text:
\section{Introduction}
The ejecta in supernova remnants (SNRs) drive the exchange of mass and the chemical evolution of the galactic medium. The structure of SNR ejecta has been proved to be knotty, and several clumps have been observed at different wavelegths in remnants of core-collapse supernovae, as G292.0$+$1.8 (\citealt{phs04}), Puppis A (\citealt{kmt08}), and Cas A, where knots have been observed also beyond the main shock front (\citealt{fhm06}, \citealt{hf08}, \citealt{drs10}).

The Vela SNR, being the nearest SNR, represents a privileged target for this kind of studies, since it is possible to observe fine structures down to small physical scales. Despite the bulk of the X-ray emission of the Vela SNR is associated with the post-shock interstellar medium, X-ray emitting ejecta have also been observed. In particular, six protruding features, with characteristic boomerang morphology, (labelled Shrapnel A-F) have been identified in the Vela SNR by \citet{aet95}, who argued an ejecta origin for these structures which appear to be detached from the remnant. The association with ejecta fragments has been supported by more recent observations performed with $Chandra$, \emph{XMM-Newton}, and $Suzaku$.
The analysis of the \emph{XMM-Newton} observation of Shrapnel D, has revealed that O, Ne, and Mg abundances are significantly larger than solar (\citealt{kt05}). A similar abundance pattern has been observed with $Suzaku$ in Shrapnel B \citep{yk09}, but in this case the overabundances of the lighter elements are less prominent, suggesting more effective mixing with the interstellar medium (ISM).
A $Chandra$ observation of Shrapnel A, whose projected distance from the center of the remnant is larger by $\sim 20\%$ than Shrapnel D, reveals instead oversolar Si$:$O ratios (\citealt{mta01}). Significant Si overabundance (Si$\sim3$) has been confirmed by \citet{kt06}, who analyzed an \emph{XMM-Newton} observation, finding solar or subsolar values for the O, Ne, Mg, and Fe abundances.
These results show differences in the chemical composition between Shrapnel A and Shrapnel B and D.
In the northern rim of the Vela shell, \citet{mbr08} discovered new X-ray emitting clumps of ejecta whose projected position is behind the main shock front. The relative abundances (O:Ne:Mg:Fe) of these new shrapnel are in good agreement with those observed in Shrapnel D. Similar abundance pattern have been observed also by \citet{lsd08}, who found ejecta-rich plasma in the direction of the Vela X pulsar wind-nebula.

The present day morphology of SNRs and the structure of ejecta are believed to reflect the physical characteristics of the SN explosion (e.~g., intrinsic asymmetries of the explosion, interaction of the early blast with the inhomogeneities of the circumstellar medium, physical processes in the aftermath of the explosion, etc.) and their detailed study promises
to contribute to our understanding of the SN explosion physics. In the light of these considerations, it is then interesting to model the evolution of the ejecta knots to understand how the current position and chemical properties of the shrapnel in the Vela SNR depend on the physical conditions at the supernova explosion and on the dynamics of the explosion itself.

The evolution of dense, supersonic clumps of SN ejecta running in a uniform medium has been studied by \citet{ajr94} and \citet{jkt94}, who identified three main stages of evolution: a bow-shock phase, an instability phase and a dispersal phase. However, these models do not describe in detail the interaction of the clump with the remnant (post-shock medium, main shock, reverse shock) and do not include important physical effects (as thermal conduction and radiative cooling). \citet{cpr96} included radiative losses in their 2-D models, but they focussed on the interaction of a knot with a very small supernova remnant ($\sim 10^{17}$ cm, i. e. more than 100 times smaller than the Vela SNR) evolving in an extremely dense medium ($10^7$ cm$^{-3}$). A hydrodynamic model (without thermal conduction and radiative cooling) specifically tuned for the Vela SNR has been developed by \citet{wc02} (hereafter WC02) who followed the evolution of a shrapnel by using 2-D simulations in spherical coordinates (because of the
geometry of their simulations, the shrapnel are modeled as toroidal structures with very large masses). WC02 did not model the early evolution of the ejecta knot, but started their simulations at the time $t_{rev}$, corresponding to the first interaction of the shrapnel with the reverse shock front. They explored different values of $t_{rev}$ and of the density contrast between the shrapnel and the surrounding ejecta, $\chi$, and found that, in order to produce an observable protrusion on the shock front (like that observed in Shrapnel A-F), a very high density contrast ($\chi\sim 1000$) is necessary. With lower density contrasts ($\chi<100$), the shrapnel are rapidly decelerated and fragmented by hydrodynamic instabilities and the observed features cannot be reproduced (for the effects of hydrodynamic instabilities on shocked clouds see also \citealt{kmc94} and \citealt{opr05}). Large density inhomogeneities in the clumps are difficult to explain in a core-collapse SN explosion. WC02 argued
that a model that includes the effects of radiative cooling may show that lower values of $\chi$ are needed to match the
observed protrusions.
Also, WC02 do not include in their model the effects of thermal conduction that, as shown by \citet{opr05}, can efficiently suppress the hydrodynamic instabilities, thus allowing the shrapnel to overcome the main shock-front without being disrupted.
Recently, the evolution of knotty ejecta in a Type Ia SNR has been modelled by \citet{obm12} (hereafter O12), who found that small clumps with initial $\chi<5$ can reach the SNR shock front after $\sim1000$ yr. Nevertheless, these ejecta knots are then rapidly eroded and do not produce significant protrusions in the SNR shock front, thus being unable to reproduce the features observed in the Vela SNR.

