text:
\section{Introduction}

The detection of GW170817 \citep{abbott2017a} and its optical counterpart
AT2017gfo \citep[e.g.][see \citealt{villar2017a} and references therein]{smartt2017a} confirmed the prediction that a kilonova would accompany the
merging of binary neutron stars (BNS) (\citealt{li1998a, metzger2010a}, see e.g. \citealt{metzger2019a} for a recent review).
The observations of a power-law luminosity decline consistent with r-process material and a sufficient event rate are consistent with binary neutron star mergers being the dominant site of
r-process element production in the Universe \citep{kasen2017a, drout2017a},
which had previously been proposed by some authors on theoretical grounds \citep{lattimer1976a, eichler1989a}.

Simulations of BNS mergers predict complex ejecta structures. The merger ejecta is comprised of material expelled on dynamical
timescales of tens of milliseconds, which is followed by secular ejecta expelled on timescales of seconds.
The dynamical ejecta typically have mass of
$10^{-4}$ -- $10^{-2}$ \ensuremath{{\mathrm{M}}_{\odot}}\xspace, and high ejecta velocities,
typically 0.2 -- 0.3c  \citep[e.g.][]{bauswein2013a, hotokezaka2013a, tanaka2013a, kruger2020a, radice2018a,ardevol2019a}.
The secular ejecta, i.e. the material unbound on longer time scales, are typically more massive
($10^{-2}$ -- $10^{-1}$ \ensuremath{{\mathrm{M}}_{\odot}}\xspace) and ejected with lower velocities
of $\sim$0.1c \citep[e.g.][]{fernandez2013a, perego2014a, just2015a, fujibayashi2018a, siegel2018a}.

The ejecta are predicted to have low lanthanide fraction material
in the polar directions, where there is a lower neutron abundance,
corresponding to electron fractions of $Y_{e} \gtrsim 0.3$, which would lead to low opacities and therefore `blue' colours in the predicted kilonova.
Higher lanthanide fractions are expected in the equatorial directions,
where there is a higher neutron abundance ($Y_{e}$ $\lesssim 0.3$)
which would lead to higher opacities and `red' colours in the predicted kilonova \citep[e.g.][]{metzger2014a, sekiguchi2015a, just2015a, perego2014a, foucart2020a, radice2022a}.

The observations of the kilonova AT2017gfo initially showed blue colours
with the spectra peaking in the UV/blue,
which rapidly evolved to redder colours with spectra peaking in the near-infrared \citep[see e.g.][]{smartt2017a, villar2017a}.
It has been suggested that to explain this rapid colour evolution,
the outermost layers of the merger ejecta must be composed of
low opacity, high $Y_{e}$ material (which would lead to low lanthanide
fraction material), while the inner ejecta layers require higher opacity,
low $Y_{e}$ material (high lanthanide fraction) to reproduce the red colours \citep[e.g.][based on the analytical two compnent model introduced by \citealt{metzger2017a}]{cowperthwaite2017a, villar2017a}.

Initial progress in this field has relied on the use of
analytic ejecta models that are described by e.g., power law density structures
or idealised geometries \citep[e.g.,][]{metzger2010a, barnes2013a, watson2019, banerjee2020a, even2020a, domoto2021a, heinzel2021a, korobkin2021a, wollaeger2021a, pognan2022a}.
Kilonova studies based on parameterised ejecta configurations avoid the complexities connected to hydrodynamics modelling, while other aspects, such as thermalisation (e.g. \citealt{barnes2016a}) can be studied in more detail.
Ultimately, however, a reliable interpretation of future multi-messenger observations of BNS will require kilonova models to be based on self-consistent simulations of the merger and its ejecta.

Of the studies that have considered simulated ejecta from BNS mergers,
these have mostly carried out radiative transfer simulations in
1D
\citep[][]{curtis2021a, gillanders2022a, wu2022a}
and 2D \citep[][]{kasen2015a, kawaguchi2021a, just2022a, kawaguchi2022a, klion2022a},
although we note some of these were based on 3D merger simulations \citep[e.g.][]{kawaguchi2021a, just2022a}.
3D radiative transfer calculations have been carried out by \citet{tanaka2013a},
but for axisymmetric merger data, and by \citet{neuweiler2022a}.
\citet{bulla2021a} and \citet{nativi2021a} have carried out 3D radiative transfer simulations
for the 3D merger simulation of a BH-NS system, and for a 3D simulation of neutrino-driven winds from a neutron star merger remnant, respectively.

In this paper, we carry out radiative transfer simulations for
merger ejecta extracted directly from a BNS
simulation.
Our hydrodynamic simulation does not only self-consistently provide the density distribution of the dynamical ejecta, but also -- thanks to its sophisticated neutrino treatment -- the electron fraction, which determines the r-process composition and therefore the energy powering the kilonova,
as well as the opacities.

\section{Methods}

\subsection{Hydrodynamical Model}
\label{sec:model}

The model we consider in this paper is of the dynamical ejecta
produced from the merger of binary neutron stars.
The merger simulation was carried out using
a 3D general relativistic smooth-particle
hydrodynamics (SPH) code \citep{oechslin2002a,bauswein2013a},
and an advanced neutrino leakage treatment, ILEAS \citep[Improved leakage-equilibration-absorption scheme][]{ardevol2019a}.
As a first step,
we consider equal mass neutron stars, each of 1.35 M$_\sun$
(gravitational mass for an orbit with infinite separation),
and each with 150000 SPH particles, using the SFHo equation of state
\citep{steiner2013a}. Hence, the chosen setup represents a system well compatible with GW170817 considering its mass and equation of state.
The stars were placed on an orbit with a separation of $\sim$38~km and we assumed no intrinsic spin of the stars.
The stellar matter was initially cold and in neutrinoless beta-equilibrium.
The simulation was evolved until 0.02 seconds after the time when both stars first touched. The calculation thus only covers the early dynamical mass ejection, while considerable amounts of ejecta may still be produced on longer time scales. The system did not collapse to a black hole within the timescale of the simulation.
For the given mass and equation of state a delayed gravitational collapse may be expected.

\subsubsection{Mapping SPH particles to a grid}
\label{sec:mappingparticles}

The SPH particles from the merger simulation
must be mapped onto a Cartesian grid for the radiative transfer simulation.
We first propagate the particles based on the velocities they had
at the end of the SPH simulation for a further 0.5 seconds.
After this time we assume homologous expansion
and map the particle positions onto a 128$^3$ Cartesian grid spanned in velocity space.
We set the maximum absolute velocity of the velocity grid (i.e. the grid boundary)
equal to 0.5c (along each axis, noting that the corners of the Cartesian grid extend to velocities up to 0.87c).
The bulk of the ejecta mass is well below this velocity.
Few SPH particles are at velocities higher than 0.5c, corresponding to 5\% of the total ejecta mass,
and we do not expect
these high velocity particles at very low densities to
have a strong influence on the predicted light curves at the times we consider in our simulation.
We map the density and $Y_e$ of the SPH particles to the Cartesian grid. The mapping of a quantity $A$ is performed via
\begin{equation}
    A(r)=\frac{1}{N}\sum_a A_a \frac{m_a}{\rho^*_a}W(|r-r_a|;h)
\end{equation}
with the sum running over all particles $a$, whose kernel function $W$ is finite at the position $r$. Here $A_a$ is the value of A associated with particle $a$, $m_a$ is the particle mass, $\rho^*_a$ is the conserved rest-mass density, $r_a$ is the position of particle $a$,
$W$ is the SPH kernel function with smoothing length $h$. $N$ is introduced for normalization and is defined by $N=\sum_a \frac{m_a}{\rho^*_a}W(|r-r_a|;h)$. For the density we do not use the normalization but compute $\rho(r)=\sum_a m_a W(|r-r_a|;h)$ (this expression includes an additional approximation, namely equating $\rho$ and $\rho^*$).
For the mapping, we adopt the smoothing length and smoothing kernel from the SPH simulation.
In order to reduce the clumpiness of the outermost ejecta (likely related to the limited particle
resolution used in the underlying SPH simulation) we increase the smoothing length by 50\% for particles
with absolute velocities $v > 0.5$c.

\subsubsection{Dynamical ejecta}

\begin{figure*}
\centering

\includegraphics[width=0.75\textwidth]{figures/3Dplot-Ye.png}

\caption{3D rendering of the dynamical ejecta mapped to a Cartesian grid.
The v$_{\rm z}$ axis corresponds to the rotation axis (or polar axis) of the system and v$_{\rm z} = 0$ represents the equatorial plane.
For visual purposes, in this figure we do not show grid cells containing density contributions from less than 5 SPH particles.
The colour scale is set by isosurfaces showing
the average $Y_{e}$ in a grid cell.
Material near the equator generally has a lower $Y_{e}$ than in the polar directions.
}

\label{fig:ejecta_3D_Ye}
\end{figure*}

\begin{figure}
\centering
\includegraphics[width=0.4\textwidth]{figures/massye_hist.pdf}

\caption{Distribution of ejecta mass (of all SPH trajectories) into electron fraction bins ($\Delta$$Y_e=0.04$) (blue),
    and separated into polar (red) and equatorial regions (green).
    The electron fraction near the poles is generally higher than near the equator.
}

\label{fig:Ye-mass}
\end{figure}

\begin{figure}

\includegraphics[width=0.5\textwidth]{figures/Ye.pdf}

\caption{Electron fraction ($Y_e$) in each model grid cell on the Cartesian grid, plotted against absolute velocity.
We mark the average $Y_e$ within 10 uniform angle bins to indicate angle dependence.
We note that due to the low resolution of the outer ejecta, at high velocities we find that one SPH particle can influence the $Y_e$ of many grid cells
(shown in this plot by a line at the same $Y_e$ for a range of velocities).
}

\label{fig:Ye-everycell}
\end{figure}

\begin{figure}

\includegraphics[width=0.48\textwidth]{figures/rho.pdf}

\caption{Cell mass densities (on the Cartesian grid) versus absolute radial velocity
at 0.52 seconds after the merger, corresponding to the time at which SPH particles are mapped to the
Cartesian grid and homologous expansion is assumed.
The average densities in ten polar angle bins have been plotted in colour to indicate the density range along different lines of sight.
The outer ejecta are less well resolved numerically, leading to scatter in the densities at high velocities.
}

