text:
Q: How to Chart.Js, change the color by pressing the button (or any element)? how can I change the line colors in the light mode of the chartjs I use when I switch to dark mode? Can you help me with this?
Here are the colors I use now:

This is how I need to change colors when I switch to dark mode:

My chartjs chart is available in the codepen link below:
https://codepen.io/korayhan-aslan/pen/QWQeMej

// bar chart start
        var chartData = {
         labels: ['Ocak', 'Şubat','Mart', 'Nisan', 'Mayıs', 'Haziran', 'Temmuz', 'Ağustos', 'Eylül', 'Ekim', 'Kasım', 'Aralık'],
         datasets: [{
            label: "Yatırımlar",
            backgroundColor: "#1355FF",
            borderWidth: 0,
            borderRadius: 5,
            data: [20423,40123,60313,80412,40414,1932,40131,10124,30578,50421,60124,14512]
            }, {
            label: "Çekimler",
            backgroundColor: "#57D3DD",
            borderRadius: 5,
            borderWidth: 0,
            data: [60732,30125,20712,50252,30689,50234,20464,30123,10245,15123,40126,60126]
            },

            ]
        };

        let value = 80000;
        var ctx = document.getElementById('barChart');
        var myBarChart = new Chart(ctx, {

            type: "bar",
            data: chartData,
            drawBorder:false,
            options: {
                responsive:true,
                maintainAspectRatio: false,
                scales: {
                    x: {
                        title: {
                            display: false
                        },
                        grid: {
                            display:false
                        },
                        ticks: {
                            color: "#718096"
                        }
                    },
                    y: {
                        title: {
                            display: false
                        },
                        min: 0,
                        max: 80000,
                        ticks: {
                            stepSize: 20000,
                            color: "#718096",
                            callback: function(value, index, values) {
                                return value * 0.001 + " K";
                            }
                        },
                        grid: {
                            color: '#EDF2F7'
                        }
                    }
                },
                plugins: {
                    legend: {
                        position:"top",
                        labels: {
                            font: {
                                size: 12,
                                weight: 500
                            },
                            color: "#2D3748",
                            boxWidth: 8,
                            boxHeight:8,
                            usePointStyle: true,
                            pointStyle: "circle"
                        }
                    }
                }
            }
        });

        // bar chart end
.container {
  max-width:1200px;
  width:100%;
  margin:0 auto;
}

  <canvas id="barChart" width="400" height="240"></canvas>

<input type="checkbox" name="chartChange" id="chartChange">
Click to change chart color text

A: You can just go inside of the chart object, into the options and change the color of the grid lines:
const lightGridLineColor = 'black';
const darkGridLineColor = 'yellow'

const myBarChart = new Chart(ctx, config);

document.getElementById('chartChange').addEventListener('click', () => {
  const toDarkMode = myBarChart.options.scales.x.grid.color === lightGridLineColor;
  if (toDarkMode) {
    myBarChart.options.scales.x.grid.color = darkGridLineColor;
    myBarChart.options.scales.y.grid.color = darkGridLineColor
  } else {
    myBarChart.options.scales.x.grid.color = lightGridLineColor;
    myBarChart.options.scales.y.grid.color = lightGridLineColor
  }

  myBarChart.update();
})

Live sample:

const lightGridLineColor = 'black';
const darkGridLineColor = 'yellow'

// bar chart start
const chartData = {
  labels: ['Ocak', 'Şubat', 'Mart', 'Nisan', 'Mayıs', 'Haziran', 'Temmuz', 'Ağustos', 'Eylül', 'Ekim', 'Kasım', 'Aralık'],
  datasets: [{
      label: "Yatırımlar",
      backgroundColor: "#1355FF",
      borderWidth: 0,
      borderRadius: 5,
      data: [20423, 40123, 60313, 80412, 40414, 1932, 40131, 10124, 30578, 50421, 60124, 14512]
    }, {
      label: "Çekimler",
      backgroundColor: "#57D3DD",
      borderRadius: 5,
      borderWidth: 0,
      data: [60732, 30125, 20712, 50252, 30689, 50234, 20464, 30123, 10245, 15123, 40126, 60126]
    },

  ]
};

let value = 80000;
const ctx = document.getElementById('barChart');
const myBarChart = new Chart(ctx, {

  type: "bar",
  data: chartData,
  drawBorder: false,
  options: {
    responsive: true,
    maintainAspectRatio: false,
    scales: {
      x: {
        title: {
          display: false
        },
        grid: {
          display: false
        },
        ticks: {
          color: "#718096"
        }
      },
      y: {
        title: {
          display: false
        },
        min: 0,
        max: 80000,
        ticks: {
          stepSize: 20000,
          color: "#718096",
          callback: function(value, index, values) {
            return value * 0.001 + " K";
          }
        },
        grid: {
          color: '#EDF2F7'
        }
      }
    },
    plugins: {
      legend: {
        position: "top",
        labels: {
          font: {
            size: 12,
            weight: 500
          },
          color: "#2D3748",
          boxWidth: 8,
          boxHeight: 8,
          usePointStyle: true,
          pointStyle: "circle"
        }
      }
    }
  }
});

document.getElementById('chartChange').addEventListener('click', () => {
  const toDarkMode = myBarChart.options.scales.x.grid.color === lightGridLineColor;
  if (toDarkMode) {
    myBarChart.options.scales.x.grid.color = darkGridLineColor;
    myBarChart.options.scales.y.grid.color = darkGridLineColor;
  } else {
    myBarChart.options.scales.x.grid.color = lightGridLineColor;
    myBarChart.options.scales.y.grid.color = lightGridLineColor;
  }

  myBarChart.update();
});

// bar chart end
.container {
  max-width: 1200px;
  width: 100%;
  margin: 0 auto;
}

  <canvas id="barChart" width="400" height="240"></canvas>

<input type="checkbox" name="chartChange" id="chartChange">
Click to change chart color text


Lined dresses A and B have princess seams, skirt back zipper, back gathers and bodice loops. Dress A has gathered insets, sleeve with elastic casing, rhinestones and pearl trim detail. Dress B has elbow length sleeve, embroidered insets and sleeve cuffs.


text:
'Ding Dong! the Witch is Dead': BBC Responds as Anti-Thatcher Campaign Pushes Song Up the Charts
The bitter row over Margaret Thatcher's legacy continues — and this time it's spilling onto the BBC's Top 40 radio program.
By Ollie John April 12, 2013
The Wicked Witch of the West, left, played by Margaret Hamilton, confronts Dorothy, played by Judy Garland, and Glinda, the Witch of the North, played by Billie Burke, right, in this scene from The Wizard of Oz
Updated: Apr. 15, 2013 at 4:00 a.m. EST
Following her death on April 8, the bitter row over Margaret Thatcher's legacy continues – with a campaign to get the song "Ding Dong! The Witch is Dead", from the movie The Wizard of Oz, to number 1 on the U.K. music charts. The song ended up reaching number two on Sunday after selling 52,605 copies. This was more than 5,700 copies behind Duke Dumont and A*M*E with "Need U (100%)," which stayed at the top for a second week. Meanwhile, a rival campaign song, "I'm In Love With Margaret Thatcher" entered at number 35 after a late push from Lady Thatcher supporters.
The former Prime Minister, whose time in office was marked by battles with workers' unions and the privatization of key industries, continues to be a divisive figure in Britain. On the day of her death a number of street parties were held throughout the U.K., some of which turned violent.
(MORE: Rage Against Simon Cowell? A British Pop Charts Upset)
Encouraged by an anti-Thatcher Facebook campaign, people are now downloading the 1939 song, sung by Judy Garland and the cast of the movie, in an attempt to make it the top-selling track of the week.
(MORE: Fondness in Finchley: Margaret Thatcher's Constituency Reflects on Her Legacy)
The activist Adam Jung, writing for the Huffington Post, called it "a creative way for Brits to correct the national narrative" of Thatcher's time in office.
But the music journalist Neil McCormick, writing in the Daily Telegraph, said that the campaign would make the song "the most inappropriate and gratuitously offensive number one hit single ever." And former Conservative Member of Parliament Jonathan Aitken told a British TV show: 'People who have respect for Lady Thatcher and her views will not find this anything other than a distasteful affair," adding that it was "a pretty feeble form of protest."
(MORE: Margaret Thatcher's Funeral: Who Will Be Attending)
But distasteful and feeble as it may be, the campaign is causing a significant headache for the BBC. By Friday, "Ding Dong! The Witch is Dea had hit number 1 in the U.K. iTunes store, and number 3 on the Official U.K. Chart. BBC Radio 1 ordinarily does a Top 40 countdown on Sunday afternoons, in which every song from number 40 down to number 1 is played in its entirety. But on Friday the broadcaster announced that the song won't be played in full. Instead, a short clip of will be played as part of a news bulletin explaining that the track has reached that place in the chart. It called the decision "a difficult compromise."
Meanwhile, a large anti-Thatcher protest in London's Trafalgar Square was organized this past weekend by a coalition of activists, anarchists and former coal miners, reports the Guardian. And the Sun reports that a London police officer resigned from his post after it was revealed that he had made a number of offensive tweets celebrating Thatcher's death.
MORE: Praise for the Baroness: Political Tributes for Thatcher

