{\pi}{24}
  \frac{v_A^2}{c L} \frac{\delta B_S^2}{B_0^2}
  \frac{\left( 1 - \alpha^2 \right)^2}{\alpha^3}
  \ln{(k_{\rm max} L)},
\end{equation}
where we have rewritten the angular dependence in terms of $\alpha =
v_\parallel / v$, the particle pitch-angle
cosine.   The result in equation \ref{eq:slowModeDiffusion} is similar to that derived earlier by \citet{Chandran2000}.   The restriction to parallel velocities much larger than $v_A$
corresponds to $\alpha \gg v_A / v \simeq v_A / c$.
Equation \ref{eq:slowModeDiffusion} corresponds to a particle acceleration time $t_{\rm
  a} \sim (\delta B_S/B_0)^{-2} (L/v_A) (c/v_A)$ .  Note  that this is independent of particle energy and is roughly the eddy turnover time divided by the fraction of the magnetic energy at low $k_\parallel$ that satisfies $k_\parallel \lesssim \omega_{\rm nl}/c$.

Equation \ref{eq:slowModeDiffusion} can be compared to the analogous result for acceleration of relativistic particles by fast modes.   The latter is predominantly via a linear resonance with highly oblique waves. Versions of this
calculation have been performed in many other contexts
\citep{Miller1996, Yan2002}, so we restrict ourselves to briefly summarizing the salient features here.

Relativistic test particles travelling along magnetic field lines can
experience a linear resonance with a highly
oblique fast mode. The linear resonance function is a delta-function,
\begin{equation}
  \label{eq:linearFastModeResonance}
  R(\boldsymbol{k}) = \pi \delta{(k v_p \pm k_\parallel v_\parallel)},
\end{equation}
where $v_p$ is the isotropic phase velocity of fast modes
(approximately $v_A$ for $\beta \ll 1$ and $c_s$ for $\beta \gg 1$).
The power spectrum of fast modes in Alfv\'enic turbulence is
believed to be isotropic. The spectral index is uncertain but
the simulations of \citet{Kowal2010a} suggest a 1D power spectrum
$P(k) \sim k^{-2}$ (though possibly shallower; see \citealt{Cho2003, Chandran2005}).

Performing the integral in Equation \ref{eq:broadenedDiffusion} with
the fast mode linear resonance and isotropic power spectrum $\sim
\delta B_F^2 L^3 (k L)^{-\alpha}$ leads to \begin{equation}
  \label{eq:fastModeDiffusion}
  D_{\overline{p}} \sim \overline{p}^2 \frac{v_p^2}{c L} \frac{\delta B_F^2}{B_0^2}
  \int_{k_{\rm min}}^{k_{\rm max}} dk k^{1-\alpha},
\end{equation}
where $\delta B_F^2$ is the energy in magnetic compressions associated with fast modes.   For
$\alpha \sim 2$, the diffusion coefficient due to fast modes
(eq. \ref{eq:fastModeDiffusion}) is of the same form as that due to
slow modes (eq. \ref{eq:slowModeDiffusion}).  For $\beta \gg 1$, a comparison of these two expressions shows that ratio of the fast mode to slow mode diffusion coefficient is $\sim (c_s/v_A)^2 (\delta B_F/\delta B_S)^2$.  At high $\beta$, fast modes lose their magnetic compressibility (becoming simply sound waves), so that the magnetic energy $\delta B_F^2$ in fast modes decreases at fixed velocity amplitude, with $\delta B_F^2 \sim \rho \, \delta v_F^2/\beta$.   By contrast, $\delta B_S^2 \sim \rho \, \delta v_S^2$.   Thus the ratio of the fast to slow mode diffusion coefficients is in fact set by the relative turbulent energy in each mode.   For subsonic turbulence, slow modes will in general dominate the particle acceleration because there is significantly more energy in slow modes.   This depends, however, on the power spectrum of the fast modes.  If $\alpha \sim 3/2$ rather than $\alpha \sim 2$ (as in \citealt{Chandran2005}) then the fast mode acceleration efficiency can be greater than that of slow modes even given the overall lower energy density in fast modes.

\section{Numerical methods}
\label{sec:numericalMethods}

Our simulations consist of charged test particles evolving in
the macroscopic electric and magnetic fields of isothermal, subsonic
MHD turbulence. Apart from modifying the particle pusher for
relativistic test
particles, which we describe below, our computational approach is
identical to that of \cite{Lynn2012}. Dimensional quantities
throughout the paper are expressed in units of the sound speed $c_s$
and the box scale
$L$, when not explicitly stated.

\subsection{Turbulence simulations}
\label{sec:turbSims}

We simulate ideal MHD turbulence with the Athena code
\citep{Stone2008}. We drive an incompressible turbulent velocity field
using an Ornstein-Uhlenbeck process, and allow
compressible fluctuations to develop naturally. The OU process
has a characteristic autocorrelation time $t_{\rm OU}$. Fiducial
properties for the MHD simulations used in this work
are summarized in Table \ref{table:fiducial}.   We show results from higher resolution calculations in Figure \ref{fig:Dp_vs_c} (discussed below) and find that the numerically determined diffusion coefficients are relatively independent of resolution. In our calculations,
the simulation box is extended along the
mean magnetic field, because otherwise the particles (which undergo
periodic boundary conditions) would interact with the same eddies
multiple times before the eddies decorrelate.

\begin{table}
  \begin{center}
    \caption{Summary of fiducial simulation properties}
    \begin{tabular}{ c c }
      \\
      \hline \hline
      Parameter & Value \\
      \hline \hline
      Resolution & $512\times128^2$ \\
      Volume ($L^3$) & $8 \times 2^2$ \\
      $\dot{\epsilon}$ ($c_s^3 / L$)\footnote{The turbulent energy input
        rate, corresponding to a sonic Mach number of $\simeq 0.35$.  Calculations with $\dot{\epsilon} = 0.01$ yield similar results.} & 0.1 \\
      $\beta$\footnote{Ratio of thermal to magnetic pressure.  Our calculations covered a range of $\beta \sim 0.1-10$.} & $1$ \\
      $t_{\rm OU} \, (L/c_s)\footnote{$t_{\rm OU}$
        refers to the correlation time in the Ornstein-Uhlenbeck turbulence forcing.}$  & $1.5$ \\
    $l_D$ ($L$)\footnote{Outer (driving) scale of the turbulence.} & $0.39$\\
     $\delta B_{\parallel}$ ($B_0$)\footnote{RMS fluctuation in the parallel magnetic field.} & $0.12$\\
     $N_{\mathrm{particles}}$ & $2^{11} \times 10^3 \simeq 2 \times 10^6$ \\
      $\Omega_0$ ($c_s/L$)\footnote{Test particle gyrofrequency.} & $2
      \times 10^5$ \\
               \end{tabular}
    \label{table:fiducial}
  \end{center}
\end{table}

\subsubsection{Measurement of turbulence properties}
\label{sec:turbulenceProperties}

An important property of our turbulence simulations for comparing test
particle results to analytical estimates is the rms deviation in
parallel magnetic field, $\delta B_{\parallel}$, since this sets the
magnitude of the magnetic mirror forces. We define this quantity as
the spatial rms average of $\mid \boldsymbol{B}\mid -
\mid\boldsymbol{B_0}\mid$, where
$\boldsymbol{B_0}$ is the initial mean magnetic field. This is equivalent
to taking the local direction of the magnetic field as the
``parallel'' direction. The magnitude of $\delta B_\parallel$ depends
on the
magnetic compressibility of the fast and slow modes at a given
$\beta$, in addition to their overall representation in the
turbulence. For our fiducial
simulation summarized in Table \ref{table:fiducial}, $\delta B_\parallel /B_0 \simeq 0.12$, while
simulations that have the same driving rate (and thus similar $v_{\rm
  rms}$) but $\beta=0.3$
($\beta=3$) have $\delta B_\parallel /B_0 \simeq 0.05$ ($0.23$).  Note
that for higher $\beta$, the  energy in magnetic compressions is
larger.

We also decompose the turbulent velocity field into the linear MHD
Alfv\'{e}n, slow, and fast modes, following the approximate Fourier
space method of \citet{Cho2003}.
For our fiducial simulation, 50\%, 45\%, and 5\% of the turbulent
energy is in the
Alfv\'{e}n, slow, and fast modes respectively.  For both higher
and lower $\beta$, the proportion of energy in fast modes decreases
substantially (to less than $1\%$), while the slow mode energy remains
at the same order of magnitude. Thus it is broadly appropriate to
assume that all of the magnetic
field fluctuation energy is in the slow modes, and that
the particle acceleration is dominated by interactions with slow modes.