\label{fig:rho-everycell}
\end{figure}
The ejecta is resolved by $\sim$2000 SPH particles, which become unbound during the simulation
(see \citealt{oechslin2002a,bauswein2013a} for ejecta criterion).
The total mass of dynamical ejecta mapped onto the radiative transfer grid was 0.0051 \ensuremath{{\mathrm{M}}_{\odot}}\xspace \ (although we note that mass ejection through different mechanisms still continues after the end of the merger simulation).
In Figure~\ref{fig:ejecta_3D_Ye} we show a 3D rendering of
the dynamical ejecta once it has been mapped to the grid, indicating the 3-dimensional structure
produced by the merger simulation.
The colour scale indicates the $Y_{e}$ of the ejecta (where $Y_{e}$ is defined at the end time of the merger simulation).
Generally, lower $Y_{e}$ material is found near the equator,
while higher $Y_{e}$ material is found in the polar directions.
This is demonstrated by Figure~\ref{fig:Ye-mass},
showing the $Y_{e}$ of the trajectories at the end of the SPH simulation.
The trend of drecreasing $Ye$ from the pole to the equator is consistent with previous works,
e.g. \citet{radice2018a, foucart2020a, kullmann2022a}.
However, we also find that lower $Y_{e}$ material is mixed with the
higher $Y_{e}$ material in the poles (i.e. the polar directions are not
composed solely of high $Y_{e}$ material).
A similar effect was reported by \citet{just2022a}.
As a result we expect lower opacities in the polar directions, due to the lower lanthanide fraction expected to be synthesised for the lower $Y_{e}$ material.
The $Y_e$ mapped to the Cartesian grid is shown in
Figure~\ref{fig:Ye-everycell}.
To analyse the 3D density structure of the ejecta, we plot the density of each model grid cell
in Figure~\ref{fig:rho-everycell}.
To indicate the angular dependence, we divide the ejecta into 10 uniform solid-angle bins in the polar direction
relative to the positive z-axis and plot the average density within
each angle bin.
Due to the limited resolution of the underlying SPH simulation, the outermost velocities
may suffer from purely numerical particle noise.
The impact of this particle noise will need to be assessed in future studies using a higher resolution.
While we would expect there to be some difference in the densities in each polar
direction due to statistical fluctuations,
we can not rule out that the relatively large difference
in density between the poles in this model could be numerical.

\subsection{Nucleosynthesis Calculations}

To obtain the energy released by the merger simulation,
time dependent nucleosynthesis calculations are carried
out for each SPH particle trajectory.
The simulation provided thermodynamical histories for all the SPH
particles only up to $t_0 \sim 20$~ms after merger. For later times,
we extrapolate the density evolution assuming homologous expansion,
i.e.\ $\rho(t) r(t)^3 = \rho_0 r_0^3$ and $r(t) = r_0 + v_0 (t-t_0)$
with the subscript $0$ denoting the end of the simulation data. This
corresponds to a density evolution as:

\begin{equation}
  \label{eq:rhot}
  \rho(t) = \rho_0 \left(\frac{\Delta+t_0}{\Delta+t}\right)^3,
\quad \Delta = \frac{r_0}{v_0} - t_0.
\end{equation}
We start the nucleosynthesis calculations at a temperature of $T=10$~GK or the lowest
temperature reached in the SPH simulation if this is higher. Under these
conditions our initial composition is well described by nuclear
statistical equilibrium.
During the nucleosynthesis calculations, the
density is evolved based on the SPH simulation data together with
equation~(\ref{eq:rhot}). We use the same nuclear reaction network
as in \citet{Mendoza-Temis.Wu.ea:2015} together with the set of
nuclear reactions labelled ``FRDM''. Briefly, it consists of
neutron-capture and photodissociation rates computed within the
statistical model using the FRDM
masses~\citep{Moeller.Nix.ea:1995}. For nuclei with experimentally
unknown $\beta$-decay rates, we use the compilation of~\citet{Moeller.Pfeiffer.Kratz:2003}.
Fission rates~\citep{Panov.Korneev.ea:2010} have been computed based on the
Thomas-Fermi fission barriers of \citet{Myers.Swiatecki:1999}.
Finally, $\alpha$-decay rates
are computed using a Viola-Seaborg formula~\citep{Dong.Ren:2005} for
those nuclei without experimental values.
We use the $Y_e$ value at the end of the SPH simulation to determine the composition at
the beginning of the network calculations.

In Figure~\ref{fig:trajectoriesQdot}
we show the specific heating rate, $\dot{\mathrm{Q}}$,
averaged over all trajectories.
$\dot{\mathrm{Q}}$ represents the total rate of energy released into the ejecta from nuclear reactions (including the contribution from neutrinos).
Also plotted are the average energies released
from $\beta$-decays and $\alpha$-decays.
Fission also contributes to the total energy released,
although the contribution is orders of magnitudes less than
$\beta$-decays and $\alpha$-decays by $10^{-3}$ seconds,
and is most significant at very early times.
Energy from $\beta$-decays accounts for most of the total
heating rate in the time range considered here.

\begin{figure}

\includegraphics[width=0.48\textwidth]{figures/heating.pdf}

\caption{Heating rates from nucleosynthesis calculations. The total energy
released (on average for all of the trajectories) is shown by the dashed line.
We also show the total energy from $\beta$-decays and from $\alpha$-particles.
}

\label{fig:trajectoriesQdot}
\end{figure}

\subsection{Radiative transfer}
\label{sec:rad_transfer}

We use the time-dependent, multi-dimensional
Monte Carlo radiative
transfer code, \textsc{artis} \citep[][based on the methods of
\citealt{lucy2002a, lucy2003a, lucy2005a}]{sim2007b, kromer2009a}
to predict the kilonova from the neutron star merger
simulation described in Section~\ref{sec:model}.
We propagate $1.15 \times 10^8$ Monte Carlo packets between 0.02 and 120 days after the merger.
We produce viewing-angle dependent light curves by assigning escaping UVOIR-packets into time and directional bins.
The bin sizes have been chosen to keep Monte Carlo noise at a low level for the observables we present here.
We define 100 uniform solid-angle bins in the polar and azimuthal directions.

\subsubsection{Opacity treatment}

\begin{table}
\centering
\caption{Mass absorption cross sections ($\kappa$) adopted in this study for each electron fraction $Y_{e}$ range. The values are motivated by the Planck-mean opacities calculated by \citet[][table 1]{tanaka2020a}. These calculations assumed a temperature range of
5000 - 10000 K
and a density of $\rho = 1 \times 10^{-13}$ g cm$^{-3}$.
*The lowest $Y_{e}$ opacity is underestimated due to
lack of complete atomic data for actinides \citep{tanaka2020a}.
}

\begin{tabular}{lc}
\hline
$Y_{e}$                  & $\kappa$ \\
                    & cm$^2$ g$^{-1}$ \\ \hline
$Y_{e}$ $\le 0.1$        & 19.5*   \\
$0.1 < $ $Y_{e}$ $\le 0.15$ & 32.2    \\
$0.15 < $ $Y_{e}$ $\le 0.2$           & 22.3    \\
$0.2 < $ $Y_{e}$ $\le 0.25$          & 5.60     \\
$0.25 < $ $Y_{e}$ $\le 0.3$           & 5.36    \\
$0.3 < $ $Y_{e}$ $\le 0.35$          & 3.30     \\
$Y_{e}$ > 0.35                   & 0.96   \\ \hline
\end{tabular}
\label{tab:opacities}
\end{table}

We adopt a temperature independent grey-opacity treatment for the propagation of all radiation
(described by \citealt{sim2007b}).
We use $Y_{e}$ dependent grey absorption cross-sections, based on the
Planck mean opacities listed in table 1 of \citet{tanaka2020a}.
These mean opacities were calculated for temperatures of 5000 - 10000 K
(with $\rho = 1 \times 10^{-13}$ g cm$^{-3}$ at a time of 1 day).
Specifically, we use the opacities listed in Table \ref{tab:opacities}
for model cells with an average $Y_{e}$ within the ranges in Table~\ref{tab:opacities}.
We note that the $Y_e$ in each grid cell is based
on the $Y_e$ of the SPH particles at the end of the merger simulation (not the $Y_e$ evolved in the nuclear network calculation).

\subsubsection{Energy from nucleosynthesis calculations}

\begin{figure}

\includegraphics[width=0.48\textwidth]{figures/Q.pdf}
\includegraphics[width=0.48\textwidth]{figures/Q_times_mass.pdf}

\caption{Total energy deposited between 0.02 and 120 days versus radial velocity. Top: Deposited energy per unit mass. Bottom: Deposited energy per cubic grid cell (constant velocity extent in x-y-z). Mean values within polar angle bins are indicated in colour.
We note that due to the low resolution of the outer ejecta, at high velocities we find that one SPH particle can influence many grid cells
(shown in the upper plot by a line at the same energy for a range of velocities).
}

\label{fig:qdot}
\end{figure}

In \textsc{artis}, the total energy in the simulation
is defined at the start of the simulation.
We then create Monte Carlo packets of equal energy which
are propagated through the simulation grid.
We define what fraction of the total energy will be deposited in each model grid cell, and place packets according to this distribution.

We define how energy is distributed in the model grid cells
according to the total energy released by the SPH particle
trajectories that contribute to that model grid cell.
The total amount of energy released along a trajectory over time
is mapped to the 3D Cartesian grid using the same
method as described in Section~\ref{sec:mappingparticles}.
These energies are shown in Figure~\ref{fig:qdot}.
This energy (in erg/g) and the total mass in the model grid cell are used to set the total energy generated in each model
grid cell, and in the framework of the code, the fraction of energy which will be deposited in the cell
(also shown in Figure~\ref{fig:qdot}).

At the start of the simulation we also define the rate at which energy will be deposited (the time at which a Monte Carlo packet will be placed in a model grid cell).
We assume that the energy in all model grid cells
is deposited at the same rate, which we take as the
average $\dot{\mathrm{Q}}$ of all unbound SPH particle trajectories
(plotted in Figure~\ref{fig:trajectoriesQdot}).
We consider energy released from 8 seconds after the merger
($\ll$ start time of radiative transfer simulation) until 120 days after the merger.
Energy released before the start of the simulation
is accounted for by placing Monte Carlo packets in the ejecta
which are advected with the homologous flow.
The energy of these packets is reduced to account for
adiabatic losses before the beginning of the simulation.

Since $\beta$-decays are the dominant source
of energy at the times we are considering,
we assume that all of the energy in our simulations
comes from $\beta$-decays.
Following the results of \citet{barnes2016a},
we assume that 35\% of the $\beta$-decay energy emerges
as neutrinos, 20\% as $\beta$-particles and 45\%
as $\gamma$-rays.
The energy from the neutrinos will never thermalise,
so this energy is ignored in the simulations.

\citet{barnes2016a} find that low energy $\beta$-particles effectively
thermalise on kilonova timescales,
and that even slightly tangled magnetic fields are effective at
trapping high energy $\beta$-particles.
We assume that all of the energy from the $\beta$-particles
will thermalise locally and instantaneously.
In reality, the $\beta$-particles will continuously
deposit energy over some distance through Coulomb interactions
with thermal electrons, by ionising or exciting bound atomic
electrons or by Bremsstrahlung emission.
The thermalisation of $\beta$-particles
is dependent on the magnetic field structure
in the ejecta, which we neglect.