redpajama_set_name: RedPajamaCommonCrawl


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The Google Drive suite allows individuals to do everything from presentations to word docs. Here are ten Google Drive add-ons to enhance your experience. Here are ten Google Drive add …... 5/05/2016 · Use Starred items to go back to the important things You can favorite a website by bookmarking it. You can also bookmark a file from Google Drive that you routinely need to access.
9/10/2012 · I keep wondering why services like Google Drive don't include simple URLs as an item type that can be added to a shared folder. I suspect there's a reason for this, as it … hammer how to add light I just used this to add Google Drive to my sidebar in Windows 10. The newest sync tool is now Drive File Stream so I set the %USERPROFILE% values to the "My Drive" folder. I also changed the two locations for "DefaultIcon" to point to the GoogleDriveFS.exe install location on my computer so that the icon wouldn't just be a folder.
I have a Google Drive account with a folder that has been shared with an edit permission link. While logged into another Google Drive account, I would like to upload some files, using drag and drop to a Chrome Browser window opened with the shared link.
12/05/2014 · When you compose an email, click on the small Drive icon, and from there pick what you want to add. When someone sends you any attachment via email, you can save it straight to your Drive.


text:
\section{Introduction}
The discovery of the gravitational waves from
a neutron star merger, GW170817,
has opened a new era of multi-messenger astronomy \citep{GW170817, Abbott2017ApJ}.
The gravitational-wave signal  was followed by multi-frequency electromagnetic emission
including a $\gamma$-ray pulse, uv/optical/IR macronova/kilonova,
and long lasting non-thermal emission ranging from radio to X-rays.
The macronova/kilonova observations show that
the typical  velocity of the ejecta is $\sim 0.1$--$0.3c$  and
$r$-process elements of a mass of
$\sim 0.05\,M_{\odot}$ are synthesized in the ejecta if the radioactive decay powers the emission
(e.g., \citealt{Andreoni2017,Arcavi2017Natur,Cowperthwaite2017,Evans2017,Lipunov2017,Kasliwal2017,Kilpatrick2017,Smartt2017,Valenti2017,Drout2017,Pian2017,Swope,Tanvir2017,Utsumi2017}, and see also the modelings, e.g.,
\citealt{Kasen2017, Tanaka2017, Waxman2017, Perego2017,Villar2017}).
This mass
estimate together with the rate of GW170817 supports early predictions \citep{Lattimer1974,eichler1989Nature}  that
$r$-process elements in our Galaxy are predominately produced
by mergers (e.g. \citealt{Cote2017,rosswog2017,hotokezaka2018}). However, the mechanism that ejects
such a large amount of material still remains an open question (e.g. \citealt{Metzger2018,Shibata2017}).

X-ray and radio signals were discovered at 9 and 16 days after the merger, respectively
\citep{Haggard2017, Troja2017, Hallinan2017}.
These signals are most likely explained by synchrotron radiation
arising from the shock formed between the merger outflow and interstellar
medium (ISM). Both off-axis and on-axis emission models are consistent with the observed data
up to $\sim 30$ days  \cite[e.g.,][]{Hallinan2017,Troja2017,Margutti2017, Gottlieb+17B}.
However,  radio observations up to $\sim 100$ days
show that the flux density  continued to rise  as $\sim t^{0.8}$ \citep{Mooley2017}.
 X-ray and optical observations subsequently confirmed this behavior
 \citep{Ruan2017,Lyman2018,Margutti2018}.

{Recently, \cite{Nakar2018} have shown that
this moderately rising light curve  implies  that the emitting matter is  moving towards us at the time of the emission,
namely, the matter   is moving within an angle $\theta <1 /\Gamma$ ($\Gamma$ is the Lorentz factor of the matter) from the line of sight towards us, otherwise the light curve would have risen much faster ($F_\nu \propto t^\alpha$
with $\alpha > 3$). They have also shown a continuous energy injection into the blast wave.  The isotropic equivalent energy increases like $E_{\rm iso}(>\Gamma) \propto
 \Gamma^{-{8\alpha+6(p-1)}/({3-\alpha})}$ (where $p$ is the electron's spectral index),
otherwise the light curve would have declined. }

{This energy injection implies that the outflow must have a structure, either radial or angular or both. Such a structure can arise naturally  from  the interaction of the jet with the surrounding ejecta that forms a cocoon \citep[see e.g.][]{Gottlieb2018MNRAS,Kasliwal2017,Gottlieb+17B,Lazzati2017,Nakar2018}.
This cocoon can arise in the case that the jet is choked or  it emerged and generated a GRB pointing elsewhere. Note that a successful jet and  cocoon are  sometimes called in the literature  ``a structured jet" \citep[see e.g.][]{Margutti2018}.
}

Here, we explore a  third possibility in which the  observed synchrotron emission arises due to the fast tail of the  dynamical ejecta and it has nothing to do with   the question whether a jet existed or not  and how it evolved.
In this dynamical ejecta scenario, suggested long ago by \cite{NP11} and elaborated  by
\cite{piran2013MNRAS,HP2015}  and others,  the synchrotron emission arises from the interaction of
the mergers' dynamical ejecta with the surrounding ISM. These earlier studies focused on the late time emission that would arise from the sub-relativistic component of the outflow, but stressed that a very strong early signal is expected if a faster component exists.

Indeed,
a high velocity (mildly relativistic) tail of the ejecta can also explain the observed emission that followed   GW170817   \citep{Mooley2017}.
Such a high velocity component was expected
but it was very difficult to estimate since only a very small amount of matter moves at these high velocities.
The profile of the high velocity tail was poorly known because of the complexity
of hydrodynamics of  mergers.
Previous attempt to calculate this  involved both analytic considerations \citep{Kyutoku2014}
and numerical simulations \citep{hotokezaka13b,bauswein2013ApJ}.  The latter were limited by their resolution.  Here we use the results of a new series of numerical simulation \citep{Kiuchi2017} with a much higher spatial resolution that allows us to explore in details the velocity profile. These simulations find, in all cases considered,  a light fast component with very steep energy profiles (see figures \ref{fig:E} -- \ref{fig:E2}).
It is remarkable that \cite{Gottlieb+17B}, who considered the conditions  for a cocoon shock breakout to produce the observed $\gamma$-rays, found that  a high velocity component with a comparable amount of matter and energy profile is needed to explain these observations.

\begin{figure*}[t]
\includegraphics[scale=0.7]{eiso_B.eps}
\includegraphics[scale=0.7]{eiso_Buneq.eps}
\caption{
The total kinetic energy and the isotropic equivalent kinetic energy distributions of the dynamical merger ejecta
at different polar angles for models B ({\it left}) and
B uneq ({\it right}). Also shown
as a solid straight line is the slow quasi-spherical model of \cite{Mooley2017}.
}
\label{fig:E}
\end{figure*}

\begin{figure*}[t]
\includegraphics[scale=0.7]{eiso_HB.eps}
\includegraphics[scale=0.7]{eiso_HBuneq.eps}
\caption{
Same as figure \ref{fig:E} but for model HB.
}
\label{fig:E3}
\end{figure*}

The structure of the paper is as follows: we show in \S\ref{sec:ejecta} that  recent high-resolution numerical relativity simulations reveal such  high velocity components and discuss their properties.
In \S\ref{sec:radio} we use these profiles to  calculate the synchrotron radiation light curves arising from the
shock between the ejecta and ISM and compare them with the observed data. Finally, in \S\ref{sec:discussion}, we discuss the generic features
and future expectations of  the dynamical ejecta scenario and summarize our conclusions in \S\ref{sec:conclusions}.

\section{The fast tail of dynamical ejecta}
\label{sec:ejecta}

A small fraction of the dynamical merger ejecta accelerates to
mildly relativistic velocities when the shock formed between
the colliding neutron stars emerges from the surface \citep{Kyutoku2014}.
This component is the high velocity tail of the dynamical ejecta.
The flux of the synchrotron radiation arising from the ISM-ejecta shock can be
significantly enhanced by even  a small amount of a fast ejecta
\citep{piran2013MNRAS,HP2015}.
While fast ejecta  have been found in previous numerical merger simulations
\citep{hotokezaka13b,bauswein2013ApJ,Metzger2015},
its amount was not clear   due to the low numerical resolution of those earlier simulations.