\subsection{Test particle integration}
\label{sec:testParticles}

For a given fluid simulation, we simulate a statistical ensemble of
charged test particles which are initialized randomly throughout the
box of fully saturated turbulence. These test particles are evolved
according to the Lorentz force
\begin{equation}
  \label{eq:lorentzForce}
  \frac{d \boldsymbol{\overline{p}}}{dt} = \frac{q}{m c} \boldsymbol{E} +
  \frac{q}{m c} \boldsymbol{\beta} \times \boldsymbol{B},
\end{equation}
where the dimensionless momentum $\boldsymbol{\overline{p}} \equiv
\boldsymbol{p} / mc$, and $\boldsymbol{\beta} = \boldsymbol{u}/c$ is
the particle's physical velocity. The $E$
and $B$-fields are those on the MHD grid, interpolated to the
particle's location using the triangular-shaped cloud
\citep{Hockney1981} method in space and time. For each simulation, we
also choose a numerical value for the speed of light $c$, which
affects the motion of the test particles. The choice of $c$ does not,
however, affect the turbulence.    Our
choice of  non-relativistic turbulence and relativistic test particles
is appropriate for studying high energy supra-thermal particle
acceleration.

Particles are integrated
using the \citet{Vay2008} particle pusher, which is sympletic and
symmetric in time, and conserves energy and the magnetic moment
adiabatic invariant to machine precision in tests with constant
fields.\footnote{The \cite{Boris1970} pusher is not as accurate when fluid velocities are non-negligible fractions of the chosen value of $c$. In tests, these errors did not significantly affect our
  results, but we nevertheless prefer the Vay pusher for the relativistic
  case.}   We initialize the test particles with sufficiently high
gyrofrequencies that diffusion and heating is independent of
gyrofrequency; i.e. $\Omega \gg \omega$ where $\omega$ is the
frequency of any turbulent motions and $\Omega$ is the relativistic
gyrofrequency.  To calculate the momentum diffusion coefficients, we further initialize particles with a specific value of
$\overline{p}$, and generally take $\overline p_\perp = \overline
p_\parallel$.
The momentum is defined with respect to
the bulk rest-frame of the simulation, though for the
relativistic particles we focus on, this choice is
unimportant because the particle velocities are much greater than the fluid velocities.

The  velocity diffusion
coefficients are calculated according to
\begin{equation}
  \label{eq:diffusionDefinition}
  D_{\overline{p}} \equiv \frac{\langle \delta \overline{p}^2 \rangle} {2 \, \delta t},
\end{equation}
where the average is over many particles with the same initial
momentum.
One subtlety is that because we initialize the particle momentum with
respect to the bulk rest frame of the simulation, they are not
initially moving with the local drift velocity. As they change their
motion to follow the drift velocity, the
particle momentum undergoes an initial transient ``jump'' which saturates
at the rms velocity of the turbulence (times the Lorentz factor of the
test particle, for ultra-relativistic particles). We sidestep this
subtlety by fitting a linear function in $t$ to $\langle \delta
\overline{p}^2 \rangle$ at later times using
least-squares.

\section{Numerical results}
\label{sec:numericalResults}

In the analytic calculations summarized in \S \ref{sec:transportProperties}, the particles are assumed to diffuse primarily in $p_\parallel$, as expected for particles interacting with long wavelength, low frequency turbulent fluctuations.    In our numerical calculations, we find that particles undergo diffusion in both $p_\parallel$ and $p_\perp$ (or, equivalently, in total momentum $p$ and magnetic moment $\mu$).  This is true for both the relativistic calculations presented here and our earlier non-relativistic test particle calculations \citep{Lehe2009, Lynn2012}.   For the non-relativistic test particle calculations, the diffusion time for $\mu$ was somewhat longer than that for the total momentum $p$, while for the relativistic test particle results presented in this paper, the two timescales are comparable.    This diffusion in $\mu$ corresponds to an effective pitch angle scattering rate and may be due to violation of magnetic moment conservation by finite amplitude low frequency turbulent fluctuations \citep{Chandran2010}.   The theory for the latter has not been fully worked out for the $\beta \sim 1$ conditions we focus on here.   In what follows, we defer a detailed analysis of the diffusion in $\mu$ to future work and focus on the diffusion in total momentum $p$.

Figure \ref{fig:Dp_vs_p} demonstrates that for relativistic test
particles, the momentum diffusion coefficient is robustly of the form
$D_{\overline p} \propto {\overline p}^2$.
\begin{figure}
 \includegraphics[width=3.25in]{Dp_vs_p.pdf}
  \caption{Test particle momentum diffusion coefficients as a function of $\overline p \equiv p/mc$ normalized by
    $\overline{p}^2$ for several values of $\beta$ (for fixed driving
    rate $\dot{\epsilon} = 0.01 c_s^3 / L$ and fixed $c=10 \,
    c_s$). For each $\overline p$,  the diffusion coefficient is measured for an ensemble of particles with ${\overline p}_{\perp} = {\overline
      p}_{\parallel} =  {\overline p}/\sqrt{2}$ that are initially at random positions in the turbulent box.   The numerical results demonstrate that $D_{\overline p} \propto    {\overline p}^2$ for    ultrarelativistic
    particles (${\overline p} \gg 1$), consistent with the analytic
    expectations from equation \ref{eq:slowModeDiffusion}.}
 \label{fig:Dp_vs_p}
  \
\end{figure}
This is in contrast to the case of non-relativistic particles where
the diffusion coefficient for particles interacting with subsonic
turbulence is roughly $D \propto p$ for supra-thermal particles
\citep{Lynn2012}.

The analytic results summarized in equation \ref{eq:slowModeDiffusion} also predict that for  relativistic particles, the magnitude of the diffusion coefficient depends on the magnetic compressibility of the turbulence and $v_A/c$.   We now test these expectations using our test particle simulations.

Figure \ref{fig:Dw_vs_dB2} shows how the measured diffusion coefficient (normalized by $\overline{p}^2$) varies
with the rms magnetic field compression $\delta B_\parallel/B_0$. The latter is directly measured in the simulations as described in \S \ref{sec:turbulenceProperties}.
Figure \ref{fig:Dw_vs_dB2} shows that the diffusion coefficient scales with the total turbulent energy in the magnetic field compressions, consistent with equation \ref{eq:slowModeDiffusion}.
\begin{figure}
 \includegraphics[width=3.25in]{Dw_vs_dB2.pdf}
  \caption{Test particle momentum diffusion coefficient for relativistic particles as a function of the strength of  the magnetic compressions $\propto \delta B_\parallel$, for several values of $\beta$.   The simulations have
   $c = 10 \, c_s$ and different turbulent driving rates $\dot \epsilon$. The numerically determined
    diffusion coefficients are $\propto (\delta B_\parallel/B_0)^2$
    (light dashed lines, with arbitrary normalization), consistent with the  analytical predictions in \S \ref{sec:transportProperties}.}
  \label{fig:Dw_vs_dB2}
\end{figure}

Figure \ref{fig:Dp_vs_c} shows the dependence of the measured diffusion
coefficient on the ratio $c/v_A$, for three different values of
$\beta$.  We reiterate that in each simulation, we
choose a value for the speed of light $c$ only for the purposes of evolving the test particles (the choice of $c$ has no impact on the properties of the turbulence).   The diffusion coefficients in Figure \ref{fig:Dp_vs_c} are normalized by the analytic
prediction in equation
\ref{eq:slowModeDiffusion}.\footnote{Specifically, we use
  $D_{\overline{p}} \simeq 0.4 \overline{p}^2 (\delta
  B_\parallel/B_0)^2 v_A^2/cL$ for the analytic prediction from
  equation \ref{eq:slowModeDiffusion}, with $\delta B_\parallel/B_0$
  calculated for each simulation, where we have used
$\ln \left( k_{\rm max} L \right) = \ln 64 \simeq 4.15$ for the fiducial simulation. For the
higher resolution simulations, the logarithmic factor is adjusted as
appropriate.}
For each $\beta$, $v_A$ and $c_s$
are fixed, so the x-axis in Figure \ref{fig:Dp_vs_c} corresponds to
different choices of $c$.
For $c \gg v_A$, the results are reasonably consistent with the analytical
predictions.  In addition to the results for the fiducial simulation,
Figure \ref{fig:Dp_vs_c} also shows two other $\beta = 1$ simulations:
(1) one with the same resolution but a larger driving scale by a
factor of two, so that the inertial range is somewhat more extended
(HR)  (2) a second higher resolution 1024x256$^2$ simulation.    The
results for both of these other simulations are very similar to the
fiducial calculation, confirming that the large-scale fluctuations
that are well-resolved in a typical MHD simulation produce the
majority of the particle acceleration.

\begin{figure}
 \includegraphics[width=3.25in]{Dw_vs_c.pdf}
\caption{Test particle momentum diffusion coefficients for relativistic particles normalized by
   the   analytic prediction of equation \ref{eq:slowModeDiffusion}
  for simulations with different $\beta$ and $v_A/c$.   For $c \gg
   v_A$, the results are well-described by the analytical predictions.
   The test particle calculations are for an ensemble of particles
   with ${\overline p}_{\perp} = {\overline p}_{\parallel} =
   {\overline p}/\sqrt{2}$.   The orange
   triangles (HR) are from a run with the fiducial number of grid
   cells but a larger turbulent driving scale, so that the
   turbulence has an inertial range that is 2 times larger.  The blue triangles (HR2) are for a higher resolution $1024\times256^2$ simulation.   Both resolution tests yield very similar results indicating that large scale turbulent fluctuations dominate the particle acceleration.}
 \label{fig:Dp_vs_c}
\end{figure}