We include $\gamma$-ray transport in our simulations,
as described by \citet{sim2007b}.
We approximate the emission energies of the $\gamma$-rays guided by the
early time $\gamma$-ray emission spectra obtained by
\citet{barnes2016a} (see their figure 3),
which peaks at several hundred keV.
The exact energies sampled and the probability of injecting a gamma-packet at each energy are shown in Figure~\ref{fig:gammaenergies}.

\begin{figure}

  \includegraphics[width=0.45\textwidth]{figures/gammaenergies4.pdf}

\caption{Approximated probability distribution of $\gamma$-ray energies for
radioactive decays of r-process material, guided by the early time $\gamma$-ray
emission spectrum by \citet{barnes2016a}. This includes 115 energy bins, which are sampled to obtain $\gamma$ energies
used in this work.
}

\label{fig:gammaenergies}
\end{figure}

\section{Results}

\subsection{Dynamical ejecta}

\subsubsection{Bolometric light curves}
\label{sec:lightcurves}

\begin{figure}

 \includegraphics[width=0.5\textwidth]{figures/plotlightcurve.pdf}

 \includegraphics[width=0.5\textwidth]{figures/plotlightcurve_gamma.pdf}

\caption{Line of sight bolometric UVOIR light curves (upper panel)
and $\gamma$-ray light curves (lower panel).
Each coloured line is the azimuthally averaged light curve
(averaged over each angle bin in cos($\theta$)), while all 100 uniformly spaced
viewing angle bins are plotted in light grey.
When presenting the angle-dependent light curves, we plot them as equivalent isotropic luminosities (i.e. from the simulation we record the energy emitted per second into each sold angle bin to obtain light curves in  erg/s/sr for each orientation; we then scale these to an equivalent isotropic luminosity by multiplication by $4\pi \cdot$sr).
Also marked is the total energy released (on average) by nuclear reactions, $\dot{\mathrm{Q}}_{\gamma + \beta}$,
excluding the energy assumed to be lost to neutrino emission (35\%).
In the upper panel we additionally plot the energy due to $\beta$-particles ($\dot{\mathrm{Q}}_{\beta}$)
and in the lower panel the heating due to $\gamma$-rays ($\dot{\mathrm{Q}}_{\gamma}$).
The bolometric light curve of AT2017gfo from \citet{waxman2018a} is plotted
with the bolometric light curves for reference.
}

\label{fig:lightcurves}
\end{figure}

\begin{figure}

 \includegraphics[width=0.5\textwidth]{figures/plotviewinganglebrightnessat1days.pdf}

\caption{Bolometric (UVOIR) equivalent isotropic luminosities in 100 uniform viewing angle bins at 1 day after the merger.
}

\label{fig:brightness1day}
\end{figure}

The bolometric light curves for the dynamical ejecta are shown in Figure~\ref{fig:lightcurves}.
From very early times photons are able to escape the ejecta,
hence we find that the light curves begin declining within a fraction of a day,
and do not show a significant rising phase in our simulations.
According to the nucleosynthesis calculations, significant numbers
of $\beta$-decays will occur in the outer ejecta layers,
hence, in our simulations, energy is deposited
in low density, low opacity outer regions, where it thermalises,
and is emitted as optical radiation from very early times.
Since we assume that all $\beta$-particle energy thermalises,
this may overestimate the true amount of energy that would thermalise,
however, at such times the thermalisation efficiency is likely to be high \citep{barnes2016a}.
The lack of rise to peak in bolometric light curves has previously been
found, e.g. by \citet{banerjee2020a}, \citet{klion2022a} and \citet{kawaguchi2022a}.
The light curves do, however, show a `shoulder' at $\sim 1$ day,
particularly in the polar directions.
At this time, the ejecta are becoming optically thin, and energy stored in the ejecta is able to escape.
Photons are preferentially emitted in the polar
directions due to the lower optical depths
in these lines of sight (see Figure~\ref{fig:lightcurves}).
At times around 1 day after the merger, we find the strongest angle variation
in the light curves (see Figure~\ref{fig:brightness1day}), however this decreases over time
as the ejecta become optically thin.
As seen in Figure~\ref{fig:brightness1day}, the light curve also exhibits $\sim 30\%$ variations in azimuthal viewing angle,
likely reflecting that the ejecta do not show perfect cylindrical symmetry.

The heating rate marked in Figure~\ref{fig:lightcurves} shows the
angle-averaged, total
amount of energy available for heating the ejecta over time.
Since we assume all energy comes from $\beta$-decays in
our simulations, the heating rate represents
the total energy from
$\gamma$-rays plus $\beta$-particles from $\beta$-decays.
The energy lost to neutrino emission is excluded
from the heating rate shown in Figure~\ref{fig:lightcurves}.
Since $\gamma$-rays thermalise inefficiently (see Section~\ref{sec:gammalightcurves})
it is predominantly energy from $\beta$-particles
powering the light curve.
By $\sim 5$ days the ejecta has become optically thin,
and the light curve is equal to the $\beta$-particle heating rate.
At this time $\beta$-particles are no longer expected
to thermalise efficiently \citep[e.g.][although we note this was for a simplified ejecta structure]{barnes2016a}
and so the $\beta$-particle heating rate is likely overestimated
here.
However, energy from $\alpha$-particles becomes more
significant at these times.
Since the late time light curve is dependent on the assumed heating
rate, this highlights the importance of calculating
the fractions of $\beta$-decay energy going into
neutrinos, $\gamma$-rays and $\beta$-particles,
by following the radioactive decays
of r-process elements in the radiative
transfer simulations,
as well as calculating how much of that energy will thermalise.
Accounting for $\alpha$-particles, and the corresponding thermalisation efficiency of the decay products
is likely also important at late times.

For reference, the bolometric light curve of AT2017gfo,
constructed by \citet{waxman2018a}, is also plotted in Figure~\ref{fig:lightcurves}.
The mass of the dynamical ejecta in our model
is relatively small ($\sim$10 times less than e.g. the mass inferred for AT2017gfo by \citealt{smartt2017a}, using an Arnett-type model, of $0.04 \pm 0.01$ \ensuremath{{\mathrm{M}}_{\odot}}\xspace)
and therefore the total amount of energy produced in
our model is lower, leading to fainter, faster evolving light curves.

\subsubsection{$\gamma$-ray light curves}
\label{sec:gammalightcurves}

We also show the emerging $\gamma$-ray light curves in
each viewing angle bin in Figure~\ref{fig:lightcurves}.
For all except the earliest times, the $\gamma$-rays
do not thermalise and are able to free-stream out of the
ejecta.
By $\sim 0.1$ days the emerging $\gamma$-ray energy is equal
to the total $\gamma$-ray energy rate, marked in Figure~\ref{fig:lightcurves}.
The $\gamma$-ray light curves do not show a
viewing angle dependence.
To observe the peak of the $\gamma$-ray light curve, observations would
need to be within the first hour after the merger.

\begin{figure}
\centering

\includegraphics[width=0.5\textwidth]{figures/meanemissionvelocity-angles-arrivetime.pdf}

\caption{Mean ejecta velocity at which Monte Carlo packets
were last emitted within a given angle bin, indicating the ejecta velocity where packets last interacted.
}

\label{fig:emission_velocity_angle_ave}
\end{figure}

\begin{figure*}
     \begin{subfigure}[b]{0.35\textwidth}
         \centering
            \includegraphics[width=\textwidth]{figures/packets_hist_0.19d_xz_pktemissiontime.pdf}
            \caption{0.2 days}
    \end{subfigure}
     \begin{subfigure}[b]{0.35\textwidth}
         \centering
            \includegraphics[width=\textwidth]{figures/packets_hist_0.45d_xz_pktemissiontime.pdf}
            \caption{0.5 days}
    \end{subfigure}

     \begin{subfigure}[b]{0.35\textwidth}
         \centering
            \includegraphics[width=\textwidth]{figures/packets_hist_0.93d_xz_pktemissiontime.pdf}
            \caption{1 day}
    \end{subfigure}
     \begin{subfigure}[b]{0.35\textwidth}
         \centering
            \includegraphics[width=\textwidth]{figures/packets_hist_1.87d_xz_pktemissiontime.pdf}
            \caption{2 days}
    \end{subfigure}

\caption{The spatial distributions (slices at v$_{\rm y} = 0$) of last interactions of escaping radiation at three epochs.
Note packets can escape in any direction -- we make no selection based on escaping angle.
Packets that escaped representing $\gamma$-rays
are excluded from this.
}

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

\subsubsection{Ejecta emission velocities}

As discussed in Section~\ref{sec:lightcurves},
initially most of the photon emission occurs
in the outer ejecta layers,
hence we find that the bolometric light curves begin declining from
very early times and do not rise to a peak within the time frame of our simulation.
Figure~\ref{fig:emission_velocity_angle_ave}
shows the mean ejecta velocity at which
escaping Monte Carlo packets underwent their last interaction in the simulation -- this gives an indication of the regions of the ejecta that are contributing to the kilonova emission.
The outer ejecta layers quickly become optically thin,
due to the high expansion velocities.
As a result, the ejecta velocities from which packets are emitted decrease rapidly
within the first day.
We show the mean ejecta velocities from which packets are emitted
in Figure~\ref{fig:emission_velocity_angle_ave}.

We also show slices of the ejecta indicating where the
Monte Carlo packets escape from at a given time in Figure~\ref{fig:emission_velocity_grid}.
Initially, all packets are emitted from the outermost (i.e. fastest) ejecta.
Until around 1 day, this resembles a photosphere, beneath which radiation
does not escape the ejecta.

\subsubsection{Temperature}
\label{sec:temperatures}

\begin{figure}
\centering

\includegraphics[width=0.5\textwidth]{figures/arrive-time-meanemissionTR-angles.pdf}

\caption{
Average radiation temperature at the last interaction locations of escaping packets, indicating the ejecta temperatures where radiation is escaping from.
We also mark the inferred temperatures from the spectra of AT2017gfo by \citet{smartt2017a}.
}

\label{fig:emission_velocity_temperatures}
\end{figure}

\begin{figure*}

\includegraphics[width=0.9\textwidth]{figures/plotlightcurves.pdf}

\caption{Light curves estimated from radiation temperature.
Also plotted are the light curves for AT2017gfo from \citet{villar2017a}, assuming a distance of 40 Mpc.
We note that the light curves show some Monte Carlo noise.
}

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

The extremely high expansion velocities cause the temperature of the ejecta to drop rapidly.
We estimate the temperature in each model grid cell
by matching the energy density of the Monte Carlo radiation field
in the cell during each timestep to that of a black body radiation field:
we denote this equivalent black body temperature as T$\rm_J$.
We show the average temperatures of the model grid cells from
which packets are escaping
over time in Figure~\ref{fig:emission_velocity_temperatures}.
Specifically, we record the cell temperature where a packet last
interacted before escaping and bin the packets in time.
The mean temperature in each time bin is plotted.