We begin by describing  the ejecta profile obtained from recent high resolution
numerical relativity simulations  \citep{Kiuchi2017},
whose the finest grid spacing, $\Delta x$, satisfies: $\Delta x\sim 70$ m.
We discuss five  models  with a total mass
of $\approx 2.7M_{\odot}$, a mass ratio of $1$ or $\approx 0.8$,
and three different neutron star equations of state: models B, HB, and H
\citep{Kiuchi2017}.
These models are consistent with the mass and tidal deformability
constraints of GW170817 \citep{GW170817}.
The parameters of these models {and the resulting total kinetic energy and mass of the ejecta }  are listed in Table. \ref{tab:model}.  Hereafter, we refer  to equations of state  which give
small (large) radius neutron stars as
``soft" (``stiff") equations of state.

{Note that, like in practically all other numerical relativistic merger simulations \citep{hotokezaka13b,bauswein2013ApJ,sekiguchi2015PRD,radice2016MNRAS,Dietrich2017,Shibata2017} in all models the total mass
of dynamical ejecta is lower than the one needed to power the observed macronova/kilonova.
This additional mass can be driven by
other  mass ejection mechanisms, such as winds from the surrounding accretion disk  or from the hypermassive neutron star  that have not been included in these merger simulations (see, e.g., \citealt{dessart09,fernandez2013MNRAS,metzger2014MNRAS,perego2014MNRAS,just2015MNRAS,fernandez2015MNRAS,fujibayashi2017,Siegel2017}). However,  the typical velocity of this wind ejecta is
much slower than that of the dynamical ejecta, and hence, this ejecta is not relevant for the early synchrotron
emission focused in this paper.}

Figures \ref{fig:E} -- \ref{fig:E2} depict the kinetic energy distributions as a function of
$\Gamma \beta$
obtained from the simulations.
Here,  $\Gamma$ is the Lorentz factor and $\beta$ is the velocity in units
of the speed of light.
The total  kinetic energy of the ejecta is  in the range from
$\sim 7\cdot10^{49}$ to $8\cdot 10^{50}$ erg.
The ejecta of the softest model B is faster than that of models HB and H.
This can be explained if the shock formed at the collision is
stronger for more compact neutron stars, and thus, the ejected
material is faster.  For unequal mass cases the ejecta are predominantly produced
through the tidal disruption of the lower mass neutron star and it contains
a larger amount of slow material and a smaller amount of fast material compared
to the equal mass cases.
{ Note also that the ejecta mass of model B is much smaller
than the other models because the merging neutron stars
promptly collapse into a black hole, and thus, the mass ejection occurs
on only a  short time scale.}

\begin{table}[t]
\begin{center}
\caption[]{Parameters }
\label{tab:model}
\begin{tabular}{lcccc}
\hline \hline
Model & $m_1,\,m_2$ [$M_{\odot}$]  & $R_{\rm ns}\,[{\rm km}]$ & $M_{\rm ej}\,[M_{\odot}]$  & $E_{\rm ej}$\,[erg]    \\ \hline
B & $1.35,\,1.35$ & $10.96$ & $5\cdot10^{-4}$ & $7\cdot 10^{49}$ \\
HB & $1.35,\,1.35$ & $11.61$ & $3\cdot 10^{-3}$ & $10^{50}$ \\
H & $1.35,\,1.35$ & $12.27$ & $3\cdot10^{-3}$ & $9\cdot10^{49}$ \\ \hline
B uneq& $1.51,\,1.21$ & $10.96$ & $10^{-2}$ & $8\cdot 10^{50}$ \\
HB uneq& $1.51,\,1.21$ & $11.61$ & $5\cdot 10^{-3}$ & $3\cdot 10^{50}$ \\
\hline \hline
\end{tabular}
{\footnotesize{ $R_{\rm ns}$ is the radius of a non-rotating cold  neutron star of $1.35M_{\odot}$.}
}
\end{center}
\end{table}

The isotropic equivalent energy distributions at different polar angles
are also shown in Figs. \ref{fig:E} -- \ref{fig:E2}, demonstrating the anisotropy of the ejecta.

For the equal mass cases, the material ejected at $30^{\circ}$--$60^{\circ}$
has more kinetic energy.  For the unequal mass cases,
more material is ejected on the equatorial plane.
Another important feature is that the ejecta
moving faster than $\Gamma \beta \sim 1$ is somewhat isotropic for all the cases.
{Therefore, the early light curve arising from this mildly relativistic tail is
expected to be rather isotropic. }

Also shown in figures \ref{fig:E}--\ref{fig:E2}, for a comparison, is the
quasi-spherical slow ejecta model used by  \cite{Mooley2017}:
\begin{eqnarray}
E(>\Gamma \beta)=5\cdot 10^{50}\,{\rm erg\,} (\Gamma \beta/0.4)^{-5}~~~({\rm for}\,\beta <0.8)\ . \label{kunal}
\end{eqnarray}
This distribution can fit the observed data up to $\sim 100$ days after GW170817.
 Note that the non-thermal afterglow up to $\sim 100$ days is produced by a component faster than
 $\beta \approx 0.6$ \citep{Mooley2017} and,
 of course, this profile cannot be extended to lower velocities $\beta \ll 0.4$.
 The total kinetic energy distributions for model B is the closest to this distribution.

\begin{figure}
\includegraphics[scale=0.7]{eiso_H.eps}
\caption{Same as figure \ref{fig:E} but for model H with equal masses.}
\label{fig:E2}
\end{figure}

\section{The  dynamical ejecta emission}
\label{sec:radio}
The interaction between the expanding merger ejecta and the surrounding ISM results in
a shock, in which particle acceleration and magnetic field amplification
occur. As a result, this blast wave emits multi-wavelength
synchrotron radiation  \citep{NP11}.
Here, we numerically calculate the synchrotron
radiation emitted by the accelerated electrons since we are interested in
mildly relativistic blast waves, for which either limits, $\beta\ll1$,
or $\Gamma\gg1$, cannot be used.
To follow the evolution of the ejecta expanding in the ISM with a constant density, $n$,
we solve the adiabatic radial expansion of the ejecta at each polar angle
using the kinetic energy distributions given in the previous section.
The synchrotron flux from the blast wave element at each solid angle
 at a given observer time  is  calculated assuming
a power-law distribution of electrons, $dN/d\gamma_e\propto \gamma_e^{-p}$,
and the standard equipartition parameters $\epsilon_e$ and $\epsilon_B$,
which reflect the conversion efficiency of the internal energy of the shocked ISM to the
accelerated electrons' energy and magnetic energy respectively (e.g. \citealt{SPN98,NP11} and see \citealt{HP2015} for details). We fix the viewing angle to be $30^{\circ}$ \citep{Abbott2017ApJ} and set $\epsilon_e$ to be $0.1$.
Therefore, there are in total  three free parameters, $n$,  $\epsilon_B$, and $p$, with which we fit the observed data in  our afterglow modeling.

\begin{figure*}
\includegraphics[scale=0.7]{fluxdensity_p21_inte008_v2.eps}
\includegraphics[scale=0.7]{fluxdensity_p21_uneq.eps}
\caption{
Light curve models of the synchrotron flare that followed  GW170817. {\it Left} and {\it right} panels
show the light curves for the equal mass and unequal mass cases, respectively.
The solid circles, triangle, and squares
show the radio data ($3$\,GHz; \citealt{Hallinan2017,Mooley2017,Margutti2018}), optical data (r-band; \citealt{Margutti2018,Lyman2018}), and X-ray data (1 keV; \citealt{Haggard2017,Troja2017,Margutti2017,Margutti2018, Ruan2017, D'Avanzo2018,Troja2018}).
The optical  and X-ray flux densities are  multiplied by  factor of $10^{2}$  and $10^{3}$ correspondingly.
The open circle shows a marginal
detection at $6$\,GHz \citep{Hallinan2017} corrected to the flux density at $3$ GHz assuming a spectral index of $-0.55$.
The solid, dashed, dotted lines show the theoretical light curve arising from
the dynamical merger ejecta for model B, HB, and H, respectively. Here we assume microphysics parameters, $\epsilon_e=0.1$ and $p=2.1$, and a viewing angle of $30^{\circ}$.
}
\label{fig:L}
\end{figure*}

Figure \ref{fig:L} shows the calculated light curves for the different models as well as the observations  of GW170817.
The light curves match the observed data,
for
$n=0.008$--$0.04\,{\rm cm^{-3}}$,  $\epsilon_B= 0.05$--$0.1$,
and $p= 2.1$.
Note that even the higher values of the ISM density are  consistent with
the upper limit on the mean ISM density of NGC 4993\footnote{This upper limit is for a neutral hydrogen component of the ISM.
 The mean density of hot ionized gas around GW170817 is currently not constrained.}, $n\lesssim 0.04\,{\rm cm^{-3}}$,  inferred from
the upper limit on the HI mass  \citep{Hallinan2017}.
For the equal mass cases,  the radio and optical light curves
continuously rise up to $\sim 100$ days  and then have a plateau phase lasting a few hundred days.
This early component
is produced by the tail of the ejecta faster than $\Gamma \beta \sim 0.6$.
Model H  contains a  lower
kinetic energy at $\Gamma \beta \sim 1$. As this  fastest  component dominates the early light curve the flux density up to $20$ days is lower than those of model B and HB.