\subsection{Long-time evolution of distribution function}
\label{sec:evolution}

The diffusion coefficients shown in Figure \ref{fig:Dp_vs_c} correspond to particle acceleration times that are many eddy turnover times.   As a result, it is computationally intensive to directly simulate the long timescale evolution of the distribution function.   To study the latter, we instead separately solve the time dependent diffusion equation for the distribution function $f(p,t)$ using the momentum diffusion coefficients determined in our test particle calculations.   In particular, we begin with a Maxwellian distribution function
having $k_B T \sim m c^2$, i.e., $\langle \overline p \rangle \sim 1$ and evolve it subject to a diffusion coefficient given by $D_{\overline p} \equiv \overline p^2/t_a$ where $t_a$ defines the acceleration time.    Figure \ref{fig:df_evol} ({\em right panel}) shows the resulting distribution function at later times.  For comparison, we also show  a Maxwell-J{\"u}ttner distribution function (black dashed lines) that has the same total energy as the final distribution function in our diffusion calculations.     Figure \ref{fig:df_evol} shows that the distribution function quickly develops a significant non-thermal tail, on a timescale of $\sim 0.25 \, t_a$.   As a consistency check, the  {\em left panel} in Figure \ref{fig:df_evol} shows that over the timescale we can directly simulate the MHD turbulence with test particles, the evolution of the distribution function is indistinguishable from the solution of the momentum-space diffusion equation.

\begin{figure*}
\includegraphics[width=7in]{f_vs_t.pdf}
 \caption{Evolution of the particle distribution function due to interaction with MHD turbulence.   \textit{Left panel:} Comparison of test particle simulations (dotted)
  with the numerical solution of the time dependent diffusion equation (solid blue) using
  a  momentum diffusion coefficient given by $D_{\overline p} \equiv
  \overline{p}^2/t_a$, where $t_a$ defines the acceleration time and is derived from the test particle results.   The particles are initially thermal and isotropic, and evolve over a
  long time baseline ($t = 20 \, L/c_s$ vs. $1 \, L/c_s$ for
  the calculations used to measure the diffusion coefficient). The numerical solution of the diffusion equation is shown at the same time and is in good agreement with the direct evolution of the test particles. \textit{Right panel:} Longer-time evolution of the numerical
  solution of the diffusion equation. The particles gain energy exponentially, with an
  e-folding time of approximately $0.25 \, t_a$.  On a comparable timescale, the distribution function develops a significant non-thermal tail.  For comparison, we also plot a thermal distribution with
  the same energy as the final distribution (black dashed curve), which highlights the substantial
  non-thermal tail at high energies.}
  \vspace{0.15in}
  \label{fig:df_evol}
\end{figure*}
\
\section{Conclusions \& Implications}
\label{sec:conclusions}

Our results demonstrate that  subsonic MHD turbulence efficiently accelerates relativistic particles with a Fermi-like momentum diffusion coefficient $D_p \propto p^2$.  This is true for both $\beta \lesssim 1$ and $\beta \gtrsim 1$ and is thus a robust property of charged particles interacting with low frequency MHD turbulence.   We have restricted our analysis to particles whose (relativistic) cyclotron frequencies are  larger than the frequencies of the turbulent fluctuations.   In practice this limits our analysis to particles that are not too relativistic.

Our key analytic result is that nonlinear broadening of quasi-linear resonances implies that slow modes in strong MHD turbulence can interact efficiently with relativistic particles, despite being
unable to satisfy the linear resonance condition (see \citealt{Chandran2000} for a similar result).
{\bf In particular, resonance broadening allows long wavelength turbulent magnetic field compressions  satisfying $k_\parallel c \lesssim \omega_{\rm nl}$ to accelerate particles, where $\omega_{\rm nl}$ is the non-linear decay rate of the turbulence at a given scale.}

Because slow modes tend to be energetically more important than fast modes in subsonic turbulence, this suggests that interactions with slow modes may dominate the overall
particle acceleration by low-frequency, weakly compressible MHD
turbulence.  This is contrary to the standard quasi-linear theory
results in the literature (e.g., \citealt{Achterberg1981}).  However, the particle acceleration efficiency by fast  modes depends sensitively on their turbulent power spectrum, which is not fully understood.  In particular,  if the fast mode spectral index is $\alpha \sim 3/2$ (which is not the case in our simulations, though it is suggested by some studies), fast modes may be more efficient than slow modes at accelerating particles even if their total energy density is smaller (see eq. \ref{eq:fastModeDiffusion}).

For relativistic particles, momentum diffusion of the form $D_p \propto p^2$ produces a power-law spectrum $dN/dp \propto p^{-1}$ so long as the acceleration time of particles (which is independent of particle energy) is shorter than the radiative loss timescale and the escape time from the acceleration region   \citep{Blandford1987}.     The total energy in the accelerated particle population depends on the efficiency with which `seed' relativistic particles are created.   Because suprathermal particle acceleration is  inefficient for non-relativistic particles interacting with MHD turbulence \citep{Lynn2012}, it is not clear if the net acceleration efficiency (by turbulent mechanisms alone) will be substantial for plasmas with non-relativistic temperatures, because the turbulence itself does not self-consistently seed relativistic particles.   By contrast, for relativistically hot plasmas, the formation of a non-thermal tail of relativistic particles by the mechanism studied here is likely to be quite efficient.    One particularly important application of our results is thus to accretion flows onto black holes, where the electrons can in some cases have $k T \gtrsim m_e c^2$ even though the disk turbulence itself is non-relativistic.

\subsection{Implications for Black Hole Accretion Flows}

Weakly compressible MHD turbulence is
generic in black hole accretion flows as a consequence of the nonlinear
evolution and
saturation of the magnetorotational instability \citep{Balbus1998}.
Non-thermal particle acceleration by such turbulence is of particular
astrophysical interest in at least two circumstances.  First, at low
accretion rates onto a black hole or neutron star, the accretion flow
can adopt a low-collisionality state in which much of the emission can
be dominated by a non-thermal population of electrons, if such a
population is present (e.g., \citealt{Yuan2003}).   Secondly, in luminous
radiatively efficient accretion flows, non-thermal emission from the
disk surface layers (a ``corona") can contribute significantly to the
synchrotron and high energy inverse Compton emission.  We briefly
discuss the implications of our results for these applications.

The momentum diffusion coefficient calculated in \S
\ref{sec:transportProperties} and Figure \ref{fig:Dp_vs_c}
corresponds to a rate of energy gain given by \begin{equation}
\label{eq:Edotacc}
\dot E_{\rm acc} \sim  \frac{c \, D_p}{p} \equiv A \, p \,
\frac{v_A^2}{L}\left(\frac{\delta B_\parallel}{ B_0}\right)^2
\end{equation}
where $A$ is a dimensionless coefficient  that
encapsulates the efficiency of the particle acceleration and can be
calibrated using our test particle simulations.   In particular,
Figure \ref{fig:Dp_vs_c} corresponds to $A \sim 1/3$  for $c/v_A
\sim 10-100$, the values expected in the inner regions of accretion
disks around black holes.
The exact value of $\delta B_\parallel/B_0$ in accretion disk turbulence is somewhat uncertain. For the $\beta \sim 10-100$ conditions expected, $\delta B_\parallel \sim 0.3 \, B_0$ is plausible.   However, the exact value depends in part on the effect of collisionless damping on the compressibility of accretion disk turbulence, which is not well understood.   Moreover, small-scale fluctuations generated by the mirror instability may contribute significantly to the magnetic field compressions in collisionless disks \citep{Kunz2014,Riquelme2014}.

The acceleration of particles by disk turbulence requires that the acceleration time is shorter than the viscous time.   Given the acceleration rate in equation \ref{eq:Edotacc} this is likely achieved in the inner regions close to the black hole.  In addition, the acceleration of particles by disk turbulence is limited by
radiative losses, in particular synchrotron and inverse Compton
emission.   Focusing on the former,
we find that the maximum Lorentz factor of accelerated electrons
is given by
\begin{equation}
\label{eq:gmax}
\gamma_{\rm max} \sim A \, \left(\frac{m_e}{m_p}\right) \tau_T^{-1} \left(\frac{\delta B_\parallel}{B_0}\right)^{2}
\end{equation}
where $\tau_{T} \equiv \sigma_T n_e L$ is the Thompson optical depth
across the outer scale of the turbulent fluctuations $L$.   Equation \ref{eq:gmax} implies that non-thermal emission from accelerated
electrons is likely to be particularly important in low-luminosity
systems where $\tau_T \ll 1$.   As a concrete example, in models of
the emission from Sgr A*, $\tau_T \sim 10^{-5}-10^{-6}$ (e.g.,
\citealt{Yuan2003,Gammie2009}) so that $\gamma_{\rm max} \sim
100$.   This implies that the particle acceleration found here
may substantially modify the electron distribution function for
electrons that emit in the mm-infrared.    This is particularly
important to understand in the context of interpreting the variable
infrared emission and resolved mm images of Sgr A* (e.g.,
\citealt{Doeleman2008, Do2009}).      In the near future, more
detailed calculations of test particle electron acceleration in
shearing box simulations can be used to quantify the uncertain
dimensionless coefficient A in the above acceleration efficiency.