The opacities we adopt from \citealt{tanaka2020a} (see Table~\ref{tab:opacities}) were calculated
for temperatures of 5000 - 10000 K.
In our simulations the temperatures are approximately in this range, at least in the regions from which packets escape,
between 0.1 -- 1 days.

At late times it is likely that we underestimate the temperature,
due to the grey and local thermodynamic equilibrium (LTE) approximations assumed here.
In the nebular phase, non-thermal processes
would provide heating to the ejecta \citep{hotokezaka2021a, pognan2022a} and likely prevent cooling to such low temperatures as suggested by our T$_{\rm J}$ estimate.

We also plot the mean ejecta temperatures at the location
of the last interaction of escaping radiation
(specifically, the temperature of the model grid cell where a packet last interacted before escaping),
binned by time
in Figure~\ref{fig:emission_velocity_temperatures},
and we show how the temperatures compare to the inferred
temperatures of AT2017gfo by \citet{smartt2017a}.
Although the model temperatures are cooler than
AT2017gfo by the time of the observations,
the evolution of the temperature is similar.
The cooler temperatures are likely due to the lower
mass of the ejecta model, and therefore the lower amount of energy generated in the ejecta,
as well the LTE assumptions made in our simulation.

\subsubsection{Colour curves from radiation temperature}

\begin{figure}

\includegraphics[width=0.45\textwidth]{figures/plotcolorevolutionH-K.pdf}

\caption{Angle-averaged colour evolution, estimated from radiation temperature. Also plotted are the
colours of AT2017gfo for points where observations were taken at the same time
    (i.e. we do not interpolate between light curve points).
    Note that Monte Carlo noise can be seen here.}

\label{fig:colourevolution}
\end{figure}

Our simulations use only grey opacities, so we do not
calculate any frequency dependence to produce
spectra or colour information from the Monte Carlo packets directly.
However, we record the temperature
of the grid cell where each packet
was last emitted from before escaping the
ejecta, i.e. the point at which the packet last
underwent an interaction (see Figure~\ref{fig:emission_velocity_temperatures}).
From this, we assign an approximate frequency to
the Monte Carlo packet by making the simplistic assumption that it is governed by the equilibrium radiation distribution (a black body function)
at the local radiation temperature, T$\rm_R$ (T$\rm_R$ = T$\rm_J$ under the LTE assumption).
We do this by randomly sampling a frequency from a
black body at the temperature in the model grid cell from which the packet escaped.
From this we obtain an approximate spectral energy distribution,
and can generate band-limited light curves,
which we show in Figure~\ref{fig:bandlightcurves}.

The elemental compositions of the kilonova ejecta are dominated by lanthanides and actinides,
which are very effective at line-blocking blue wavelengths,
and therefore we would expect that the true spectra would be redder
than a pure black body, particularly at later times \citep[e.g.][]{gillanders2022a}.
However, we would also expect the temperature evolution
to change in non-grey and non-LTE simulations, which would also affect
the colour evolution.
To accurately determine band-limited light curves,
frequency dependent simulations are required, which goes beyond the scope
of this work.

The light curves show an angle variation in magnitude of up to
$\sim$1 mag.
The emission from polar directions is brighter than from equatorial directions.
As discussed in Section~\ref{sec:model},
we have a higher $Y_{e}$, and therefore lower lanthanide fraction
in the polar directions,
which represents a `blue' component,
and a lower $Y_{e}$ in the direction of the equator,
which would lead to a higher lanthanide fraction,
representing a `red' component.
However, this does not lead to significantly
redder colours in the equatorial direction than the polar directions.
We show the angle dependent colour evolution in Figure~\ref{fig:colourevolution}, which does not show a significant
angle variation.

Due to the evolution of the temperature alone, we find that
the colours show a rapid evolution from blue to red over time
in all lines of sight,
which can be seen in Figure~\ref{fig:colourevolution}.

\subsubsection{Comparison to AT2017gfo}

We plot the light curves of AT2017gfo \citep[from][]{villar2017a} in Figure~\ref{fig:bandlightcurves}
for reference,
although again we note that the model we consider here is much
less massive than what was inferred for AT2017gfo, and therefore
we do not expect to match the brightness.
The light curves have been corrected for foreground reddening,
assuming an extinction of E(B-V) = 0.11 mag \citep{smartt2017a}.

Interestingly, the model light curves show a similar evolution
to AT2017gfo, although the model light curves are fainter
and evolve faster.
This could suggest that in future events where less mass is
ejected than in the case of AT2017gfo, the light curves
would show a faster decline and may have already faded
in the bluer bands by the time the first detections
of AT2017gfo were made.
The red bands, however, remain brighter for longer, suggesting that
searches for the electromagnetic counterparts of future kilonova events should
focus on these bands.
We note that the model H and K band light curves are likely too red,
since these are similar in brightness to AT2017gfo.
As discussed in Section~\ref{sec:temperatures},
due to our grey approximation we likely underestimate the
temperature at later times, which could be responsible for the
very red late-time colours.

The rapid blue to red colour evolution found for our model is similar to that observed for AT2017gfo (see Figure~\ref{fig:colourevolution}).
Since we only include dynamical ejecta in this simulation,
this shows that a late-time, high opacity component is not necessarily
required to explain the colour evolution shown by AT2017gfo,
as has been found by e.g. \citet{cowperthwaite2017a},
although we note that we do not claim there was no secondary component.
This suggests that the colour evolution could be driven by the cooling of the ejecta.
Future frequency dependent simulations will be required to
confirm this.

\subsection{Late-time ejecta}

So far, we have only considered the dynamical ejecta,
expelled on timescales of tens of milliseconds.
Now we investigate in an approximate manner the effects of ejecta expelled on longer timescales.

\subsubsection{Model for late-time ejecta}

\begin{figure}

\includegraphics[width=0.5\textwidth]{figures/rho_plus_torus+wind.pdf}

\caption{Same as Figure~\ref{fig:rho-everycell} but including the spherically averaged late-time ejecta. The densities of the late-time ejecta have been scaled (assuming homologous expansion) to match the time in Figure~\ref{fig:rho-everycell} of 0.52 seconds.
}

\label{fig:cell_densities_plus_late_ejecta}
\end{figure}

We base the density structure for the secular ejecta on
a simulation of a BH-accretion torus, which is formed after the collapse of the hypermassive neutron star.
The BH-torus model is similar to the models
of \citet{just2015a}, but includes a special relativistic treatment as well as additional, manually constructed ejecta components.
The components represent dynamical ejecta and a neutrino-driven wind from a hyper-massive neutron star (HMNS) as described by \citet[][see therein for more details]{ito2021a}.
The initial disk mass was 0.1 M$_\sun$, the mass of the HMNS wind was 0.006 M$_\sun$, the black hole mass was 2.7 M$_\sun$, and the assumed time of BH formation after the merger was 0.05 s.
The torus and wind components from the long term evolution simulation
are spherically averaged and then mapped to the 3D Cartesian grid (i.e. the dynamical ejecta component from this simulation is neglected).
In each cell of our Cartesian grid, we add the corresponding mass from the remnant simulation to the mass of the dynamical ejecta,
described in Section~\ref{sec:model}.
We do not use the $Y_{e}$ information from the remnant model, but keep the $Y_{e}$ and energy (per unit of mass) distributions
that were determined for the dynamical ejecta.
Any empty cells in the original dynamical ejecta model without a $Y_{e}$
(close to the centre where the bound remnant was removed)
are given a $Y_{e}$ of 0.5
and a total heating energy equal to the average heating rate of the
dynamical ejecta trajectories
(marked in Figure~\ref{fig:trajectoriesQdot}) integrated over time.
The additional mass of the late-time ejecta is 0.019 \ensuremath{{\mathrm{M}}_{\odot}}\xspace,
which gives a total ejecta mass of 0.024 \ensuremath{{\mathrm{M}}_{\odot}}\xspace.

In Figure~\ref{fig:cell_densities_plus_late_ejecta} we show
the model cell densities after including the mass
from the torus and wind ejecta.
Due to the very high central densities introduced by the
late-time ejecta model, significantly higher amounts of energy will be generated in the low velocity, central regions of the ejecta (since energy released is proportional to mass).
We therefore expect the light curve to be brighter
at late times when this energy diffuses out of the ejecta.

\subsubsection{Effect on light curves of late-time ejecta}
\label{sec:late-time-ejecta-lightcurves}

\begin{figure}
\includegraphics[width=0.45\textwidth]{figures/plotlightcurve-secularejecta.pdf}

\caption{Bolometric angle-averaged light curves for the model including the secular ejecta component and without.
When presenting the angle-dependent light curves, we plot them as equivalent isotropic luminosities (multiplied by $4\pi \cdot$sr).
We note that Monte Carlo noise can be seen in this plot.
}

\label{fig:lightcurves-angleave-secularejecta}
\end{figure}

We carry out a radiative transfer simulation on the model combining the late-time ejecta with the dynamical ejecta.
This simulation was carried out between 0.05 and 120 days with $2.88 \times 10^7$ Monte Carlo packets.

To demonstrate the effect of the late-time ejecta on the
bolometric light curve in comparison to the dynamical ejecta alone,
we plot the angle-averaged bolometric light curves of
each model
in Figure~\ref{fig:lightcurves-angleave-secularejecta}.
Due to the greater mass in the center of this model,
the increased energy generated in the high density inner regions
leads to a peak (or shoulder) in the bolometric light curve at $\sim 5$ days
after the merger, which was not produced by the dynamical ejecta
alone.
The increased energy thermalising
at low velocities and high optical depths
takes longer to diffuse out of the ejecta,
and we find a later peak in the bolometric light curve.
This highlights the necessity of long term hydrodynamic simulations,
since the late-time light curve is dominated by the lower velocity,
late-time ejecta.
At the same time, the small difference between the two cases at early times ($\lesssim 1$ day) suggests that the early light curve
may be dominated by the dynamical ejecta.

At late times (>10 days) the model light curve shows a slower decline than the observations of AT2017gfo.
This is likely due to our assumption that all $\beta$-particle
energy will thermalise at all times, and suggests that by these times the actual thermalisation rate is lower than we assume.

The late time light curve is now a similar brightness to AT2017gfo,
suggesting the mass of our model at low velocities may be similar
to that of AT2017gfo.
However, the relative faintness at early times indicates that our model
would require more mass at higher velocities to match the brightness
of AT2017gfo.

\subsubsection{Effect on mean emission velocities}

\begin{figure}
\includegraphics[width=0.45\textwidth]{figures/meanemissionvelocity_arrivetime.pdf}

\caption{Mean angle-averaged ejecta radial velocity ($v=rt$) of last interaction point of escaping radiation.
}

\label{fig:emission_velocity_secular_ejecta}
\end{figure}

We show the mean angle-averaged ejecta velocities at
which Monte Carlo packets are emitted from for
the simulations with and without the late time ejecta component
in Figure~\ref{fig:emission_velocity_secular_ejecta}.
At early times, the mean velocities are the same in both models,
but at later times the mean velocities
are much lower in the model with combined dynamical and late-time ejecta.
At these times the emission is primarily from the
low velocity, high density late-time ejecta component.