Here we present a set of 2-D hydrodynamic simulations of the evolution of an (initially spherical) ejecta shrapnel in the Vela SNR. We include in our model both thermal conduction and radiative cooling and explore different values of $\chi$ and of the initial position of the shrapnel in the ejecta profile. We aim at addressing the role of thermal conduction and radiative cooling and at understanding how the initial properties of the shrapnel influence its evolution. We also aim at evaluating whether values of $\chi$ lower than 100 ($\chi=10-50$) can reproduce the observed features.

The paper is organized as follows: the hydrodynamic model is described in Sect. \ref{Hydrodynamic modeling}, the results of the simulations are shown in Sect. \ref{Results}, and our conclusions are discussed in Sect. \ref{Conclusions}.

\section{Hydrodynamic modeling}
\label{Hydrodynamic modeling}

\subsection{Initial conditions and model equations}
\label{initcond}

We model the evolution of a shrapnel in a SNR by performing a set of 2-D simulations in a cylindrical coordinate system $(r, ~ z)$, assuming axial symmetry. The system setup consists of a spherically symmetric distribution of ejecta with initial kinetic energy $K=10^{51}$ erg (the initial thermal energy is only the $0.2\%$ of $K$) and mass $M_{ej}=12$ M$_{\sun}$ (representing the initial blast wave), where we place a dense, spherical, knot (the shrapnel) in pressure equilibrium with the surrounding ejecta and with central coordinates $(0,~R_s)$.

The radial density profile of the ejecta consists of two power-law segments ($\rho\propto r^{-m}$ on the inside and $\rho\propto r^{-b}$ on the outside), in agreement with the density structure in a core-collapse SN described by \citet{che05}. For our simulations, we use $m=1$ and $b=11.2$, and the position of the transition between the flat and steep regimes is derived by following \citet{che05}. The initial velocity of the ejecta increases linearly (up to $6\times10^{8}$ cm/s) with their distance from the center. The maximum velocity is reached at the initial radius of the ejecta, i. e., $R^{0}_{ej}=4.5\times10^{18}$ cm. These values correspond to $\sim240$ yr after the explosion, appropriate for the relatively late stages of the SNR evolution that we address in this study. In fact, the starting time of our simulations corresponds to only $\sim2\%$ of the Vela SNR age and the shrapnel reaches the reverse shock $\sim2500-3000$ yr after the explosion in all our simulations (i. e., the system has enough time
to evolve, before the interaction of the shrapnel with the SNR reverse shock occurs).
We then conclude that our simulations can provide a realistic description of the actual conditions in the Vela SNR.

The initial mass of the shrapnel is $0.05 ~ M_{ej}$ ($1.19\times10^{33}$ g), its density is $\chi$ times larger than that of the surrounding ejecta at distance $R_s$ from the center\footnote{The size of the clump varies accordingly.}, and its velocity is the same as that of the ejecta at distance $R_s$ from the center. We aim at showing that the detached shrapnel observed in the Vela SNR can be the result of moderately overdense clumps of ejecta originating in relatively internal layers. We explored different values of $\chi$ and of $R_s$, namely $\chi=10,~20,~50$, and $R_s=1/6~R^{0}_{ej},~1/3~R^{0}_{ej}$. Figure \ref{fig:setup} shows the initial density and temperature conditions for the case with $\chi=20$ and $R_s=1/3~R^{0}_{ej}$. The simulation setups discussed in this paper are summarized in Table \ref{tab:setups}.