A second potential application of our results is to high energy emission from luminous accreting black holes, which can be produced by a combination of thermal and non-thermal processes.   However, phenomenological models of this emission suggest that $\tau_T \sim
0.1-1$ in the emission region \citep{Haardt1991,Esin1997}.   As a
result, it is unlikely that the particle acceleration found here is
sufficiently rapid to compete with radiative losses by synchrotron and
inverse Compton emission.

\begin{acknowledgements}
This material is based on work supported by the National Science
Foundation Graduate Research Fellowship under Grant
No. DGE-1106400. This work was also supported in part by
NASA HTP grant NNX11AJ37G, NSF grant AST-1333682, a Simons Investigator award from the Simons Foundation, the David and Lucile Packard Foundation,
and the Thomas Alison Schneider Chair in Physics at UC Berkeley.
Computing time was provided by the National Science Foundation
TeraGrid/XSEDE resource on the Trestles and Kraken
supercomputer.
\end{acknowledgements}

\bibliographystyle{apj}

redpajama_set_name: RedPajamaArXiv


At Prohobitox we work with the four seasons to create a new kind of style cooking namely 'Asian Crossover´,which is based on regional Chinese cuisine, specialising Asian tapas or 'Dim Sum'.
We produce everything in-house and source the finest raw produce form Malaga, Andalusia, Europe and Asia.
Belly of Pork "Dong Po"
G Gluten (eg: wheat, rye, barley, oats, spellet). NE Nuts (almond, hazelnut, cashew, pecan, Brazil, pistachio). SH & M Shells and Molluscs (scallops, snails, clams, squid). F Fish. PN Peanuts. SY Soya. MK Milk. CEL Celery. SEM Sesame. SH Shellfish. LU Lupine. E Egg.


No matter which Eucharistic Prayer we use, (1, 2, 3, 4 or the various Eucharistic Prayers for Reconciliation or for Masses for Children) they all end the same with the "Eucharistic Doxology." A "doxology" is the English translation of a Greek word which means a short hymn of praise to God.
The priest proclaims: "Through Him, with Him, in Him, in the unity of the Holy Spirit, all glory and honor is yours almighty Father, forever and ever," as he raises the Eucharistic Lord in the consecrated host and in the Precious Blood in the sacred chalice for the entire congregation to see and ponder.
Who is the "Him" in this hymn of praise? Jesus Christ, of course. So, this short prayer is a Trinitarian formula of praise to God the Father through Christ, with Christ, and in Christ, in union with the Holy Spirit.
The Mass is clearly a prayer of praise to the Father, by the Son, through the Holy Spirit.
There's a lot going on at each Mass, isn't there?
Next:What does it mean to repent?


It would be easy to roll your eyes at Francis Mallmann. The 61-year-old Argentine super chef, who came to global attention after appearing on Netflix's Chef's Table, speaks in gravelly, earnest platitudes. When I meet him in London in June, he sits there, all silk cravat, linen suit and grizzled white beard and doles out lines about freedom and the power of nature. It would be easy to scoff, sure, but the thing is, you'd be hard pressed to prove any of this was inauthentic.
Mallmann practises what he preaches. The chef, born in 1956 in Buenos Aires but raised in the wilds of Patagonia, has long eschewed any semblance of a normal life. In any one week, he can be in five different countries, he sees his wife two weeks a month, has "lost respect" for most of his sedentary friends, and lives mostly on a remote Patagonian island, where he long ago rejected the kitchen for vast fire pits outside.
Bizarrely, it all began in the '60s when he heard The Monkees. Something about their music proved a catalyst for his sense of adventure and he flew off to Paris to study under Michelin-starred chef Alain Chapel. There, he began to learn his craft, but his efforts to master traditional French cuisine were not met without criticism. It took an unimpressed French business man – the head of Cartier to be exact – to tell him his food was, well, lacking. "This is not French food" were his exact words.
This seemingly catastrophic encounter was actually exactly what Mallmann needed to find his own culinary signature. "I went back to my memories of childhood," he says. "Slowly I started creating this language of cooking with fire that I think represents the naked cooking of South America so much." One of Mallmann's favourite ways to cook is in a pit dug out of the earth, a technique he grew up with and one that goes back thousands of years.
He now has 11 restaurants across South America, France and Miami, with a London outpost coming next year. This July, he will be collaborating with Krug for their Into the Wild festival in the English countryside.
So how does this self-possessed wandering chef find himself cooking at a luxury festival for a high-end Champagne house? Set in the grounds of the Grange, a romantic 19th century estate in Hampshire, this is a luxury event, yet it oddly chimes well with Mallmann's philosophy.


text:
ISC announces win...
ISC announces winner of the Hans Meuer award
A paper which focuses on the area of in-memory architecture will be the recipient of the first Hans Meuer award, to be presented at this year's European Supercomputing Conference, ISC High Performance, in July. The award is in memory of one of the pioneers of European supercomputing, Hans Meuer, the charismatic founder of the ISC conference series and co-developer of the Top500 list of the world's fastest machines, who died last year.
The paper 'Accelerating LBM & LQCD Application Kernels by In-Memory Processing' was submitted jointly by a team of seven researchers representing the Juelich Supercomputing Centre (JSC), IBM Germany, and the IBM Watson Research Center in the USA. It was selected by the research paper committee out of the three papers with the highest review scores.
The team examined the run-time performance of Lattice Boltzmann Method (LBM) and Lattice Quantum Chromodynamics (LQCD) kernels that can be achieved when using Active Memory Cube technology, an in-memory architecture aimed at exascale computing.
The architecture uses 3D memory technology and is designed to significantly reduce energy consumption by performing computation within the memory module. Performance results were obtained by using cycle-accurate simulations.
Thorsten Hater of JSC will present a keynote during the research paper session 1 on Monday afternoon. Thorsten will be representing his colleagues, Paul F Baumeister, Andrea Nobile, and Dirk Pleiter of JSC; Hans Boettiger and Thilo Mauer of IBM Germany (Research & Development); and Jose R Brunheroto from the IBM Watson Research Center.
The winners will also receive a cash prize of €3,000, an award certificate, and a free conference pass for ISC 2016.
ISC High Performance

redpajama_set_name: RedPajamaCommonCrawl


Vegan powerlifters and fitness fanatics are rejoicing today following yesterdays announcement from Redcon1 CEO Aaron Singerman that they would be rolling out their first Vegan Protein Powder. Aaron himself said never in a million years did he think he would be rolling out a naturally sweetened vegan protein but after tasting this formula he was sold. A full list of flavors has yet to be released, however Strawberry has been confirmed as at least one possible flavor. The official release date has not been announced but Green Beret should become available in early March which is just a few weeks away. Stay tuned to the Best Price Nutrition blog for updates on the release of this first of it's kind product.