\subsubsection{Effect on light curve angle-dependence}

\begin{figure}
\includegraphics[width=0.5\textwidth]{figures/plotlightcurve-secularejecta-angles.pdf}

\caption{Line of sight dependent bolometric light curves for the model including the late-time ejecta component.
We note that Monte Carlo noise is visible in this plot.}

\label{fig:lightcurves-angles-secularejecta}
\end{figure}

We also show the angle-dependent bolometric light curves for the model with the late-time ejecta
in Figure~\ref{fig:lightcurves-angles-secularejecta}.
We note that the higher densities, and therefore larger amount of energy at low velocities, have slightly increased
the predicted variation with observation angle.
We find that the brightest lines of sight are still in the polar directions,
which have the lowest densities and lowest opacities,
and therefore we find photons are preferentially emitted in these directions.
The faintest lines of sight are those near the equator,
as these have the
highest densities and highest opacities.
The increased viewing angle dependence is due to
more packets of photons being generated at lower velocities
in the central regions of the ejecta.
Instead of the packets escaping quickly from the lower
density dynamical ejecta
(mostly in the line of sight where the packet was created),
the packets take longer to diffuse
out of the higher density material, but preferentially in the
polar directions since these have lower opacities,
which leads to the increased angle dependence.
This highlights the need for long-term evolution simulations,
and the need to include ejecta expelled on longer timescales.
Future simulations where the late-time ejecta are self-consistently
calculated are required.

\section{Discussion and conclusions}

In this paper we aimed to predict the kilonova emission
from the ejecta density and composition directly from a neutrino-hydrodynamics simulation of a binary neutron star merger.
Initially, we considered the dynamical ejecta alone,
which are expelled up to $\sim 20$ milliseconds after the merger.
We presented bolometric light curves, and found that we do not
expect a rise to peak within the time frame of our simulation (starting at 0.02 days). This is due to the distribution
of energy generated in the ejecta.
Energy is generated and thermalised at very high velocities
and due to low optical depths is able to immediately diffuse out
of the ejecta, leading to a bolometric light curve that begins declining
from very early times after the merger.
A similar result has previously been
reported, e.g. by \citet{banerjee2020a}, \citet{klion2022a} and \citet{kawaguchi2022a}.

We do however, find a `shoulder' in the light curve,
particularly in the polar directions, around the time when
the ejecta start to
become optically thin.
\citet{just2022a} predicted light curves for a similar model
to the dynamical ejecta model we consider here (they also consider a 1.35-1.35 M$_\sun$ model using the SFHo equation of state and the neutrino leakage scheme ILEAS).
They also find a `shoulder' feature at a similar time, although their shoulder luminosity is lower than ours by a factor of a few.

We find that light curves are brighter in the polar directions
around the time of the shoulder compared to the equatorial
lines of sight.
After the shoulder, once the ejecta become optically thin
we no longer see any angle dependence.
The angle variation is similar to the level found by \citet{just2022a} and \cite{kawaguchi2021a}.

We assumed that all energy came from $\beta$-decays.
We found that \mbox{$\gamma$-rays} are only thermalised within approximately the first hour after the merger.
The late time light curve (after the shoulder) closely follows the injected heating rate, since the ejecta have become optically thin.
In future simulations it will be important
to calculate the fraction of thermalised heating energy self-consistently.

We showed that in the day after the merger, most Monte Carlo packets of radiation were emitted
from the outer layers of the ejecta, which at early times resembles a photosphere.
This suggests that photospheric approximations may be reasonable
at early times.
We note that the angular dependence of this photospheric-like emission
(e.g. 0.5 days)
does not necessarily lead to strong asymmetries in the light curves
(i.e. the structure of the photospheric-like emission does not correspond to structure in the angle variation of the light curves).
Due to the high expansion velocities, the density of the ejecta
quickly decreases, as does the optical depth, leading to lower
emission velocities.
By $\sim$ 2 days we find packets are emitted from all velocities in the
ejecta, and the emission no longer resembles a photosphere.

The ejecta temperatures also rapidly decrease,
again due to the high expansion velocities.
Although we do not carry out frequency dependent simulations,
we estimate the frequency of escaping packets from the radiation
temperature in the cell from which the packet escaped.
We did this by sampling a black body distribution at the radiation
temperature.
We generated band light curves based on this, and showed that
due to the temperature evolution we find a rapid evolution from
blue to red colours, which is similar to that observed in AT2017gfo,
however, the evolution is on much shorter timescales.
This suggests that cooling of the ejecta could drive the colour evolution.
However, frequency dependent simulations of models including
self-consistently evolved late time ejecta will be required
to investigate this further.
Since this model was not tuned in any way to match the observations of AT2017gfo, it is promising that we find a similar colour evolution from our model with relatively simple assumptions.

We also carried out a simulation where we included,
in an approximate, spherically symmetric manner, ejecta expelled
from the merger remnant.
We investigated the effect on the predicted light curves,
and the extent to which dynamical
ejecta may be responsible for the observed light curve of AT2017gfo.
We found that the light curve at early times does not show a strong
sensitivity with respect to the late-time ejecta component,
although it becomes increasingly important with time.
After $\sim$1 day the light curve is dominated by the late-time ejecta
component, due to the higher densities, and therefore higher energy in the center
of the ejecta, which is able to diffuse out at later times.
The late time light curve is of similar brightness to that of AT2017gfo,
however, we still do no match the initial brightness.
This suggests that the higher masses of high velocity
ejecta to match the initial brightness of AT2017gfo.

We also showed that the viewing angle dependence does not disappear, and even increases, with the addition of a massive, spherically symmetric late-time ejecta. This suggests that the dynamical ejecta can have a significant impact on the angle dependence even at late times.
This highlights the importance of long-term evolution simulations
for predicting kilonovae.

 \section*{Acknowledgements}
We thank Ricard Ardevol-Pulpillo and Thomas Janka for providing the ILEAS scheme. CEC, AB and OJ acknowledge support by the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program under grant agreement No. 759253.
AB, G.M.-P and OJ acknowledge support by Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) - Project-ID 279384907 - SFB 1245.
AB and VV acknowledge support by DFG - Project-ID 138713538 - SFB 881 ("The Milky Way System", subproject A10). AB and G.M.-P acknowledge support by the State of Hesse within the Cluster Project ELEMENTS.
The work of SAS was supported by the Science and Technology Facilities Council [grant numbers ST/P000312/1, ST/T000198/1].
G.M.-P and LJS acknowledge support by the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (ERC Advanced Grant KILONOVA No. 885281).
This work was performed using the Cambridge Service for Data Driven Discovery (CSD3), part of which is operated by the University of Cambridge Research Computing on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk). The DiRAC component of CSD3 was funded by BEIS capital funding via STFC capital grants ST/P002307/1 and ST/R002452/1 and STFC operations grant ST/R00689X/1. DiRAC is part of the National e-Infrastructure.
OJ is grateful for computational support by the HOKUSAI computing facility at RIKEN.
CEC, OJ and VV are grateful for computational support by the VIRGO cluster at GSI.
NumPy and SciPy
\citep{oliphant2007a}, IPython \citep{perez2007a}, Matplotlib
\citep{hunter2007a}, PyVista \citep{sullivan2019pyvista} and \href{https://github.com/artis-mcrt/artistools}{\textsc{artistools}}\footnote{\href{https://github.com/artis-mcrt/artistools/}{https://github.com/artis-mcrt/artistools/}} were used for data processing and plotting.

\section*{Data Availability}

Data will be made available upon reasonable request.

\bibliographystyle{mnras}

redpajama_set_name: RedPajamaArXiv


The post discusses a simple monostable based power switch ON alarm circuit which automatically switches OFF after an adjustable preset delay. The idea was requested by Mr. Will Boswell.
Hi there, my name is Will Boswell. I am currently working on a project that involves adding an alarm sounder to an existing circuit, I shall try and explain as best possible.
The existing system is a warning light system whereby when the high voltage kit that I use is turned on, red beacon lights flash in order to warn those inside and outside of the testing area. These lights operate at 24V.
I would like to put a sounder in that sounds for 5 - 10 seconds when the system is turned on, in addition to the lights.
I was rather hoping that I would be able to just piggyback off of one of these lights for my supply but after my own research I have begun to get rather lost and it is a few years since I was at college!
So in a short summary, I am looking for some assistance in regards to having an alarm sound for 5 - 10 seconds every time the system is turned on / lights are activate.
Please any questions, just ask!
The requested power switch ON alarm circuit using a delay OFF circuit may be witnessed in the given diagram.
When power is switched on across the circuit, the 0.1uF capacitor momentarily grounds pin2 of the IC, sending an instantaneous triggering signal to the 555 monostable.
This immediately prompts the output of the IC to go high causing a toggling voltage to be activated for the attached relay.
The relay switches ON itself and the alarm unit connected with its N/O and the pole.
The alarm begins buzzing only until the relay shuts off automatically due to the featured monostable one shot characteristic of the IC 555.
The ON period of the relay or the IC output is determined by the values of the 100kresistor and caapcitor C. Different values for C may be tried in between 10uF and 100uF for achieving the closest possible duration of 5 to 10 seconds.
Hi there does this circuit: https://homemade-circuits.com/power-switch-on-alarm-with-auto-off/ reset when power is removed?
Thank you for getting back to me. Forgive my ignorance as I am a mechanical guy, but I have built this circuit and can't get it to work. Must the 0.1uf capacitor be of the ceramic type or can electrolytic also work? And capacitor C – can it be made bigger to achieve 30sec to 1 minute time?
the values of C and the 100k can be dimesioned as preferred by you for getting longer start ON delays.
Thanks Swagatam – I finally got to this circuit today: it works well. Thanks again for an excellent website!!
You are welcome Theuns, I am glad you coold make it successfully….
I have already answered your question with appropriate links, please check your previous comments.
Thanks for your quick reply. Sir, I already completed this circuit.in this circuit not having phase revers protection and no low , high voltage protection.pls help me.
If possible… I'll try to design them and publish in this blog soon.
Im using three phase motor, some time one phase fail. I want three phase preventer with time delay out put and phase revers , low voltage, high voltage detector. Please help me.
Suresh, you can try the following circuit which is a single phase preventer circuit only, without high, low cut off….make this first if it works as per the requirement, we can later on add the high/low cut off in it.