For unequal masses, the flux densities continuously rise until $1000$ days because
of the larger amount of material at low velocities. However, the slope of the calculated
light curves is steeper than the observed one because the kinetic energy distribution
of the these  models declines more steeply
 at high velocities.

An important feature of the X-ray light curves
is that they peak on a time scale of a few months to a year and then their temporal evolution is different from that of the radio and optical light curves once   the synchrotron cooling
frequency becomes lower than $1$ keV.
For model H, in particular,  the cooling frequency falls  below 1 keV
at early times $\sim 10$ days because of the required relatively large values of the ISM density and $\epsilon_B$.
Note that the exact location of the cooling frequency can be
higher due to several uncertainties (see the discussion in the next section). However,
it is generally expected that the cooling frequency crosses the X-ray band
on a time scale of a few months to a year in this  scenario.

\section{Discussion}
\label{sec:discussion}
{\it Cooling frequency:}
An important feature of the synchrotron light curves obtained
in \S \ref{sec:radio} is the evolution of the synchrotron cooling frequency,
that crosses the X-ray band on a time scale of a few months to a year.  After this time,
the  X-ray flux density declines with time faster than the radio and optical flux densities.
In the Newtonian limit ($\beta\ll 1$), the cooling frequency at a given time, $t$,
is approximately estimated as (e.g., \citealt{SPN98})
\begin{eqnarray}
\nu_c & \sim &0.5\, {\rm keV}  \left(\frac{\beta}{0.6}\right)^{-3} \left(\frac{n}{0.01\,{\rm cm^{-3}}}\right)^{-3/2} \\
& & ~~~~~~~~~~~~~~\times\left(\frac{\epsilon_{B}}{0.05} \right)^{-3/2} \nonumber
\left(\frac{t}{100\,{\rm days}} \right)^{-2},\label{eq:nuc}
\end{eqnarray}
or the cooling frequency for a given flux density is
\begin{eqnarray}
\nu_c  \propto \beta^{\frac{5p-6}{3}}n^{\frac{p-4}{6}}\epsilon_B^{\frac{p-8}{6}}
\epsilon_e^{\frac{2(p+1)}{3}}F_{\nu}^{-\frac{2}{3}}

\end{eqnarray}
where $F_{\nu}$ is the flux density at a frequency in the range of $\nu_a,\,\nu_m<\nu<\nu_c$.
Note that, for a given flux density, the cooling frequency  increases by
decreasing $n$ and $\epsilon_B$ and by increasing the velocity for the expected range of
the electrons' power-law index, $2<p<3$.
In other words, it depends sensitively on the kinetic energy of the fast tail.
The cooling frequency  can be higher than those of our models if
the kinetic energy at velocities faster than $\beta\sim 0.6$ is only slightly larger.
For instance, the kinetic energy distribution of Eq. (\ref{kunal}) results in $\nu_c \gtrsim 10$ keV at $100$ days \citep{Mooley2017}.
Note also that the cooling frequency is much higher for the cocoon  models \citep{Mooley2017,Nakar2018,Margutti2018,Lyman2018}, that involve an outflow much faster  than the fast tail of the dynamical ejecta \citep[see, e.g.,][]{Gottlieb+17B,Lazzati2017,Nakar2018}.

The X-ray observations around $100$ days
show that the X-ray flux density and the photon index in the X-ray band  are
consistent with a single power-law spectrum from the radio to  the X-ray bands \citep{Mooley2017, Margutti2018, Ruan2017, D'Avanzo2018,Troja2018}.
This suggests that the cooling frequency is above the X-ray band, ruling out models with much lower   cooling frequency, e.g., model H.
However,
it should be noted that
the estimate of equation (\ref{eq:nuc}) and  the cooling frequency used in our light curve modeling are correct only within
an order of magnitude.  In fact, \cite{GranotSari02} obtained the spectral breaks of the afterglows
for the Blandford-McKee solution and found that  the cooling frequency was higher by a factor of $\gtrsim 3$  than  the simple order of magnitude estimate \citep{SPN98}.
Therefore,
 models B and HB for the equal mass caes can be considered as  consistent with the current observed data.
However, a generic expectation of the dynamical ejecta scenario
 is  that the cooling frequency will cross the X-ray band on a time scale not much longer than a few months.

 Therefore further multi-frequency observations  will easily confirm or rule out this model.

{\it Late-time signal:}
In addition to the fast moving  dynamical ejecta,  there should be a main, sub-relativistic   ejecta component
that have produced the uv/optical/IR macronova/kilonova signal. As already mentioned
the  dynamical ejecta masses of our models,
$5\cdot 10^{-4}$--$10^{-2}M_{\odot}$,
are much smaller than those estimated from the macronova observations,
$\sim 0.05M_{\odot}$  (e.g., \citealt{Kasliwal2017}).
This component has the photospheric velocities of $\sim 0.1$--$0.3c$ and a kinetic energy of $\sim 10^{51}$\,erg,
which is also larger than the kinetic energy of the dynamical ejecta  in our dynamical ejecta models\footnote{The typical velocity of the macronova ejecta can be slower than
the photospheric velocities of $0.1$--$0.3c$. Numerical simulations show
that the velocity of the wind outflows, that we consider here as the dominant
outflow component producing the macronova/kilonova emission,
 is typically $\sim 0.05$--$0.1c$
(e.g., \citealt{fernandez2013MNRAS,fujibayashi2017,Siegel2017}). }.
Some other processes, not taken into account in the simulations used in this work,
must be responsible for the ejection of this additional mass.

\begin{figure}[t]
\includegraphics[scale=0.7]{fluxdensity_p21_long_B.eps}\\
\includegraphics[scale=0.7]{fluxdensity_p21_long_B_b01.eps}
\caption{
Same as figure \ref{fig:L} but on a longer time scale.
The radio flare arising from the ejecta component that
produced the uv/optical/nIR macronova signal is also shown.
For this component, we assume a mass of $0.04M_{\odot}$
and a single velocity of $0.2c$ ({\it top}) and $0.1c$ ({\it bottom}),
and the ISM density and microphysics
parameters are the same to the dynamical ejecta component of
each model.
}
\label{fig:L2}
\end{figure}

Considering now the total ejected mass as observed from the  uv/optical/IR macronova, we estimate the
 peak time and flux density of this slow component  \citep{NP11}:
\begin{eqnarray}
t_{\rm p} & \approx & 10^4\,{\rm day}\,\left(\frac{E}{10^{51}\,{\rm erg}} \right)^{\frac{1}{3}}
\left(\frac{n}{0.01\,{\rm cm^{-3}}} \right)^{-\frac{1}{3}}
\left(\frac{\beta}{0.2} \right)^{-\frac{5}{3}},\\
F_{\nu,{\rm p}} &\approx& 2\,{\rm mJy}\, \epsilon_{B,-1}^{0.775}\epsilon_{e,-1}^{1.1}
\left(\frac{E}{10^{51}\,{\rm erg}} \right) \label{eq:F}
\\
& & ~~~~~~\times \left(\frac{n}{0.01\,{\rm cm^{-3}}} \right)^{0.775}\left(\frac{\beta}{0.2} \right)^{1.75}
\left(\frac{\nu}{3\,{\rm GHz}} \right)^{-0.55}, \nonumber
\end{eqnarray}
where $\epsilon_{B,-1}$ and $\epsilon_{e,-1}$ are normalized by $0.1$ and
we set $p=2.1$. Figure \ref{fig:L2} depicts the flux densities from the
dynamical ejecta and the macronova ejecta.  Here we assume that the macronova
ejecta has a mass of $0.04M_{\odot}$ and a single velocity of $0.2c$ ({\it top} panel) and $0.1c$ ({\it bottom} panel),
and set the ISM density and the same microphysics parameters as those used for the
dynamical ejecta models (see figure \ref{fig:L}).
The bumps around $10^4$ --$10^5$ days in the light curves
are produced by the macronova component.
The actual shape of
the peak of the light curves is expected to be
broader due to the velocity structure of the macronova
ejecta. {Note that the cooling frequency of the
late emission is around  the uv/optical bands so that the
estimate of  equation (\ref{eq:F}) is applicable up to the optical band and
the X-ray flux density of the macronova component is much fainter than
that estimated by equation (\ref{eq:F}).}

This late-time emission  is one of the  notable differences between the dynamical ejecta and cocoon/structure jet scenarios.
For the cocoon/structure jet scenario, in which the ISM density
is much lower than that of the dynamical ejecta scenario,
the flux density from the macronova ejecta is expected to be
much fainter $\lesssim 50 \,{\rm \mu Jy}$ and the peak time is much longer, $\gtrsim 100$ yr.