text:
Slut & Sons
True tales of a pervert and her progeny
June 14, 2021 July 6, 2021 Janet W. Hardy
The Third Child – 06/14/2021
I can't write about Miles and Ben and me without writing about the third child – the one that made me famous and cost me some important relationships, that led me up to the edge of a nervous breakdown and made me friends all over the world, the one with whom we all shared our lives.
The ovum of that child was released, I guess, when I wrote an article distilling my three whole years of experience into a few thousand words, called it "How to Be a Sexually Dominant Woman," and fired it off to Cosmopolitan.[1]
The sperm was the owner of a local erotic boutique. She'd invited me to teach a workshop for novice dommes and their partners. She asked me what name I wanted to use, and, more or less at random, I said "Lady Green." I showed her my article, and she said, "This is great – can we use it as a handout?"
"I've already submitted it to Cosmo, so that won't work," I said. "But I could rewrite it and we can use that instead."
And the zygote – I promise I'll stop belaboring this metaphor now – began to form. The article grew and grew, and Jay said, "You know, that's enough words for a small book" – and, well, things kind of took off from there.
But at the same time that Greenery Press was being born, my career in advertising was dying.
I was working as a copywriter at a small Silicon Valley agency specializing in high-tech clients. I'd been their cherished darling when they first hired me – the skills that later gave me a career in explaining weird sex to the masses served me well in talking to engineers, figuring out what they were trying to say, and translating that into fun, benefit-oriented prose that an executive or purchasing agent could understand.[2]
I was having fun, I was making more money than I ever had before, I adored my coworkers and they adored me. Until, gradually, they didn't.
Having just joined the actual kink community, I was newly in love with being able to speak what had formerly seemed unspeakable. Like many newbies, I wasn't being terribly careful about the boundaries between my erotic self and all my other selves. The kind of issues that would have been unexceptionable if I'd been putting energy into the PTA or my bowling team were a problem when they were about scheduling a play party or mediating a community conflict – and although I tried to be careful to keep my personal business personal, it seeped through.
Things came to a head at a mandatory company retreat. I loathe, as a matter of principle, such exercises in forced bonding (I already have friends, and the reason they're my friends is that I chose them), but at this one we were being encouraged to drink. A lot.
By this point in the book, you have probably figured out that I am not very inhibited when I'm sober. So you can just imagine what I get up to with four or five drinks in me.
The weekend is kind of a blur, but I have a patchy memory of a series of skits in which we were asked to pretend we were one of our coworkers. Which somehow led to my bright idea that acting my part involved grabbing the assistant media buyer by the crotch.
In short, the weekend was the end of any illusions the company might have had that they had hired a nice girl.
What happened next, quite quickly:
A companywide memo went out forbidding personal calls on company time. It was summertime, the Dudes were in day camp[3] but home with Jay in the afternoons, and I had been checking in with them once or twice a day to forestall mayhem – but I obeyed the rule and stopped making those calls.
Jay began complaining that his work was being interrupted by six or seven hang-up calls a day.
I was called into the boss's office, shown a phone bill that included six or seven calls a day to my home number, and fired on the spot.
I suppose I could have applied for other copywriting jobs, but I was too shocked and dispirited to try – plus, I'd only been in the Bay Area for a year, and I had no career support network there.
I already had the Sexually Dominant Woman piece drafted. Jay had a manuscript he called SM 101: A Realistic Introduction that he'd been working on for years, and had submitted to several mainstream publishers to no avail.
With my salary gone (and no hope of receiving unemployment, as I'd been "fired with cause"), we were staring bankruptcy in the face.
For his first book, The Bay Area Sexuality Resources Guidebook, Jay had already figured out a strategy that presaged today's "print-on-demand" system: he'd get an order from an erotic boutique or leather store, then call the copy shop to order that many copies of the book, photocopied and comb-bound. We'd pick up the books, deliver them to the retailer, and rush the resulting check to the bank quickly, before our check to the copy shop[4] bounced.
So we had three books, and we had a (funky but functional) distribution system. I'd spent my decade in advertising looking over the shoulders of excellent graphic designers, so I had a smidgen of understanding of basic layout principles and techniques. I spent money we didn't have on a copy of Quark XPress layout software and got to work – and within six weeks of my expulsion, we had camera-ready art on both Jay's and my books.
We started out as two separate companies – Jay Wiseman Books and Greenery Press. It didn't take long for Jay to realize that he had no ability or desire to be a publisher, so we combined the two companies under the Greenery Press banner, and I got busy.
Within a year or two, I was hearing from mainstream bookstores saying they'd like to carry our books, but couldn't accept the comb binding – they needed books to be perfect-bound[5].
If Jay's precognitive contribution to Greenery was print-on-demand, mine was crowd-funding. I found folks who were willing to front us money for a print run, in exchange for a credit in the book and repayment of the loan out of book sales.
The Sexually Dominant Woman: A Workbook for Nervous[6] Beginners was our first "real" book, followed in short order by The Bottoming Book and The Topping Book. Our next big step was publishing a book that neither Jay nor I had played any part in writing, Miss Abernathy's Concise Slave Training Manual. (All four books are still in print in some form.) By then, we were well and truly launched.
This was about the time that the world, especially the Bay Area, got wildly excited about a buzzy new concept called the World Wide Web. Huge amounts of money were getting invested in startups, and I wanted some of it.
I'd met a man – a former member of the Kerista family[7] – at a polyamory conference, where he'd announced himself as a financial consultant specializing in publishers. With his help, I crafted a (wildly overoptimistic) business plan, incorporated the business, found some investors, hired some employees, and committed to a minimum of four books a year.
The odd thing is that in that couple of years, I published more books that would go on selling well for years than I ever did afterwards – but it still wasn't enough. Greenery Press made itself an ironic name by running constantly in the red. I got incredibly lucky in the folks assigned to our tax accounts – the guy from the IRS collected vintage Chinese erotica, and the guy from the California Board of Equalization was the biological son of a publisher whose obscenity case had gone to the Supreme Court – and they truly did want to help me. But the fact was that we were hugely, terrifyingly in debt, and likely to go on getting more so. I owed money to printers, to authors, to suppliers, to back payroll. (The authors were a particular source of tension, as many of them were personal friends. I started to avoid scene events because of the likelihood of running into people to whom I owed hundreds or thousands of dollars.)
The constant financial and emotional stress (this was also happening concurrently with Miles's illness) spelled the end of my relationship with Jay. But the company owed him a lot of money that we couldn't repay, and I couldn't see any way to separate without putting him out on the street.
Then, I woke up one morning with an epiphany: If I rented an industrial loft and moved into it, I could lose the monthly cost of the office Greenery was subletting, and Jay could have our place[8]. I let go all but one employee and cut that one back to part-time, and started in on the next chunk of my life.
That was a very bad few months. I am not by nature an anxious person, but I'd been pushed far beyond the amount of stress I could manage. The breakup was the only really acrimonious one I've ever had; Miles was in and out of the hospital; I was drowning in debt; my closest friends were angry with me over the royalties situation. But slowly, aided by a lot of medication and the support of the friends to whom I didn't owe money (and the few, god bless them, who were able to compartmentalize our friendship away from our finances), I gradually began to craft a new life. I sold my place in San Francisco, signed the proceeds over to the company, and paid off one debt at a time – first the printers, then the tax guys, and then the authors. Bit by bit, I clawed my way back from the brink.
I'd reached the point where I wasn't living in a state of constant panic, but the company wasn't in the black, or likely to get there anytime soon. After a couple of years of brinkmanship, I cut a deal with our distributor for them to buy the company from me over a five-year period. The proceeds were enough to get us caught up with the authors, and SCB took over all the company finances. They kept me on board as an editorial consultant, and we went on producing a book or two a year.
But the tide, inevitably, turned. We'd been very lucky to have caught the wave of kink culture just as it was cresting, and we rode that sucker for a couple of decades (with a huge boost, I regret to say, following the publication of 50 Shades of Grey). The Ethical Slut, which was our biggest title, had been sold to Ten Speed/Random House some years before, and the handful of other polyamory books we published never came close. Sales of all the kink books ebbed as BDSM stopped being a hot new trend (and as kink education became increasingly available on-line).
It was time. In 2019, I resigned my consultancy and Greenery stopped publishing new books.
There was, of course, the small issue of all the infinitely patient shareholders who had invested in us back during the halcyon days of the dot-com boom. I did eventually get them paid off too – I actually, no shit Sherlock, had a maiden aunt who died and left me some money. So that final debt was paid, and I was free to move forward into whatever comes next.
So, that's how I raised Greenery to the ripe old age of twenty-seven. It's still out in the world making a living off the backlist. Greenery made me famous (in my own odd way), and it supplied me with as much joy and as much misery as any human child could provide. It was a great run – but, honestly, I am so glad it's over.
[1] Fat fucking chance. Cosmo accepts that kind of material now, but in 1992 its fare was more along the lines of "How to Make Him Like You as Much as You Like Him," "Cover Girl Meets Rocker and… It's Magic," and "For That Fantasy Romance Among the Too Rich, Read Ivana Trump's 'For Love Alone'." You can't make this stuff up.
[2] This sector of the advertising industry is called "business-to-business," and is looked down on as more workmanlike and less glamorous than consumer advertising. My talents have never been a great fit for consumer advertising. I was, however, a very, very good business-to-business writer.
[3] It may be relevant to note that only one other person in the company had kids, and he had a stay-at-home wife to take care of them.
[4] There was a small disturbance when the copy shop found that their practice of binding discarded pages into scratch pads for distribution at local schools had suddenly become a problem. Fortunately, it wasn't our problem.
[5] The kind of binding you see on nearly all paperback books, with a flat, printed spine.
[6] Another Jay contribution: I was going to call it A Workbook for Eager Beginners. He was right.
[7] Too much to explain here. Look them up; they're fascinating.
[8] He decided not to stay, but at least I'd made the offer.
Tags: getting fired, kink, parenting, publishing