Matt Nagy? Is that pronounced Naggy? Are we sure on that? Not Naygee or Noggee? Maybe if Bears fans had heard more about him in the run-up to his hiring as head coach, they'd know for sure.
Guess they can just call him Coach Matt for now. There's plenty of time between now and the first opportunity to second-guess him to get that worked out.
The 39-year-old Nagy was hired Monday as the Bears' new coach, the 16th in team history, replacing John Fox. Born in Plainfield, N.J., Nagy grew up in Lancaster, Pa., and quarterbacked his Manheim Central High School team to back-to-back state finals in the mid-1990s. He went on to become a record-setting quarterback at the University of Delaware and played six years in the Arena Football League. Most recently, he was an assistant under highly regarded coach Andy Reid with the Kansas City Chiefs.
Chicagoans love nothing more than to rally around a Bears coach. If, unlike his crotchety predecessor, he has a reasonably engaging public persona, comes across as candid and genuine and, of course, wins more often than not, Coach Matt will be a household name soon enough.
It's not as though Nagy is a complete unknown or was ignored in coverage of coach casting. Nagy was reported to be in the mix to potentially replace Fox as far back as a month ago, when many in the media still hedged on the inevitability of Fox's dismissal.
NFL Network reported Tuesday that the Bears had requested the Chiefs' permission to talk with him, which they did over the weekend. Nagy's run as the Chiefs' offensive coordinator ended when the defense failed to hold a 21-3 halftime lead Saturday against the Titans to get bounced from the playoffs.
Given the sheer volume of reporting, analysis and commentary devoted to how the Bears would fill their coaching vacancy, however, fans shouldn't have been as surprised by his hiring as they seemed to be.
Nagy seemed just another name as the Patriots' Josh McDaniels, the Vikings' Pat Shurmur and the Eagles' John DeFilippo, along with Bears defensive coordinator Vic Fangio, dominated chatter.
Nagy's credentials were solid, and his story — that of a guy who eight years ago gave up a secure job in real estate for a chance to remain in football — had its own pull. But he wasn't cast as a consensus front-runner by any means.
Even Michigan's Jim Harbaugh, whom no one actually expected to entertain the Bears opening, probably had his name come up more often, if only because people enjoyed the fantasy.
As so often happens in coverage from Halas Hall, where the franchise has become better known for being opaque than its T formation, it was hard to know what exactly the brain trust was thinking and harder still to know what it would do.
That fuzziness has only been compounded by the fact Bears general manager Ryan Pace is still establishing a predictive track record. He remains hard to chart.
It's the same dilemma that had most analysts as blindsided as newly signed quarterback Mike Glennon last April when the Bears drafted quarterback Mitch Trubisky.
The need to help Trubisky develop and for the Bears to tailor their game plan to him correctly pointed observers toward coaches with offensive backgrounds.
Trubisky, though, is far from the only thing Nagy needs to develop in his new job.
Nagy, who doesn't have to be Mike Ditka but better not be Marc Trestman or John Fox, needs to help reinvigorate a fan base that still watches games on TV but eats pricey tickets rather than show up at Soldier Field.
These are die-hards who have grown weary of a head coach unwilling or unable to explain to fans what's really going on.
Chicagoans no doubt would celebrate a confident, competent, personable Bears coach capable of making the winters a little more tolerable and the football seasons extend to February.
Some football smarts and energy, along with his background in sales, would give Coach Matt a pronounced edge in making a name for himself locally.
If he wins, of course.


Kerio Connect does have harvest attack protection. The setting is in the SMTP server Security Options tab. I think that Kerio Connect should have more granular settings for password guessing. That would help with what you described above. Also, you could block these IPs on your firewall if it is capable of that function. I have my own servers setup to only allow port 25 connections from our spam filter. Therefore, all unauthorized incoming port 25 connections are refused. That guards against spammers and attackers who bypass MX record lookups and target the mail server directly.


text:
Health Workers Strike: NSHA Appeals For Special Scholarship To Indigenous Medical Students
The Nasarawa State House of Assembly, has urged the state government to initiate special scholarship for the state indigenous medical and other science related courses students to encourage them in their studies to boost the health manpower of the state in the long runThis,the assembly said would go a long way in boosting the capacity of the state indigenous doctors,pharmacists and other health professionals who will have the health interest of the people of the state at heart not like the non indigenes doctors and other health professionals who always embarked on strike without due considerations.Rt. Hon Ibrahim Balarabe Abdullahi, the Speaker of the House made the call after Hon Usman- Labaran Shafa(APC Toto/Gadabuke)the Chairman, House Committee on Health raised the issue under matters of public interest during the House proceedings in Lafia today.The speaker said that if the state government encouraged the indigenous students to read medicines and other science related courses via provision of special scholarship to them it will go a long way in addressing a lot of problems associated with health workers strike in the state." I want to thank Hon Shafa,the mover of this motion and all of you for contributing positively on this important matter of the health of our people." When I heard about the health workers strike by the state and local government workers, I immediately directed the House committees on Health and Local government respectively to intervene and resolve all their differences amicably." The health workers at the local government level suspended their strike by reasoning with us as most of them are our indigenes while those at the state level refused to suspend their strike despite the house intervention,our fathers the traditional rulers also intervened and the state government through the deputy Governor who is their colleague also spoke to them severally on the matter but they refused.I was surprised even with the threat of COVID 19."I am not saying that doctors and other health workers should not be giving what belongs to them or that they should not pursue their rights no,I am saying that they should be considerate and have human feeling as they took oath to protect lives and strike should be the last option not first option"" Honestly, I have agreed with all the contributions made by all of you by passing the following resolutions to the effect that -" 1,The state government as a matter of urgency initiate the establishment of medical school in the state, particularly at the state owed university, Keffi and to encourage our indigenous students to read medicines and other science related courses to serve our people."2.The state government is encourage to arrange for special scholarship for our medical students studying in different universities." And 3.the state House of Assembly is also of the view that professional ethics of medical doctors should be respected and establishment of private hospitals by engaged medical doctors by the state government should be discouraged or possibly be scrapped, " he said.He directed the clerk to communicate the House resolution to Gov. Sule for his action.Earlier, Hon Usman- Labaran Shafa( APC-Toto Gadabuke) the Chairman, House Committee on Health while moving the motion appealed to his colleagues to support his motion to enable the state government train indigenes in medicine and other science related courses for long run benefit.Shafa while giving reasons for his motion said that most of the doctors that always went on strike without considering its implications on citizens or putting the interest of the state in their hearts do find it easier because they are non indigenes, hence the need for the state government to train its indigenous students in medicines and other science related courses." I want this Honourable House to give optimal consideration on my motion that the state government should as a matter of urgency and necessity to initiate an avenue or intervention." Such as special scholarship that will encourage and train our indigenes in medicines, pharmacies and other science related courses so that in the long run between 5 and 8 years or above."We will begin to have our indigenous medical professionals and the general health being of the citizens will be guaranteed through a bond between the state government and the beneficiaries of the scholarship, " he said.This Shafa said by then the state will be exporting doctors to other states instead of importing.Hon Daniel Oga Ogazi, the House Deputy leader seconded Hon Shafa's motion and Members who spoke during the deliberation also thrown their weights on the motion, urging the state government to encourage indigenous students read medicines and other science related courses.In a related development, A bill for a law to Repeal the Nasarawa State Local Government Staff Pension Board Edict 1998 and Re-Enact Nasarawa State Local Government Pension Board Law 2020 scaled first reading during the House proceedings as it was sponsored by Hon Muhammad Odege Okpoku (APC), member representing Udege/Loko constituency.
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redpajama_set_name: RedPajamaCommonCrawl


[Distribution and schistosomiasis transmission risks of Biomphalaria straminea in inland China].
[Impact of Toxoplasma gondii infection on pregnancy outcomes in early pregnant women].
[Investigation of Toxoplasma gondii infection in pregnant women in Qingdao area].
[Plasmodium vivax specific peptides prediction and screening based on repetitive protein sequences and linear B cell epitope].
[Construction and identification of recombinant Mycobacterium smegmatis vaccine expressing Cysticercus cellulosae cC1 antigen].
[Nursing of advanced schistosomiasis patients: a report of 52 cases].
[Academic influence of institutes in field of schistosomiasis control and research in China].
[Molluscicidal effect comparison between TDS and MNSC in field].
[Comparative study on EEG and neuroimaging of patients with cerebral cysticercosis before and after treatment].
[Analysis on depression of patients with advanced schistosomiasis and its influencing factors].


A unique figural covered container that stands 5 in. tall. Measures 3.5 in. diameter at the top.Made of copper and decorated with brass. No makers mark. I believe this item is from the late 1950's-early 1960's. I find no damage. The girl or lady has a blue, green colored dress and hat.


text:
iBreathe: Ready to Start Stopping?
James Dylak
We're delighted to announce that we have been appointed by iBreathe UK to create and implement a rebrand and repositioning for the UK-based vaping and e-liquid brand, which operates from over 6000 locations across the world.
Gary Young, our Creative Director, said "We are delighted to be working with iBreathe. They came to us with what appeared to be a common problem in a massively saturated market; 'Make us different'. Our research and initial creative tests indicated a route that we thought was both right and controversial. Always a heady mix.
'Start Stopping' will be the central thread that glues everything that iBreathe does together. From e-liquids to equipment, everything is based around a simple, two word premise that actively targets tobacco smokers in the UK and beyond. So not just a healthier alternative to smoking, but one which will allow smokers to lead happier lives. It's a big promise and it was a brave decision by iBreathe to follow the route. But both we and they are already delighted with the results. We're excited to see what the future holds, as we continue to work with them on every aspect of their branding, marketing and communications for the next two years.
iBreathe have made it clear that they want to compete with the big name brands such as Logic, Vype and Blu over the coming period. We're pleased to help them play a part in making that happen".
Alaur Rahman, Chief Marketing Director for iBreathe said "We were hugely impressed by the standard of the work carried out by CreationADM. Every member of their team was involved in the rebrand. They went beyond our expectations, suggesting plans and ideas that we had not yet considered, but which we could see would have a huge impact on sales and reach. We hope that the new simple, clean, lifestyle approach to vaping which our rebranded position encourages, will inspire more and more people to quit smoking, start vaping, and adopt a healthier lifestyle".
The rebrand will position iBreathe front and centre as the first vaping company with an explicit, targeted focus on the use of e-cigarettes and vaping both as a method of stopping smoking and as a healthier, cleaner, smoking replacement. The iBreathe experience will also extend beyond the point of purchase, as partnerships with healthcare providers and sports facilities are already in place. A range of supporting educational materials and booklets have also been created to make sure that the iBreathe experience is both memorable and continuing.
We will work across the whole of the iBreathe offer globally, including a new website, all social media and PR, branding and packaging, product launches, store design and a new UK-wide advertising campaign in time for the festive period.
Whether you have an existing company ripe for a rebrand, or an entirely new business venture in need of someone to turn your ideas into a brand with an identity, get in touch.
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Taking the road that leads from Calderino to Mongiardino, in the lush green heart of the Apennines surrounding Bologna is the Nuova Roma, housed in a renovated old farmhouse. In a rustic, yet classical and elegant setting, sisters Nanni, Marinella and Patrizia carry on this family business, which has now been handed down for four generations, with great love and passion serving traditional local cuisine. Patrizia, who works in the kitchen with her staff (who are all women), also buys all the ingredients, favouring locally-sourced, seasonal produce. All the pasta is homemade and is hand-rolled. Traditional dishes include tortellini, only ever served in broth, gramigna pasta with sausage sauce and skewered pork livers wrapped in netting, which are served alongside seasonal vegetables, mushrooms and truffles, all fresh and locally-sourced. In the dining room, Marinella works alongside her son Omar, a sommelier and great connoisseur of spirits. The wine list has over 700 labels - including 80 champagnes - and a selection of regional wines. Also worth mentioning is the fine list of spirits. At Nuova Roma guests can even stop for a quick snack of fried flatbread and premium cold cuts, served on the large veranda in summer.