{\it Angular size}:
The velocity of the fast tail that produces the afterglow at $100$ days is $\sim 0.6c$.
Therefore, the angular size of the afterglow is
$\lesssim 500\,{\rm \mu arcsec} (t/100\,{\rm day})$ for $> 100$ days.
 This is smaller by a factor a  few compared to that expected in the cocoon and structured jet models.
Therefore, these scenarios can be distinguished by future  VLBI observations  (\citealt{Hallinan2017}).

\section{Conclusion}
\label{sec:conclusions}
The fast tail ($\Gamma \beta \sim 1$) of the dynamical ejecta  of binary neutron star mergers, calculated in recent high resolution numerical simulations by \cite{Kiuchi2017}
contains kinetic energy of $10^{47}$ -- $10^{49}$ erg, depending on the neutron star equation
of state and on the binary masses. Mergers with  a softer neutron star equation of state, which gives
 smaller radius neutron stars, and
with a mass ratio close to unity eject larger amounts of the fast tail. The fast tail has somewhat isotropic
shape even for  models in which the bulk of the material is  large aspherical.

The interaction of this fast tail with  the surrounding ISM produces a blast wave whose synchrotron emission \citep{NP11} is  observed as the radio to X-ray signals that followed GW170817.
We compute this synchrotron emission  arising from  the ejecta profile obtained from the high resolution  numerical  relativity simulations and
 compare them  with the observed data of the non-thermal radiation that followed  GW170817.
We find that the multi-frequency observed data  can be
reproduced well for the equal mass binary models with a relatively soft equation of state.
In all cases, an ISM density of $\sim 0.01\,{\rm cm^{-3}}$ is required to obtain
the observed flux level at $\sim 100$ days after the merger.
For unequal mass cases, the  velocity gradient of the ejecta profile is steeper and the light curves rise more steeply than the observed one so that nearly equal mass mergers are favored in this scenario.

The dynamical ejecta scenario has three generic predictions:
\begin{enumerate}
\item The cooling frequency crosses the X-ray band on a time scale of a few months to a year leading to a cooling break in the X-ray light curve.
\item The outer ejecta velocity is $\lesssim 0.6c$ at $t \gtrsim100$ days so that the angular size
of the ejecta will be   $\lesssim 500 \,\mu{\rm arcsec}(t/100\,{\rm day})$.
\item The emission of the sub-relativistic  macronova/kilonova component of a mass of $\sim 0.05M_{\odot}$ and a velocity of
$\sim 0.1c$ will be continuously observable with flux densities of $0.1$--$1$ mJy on time scales of $10^3$ -- $10^5$ days \citep{NP11,piran2013MNRAS,HP2015}.
\end{enumerate}
These  features will enable us to observationally confirm or rule out this model in the near future.

\acknowledgments
We thank Paolo D'Avanzo, Gregg Hallinan, Raffaella Margutti, Kunal Mooley, David Radice, and Eli Waxman for useful discussions.
K.H. was supported by Lyman Spitzer Jr. fellowship at Department of Astrophysical sciences at Princeton University.
T.P. was partially supported by an advanced ERC grant TReX and by a grant from the Templeton foundation.
T.P. and E.N. were supported by the I-Core center of excellence of the Israeli Science Foundation.
Numerical  simulations were performed on K computer at AICS (project
numbers  hp160211, hp170230, hp170313),  on  Cray  XC30  at cfca  of
National  Astronomical  Observatory  of  Japan, FX10 at Information
Technology Center of the University  of  Tokyo,  HOKUSAI  FX100  at
RIKEN,  and  on Cray XC40 at Yukawa Institute for Theoretical Physics,
Kyoto  University. This  work  was  supported  by  Grant-
in-Aid  for  Scientific  Research  (16H02183, 17H06361,  15K05077)  of  JSPS  and
by a  post-K  computer  project  (Priority  issue  No.  9)  of Japanese
MEXT.

redpajama_set_name: RedPajamaArXiv


This site is dedicated to youth and their families working hard to create a better life for tomorrow and searching for a few resources to meet immediate needs today. Gainful.edublogs.org is constructed to be (youth) user-friendly and intuitive. Although several resources are listed on this site, thousands more can be found at www.211.org or other non-profit organizations in your area.
Hey Steffannie, Why Did You Create This Site?
Because I care. I'm a local counselor who works with youth and families. When they are in need of a helping hand, time is of the essence. Some of my clients find traditional information/resource sites difficult to navigate. This is a simple site, easy to navigate, and allows me to share resources that have proven successful over the years (as well as links to other tradition 'help' like National #211). Even more importantly, it's available 24-hours a day, 7-days a week from a cell phone or laptop. It was a labor of love to create, but worth every moment.


In the financial year 2018-19, funds have been released for the reorganisation, rejuvenation and strengthening of urban drinking water schemes. Funds worth Rs 1 crore have been sanctioned by Jal Sansthan for financial year 2018-19 for the reorganisation, rejuvenation and strengthening of under-maintenance urban drinking water schemes. For the reorganisation work of the Tudiyakot Drinking Water Scheme of Development Block of Mori of Uttarkashi District and giving the administrative and financial approval to reorganisation work of Saras Dhumrali Drinking Water Scheme, according to the budget manual, a financial sanction for the first phase amounting to Rs 7.27 lakh and total amount of Rs 14.23 lakh has been sanctioned. For the supply and installation work of separate size water meters for different zones of Pithoragarh, total amount of Rs 211.98 lakhs have been found justified, on the basis of which the abovementioned amount has been sanctioned. In the government order, while giving the administrative and financial sanction of funds, in the financial year 2018-19, the first instalment of Rs 84.79 lakh has been released.


text: define({save:"Gorde"});

redpajama_set_name: RedPajamaGithub


To train Welders on the MIG welding process from the basics, to a terminal test and through to ASME 1X and BS/EN 9606-1 or BS/EN 9606-2.
Previous knowledge of Manual Metal Arc Welding would be advantageous.
5 to 20 days, dependent upon the ability of the learner.
Visual inspection of the trainees' practical work and a terminal test to ASME 1X and BS/EN 9606-1.


A mid 19th century building converted from three cottages with some later additions. The original pub entrance was the other side of where it is today although no external traces of it remain since the pub was extended many years ago. An old photo behind the bar shows how it would have looked. There are two distinct bar areas with the much larger split level lounge to the front. This is very much a locals' pub but visitors are made welcome and raising the subject of beer is almost guaranteed to get several conversations going!


Before setting out for 5 weeks of travel through Southeast Asia, I stocked up on the Rough Guides to the region.
For my time in Vietnam, Cambodia and Thailand, I not only researched using the individual country guides but was delighted to find that they publish a complete guide to the area called Southeast Asia on a Budget. This guide includes Brunei, Cambodia, Indonesia, Laos, Malaysia, The Philippines, Singapore, Thailand and Vietnam, plus Hong Kong and Macau.
A comprehensive guide like this has 2 huge benefits. The bennie of most value to me is that if I'm visiting more than one of the included destinations, I don't have to carry around more than one guide. But, the other great bennie is that the budget traveler won't have to pay for multiple guides. Backpacker heaven!
In addition to the great ideas for budget travel, the SE Asia guide also includes highlighted boxes for treating yourself to a night out. A nice little perk if you find yourself with a little extra cash.
The country guides, such as the Rough Guide to Vietnam, are less about budget travel but provide a great overview of the area including a wide range of restaurants, cafes, hotels and bars. There's also loads of information on culture and history.
The Rough Guides are all available on Amazon.
Join other Wanderlusters and stay updated on travel-related items by subscribing via email or RSS feed.
Big fan of the RGs, me. They're invariably brilliantly written (and therefore a good read in their own right, even when back home) and I've always found them reliable.
Rough Guide and Lonely Planet are my reference staples (with National Geographic filling every other corner of my bookcase).
Have you seen the recently reprinted National Geographic guide to Vietnam? Gorgeous!
I have yet to visit Southeast Asia. I have been inspired to do so, but I would have to do much researching before making the plunge. I used to use Lonely Planet for many things or Let's Go, but any other recommendations like the Rough Guide that would be an all in one would be great.
Nice, but I wonder how the guides compare to the Lonely Planet ones which I have used in the past. I have found that the LP guides are sometimes very helpful, but sometimes caused me some trouble with inaccuracy!