text:
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Hank Aaron, baseball's one-time home run king, dies at 86
11 months 4 weeks 2 days ago Friday, January 22 2021 Jan 22, 2021 January 22, 2021 10:09 AM January 22, 2021 in News
Photo: Chris Evans / CC BY 2.0
ATLANTA (AP) — Hank Aaron, who endured racist threats with stoic dignity during his pursuit of Babe Ruth's home run record and gracefully left his mark as one of baseball's greatest all-around players, died Friday. He was 86.
The Atlanta Braves, Aaron's longtime team, said he died peacefully in his sleep. No cause was given.
Aaron made his last public appearance just 2 1/2 weeks ago, when he received the COVID-19 vaccine. He said he wanted to help spread the to Black Americans that the vaccine was safe.
"Hammerin' Hank" set a wide array of career hitting records during a 23-year career spent mostly with the Milwaukee and Atlanta Braves, including RBIs, extra-base hits and total bases.
But the Hall of Famer will be remembered for one swing above all others, the one that made him baseball's home-run king.
It was a title he would be hold for more than 33 years, a period in which the Hammer slowly but surely claimed his rightful place as one of America's most iconic sporting figures, a true national treasure worthy of mention in the same breath with Ruth or Ali or Jordan.
Before a sellout crowd at Atlanta Stadium and a national television audience, Aaron broke Ruth's home run record with No. 715 off Al Downing of the Los Angeles Dodgers.
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The Hall of Famer finished his career with 755, a total surpassed by Barry Bonds in 2007 — though many continued to call the Hammer the true home run king because of allegations that Bonds used performance-enhancing drugs.
Bonds finished his tarnished career with 762, though Aaron never begrudged someone eclipsing his mark.
His common refrain: More than three decades as the king was long enough. It was time for someone else to hold the record.
No one could take away his legacy.
"I just tried to play the game the way it was supposed to be played," Aaron said, summing it up better than anyone.
He wasn't on hand when Bonds hit No. 756, but he did tape a congratulatory message that was shown on the video board in San Francisco shortly after the new record-holder went deep. While saddened by claims of rampant steroid use in baseball in the late 1990s and early 2000s, Aaron never challenged those marks set by players who may have taken pharmaceutical short cuts.
Besides, he always had that April night in 1974.
"Downing was more of a finesse pitcher," Aaron remembered shortly before the 30th anniversary of the landmark homer. "I guess he was trying to throw me a screwball or something. Whatever it was, I got enough of it."
Aaron's journey to that memorable homer was hardly pleasant. He was the target of extensive hate mail as he closed in on Ruth's cherished record of 714, much of it sparked by the fact Ruth was white and Aaron was black.
"If I was white, all America would be proud of me," Aaron said almost a year before he passed Ruth. "But I am black."
Aaron was shadowed constantly by bodyguards and forced to distance himself from teammates. He kept all those hateful letters, a bitter reminder of the abuse he endured and never forgot.
"It's very offensive," he once said. "They call me 'nigger' and every other bad word you can come up with. You can't ignore them. They are here. But this is just the way things are for black people in America. It's something you battle all of your life."
After retiring in 1976, Aaron became a revered, almost mythical figure, even though he never pursued the spotlight. He was thrilled when the U.S. elected its first African-American president, Barack Obama, in 2008. Former President Bill Clinton credited Aaron with helping carve a path of racial tolerance that made Obama's victory possible.
"We're a different country now," Clinton said at a 75th birthday celebration for Aaron. "You've given us far more than we'll ever give you."
Aaron spent 21 of his 23 seasons with the Braves, first in Milwaukee, then in Atlanta after the franchise moved to the Deep South in 1966. He finished his career back in Milwaukee, traded to the Brewers after the 1974 season when he refused to take a front-office job that would have required a big pay cut.
While knocking the ball over the fence became his signature accomplishment, the Hammer was hardly a one-dimensional star. In fact, he never hit more than 47 homers in a season (though he did have eight years with at least 40 dingers).
But it can be argued that no one was so good, for so long, at so many facets of the national pastime.
The long ball was only part of his arsenal.
Aaron was a true five-tool star.
He posted 14 seasons with a .300 average — the last of them at age 39 — and claimed two National League batting titles. He finished with a career average of .305.
Aaron also was a gifted outfielder with a powerful arm, something often overlooked because of a smooth, effortless stride that his critics — with undoubtedly racist overtones — mistook for nonchalance. He was a three-time Gold Glove winner.
Then there was his work on the base paths. Aaron posted seven seasons with more than 20 stolen bases, including a career-best of 31 in 1963 when became only the third member of the 30-30 club — players who have totaled at least 30 homers and 30 steals in a season.
To that point, the feat had only been accomplished by Ken Williams (1922) and Willie Mays (1956 and '57).
Six-feet tall and listed at 180 pounds during the prime of his career, Aaron was hardly an imposing player physically. But he was blessed with powerful wrists that made him one of the game's most feared hitters.
Hall of Famer Mike Schmidt described Aaron as "an unassuming, easygoing man, a quiet superstar, that a '70s player like me emulated."
"He was one of my heroes as a kid, and will always be an icon of the baby boomer generation," Schmidt said. "In fact, if you weigh all the elements involved and compare the game fairly, his career will never be topped."
Aaron hit 733 homers with the Braves, the last in his final plate appearance with the team, a liner down the left field line off Cincinnati's Rawley Eastwick on Oct. 2, 1974. Exactly one month later, he was dealt to the Brewers for outfielder Dave May and minor league pitcher Roger Alexander.
The Braves made it clear they no longer wanted Aaron, then 40, returning for another season on the field. They offered him a front office job for $50,000 a year, about $150,000 less than his playing salary.
"Titles?" he said at the time. "Can you spend titles at the grocery store? Executive vice president, assistant to the executive vice president, what does it mean if it doesn't pay good money? I might become a janitor for big money."
Aaron became a designated hitter with the Brewers, but hardly closed his career with a flourish. He managed just 22 homers over his last two seasons, going out with a .229 average in 1976.
Even so, his career numbers largely stood the test of time.
Aaron still has more RBIs (2,297), extra-base hits (1,477) and total bases (6,856) than anyone in baseball history. He ranks second in at-bats (12,354), third in games played (3,298) and hits (3,771), fourth in runs scored (tied with Ruth at 2,174) and 13th in doubles (624).
"I feel like that home run I hit is just part of what my story is all about," Aaron said.
While Aaron hit at least 20 homers in 20 consecutive seasons, he was hardly swinging for the fences. He just happened to hit a lot of balls that went over the fence.
Through his career, Aaron averaged just 63 strikeouts a season. He never whiffed even 100 times in a year — commonplace for hitters these days — and posted a career on-base percentage of .374.
He was NL MVP in 1957, when the Milwaukee Braves beat the New York Yankees in seven games to give Aaron the only World Series title of his career. It also was his lone MVP award, though he finished in the top 10 of the balloting 13 times.
Aaron also was selected for the All-Star Game 21 consecutive years — every season but his first and his last.
His only regret was failing to capture the Triple Crown. Aaron led the NL in homers and RBIs four times each, to go with those two batting crowns. But he never put together all three in the same season, coming closest in 1963 when he led the league in homers (44) and RBIs (130) but finished third in hitting (.319) behind Tommy Davis of the Dodgers with a .326 average.
"Other than that," Aaron said, "everything else was completed."
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There's a reason musicians write songs about us. It's the same reason we're home to the world's most iconic entertainment brands.
It's why trendsetters, dealmakers and record-breakers visit with suitcases, and come back in moving trucks. In Tennessee, we're not just committed to music and entertainment – we are music and entertainment.
Why bring your business to Tennessee? Because we're home to Music City, U.S.A and Soulville, U.S.A—the top cities in the nation for the music and entertainment industries. More than a quarter of the country's music publishers are located in Tennessee. In Nashville alone, 7.8 per 1000 jobs are in the music industry cluster, compared to 2.8 in New York, 2.6 in Austin and 2.0 in Los Angeles.
We have a sound fiscal management philosophy, and we back it up with continuous investments in our economic ecosystem. Our strategies for cultivating an attractive business climate are long-term, not short plays for quick headlines.
We have the lowest state debt per capita out of all 50 states. We also have the second lowest cost of living, and the second lowest state and local tax burden. Did we mention that we have absolutely no personal income tax on wages?
In Tennessee, we know job creation only happens when multiple parties are willing to risk capital. So we're committed to cultivating a climate that encourages investment. We believe your business deserves an environment with minimal risk and a climate that yields greater profitability. That's why our state operates with fiscal responsibility, and we have the stats to back it up.
Since 2011, more than 156,000 jobs have been created, and more than $12.8 billion has been invested in Tennessee businesses. An important part of our success has been our balance sheet. Our state government has a long-term track record of quality, conservative fiscal management that spans generations. Businesses can confidently invest in Tennessee without worrying that our state budget will later be balanced on their backs with new taxes and fees. That's the way we've always done business in Tennessee and we have no plans to change our tune. It's no wonder Business Facilities Magazine named us 2013 State of the Year.
We know that the longevity of your business relies on a developed workforce. In Tennessee, we're creating a seamless path between high school, post-secondary education and entering the workforce. We're creating innovative workforce partnerships and enacting game-changing education reform in order to develop a skill set that holds demand in today's labor market. The result is a steady pipeline of qualified candidates that are available to ensure your business makes the grade for years to come.
Tennessee is leading the way in K-12 education reform on a national level. We have continued that momentum and expanded our focus to include post-secondary education through Drive to 55 and the Tennessee Promise.
Drive to 55 is a critical mission to bring the percentage of Tennesseans with college degrees or certifications to 55% by the year 2025. It's not just a mission for higher education, but a mission for workforce and economic development, a drive to reduce unemployment and improve quality of life.
Beginning in 2015, the Tennessee Promise ensures high school graduates can attend two years at a community college or technical college absolutely free of tuition and fees.
We are the only state in the country that will be making this promise. It makes a clear statement to Tennessee families that education beyond high school is a priority in our state. It is a bold promise that will make college a reality for more high school graduates. It speaks volumes to current and prospective employers, and it will make a difference for generations of Tennesseans.
Additionally, we have the education pipeline to maintain a sustainable workforce. Last year, more than 2,600 degrees in entertainment industry completions were awarded at 51 institutions statewide, including Belmont University, Middle Tennessee State University, The University of Tennessee-Knoxville, University of Memphis, and Vanderbilt University.
Those numbers don't just talk – they sing. We have the musicians, vocalists, composers and sound engineers who can take your business wherever it needs to go. Tennessee is committed to competing nationally and globally. We have the workforce, and you'll have our support. Come and jam where the music's already playing.
From Bristol to Memphis, Tennessee has fostered the blues, soul, R&B, country, rockabilly and rock 'n' roll sounds that have revolutionized the music industry. But Tennessee isn't just where legends make music; it's where they make their homes. Justin Timberlake, Taylor Swift, and members of The Black Keys and Kings of Leon have all chosen to live in Tennessee. This is where entertainment industry professionals come to work, and never leave.
Because it all goes back to our Tennessee culture. We think work should feel like a vacation, and that culture and industry shouldn't stop at the borders of Knoxville, Nashville and Memphis. It's our unmatched lifestyle that garnered two Academy Awards for best original song for Memphis artists Isaac Haynes and Three 6 Mafia. We're passionate about what we do, and that passion exists in the heartbeats of the people who call this state home. From the Smoky Mountains of East Tennessee, through the rolling hills of the state's heartland, and all the way to the banks of the Mississippi River in West Tennessee, we are the soundtrack for America.
We're the oasis – the state where a little gets you a long way. Tennessee has the second lowest Cost of Living ranking in the nation. Memphis and Nashville's average home price is 63% lower than the average home price in Los Angeles, and 79% lower than the average home price in New York.
Come and join the movement, where the community is the network, and craftsmanship is the way of life.
READY TO GET STARTED IN TENNESSEE?
When a company is ready to discuss their project, they get Bob Raines. Bob works with the music and entertainment companies that are interested in relocating, expanding or starting a business in Tennessee.