Which states might experience the next wave of teacher strikes?
Tens of thousands of public school teachers have been involved in teacher strikes and protests spanning four states in the past two months. Though West Virginia's disputes resolved early last month and Oklahoma's walkout just ended, tensions are still simmering in Arizona and Kentucky.
Last week, I offered my take on some of the underlying factors lurking behind the teacher strikes. Importantly, the commonalities between these striking states are also shared by other states, and in this post I'll do a quick analysis that may indicate where conditions are ripe for future actions. Based on this analysis, Southern states share many of the features that characterize states where we've seen recent strikes.
Low average teacher salaries in comparison to the national average: Because many states have been citing statistics from a report produced by the National Education Association, the largest teachers union, we'll also use these rankings (even though the numbers differ slightly from official sources for the same school year).
Reductions in inflation-adjusted teacher salaries since the onset of the Great Recession: Nationally, average teacher salaries are down nearly 5 percent after inflation is considered, and some states are down even further. We take data for this calculation from the 2017 Digest of Education Statistics, comparing the most recent data with 2009-10.
Reductions in per-pupil spending since the onset of the Great Recession: According to a report from the Center on Budget and Policy Priorities last year, school funding in 29 states had not returned to pre-recession levels through the 2015 fiscal year.
State-determined salary schedules: Though not an obvious factor, I believe this is an important common feature of the current teacher strikes, as having salaries determined by the state focuses any public protests on a single target in the state Capitol, rather than peppering small demonstrations across many local administration offices. Fifteen states determine some form of minimum salary schedules for their teachers, according to the National Council on Teacher Quality's Teacher Contract Database. It is worth noting this feature of policymaking does have a high degree of overlap with right-to-work laws (12 of the 15 states are also right-to-work states).
Here are the results for how each of the four striking states scored on these economic factors.
As can be seen in the table, the striking states share many of these characteristics. Also, characteristics in one state that seem out of step with other striking states correspond to some of the real differences that we're seeing across the teacher strikes. For example, Kentucky teachers' salaries are essentially in the middle of the pack nationally, and it is the one strike where teachers are not advocating for higher salaries but against changes to the state's pension benefit calculation. Also, consider how teachers in both Oklahoma and Arizona have been tying demands for education funding with their demands for salary increases, where this was not part of what motivated teachers in West Virginia. Teachers in Arizona have not actually gone on strike, but have organized protests only.
So what other states have favorable economic conditions for a statewide teacher strike, based on the characteristics of the four states involved in the current strikes and protests? If we consider these conditions as possible risk factors, then both Mississippi and North Carolina appear to be particularly at risk, with Mississippi showing slightly more unfavorable conditions for teachers.
Several other states, however, share these economic factors and thus may also be at risk.
This list includes three Southern states, all of which have modest to low levels of teacher pay, deterioration in both salaries and general education funding over the last decade, and state-determined salary schedules. Combining these three states with the two shortlist states above suggests that teachers in much of the South endure conditions similar to states where teachers have already organized.
This final list also includes four states that do not have state-determined salary schedules. As I suspect, this feature is one that helps galvanize teacher and media attention on a broad scale, I believe organizing a statewide strike would be a logistical challenge in these states. Yet, this should not preclude teachers from organizing protests and perhaps striking in some districts as economic conditions are generally unfavorable to teachers in these states.
Could future strikes really happen in other states?
Whether strikes will come to fruition in any of these states, or any other for that matter, is hard to predict due to the variable contexts across the country. The four economic factors highlighted here are insufficient to explain what has happened in these states, as current tax and school finance policies, partisan divides, union influence, and many other state-level features contributed to the strikes that are now happening. Therefore, these myriad factors would also be important in understanding which states actually witness teacher unrest in the near future.
Despite the complexity of predicting where the next strike might occur, the multi-state teacher actions have certainly prompted discussions in other schools beyond their border. In recent days, rumors of gathering calls for action have been reported in Indiana and Texas. Further teacher action in North Carolina seems almost inevitable, with a call for a march on the state Capitol set for a date next month. These conversations are not just happening among teachers in other states, but some state legislatures (including several on my list) have begun making moves in recent months to pay teachers more. Given the recent timing of their actions, they were likely motivated at least in part by the teacher victory in West Virginia. Yet, only time will tell if these moves are enough to forestall future demands for more.
Also, quite a few of these states have been dealing with teacher shortages and other difficulties with recruiting and maintaining a quality workforce—an expected byproduct of low salaries. Perhaps teachers in these states could use this apparent need for good teachers as leverage to bring state legislators to the bargaining table.
Lawmakers, education leaders, and the public need to pay attention. Based on what we can infer from other research, weak teacher workforces often disproportionately harm disadvantaged student groups. Without remedying teacher pay and benefits, the quality of the teacher workforce and the pipeline leading to it will continue to suffer in not just those states that are striking but in all states where teacher and educational conditions are weak.
Max Rombado contributed to this post.


Factories support this interface creating instances giving a name, e.g. a service name.
Note: Although this interface deals with the notion of "services", this is not generally be meant. In general this interface can be used for all kinds of factories for all kinds of instances, indeed not only UNO services.
createInstance Creates an instance classified by the specified name.
createInstanceWithArguments Creates an instance classified by the specified name and passes the arguments to that instance.
getAvailableServiceNames Provides the available names of the factory to be used to create instances.
Creates an instance classified by the specified name.
Creates an instance classified by the specified name and passes the arguments to that instance.
Provides the available names of the factory to be used to create instances.


This could be another one of those "waiting for Player X to sign" spring trainings, and the Red Sox aren't immune to playing this game for the second straight year.
While Bryce Harper and Manny Machado will dominate the baseball headlines until they sign, Craig Kimbrel is in a similar boat as a 30-year-old on a Hall of Fame track who just entered free agency for the first time.
There are flaws and down-trending numbers to be concerned about, but he remains one of the best relievers in baseball, having held hitters to the lowest contact rate (62.7 percent) in the game in 2018.
It's hard to see Kimbrel signing for anything close to what most would consider a bargain. Even if that takes him into February without a contract.
The safe bet is to assume the Red Sox aren't going to be involved. President of baseball operations Dave Dombrowski has said multiple times this offseason that the Sox won't swallow a large expenditure to add a closer.
And with the club already pushing a $238 million payroll for luxury tax purposes (tax kicks in at $206 million this year), they have less than $8 million to work with if they want to avoid paying the highest penalty and losing 10 spots on their draft pick for a second straight year.
Money is finally an issue for this team. It was always going to catch up to them.
So while most of the best relievers have been plucked off the free agent market, only Kimbrel and Adam Ottavino remain among the elites. Cody Allen (4.70 ERA in 2018) and Brad Brach (3.59 ERA) are there, too.
Either Allen or Brach seems most likely to end up in a Red Sox uniform. And aside from another minor league signing or perhaps a decent reliever that could be picked up in exchange for one of the Sox' extra catchers, it seems unlikely that any other additions will be made to a bullpen that saw Joe Kelly and Kimbrel hit the free agent market.
What the Red Sox have now could be very similar to what they'll have entering the season. That means there's a legitimate chance that either Matt Barnes or Ryan Brasier will enter the year as the closer, unless manager Alex Cora wants to take the stomach-turning "closer by committee" approach.
Even without another big-name addition, the Sox can point to their Nathan Eovaldi signing as the key move of the off-season. Remember, Dombrowski chose to acquire Eovaldi instead of Zach Britton at the trade deadline last year because he thought Eovaldi gave the Sox more flexibility.
It seems like he made the same choice again this winter, and it's probably the right one (again).
With Eovaldi, the Sox get the potential of a top-of-the-rotation starter. Worst-case, he struggles or encounters injury issues that force him to the bullpen where he could become a dominant weapon there.
But most likely he'll be in the rotation with Chris Sale, David Price, Rick Porcello and Eduardo Rodriguez.
All of a sudden the Sox bullpen is one man deeper, with knuckleballer Steven Wright adding to the mix. If his knee isn't an issue, Wright has proven to be as consistent as any knuckler in the last decade. No, he's not a traditional set-up guy. But he could do voluminous work as a multi-inning weapon on days Rodriguez or Eovaldi can't get out of the fifth inning. And the Sox will undoubtedly need a sixth starter at some point during the season.
Could Brian Johnson and Hector Velazquez find a way to generate more outs in a redefined one-inning role? Johnson has the dominant curveball that can be filthy when he's spotting his high-80s fastball to keep people off-balance. Perhaps the fastball will play up if Johnson is no longer asked to provide length and simply lets it rip over 10-20 pitches.
It's all a guessing game, but if Wright, Velazquez and Johnson get you to the sixth or seventh, the Sox aren't in the worst shape.
Barnes has been plagued by walk issues his entire career, but showed tremendous growth in 2018, easily his best season, and is a worthy set-up man on any team. Brasier clearly has the talent and guile to handle the closer role. Brandon Workman and Heath Hembree are solid options in the middle innings.
The Sox love Colten Brewer, who they acquired from the Padres, and hope he can be the 2019 version of Brasier. Tyler Thornburg is still under contract, if his thoracic outlet issues will ever subdue. Last year's third-rounder, Durbin Feltman, projects as a talented reliever who isn't far from the majors. And though lefty Darwinzon Hernandez will begin the year as a starter in the minors, there seems to be a strong belief that he's slated for relief work in the majors when he matures.
This isn't to say that the Red Sox bullpen has no flaws, or that they don't need Kimbrel or Ottavino.
But there are numbers here. There is upside. And if the Sox want to avoid spending big on another reliever, the wise move with so many players up for free agency in the next two seasons, the bullpen should hold up.
If not, there's always the mid-season acquisition.


You will feel like a Gypsy Queen in our amazing Ravennah Maxi Dress! This exquisite gown features a cami-style top with adjustable straps making it cool and perfect for warm sunny days. Add your favourite faded denim jacket for those cooler nights and you have the ideal maxi to take you through the seasons. The dress features a comfortable and flattering elastic waist, perfectly finished with our beautiful handmade tassels. With a swirl of lavish fabric flowing around you – you will be making magic in this gown! Featuring our stunning Lost in Paradise print with vibrant flowers, this gorgeous dress is available in three colours, Rococo Red, Lapis Lazuli and Lotus.
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Taking the Hyangdobong funicular train to the top of Mt. Paekdu. In the DPRK, many companies and brands are named after Korean geographic place names — in this case the funicular train has been named after Mt. Paekdu's Hyangdo Peak.


text:
The culture of the Republic of the Congo is rich, diverse and made up of a mix of about 4.5 million people in 2015 and just as many languages and customs.