The NXT Takeover: New York card continued to take shape with the North American title now on the line as well.
NXT General Manager William Regal announced last night on Twitter that champ Velveteen Dream will take on number one contender Matt Riddle.
This is the fifth and probably last match to be part of the main card.
The NXT Women's title match was also confirmed last week with a big fatal four-way match involving Shayna Baszler defending her title against Kairi Sane, Bianca Belair, and Io Shirai.
This year's NXT Takeover will take place on Friday rather than Saturday and will stream live only on the WWE Network.


text:
A Dissertation on the Prophecies Relative to Antichrist and the Last Times ...
De Ethan Smith
the battle of the great day. And among other de. scriptions, this Beast is represented as having a dead. ly wounded head healed; or as having a wound by a sword, yet afterwards living. And this trait of his character is referred to, in the above verses, in the course of the description of the second Beast: The reason of which is this; the pagan Beast's having been wounded to death in the head, yet afterwards living, was his most remarkable characteristic.
By this therefore, he would naturally be spoken of, when allusion was had to him. But this reference was not designed to indicate, that this healing of the wounded head was then already effected, nor to indicate any thing relative to the time, when the Roman Beast was to recover life. The fact, I believe, will appear to be, that this recovery of life was then far future, and that the Roman Beast lived, through all the ages of the prosperity of the Papal Beast, only by his image in the management of that officious Pontificate. But that he himself, all that time, lay dead. The idea of two Beasts prevailing at the same time, and on the same ground, for 1260 years; or existing at all collaterally; is a solecism, an absurdity never to be admitted. Each one of two things cannot be the greatest. A Beast, as a predominant power, a dynasty, and the sum of an empire, may have a number of collateral horns. But he cannot admit another Beast on the same ground; and both continue. There cannot be in any body, at the same time, more than one supreme power. Symbolical language cannot admit of two Beasts in Christendom at the same period. When the last head of the Roman Beast arises, and takes Popery into its possession, the latter then ceases to be, or to be called, a Beast. It is henceforward called the false prophet,* the mother of harlots;t and the horn of the Beast. But it is never after this called a Beast.
* Rev. xix, 20, and xvi, 13. + Rev. xvii, 5. Dan. vii, 11.
Si am aware it may here be objected to my proposition, that we read in Dan, vii, 12; As concerning the rest of the Beasis, they had their dominion taken away; yet their lives were prolonged for a season and time: as though they all existed, as Beasts, at one and the same time. But this cannot be the mcan.
The only remaining passage, which seems to militate against the explanations given, is in verse 14th, on the
ing of the prophet. When the real sense of the passage is ascertained, I think it will afford no objection to my proposition, that two Beasts cannot exist on the same ground, at the same time. The pasage, it seems, was designed to note the contrast between the manner, in which the Antichristian Beast shall be destroyed; and the manner, in which the preceding ancient Beasts were overthrown. The former loses not only his dominion as a Beast, but his existence on earth, at the time of his overthrow; being not subjugated by a human conqueror, as were the others, but utterly destroyed by the Lord from heaven, in the battle of that great day of God Almighty: when not only the Beast is slain, but his body is destroyed and given to the burning flame; as in the preceding verse. But so it was not with the former and ancient Beasts, when they lost their dominant power. How many soever of their soldiers were in fact slain in battle, nothing took place, which was like the bodies of those Beasts (the multitudes, who had constituted them) being destroyed, and given to the burning flame; as is to be the case with Antichrist. The powers symbolized by those Beasts, instead of being utterly destroyed, were only subjected, each in his turn, to the dominion of the succeeding power; and there received tolerable treatment as subjects. And to express this difference of treatment, in the immediate view of the body of the Antichristian Beast, being destroyed, and given to the burning flame, at the same time, in which the Beast is slain, as in the preceding verse; it is said, of the rest of the Beasts, they had their dominion taken away; yet their lives were prolonged for a season and time. This elliptical mode of expression was most naturally adopted, instead of expressing the whole evident sense, as follows: Concerning the rest of the Beasts, they had their dominion taken away; yet the multitude who had constituted their body, instead of being destroyed and given to the burning flame, as shall be the case with Antichrist, were chiefly spared, and received tolerable treatment under their new masters. But the prophet could not mean to teach us, that all these Beasts had existed, as Beasts, at one and the same time! Nothing could be more unnatural; or untrue. When the Macedonian he-goat, for instance, stamped upon, and slew the Persian ram, this ram is never represented to be in existence, as a Beast, afterwards; although the people of Persia still existed for a season and time; and to the present day.
The opinion, that the two Beasts, in Rev. xiii, were co-existent for 1260 years, must be an absurdity, A universal or a great empire, disposed to persecute the Church, is in prophetic style a Beast; whether the empire be of secular dominion; or a hierarchy, But when did iwo such independent, persccuring
subject of the Papal Beast, And deceiveth them that dwell on the earth, by the means of those miracles, which he had power to do in the sight of the Beast. Here it seems to be suggested, that the Papal Beast wrought miracles in the sight of the Pugan Beast; as though the latter were already revived. But if he were already revived, what need of an image being inade to him? And it has been noted that two Beasts cannot exist on the same ground, at the same time. It cannot mean then, that the Pagan Beast was already revived. The clause, in the sight of the Beast, must therefore
powers co-exist on the Roman earth; or in the world? Were it possible for two vast empires to be found independent of each other, and acting in no concert, yet both persecuting the cause of Christ; possibly they might be symbolized by two co-existe ent Beasis. But two such powers never co-existed on the Roman earth. Popery fully answered to such a power. But no civil power, within the Papal influence, did at the same time exist, which could answer to such a power. However independent of the Pope the emperors of Germany, or any other civil powers within the Roman earth, might have been, as to their civil jurisdictions during the Papal supremacy; yet those civil powers never persecuted the cause of Christ, only at the Papal instigation. The hierarchy was the system, during its supreme power, that persccuted the witnesses. The civ. il authorities were only iis executioners. "The fourth council of Lateran (says Bishop Burnet) decreed that all heretics should be delivered to the secular power, to be extirpated." In the time of Pope Innocent the third, false accusations were raised against the Waldenses and Albigenses;-upon which, the Pope decreed a crusade against them. And he sent his emissaries into the west, enjoining it on sovereign princes, and other Christian people, to extirpate those heretics. Upon this Vitringa observes, that in France alone, a million were destroyed. The persecution (though executed by the civil powers) originated in the Papal Beast. The same is true of all the perseculions during the Papal supremacy. In this thing the hierarchy was what great city, which reigned over the kings of the (Roman) earth."
The reign was not theirs; but hers. The imperial authority, co-existent with Popery, was nothing more (us a persecuring power) than one of the invo horns of the Pa
This Beast is presented with two horns. And his clergy, and the civil powers under his superstition, were most fity symbolized by these two Papal hórns:--- As was his system (f real idolarly, under the Christian name by an image made to inc oid Pägan Bomst.
pal Beast.
mean, either in the sight of the image of the Beast; putting by a metonymy, the prototype for the copy; or, in admiration, or imitation of the Pagan Beast; i. e. that the Papal hierarch wrought his deceptive miracles with a view to confirm a system no better, than the old Pa. gan system. This he actually did, in what was called the image of the Beast, before described. "In the sight of the beast; i. e. to his honor, and to gain him a reputation!" (Pool on the passage.) And what follows the above clause, as an explanation of it, appears to confirm this as being the true sense; saying to them, who dwell on the earth, that they should make an image to the Beast. As the Papal Beast caused the earth to worship the Pagan Beast, (v. 12) by causing them to worship his image; (v.14) so the miracles wrought by the Papal Beast were done in the presence of the Pagan Beast, by being done in the presence of his image. Mistaking the sense of these several passages, and the one before explained, relative to the continuance of the first Beast forty and two months, I conceive, has been the occasion of perplexing commentators, and of leading them erroneously to blend and confound the Roman and Pa. pal Beasts. I have shown that the two powers in Daniel are given as distinct; also in Revelation xiii, just rioted. And they are thus presented, in Revelation xvii; to which I shall now attend. sage, the terrible Power of the last days is strikingly exhibited.
One of the Angels, who in the xvith chapter had poured out the vials of the wrath of God, proposes to show to the evangelist the judgment, or destruction, of the Papal harlot. John is carried into the wilderness. The harlot in her turn is in trouble: She is bewildered. John beholds a woman in lewd attire; with the superscription of her abominable character upon her forehead; indicating, that she, as the worst of criminals, is presented for speedy execution. Bishop Pearson and Doctor Lardner, upon the superscription over the head of our Savior, have shown, that it was a custom among the ancient Romans to place on, or over, the foreheads of the worst of criminals, the superscrip
In this pas. tion of their guilt, at the time of their execution. The superscription upon the cross of our Savior was upon the same principle. The great harlot is present. ed with this her superscription upon her forehead, inscribed in capitals; MYSTERY, BABYLON THE GREAT, THE MOTHER OF HARLOTS, AND ABOMINATIONS OF THE EARTH. And she has also upon her the symbols of her past magnificence, and of her allurements, and crimes; in order to shew her to be the Papal hierarchy. She is mounted on a Beast, that may be said to be bearing her to her judgment or execution. * This Beast is of a scarlet color, to denote his cruel and bloody character. He is full of the names of blasphemy, to denote his Infi. delity and wickedness. And he has seven heads, as well as ten horns, to identify in him the old heathen Roman empire now revived.
The Angel, in explaining the mystery of the Beast, informs, that he was, and is not; and shall ascend out of the bottomless pit, and go into perdition; and they, who dwell on the earth, shall wonder / whose names were not written in the book of life from the foundation of the world) when they behold the Beast, that was, and is not, and yet is. The seven heads, the Angel informs, (in addition to their being seven mountains, on which the woman sitteth, or on which Rome was built,) are seven king's, or forms of government, in the different periods of the Roman empire. "Five are fallen," those of Kings, Consuls, Tribunes, Decemvirs, and Dictators, were past, when John had his vision. "One is;" the then present form was Imperial, and was the sixth head, or form of government, "Liid the other is not yet come, and when he cometh, lte must continue a short space." Concerning this seventh head, or form of government, then future, which when it should come should continue a short space, expositors have been divided and perplexed. Every scheme, which they have adopted, appears attended with unanswerable objections. The reason I think is obvious. Nothing had taken place, to
* This is not a woman directing and governing an empire; but just the reverse.