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Our team was originally formed in 1974 and for the last forty years we have been playing teams all over the world. The Princeton Athletic Club was previously a member of the Metropolitan New York Rugby Union, beginning in 1996.
Since 2012, the Club has been a full member of the Empire Rugby Football Geographic Union. We compete against teams in New Jersey, New York and Connecticut. In 2013, PAC Rugby was the EGU Champion and earned a trip to the USA Rugby Division II National Championship Series.
PAC Rugby finished the 2013 season in the Elite Eight of Men's Division II Rugby in the United States. Today we have over 100 worldwide members, with several certified coaches and referees on the roster. Will you be the next to join? Click the button below!
Join PAC Rugby
Who Can Be a Rugby Player?
Height: 5'2" to 6'10"
Weight: 130 lbs to 320+ lbs
Speed: Tortoise to Lightning Bolt
Athletic Background: Horseshoes to NFL
Rugby is filled with a diversity of positions and skill requirements, so almost anyone can play rugby at some level. Skills that you may already possess from other sports will help you, such as:
Basketball: Ball handling, jumping, and possession tactics
Soccer: Kicking, positioning, vision, and strategy
Football: Tackling, ball carrying, and leg strength
Wrestling: Grappling, strength, and endurance
PAC Rugby is always looking for new members.
If you're interested in joining the club, click the button below and fill out the form.
See you on the pitch!
To LEarn more, read the PAC rugby FAQ guide
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Sports is a common topic mostly among the guys. In America, the three biggest sports are baseball, basketball, and American football. Due to the popularity of these sports, I will have individual lessons for them, but I will not have individual lessons for other sports such as soccer, volleyball, etc. For this lesson however, I will briefly talk about most sports and the most common language used among each one.
"What do you like to do in your free time?"
"What sports do you like to play?"
"I like to play sports. It's good for my health and I think it's very fun."
"I like competitive sports because winning feels good."
"I like to play tennis and I like to swim."
"Jeff is pretty athletic so he picks up on sports real quick."
"If you need a girl to play, you should get Jessica. She's very athletic."
"I like to play basketball."
"Do you like to play basketball?"
This would also work for football, baseball, tennis, volleyball, soccer, and softball.
However, sports such as swimming, bowling, and golf do not use the word play. Here is how you would say it.
As you may have noticed, each of the sports that do not use play is the ones with an 'ing' at the end. So if the sport is primarily used with an 'ing' at the end, then do not use play with that sport name.


Valentine's Day was celebrated in style with a sold-out show blending writing, sculpture, and music by these esteemed Twin Cities artists. Nor Hall presented a scintillating illustrated discursus on eros; Franz Kamin and fellow musicians performed "Coilular Angel;" and Harriet Bart read from her new artist's book, PUNICA GRANATUM: A Symposium on the True Nature of the Pomegranate & the Myth of Aphrodite.
The book launch reading and reception for Dobby Gibson's debut book of poems, Polar, was a great success with standing-room-only poetry enthusiasts packing the newly relocated Rogue Buddha Gallery for a taste of Gibson's perceptive and humorous take on American life. A great time was had by all!
Two fantastic West coast poets read to a rapt crowd on a blustery spring day. Rusty Morrison read from her first collection of poems, Whethering, "agile lines that canyon-open" (Forrest Gander). Gillian Conoley read from her fifth collection called Profane Halo, where "out of old beliefs a new language speaks" (Barbara Guest).
Internationally renowned writer Paul Auster read a stunning prose poem from his new collection, Collected Poems, and then proceeded to discuss his career in writing with Rain Taxi editor Eric Lorberer. If you missed this standing-room-only event, you may go to the Walker Art Center website and view the webcast.
Acclaimed experimental writer-raconteur Raymond Federman read from his latest meditation on memory, imagination, and the self, My Body in Nine Parts.
Co-sponsored by the Creative Writing Program, the French and Italian Departments, the Center for Holocaust and Genocide Studies, Jewish Studies, and the Institute for Advanced Studies.
Guest authors for this day-long celebration of books included Harvey Pekar, Audrey Niffenegger, Rick Moody, Ana Castillo, Chitra Banerjee Divakaruni, Siri Hustvedt, Alison McGhee & Pete Hautman, and Eliot Weinberger & Forrest Gander.
In her first appearance in the Twin Cities, acclaimed poet Alice Notley read from as yet unpublished work to a rapt audience. Notley, a New York School poet, now resides in Paris. Rain Taxi also celebrated the just-published Collected Poems of Ted Berrigan, which Notley edited along with Anselm and Edmund Berrigan, with a salon reading the following night.
Rain Taxi Review of Books turned ten this year, and we had to mark the occasion with a little shindig. Find out more about this event by clicking here!


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Q: Prompt a set of possible options Recent versions of Mathematica dynamically prompt a list of possible options. For example, when typing
Plot[x, {x,0,1}, PlotStyle->

After typing the arrow, Mathematica prompt a list Gray, Dashed, Thick for choice. How to define similar behavior for user defined functions? For example,
Options[myFun] = {myOpt -> value};
myFun[OptionsPattern[]] := 1;

How to prompt a set of possible options, like opt1, opt2, opt3 right after typing
myFun[myOpt->

A: Thanks for asking this question; I might not have discovered this customizable area without it.
The auto-completion option values are automatically loaded on Front End start from:
FileNameJoin[{$InstallationDirectory, "SystemFiles", "FrontEnd",
  "SystemResources", "FunctionalFrequency", "OptionValues"}]

This directory contains a series of Package (.m) files each with the name of a function, e.g. ArrayPlot.m.  The file name itself determines that this will apply to the function ArrayPlot.  It also contains an additional file that appears to apply to all functions: CommonOptions.m
The structure of each file is a list of Rules:
{Extension -> {"Automatic"}, Trig -> {"True", "False"}}

*

*The right hand side of each rule is always a list of Strings or an empty list {}

*Option values that are actual strings must be escaped: "\"string\""

*Option names must be Symbols (thanks Kuba)

A special Rule form exists for icons within the menu, e.g. from ArrayPlot.m:
PlotTheme ->
 {{"\"Web\"", "PlotTheme-ArrayPlot-Web.png"},
  {"\"Minimal\"", "PlotTheme-ArrayPlot-Minimal.png"},
  {"\"Detailed\"", "PlotTheme-ArrayPlot-Detailed.png"},
  {"\"Business\"", "PlotTheme-ArrayPlot-Business.png"},
  {"\"Marketing\"", "PlotTheme-ArrayPlot-Marketing.png"},
  {"\"Scientific\"", "PlotTheme-ArrayPlot-Scientific.png"},
  {"\"Monochrome\"", "PlotTheme-ArrayPlot-Monochrome.png"},
  {"\"Classic\"", "PlotTheme-ArrayPlot-Classic.png"},
  {"\"Default\"", "PlotTheme-ArrayPlot-Default.png"}}

Each of these icon files reside in:
FileNameJoin @ {$InstallationDirectory, "SystemFiles", "FrontEnd",
  "SystemResources", "Bitmaps", "Popups", "CodeCompletion", "Thumbnails"}

I have not checked to see if other paths are also searched.
As an example I created a new file foo.m in the OptionValues directory with the content:
{myOption -> {"Doc", "Grumpy", "Happy", "Sleepy", "Bashful", "Sneezy", "Dopey"}}