Half of Congolese people follow traditional beliefs, and there are 15 principle Bantu groups and more than 70 subgroups. The other half are 35% Roman Catholic, 15% other Christian and 2% Muslim.  The region was dominated by Bantu-speaking tribes, who built trade links leading into the Congo River basin. Congo-Brazzaville was formerly part of the French colony of Equatorial Africa.

Language and writings

The official language of the Republic of Congo is French. French is spoken by 56% of the Congolese population (78% of the population over 10 years), the second highest percentage of Africa in 2010, behind that of Gabon2. About 88% of Brazzavillans over 15 years of age say they have an easy expression in French.
The Republic of Congo has a number of well-known writers in Africa and the French-speaking world: Alain Mabanckou, Jean-Baptiste Tati Loutard, Jeannette Balou Tchichelle, Henri Lopes, Lassy Mbouity and Tchicaya U Tam'si.

Several artistic genres such as Congolese cinema struggle to make their breakthrough. After a promising start in the 1970s, the turbulent political environment and the closing of cinemas made production difficult. The country produces no feature films a year and filmmakers broadcast their production directly in video. In the end, in Congo-Brazzaville, culture remained until then the poor relation of the investments of successive governments.

redpajama_set_name: RedPajamaWikipedia


As of April 2015 Elm Practice became a single handed GP Practice (1 GP partner). Dr Denyse Hosein is the sole partner of Elm Practice. The practice also has 2 permanent Salaried General Practitioners, Dr Sven Baumgarten and Dr Nick Lawrenson.
Anyone living within the practice area, who is not already registered with a local GP may join our list. You will be asked to complete our practice questionnaire or you can make an appointment with our practice nurse for a new patient check. From this first meeting, the nurse and doctors will become aware of any important medical conditions, allergies etc. you might have. You will also have your blood pressure and urine checked. It can take some time for your notes to arrive from your previous doctor; therefore it will be helpful to get some details in the meanwhile.
Out of Hours Service: If you need urgent treatment or advice when the practice is closed called NHS-111.
The Accessible Information Standard aims to ensure that patients (or their carers) who have a disability or sensory loss receive information they can access and understand. For example in large print, braille or via email.
- Identify patients who may have an additional communication need.
- Record the patient's need in our clinical GP system.
- Act to ensure our staff can effectively communicate with patients who may have additional communication needs.
Click on the Patient Access icon to book your appointment or to consult with a GP online, click 'Get Started' on the blue icon!


text:
www.organcompetition.ru > News > IХ Mikael Tariverdiev International Organ Competition - The University of Kansas School of Music will host the North American Round
04.04.2015 IХ Mikael Tariverdiev International Organ Competition - The University of Kansas School of Music will host the North American Round
IХ Mikael Tariverdiev International Organ Competition
First round takes place:
USA, Kansas, April 8-11
Germany, Hamburg, April 20-24
Russia, Moscow, August 28-31
Second, Third Rounds: ,br> Russia, Kaliningrad, September 3–9
The University of Kansas School of Music will host the North American Round of the Tariverdiev (Russian) International Organ Competition Apr. 8-11.
The competition rounds are free and open to the public and will be held in Bales Organ Recital Hall. They will be held: Thursday, Apr. 9 from 2-5 p.m., Friday, Apr 10th 9 a.m.-12 p.m. & 2-5 p.m., and Saturday, Apr. 11th 9 a.m.-12:30 p.m.
Additionally, special guest artist Lada Labzina, Honoured Artist of the Republic of Tatarstan and senior lecturer at the faculty of organ and harpsichord studies at the Kazan State Zhiganov Conservatoire, will present a free recital on Friday, April 10 at 7:30 p.m. in Bales Organ Recital Hall. She will perform a program featuring organ transcriptions of works by Tschaikovsky, Rimsky-Korsakov, and Mussorgsky.
This will be the third time that KU has hosted the Competition. Other international sites for first round competitions include Hamburg, Germany and Moscow, Russia. The winner of the Competition will present a recital at the Bales Organ Recital Hall of the University of Kansas. The top three finishers will proceed to Kaliningrad, Russia in the fall of 2015 to compete for the international prize.
Judges for the KU Competition include KU organ faculty members Michael Bauer and James Higdon; Wichita State organ professor Lynne Davis; Martin Jean, Dean of the Yale Institute of Sacred Music; and Karel Paukert, emeritus professor of organ at Northwestern University.
The Mikael Tariverdiev International Organ Competition is the only international competition for organists hosted by Russia. For those who play this instrument, it has the same significance as the Tchaikovsky competition has for pianists and violinists. 2015 will see the competition held for the ninth time. Thierry Escaich, Chairman of the Jury of the 8th competition: "The participating musicians have shown a high level of performing mastery in all rounds. Comparing the Mikael Tariverdiev International Organ Competition to similar contests, one notes that this competition's participants markedly surpass others. Equally important is the friendly atmosphere during the competition."
The first round of the competition is to be held in Kansas, USA, Hamburg, Germany, and Moscow, Russia. Kaliningrad is to host the second and third rounds, from 3 to 9 September 2015. www.organcompetition.ru
The Mikael Tariverdiev Organ Competition has been held in Kaliningrad since 1999, with support from the Russian Ministry of Culture and Foreign Ministry, the Kaliningrad City Hall and the Kaliningrad Oblast government. At all of its stages, the competition is held at famous venues with outstanding organs: The Dane & Pole Recital Hall at the University of Kansas, the great organ at the Church of St. Michael in Hamburg, the Prokofiev Hall of the Glinka Museum of Musical Culture, and the Concert Hall of the Kaliningrad Philharmonic (2nd round). The third round uses one of the best organs in Russia and Europe, located at the Kaliningrad Cathedral.
The competition aims for maximum publicity. Its opening and closing ceremonies feature both the musicians directly involved with the competition and specially invited stars of classical music. Thus the opening ceremonies have, in various years, featured Gidon Kremer and the Kremerata Baltica orchestra, or the Viennese Academy orchestra with Martin Haselböck. In 2011, the Organ+ programme included organ-accompanied performances by the Terem Quartet, the Hide Hide duo (Japan, shakuhachi and shamisen), Gevorg Dabagian (Armenia, duduk), and in 2013, by the Synodal Choir and the Russian Horn Orchestra. This started a new tradition: the Organ+ festival, which now accompanies the competition every year.
The ninth competition will be held in 2015. The schedule is as follows: Kansas — 8 to 11 April; Hamburg — 20 to 24 April; Moscow — 28 to 31 August; Kaliningrad — 3 to 9 September.
The University of Kansas School of Music will host the North American Round of the Tariverdiev (Russian) International Organ Competition Apr. 8-11. The competition rounds are free and open to the public and will be held in Bales Organ Recital Hall. They will be held: Thursday, Apr. 9 from 2-5 p.m., Friday, Apr 10th 9 a.m.-12 p.m. & 2-5 p.m., and Saturday, Apr. 11th 9 a.m.-12:30 p.m. (www.music.ku.edu)
The 3 September opening of the competition in Kaliningrad will be marked by a concert by two outstanding musicians, the organist and composer Jean Guillou and multiple competition winner Alexander Kniazev (organ and cello). This concert will inaugurate a series of events dedicated to Jean Gillou's anniversary. At eighty-five, this living legend of 20th-century music is as open as ever to experiments. At the opening concert of the 9th Mikael Tariverdiev International Organ Competition, the maestro will for the first time play in ensemble with a Russian traditional instrument orchestra.
Jean Guillou will join the jury, along with a number of outstanding representatives of organ schools from four continents.
The second round will be held on 4–5 September at the Concert Hall of the Kaliningrad Philharmonic, and the third round, at the city Cathedral on Kant Island, on 7 September.
A concert by the prize winners will follow on 8 September (also at the Cathedral). Any listener or organization has the opportunity of setting up their own special prize alongside the existing ones.
On 7 September, the contestants, jury members and competition guests will take the traditional trip to the Curonian Spit, where they can enjoy the incredible beauty of nature together. And realize that —
WE ARE HAPPY BECAUSE WE ARE TOGETHER.
The level of interest in the competition is evidenced by the number of applications submitted. There were 19 applicants for the first round in Kansas, 17 of whom have advanced to the competition. They are organists from various parts of the United States as well as from Austria, Japan, South Korea and Uzbekistan.
25 applications were received in Hamburg, with 20 advancing into the first round. These are musicians from Germany, Russia, Italy, Hungary, the Netherlands, Denmark, the US, Italy, Slovakia, the Czech Republic, Poland, South Korea and Japan.
Concerts that are part of the Organ+ festival will also be held in Kansas and Hamburg.
8 April, Dane & Pole Recital Hall, Lawrence, Kansas
Russian musical highlights in organ transcription
Lada Labzina, soloist at the Tatar Philharmonic, Mikael Tariverdiev International Organ Competition winner
24 April, Church of St. Michael (Hamburg)
Az i Ya
Mikael Tariverdiev International Organ Competition winners Lada Labzina (Kazan, Russia) and Hiroko Innoue (Japan)
Excerpts from works by Chingiz Aitmatov read by German actor Peter Bouse
6 September, Friedrichsburg Gate (Kaliningrad)
Arabesque (A One-Picture Concert)
International competition winners Olesya Petrova (soprano), Alexei Goribol (piano), Rustam Komachkov (cello), Natela Toidze, People's Artist of Russia, member of the Russian Academy of Arts.
9 September, the Music Tram and Depot No. 1: Organ+ Festival Closing
Lost in the Music: a concert programme
British composer and instrumentalist Stephen Coates and The Real Tuesday Weld will present English-language songs and music by Mikael Tariverdiev. CDs and vinyl records released in the UK will be presented as part of the event.
The Jury:
Arvid Gast (Germany), Chair
Guy Bovet (Switzerland)
Martin Jean (USA)
Rie Hiroe (Japan)
James Higdon (USA)
Jeremy Josef (South Africa, Austria)
Alexander Kniazev (Russia)
Alexey Panov (Russia)
Ville Urponen (Finland)
Erwin Wiersinga (Netherlands)
Jean Guillou (France), Martin Haselböck (Austria) and Daniel Zaretsky (Russia) participate in the Jury for the third round.
James Higdon (Chair)
Martin Jean
Arvid Gast, Germany (Chair)
Christoph Schoener (Germany)
Daniel Zaretsky (Russia)
Anjei Horoshinsky (Poland)
Ivan Rozanov, Russia (Chair)
Lubov Shishlanova (Russia)
James David Christy (USA)
Talivaldis Deksnis (Latvia)
Toomas Trass (Estonia)