text:
<?php

namespace Panza\Library;

use Panza\Library\BranchMapping;
use Panza\Library\Issue\Comment;
use Panza\Library\Issue\StatusTransition;

/**
 * Interface Issue
 * @package Panza\Library
 */
interface Issue
{
    /**
     * Returns unique id of issue.
     *
     * @return mixed
     */
    public function getId();

    /**
     * Returns issue field value.
     *
     * @return mixed
     */
    public function get($name);

    /**
     * Returns issue links value (by specific $type).
     *
     * @return Issue[]
     */
    public function getLinks($type);

    /**
     * Returns the array with mappings of sources and destinations.
     *
     * @return BranchMapping[]
     */
    public function getBranchMappings();

    /**
     * Returns the mapping by name.
     *
     * @param string $name
     * @return BranchMapping
     */
    public function getBranchMappingByName($name);

    /**
     * Returns the title.
     *
     * @return string
     */
    public function getTitle();

    /**
     * Returns the description.
     *
     * @return string
     */
    public function getDescription();

    /**
     * Returns information about status transitions.
     *
     * @return StatusTransition[]
     */
    public function getStatusTransitions();

    /**
     * Returns comments.
     *
     * @return Comment[]
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Can an estate make a valid installment election on a late-filed return?
Taxpayer Says: The estate fully complied with the requirements of the Internal Revenue code and substantially complied with the requirements of the related estate tax regulations for making an election to pay the tax due on an installment basis.
Internal Revenue Service Says: A valid installment election can only be made on a timely filed estate tax return. Because the estate filed the tax return late, the election was untimely and denial of the election was appropriate.
From Internal Revenue Code Section 6166: Under section 6166, a qualifying estate may elect to pay the estate tax in installments over an extended period.
From Internal Revenue Code Section 6166(a): Extension of time for payment of estate tax where estate consists largely of interest in closely held business. (a) 5-Year Deferral; 10-Year Installment Payment.–(1) In general.–If the value of an interest in a closely held business, which is included in determining the gross estate of a decedent who was (at the date of his death) a citizen or resident of the United States exceeds 35% of the adjusted gross estate, the executor may elect to pay part or all of the tax imposed by section 2001 in two or more (but not exceeding 10) equal installments. ***Remaining paragraphs omitted.
From Internal Revenue Code Section 6166(d): Election.–Any election under subsection (a) shall be made not later than the time prescribed by section 6075(a) for filing the return of tax imposed by section 2001 (including extensions thereof), and shall be made in such manner as the Secretary shall by regulations prescribe. If an election under subsection (a) is made, the provisions of this subtitle shall apply as though the Secretary were extending the time for payment of the tax.
(a) In general.–Section 6166 allows an executor to elect to extend payment of part or all of the portion of the estate tax which is attributable to a closely held business interest (as defined in section 6166(b)(1)). If it is made at the time the estate tax return is filed, the election is applicable both to the tax originally determined to be due and to certain deficiencies. If no election is made when the estate tax return is filed, up to the full amount of certain later deficiencies (but not any tax originally determined to be due) may be paid in installments.
(6) The facts which formed the basis for the executor's conclusion that the estate qualifies for payment of the estate tax in installments.
In the absence of a statement in the notice of election as to the amount of tax to be paid in installments, the date selected for payment of the first installment, or the number of installments, the election is presumed to be for the maximum amount so payable and for payment thereof in 10 equal installments, the first of which is due on the date which is five years after the date prescribed in section 6151(a) for payment of estate tax.
In general, federal estate tax returns (Form 706) are due within nine months of the date of death. The estate tax is generally due at that time, too.
As an executor, you can request a six-month extension of time to file the estate tax return. If you have reasonable cause, such as insufficient liquid assets, you can request an extension of up to a year to pay the estate tax.
When 35% or more of the estate assets consist of interests in a small family business, you can request to pay the estate tax related to the business in up to ten annual installments. The request is known as a section 6166 election.
In this case, the estate tax return was due June 27, 2007. The taxpayer requested an extension of time to file, which was granted, until December 27, 2007. Along with the extension, the taxpayer attached a letter stating the intention to elect the section 6166 installment option, and included a check for the initial payment of $9,500,000.
In December, on the advice of an attorney, the taxpayer requested a second extension of time to file. The taxpayer attached a second letter to this extension, reiterating the estate's intention to elect the installment option for payment of the estate tax.
The IRS disallowed the second extension of time to file, stating the additional time was not allowed under the statute.
The taxpayer filed the estate tax return on June 1, 2010. The taxpayer checked the box on Form 706 to elect installment payments and provided all the information required in the tax regulations, including detail of interests in closely-held businesses. In between the second extension request and the actual filing of Form 706, the estate made annual payments approximately consistent with the installment election and noted on the payments that they were related to the election.
The Internal Revenue Service denied the section 6166 installment request because the estate tax return had not been filed on time. The IRS says a valid installment election under section 6166 can only be made on a timely filed Form 706. Because the estate tax return was filed late, the election under section 6166 was untimely and denial of the election was appropriate.
The taxpayer says section 6166 of the Internal Revenue code only prescribes the time frame in which the election must be made, and does not state that the election must be made on, or in conjunction with, a timely filed estate tax return. In addition, despite the failure to comply with the literal requirements of the related regulation, the taxpayer argues the estate substantially complied because its actions of attaching a statement, checking the box and making payments put the IRS on notice that an election had been made.
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For the IRS. The information mandated by section 20.6166-1(b)(5) and (6), Estate Tax Regs., is indispensable to the making of an election. Such information is necessary to enable the Internal Revenue Service, as well as the estate itself, to determine whether the estate qualifies for an election under section 6166. In other words, such information goes to the essence of the statutory purpose.
By failing to provide essential information regarding the estate's closely held business interests–information that goes to the essence of the statutory purpose–the estate did not substantially comply with regulatory requirements, and relief under the doctrine of substantial compliance is not available.
In addition, the time to make an election under section 6166 is fixed by statute. The estate did not timely file its return, nor did it make a timely election under section 6166. Therefore, the estate did not properly make a valid election under section 6166.
Definition — Capital or Ordinary?


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The Dead South have been described as outlaws and modern hillbillies, but the best way to describe the Regina-based band is fearless. They're a rare musical commodity, a band that's equally compelling on record as they are on stage.
While The Dead South's signature blend of bluegrass and classic folk is familiar, it's also eminently fresh; fuelled by the kind of energy and ethic you'd associate with a punk band. "A lot of our inspiration comes from an old school feel, but our sound is an amalgamation of the we all like, and the punk influence is definitely there," says vocalist/guitarist Nate Hilts.
Since the release of their second record, Illusion & Doubt, in late 2016, The Dead South have proven themselves a force to be reckoned with on both sides of the 49th parallel and even in Europe; selling out the entire previous tour in 2017. Enough reasons to have them back over again. In March 2019 the Dead South is coming back for two shows in the Netherlands:
27/03 Amsterdam NL Melkweg
28/03 Eindhoven NL Effenaar
Related artist: The Dead South back