Now after (re)starting Mathematica:

redpajama_set_name: RedPajamaStackExchange


It is a copy made in a cinema using a camcorder or mobile phone. The sound source is the camera microphone. Cam rips can quickly appear online after the first preview or premiere of the film. The quality ranges from terrible to very good, depending on the group of persons performing the recording and the resolution of the camera used. The main disadvantage of this is the sound quality. The microphone does not only record the sound from the movie, but also the background sound in the cinema. The camera can also record movements and audio of the audience in the theater, for instance, when someone stands up in front of the screen, or when the audience laughs at a funny moment in the movie.
It is just a new source of the above quality.
A telesync (TS) is a bootleg recording of a film recorded in an empty movie theater, sometimes filmed using a professional camera on a tripod in the projection booth. The main difference between a CAM and TS copy is that the audio of a TS is captured with a direct connection to the sound source (often an FM microbroadcast provided for the hearing-impaired, or from a drive-in theater). Often, a cam is mislabeled as a telesync. HDTS is used to label a High-definition video recording.
A copy captured from a film print using a machine that transfers the movie from its analog reel to digital format. Telecine has basically the same quality as DVD, since the technique is the same as digitizing the actual film to DVD. However, the result is inferior since the source material is usually a lower quality copy reel. Telecine machines usually cause a slight left-right jitter in the picture and have inferior color levels compared to DVD. HDTC is used to label a High-definition video recording.
R1 and R2 are considered the best quality.
HDRip is an encoded version of any HD source, like BRRip, BDRip or HDTV, into a smaller file size.
HDTV Rips often come from Over-the-Air transmissions. It is the HD recoding of the movie displayed on TV by a cable or satellite TV service. With an HDTV source, the quality can sometimes even surpass DVD. Some advertisement and commercial banner can be seen on some releases during playback.
This is a file losslessly ripped from a streaming service, such as Netflix, Amazon Video, Hulu, Crunchyroll, Discovery GO, BBC iPlayer, etc. This is also a movie or TV show downloaded via an online distribution website, such as iTunes. The quality is quite good since they are not re-encoded. The video (H.264 or H.265) and audio (AC3/AAC) streams are usually extracted from the iTunes or Amazon Video and then remuxed into a MKV container without sacrificing quality. An advantage with these releases is that they mostly have no network logos on screen.


After much speculation with regards to just what the legendary Metalheadz would select to mark their 100th release, the label have now officially confirmed that it will be a track from head honcho Goldie. Entitled 'Freedom', it features vocals from Natalie Duncan, a young musician he mentored in last year's BBC TV programme Goldie's Band – By Royal Appointment.
'Freedom' will be released on Metalheadz on 2nd April.


The team at Automotive Recruitment Ltd is extremely well connected with individuals from the Middle East (Dubai, Doha Qatar, Kuwait, Saudi Arabia, Oman and Sri Lanka). The depth and breadth of these networks provides access to quality candidates who are highly skilled with many years of franchise dealership experience. We also have links to schools & associations within these countries and we utilise these partnerships to tap into an even greater pool of talent.
As we are 'in' the migrant community, we have a vested interest in the success of the placements we make and we maintain regular contact & engagement with the candidates we assist. Similarly, the candidates we place are appreciative of our assistance and work hard to ensure they don't let us down, which increases their commitment and loyalty to their new employer.
In the two years we have been operating, we have assisted large number of migrants to secure employment in NZ. This track record of successful delivery means we have become a trusted partner of many large automotive dealerships within NZ and they now turn to us when they need highly skilled candidates.
We are also credible within the Middle Eastern community and often receive candidate referrals because we are the "go to" partner for skilled automotive professionals who are keen to immigrate to NZ.
We know the business impact of being short-staffed, and therefore understand the urgency around recruitment. We do everything within our power to minimise delays and remove the hassle from recruitment, therefore giving our clients more time to focus on other aspects of their business. Our relationships with licensed immigration lawyers and in-depth knowledge of the immigration process simplifies the paperwork trail and saves time & money for our clients.
Our recruitment fees are only payable on the successful completion of a placement, therefore if a company chooses not to employ a candidate presented to them by Automotive Recruitment Ltd, they pay nothing. There is zero risk for our clients.


Solukhumbu: Two persons were killed and five others injured critically on Sunday after a plane collided with helicopter at Tenzing-Hillary airport in Nepal.
The helicopter was stationary at the airport when the incident occurred, reports said .The Tenzing-Hillary airport comes under Solukhumbu district in Nepal.
Media reports said the Summit Air plane was taking off for Kathmandu from the Lukla airport in the district.Officials said the injured including a police personnel were airlifted to Kathmandu for treatment.


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'Netflix correct your mistake' is trending on Twitter as fans vent about the cancellation of 'Warrior Nun'
The Netflix logo is seen on in this illustration photo in Warsaw, Poland on 12 October, 2022.
Photo by STR/NurPhoto via Getty Images
Netflix canceled its fantasy drama series "Warrior Nun" in December, and fans are not happy.
They have taken to Twitter to slam Netflix's decision with the hashtag #savewarriornun.
This snowballed into "#NETFLIX CORRECT YOUR MISTAKE" trending on Twitter.
Angry fans of "Warrior Nun" — a popular Netflix show that was scrapped after two seasons — have taken to Twitter to express their ire, and now "#NETFLIX CORRECT YOUR MISTAKE" is trending on the social media platform.
"Warrior Nun," a show about a young girl who wakes up in a morgue with superpowers and is tasked with fighting demons on earth, was canceled by Netflix in December, per Variety.
In response, angry fans called out Netflix for ending shows before they reach a coherent ending. In this case, Warrior Nun's season two ended with a cliff-hanger, just a month before the show's cancellation.
As of Wednesday evening Singapore time, "Netflix correct your mistakes" has garnered over 31,900 tweets. The hashtag #savewarriornun has been used over 5 million times since December 13.
And angry fans are not just tweeting their disappointment. Over 108,000 people have signed an online petition on Change.org to renew "Warrior Nun" for its third season.
The show's creator, Simon Barry, tweeted on January 6: "Holy Halo. 5 MILLION #SaveWarriorNun tweets since Dec 13. I am in awe of this fandom. Thank you!!"
Henry T. Casey, a senior editor at Tom's Guide, an online publication that reviews tech products, tweeted: "Honestly, respect to the Warrior Nun fans. 'NETFLIX CORRECT YOUR MISTAKE' is a hell of a phrase to pick and get trending."
Once the hashtag started trending, fans of other canceled shows started piggybacking on the phrase — fans of Netflix's serial-killer show "Mindhunter," animated sci-fi sitcom "Inside Job," and teen drama "The Society" have since joined the Twitter conversation.
Protesters also dug up an old Netflix tweet from 2017, in which the streaming service appeared contrite about ending the sci-fi drama "Sense8" before it's ending.
"We don't like leaving a story unfinished. We learned a lot from Sense and we're going to try not to do this in the future," Netflix tweeted.
← Michael Novakhov retweeted: Guerre en Ukraine : le ministre de l'Intérieur ukrainien tué dans le crash d'un hélicoptère près de Kiev, 18 morts dont deux enfants à déplorer #Ukraine #GuerreEnUkraine rtbf.be/article/guerre… → Dissent Episode One: Tipping the Balance


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Florida Emergency Medical Care Rated Below Average
When it comes to emergency medical care, when split-second decisions can mean the difference between life-and-death, it's imperative that hospitals establish strong practices and protocols to allow health care professionals to do their job effectively.
Unfortunately, Florida has been given a barely passing grade in terms of the overall state of its emergency care system, per the American College of Emergency Physicians' Emergency Care Environment Report Card. Florida was given a C- overall, having dropped a few points from five years ago.
West Palm Beach medical malpractice attorneys understand that while the state has developed strong disaster preparedness plans and many hospitals have made strides in terms of patient safety, the state is plagued by a health care workforce shortage. There are also major financial barriers to care and we have a limited hospital capacity.
Researchers called the health care workforce shortage in Florida "severe," which heightens concerns about medical malpractice incidents. Providers who who are fatigued and stretched thin are more prone to making avoidable mistakes. In an emergency care setting, that can be deadly.
Florida has a particular shortage of emergency physicians, neurosurgeons, ear, nose and throat specialists, orthopedists and registered nurses.
Especially troubling, Florida ranks very last in the country for children's accessibility to health care providers.
This is compounded by the fact that there has been a lack of Medicaid expansion in the state, and we already had one of the greatest needs for additional primary care providers in the country. That need is only growing as our population expands.
What has also been a major problem is the lack of psychiatric care beds, which are just 13.3 per population of 100,000. This means that those with psychiatric problems may have those illnesses untreated, which contributes not only to the decline of mental and physical health for the individuals themselves, but also can have a negative impact on society overall in terms of crime and devotion of emergency services that might be better used elsewhere.
With regard to emergency departments, where there are just 8.1 beds per 1 million people. This contributes to extremely long wait times, averaging some 315 minutes (or 5 hours and 15 minutes) from the time someone arrives until the time they leave.
And even when they do receive prompt treatment, there is no guarantee that hospitals will have the necessary medications to treat them. The report indicates that there is a "severe" medication shortage in Florida, both in pre-hospital and emergency care settings.
While the state received an overall C-, it received an F in terms of Access to Emergency Care, ranking 49th in the country. In terms of Public Health and Injury Prevention, we received a D+. And while we received a C+ in terms of Quality and Patient Safety, that reflected a significant drop from the A- grade the state received in its 2009 report card.
Researchers recommended that Florida work harder to recruit, train and retain all types of health professionals, with a special focus on emergency physicians and specialists willing to be on-call in emergency departments.
It's also recommended that emergency departments develop a uniform system for pre-arrival instructions and that state field triage protocols align with guidelines from the U.S. Centers for Disease Control and Prevention.
West Palm Beach medical malpractice claims are handled by the Hollander Law Firm. Call 888-751-7770 for a free and confidential consultation. There is no fee unless we win.
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