Certain information, like your name, current profile picture and cover photo, will always be viewable by strangers. So that was basically where that all began. In Legacy Josh breaks up with Reed when he finds her with Dash. But don't worry, you still have the final say. Your browser does not support the video tag. Halls of residence[ edit ] Easton Academy is unofficially distinguished by a caste -like environment, socially divided by lower-, middle-, and upper-class dormitories. As the series progresses, Noelle becomes Reed's best friend and ally. And then it just from there became, 'Who is my main character going to be?
Reed Brennan The collected, curious protagonist, Reed is a brown-haired girl from Pennsylvania who enters Easton Academy for her sophomore year on a scholarship at the beginning of the first book. Your browser does not support the video tag. She becomes a secondary character following the completion of the series' first arc. All you need to do next is to put the finishing touches and enjoy your memories once the book arrives at your door. But you can determine who sees other kinds of content. However, halfway through Vanished Reed is forced to break up with Josh, because someone is holding Noelle hostage and is giving Reed tasks to win her life back. The series' original Billings Girls Billings House An upperclassmen dorm for girls, recognized as the most prestigious of all houses in the series. Hull Hall Hull Hall is where members of staff reside. Simply tell us where you would like your photo book delivered and it will be with you in a flash. Coming from a shaken family and a mundane everyday life, she is eager to explore the brand new setting that awaits her in Connecticut. Like Kiran, Taylor becomes a secondary character following the completion of the series' first arc. Furthermore, some are not above resorting to methods such as bribery, blackmail, and treachery. She has extremely good sense in fashion, and is capable of turning people into superstar lookalikes. Drake House Drake is a dormitory for upperclassmen boys, nicknamed "Dreck" because it is supposedly where all the unsavory boys at Easton live. Don't worry, it is all fully private as it all happens on your phone or tablet and your photos are not uploaded anywhere. Where are we going to get the mystery from? It was pretty natural. Of the original covers, the models appearing on the first book—who grace the next three installments as well—portray the following characters according to Kate Brian: Halls of residence[ edit ] Easton Academy is unofficially distinguished by a caste -like environment, socially divided by lower-, middle-, and upper-class dormitories. Moenks and co-photographer Laurent Alfieri had collaborated before working on Private, at some points taking photos of young businesswomen from around the world to illustrate a series of articles written by David Benaym for L'Officiel. Characters[ edit ] Private has an expansive cast and a regularly changing hierarchy. She is also known to be shallow and 'bratty' to others. Add photos from your camera roll, Instagram, Dropbox or Facebook. To do so, go to your profile page and click the three dots in the bottom right corner of your cover photo. Our Magic Books algorithm will do it for you in seconds and you can just focus on the best part — putting on the finishing touches and enjoying your memories. Though gifted both academically and athletically, her first major aspiration at Easton is to get into Billings House, which holds the allure of great social privileges and respect.
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The record cover & vinyl comes with full Letter's of Authenticity by James Spence Authentication (JSA). Record Cover (Certification Number: Z19411) & Vinyl (Certification Number: Z19947). The record cover has some wear from the years.
If you have any questions at all, free to message us anytime! Be sure to check out our other great items! The item "LEONARD COHEN The Best Of Album Cover & Vinyl Record Signed! JSA Certified" is in sale since Sunday, July 16, 2017.
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The gospel legend invited almost all the female artists performing at Luck on stage for a powerful cover of "The Weight"
Willie Nelson's ranch is a little bit like Disney World, except with less cotton candy and a lot more marijuana—but just as many attractions.
At this year's Luck Reunion, which happened, as it does annually, smack in the middle of South By Southwest week on Thursday, March 14, cowboys and country fans converged at Nelson's sprawling property outside Austin in Spicewood, Texas for a day of music, food and merrymaking. The one-day music festival, which was sponsored by Southwest, showcased acts from across the rock, country and Americana spheres including Nathaniel Rateliff, The Marcus King Band, Mountain Man and Austin's own Shakey Graves. Far removed from the chaos of downtown Austin, Luck Reunion was the gloriously laid-back respite attended by leather-clad roadies and Nashville sceners I didn't know I needed. The night wound down with a career-honoring performance from Willie Nelson himself.
It's hard not to love her, right? Staples did it again at Luck. Wrapping up a joyful, dance-move inducing set that included a cover of the Talking Heads' "Slippery People," the always soulful 79-year-old, a festival headliner with a stage named in her honor, welcomed a troupe of fellow Luck artists—Nathaniel Rateliff, Mountain Man, Yola, Haley Heynderickx, Courtney Marie Andrews and pretty much every other female artist who performed that day—for another rendition of "The Weight." Staples is proof that music is still an overwhelming force for good, possessing the power to inspire social change and, as one 2019 organization icon might say, "spark joy." Seeing her up there alongside a fiery team of up-and-coming women artists, growling out every "Take a load off Fanny" with equal parts intensity and compassion, was a religious experience. Staples is pure and good and we need her as much now as we did in the 1960s. She preaches love without sounding preachy, and that night at Luck, she delivered a sermon I'll not soon forget. Be still my beating heart.
Want more Mavis? Read our list of 10 things you didn't know about Mavis Staples. Below, watch a 2011 interview with Staples at Bonnaroo. For more information about Luck Reunion, visit the festival's website.


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The conference will include a mix of keynote speeches and practical workshops on a range of issues, including finance, HR and wellbeing.
Click here to for conference session outlines.
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The conference will take place on Thursday 13 June 2019 at St James' Park, Newcastle, within easy access of the A1 and walking distance from Newcastle city central station.
Registration will be from 8.00am and it is expected to finish around 4.00pm.
Over lunch and coffee breaks you will be able to tour the conference exhibition and engage with our range of specially selected provider organisations, meet new colleagues and expand your personal network.
Large discounts available when booking a group of 5 or more delegates. Contact us for more details.


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Home / Opinion / Put a pause on the straws
Put a pause on the straws
By Rachel Schmid on February 9, 2018
Over 500 million straws are used daily in America alone.
In a lifetime, it is estimated that the average human will use over 35,000 straws, and this is a low estimate.
If every American used two plastic straws a day for 70 years, that is over 51,100 plastic straws in a lifetime.
Not only are these small tubes of plastic unnecessary for beverage consumption, but they are also the sixth most common type of litter. Since plastic straws are too small to recycle and usually made of other materials, they end up in garbage cans, landfills and most importantly the ocean.
It is estimated that 8 million tons of plastic are dumped into the ocean annually. An estimated 71 percent of seabirds and 30 percent of turtles have been found with plastics in their stomachs. When they ingest plastic, marine life has a 50 percent mortality rate.
Once Sophomore Sophia Schillinger and 2015 graduate Hiram Marquez heard about this issue, they decided to take action.
"One day I went home and my dad told me, 'Hey, stop using straws. They are bad for you.' At first I was jokingly saying I wouldn't use straws anymore. I would tell other people not to use straws, and they would ask me why do I decided to do my own research. I learned how bad they are and how stupid it is that people even use them," Marquez said.
Sophia saw the passion of Marquez through an Instagram post and was influenced by a funny picture with a powerful message.
"Hiram Marquez, who is a small activist at UNI, posted a photo on Instagram about straws getting stuck in penguins' throats. It was a funny photo because he is a really funny guy, but it really got my attention. I also look up to him, so I decided that I should stop using plastic," Schillinger said.
Schillinger has known Marquez for years and looks up to him greatly as a runner and a person. His influence impacted her, and she decided not to only make changes herself, but influence her friends similar to the way Marquez influenced her.
"Right after a cross country meet, my friends and I went to Rudy's. They have a straw dispenser where you push the button and the straw comes out. They were all using straws, so I told them how they hurt the environment. Now every time we go out to eat, I tell them and everyone I see not to use a straw," Schillinger said.
Marquez also influences others not only through Instagram and Snapchat where he "exposes" people on his stories for using straws, while showing others the effects through real videos.
"In the beginning, my approach wasn't the greatest because I would just tell people not to use them and attacking them, which doesn't work. Usually people will just use them more if you do that. I show people the sea turtle video with the straw in its nose and just educating others on the issue," Marquez said.
After a video of scuba divers pulling a small plastic straw from a turtle's nose swept the Internet activists have jumped onto the "The Last Straw" campaign. This has sparked a chain reaction similar to Marquez and Schillinger for people to start making changes. California is trying to pass a bill where restaurants cannot give straws to customers without asking, and may different campaigns and companies have started to end the use of the plastic straw.
With the amount of plastic being used daily increasing, it seems like one little straw would not make that big of an impact. However, both Schillinger and Marquez disagree.
"People tell me that there is so much more than straws. It is a one step at a time type of deal. When you tell people about straws, they usually start thinking about plastic in general, and that creates a movement," Marquez said.
The movement itself is not only a personal choice, but something much bigger than oneself. The use of a single plastic straw.
"Think about if you really need this piece of plastic and not only how it will affect you, but the world around you," Schillinger said.
Schillinger and Marquez are also both very optimistic for a future without plastic straws.
"I hope for a future without straws. I do see one, but not that close unless people do start caring. There are people who I tell how bad straws are, and they would rather suck on their smoothie with a straw without realizing," Marquez said.
Most of the plastic straw waste is a result of ignorance of many people across the nation.
"I definitely see a future without straws. I feel like we will get there. It will take awhile to get people to adjust—especially if we keep taking things from the world and we want to keep living on it," Schillinger said.
Both Marquez and Schillinger have a growing straw collection where they pick up straws on tables at restaurants, the ground and other various places. Marquez simply keeps a box in the backseat of his car, but Schillinger has a bigger plan for her growing collection.
"At first it was just a crazy idea that I had the night I went to the restaurant with my friends," she said, "but then I started collecting more and more. I planned to build a penguin holding a straw, out of straws. This could be going on over years depending on how many I collect."
It is estimated that by the year 2050, there will be more plastic in the ocean than fish. However, Americans still persist on using straws full throttle.
It is just a small piece of plastic anyway, right?
Related ItemsHiram MarquezopinionSophia Schillingerstrawswaste
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