 \begin{figure}
  \centerline{\hbox{
      \psfig{figure=dens-temp-cond_iniz.ps,width=7cm}}}
 \centerline{}
 \centerline{}
 \centerline{}
  \centerline{\hbox{
      \psfig{figure=barra1.eps,width=5cm}}}
 \caption{Density (\emph{left panel}) and temperature (\emph{right panel}) 2-D cross-sections through the $(r,~z)$ plane showing an example of the initial conditions of our simulations (namely, $R1/3-CHI20$, see Table \ref{tab:setups}). The system consists of an expanding spherically symmetric distribution of ejecta where we place a dense, isobaric, and spherical knot. In this case the knot is 20 times denser than the surrounding ejecta.}
\label{fig:setup}
\end{figure}

Vela SNR is the result of a core-collapse SN and we expect the ambient medium to be ``perturbed'' by the wind residuals of the massive progenitor star. However, we assume for simplicity a uniform ambient medium as in WC02, since here we are not interested in modeling the details of the remnant evolution. The final (i.~e. after 11000 yr, the age of the Vela SNR, \citealt{tml93}) radius of the remnant strongly depends on the choice of the ambient density value, $n_{ISM}$. We set $n_{ISM}=0.5$ cm$^{-3}$, because with this value (and with the chosen values of $K$, $M_{ej}$, $n_{ISM}$, $b$, and $m$), the radius of the shell after 11000 yr is $R_{shell}\sim 5.4\times10^{19}$ cm, in good agreement with the observed radius of the Vela SNR, that ranges between $5\times10^{19}$ cm and $5.5\times10^{19}$ cm (by assuming a distance of $250$ pc, in agreement with \citealt{bms99}, \citealt{csd99}).

Our model solves the time-dependent compressible fluid equations of mass, momentum, and energy conservation. In three cases we ran the same simulation with/without thermal conduction and radiative cooling inside our system, as shown in Table \ref{tab:setups}. As for thermal conduction, we considered both the Spitzer and the saturated regimes, while radiative losses (that can play an important role in the Vela SNR, as shown by \citealt{mro06}) were computed for an optically thin thermal plasma. The model equations are described in \citet{mro06} (equations 1-5 therein) and were solved by using the FLASH code (\citealt{for00}).

The computational domain extends over $8\times10^{19}$ cm in the $r$ and $z$ directions.  We use axisymmetric boundary conditions at r = 0, reflection boundary conditions at z = 0, and zero-gradient (outflow) boundary conditions (for v, $\rho$, and $p$) elsewhere. We trace the motion of the ejecta material and of the shrapnel with passive tracers\footnote{Both tracers have zero mass and do not modify the dynamics of the system.}.
Considering the large range in spatial scales of our simulations, we exploited the adaptive mesh capabilities of the FLASH code by adopting up to 10 nested levels of resolution (the resolution increases by a factor of 2 at each level). The refinement$/$derefinement criterion \citep{loh87} follows the gradients of density, temperature, and tracers. The finest spatial resolution is $1.95\times10^{16}$ cm at the beginning of the simulation, therefore there are 230 computational cells per initial radius of the ejecta, and $\sim10$ cells per initial radius of the shrapnel (that varies in the range $1.8-2.9\times10^{17}$ cm). Because of the expansion of the system, the resolution is reduced by a factor of 2 after 2500 yr. We verified that by changing the resolution of our simulations by a factor of 2, the results do not change significantly (see Appendix \ref{convergence} for further details).

\begin{center}
\begin{table}
\begin{center}
\caption{Physical parameters of the model setups (see Sect. \ref{Hydrodynamic modeling}). TC-RL indicates that the simulations were perfomed by including thermal conduction and radiative losses. In all the setups the initial radius of the ejecta is $R^{0}_{ej}=4.5\times10^{18}$ cm.}
\begin{tabular}{@{}lcccc}
\hline\hline
Model setup     &  $\chi$  &       $R_s$ (cm)     & TC-RL   \\ \hline
$R1/3-CHI10$    &    10    &  $1.5\times10^{18}$  &  No     \\
$R1/3-CHI10-TR$ &    10    &  $1.5\times10^{18}$  &  Yes    \\
$R1/3-CHI20$    &    20    &  $1.5\times10^{18}$  &  No     \\
$R1/3-CHI20-TR$ &    20    &  $1.5\times10^{18}$  &  Yes    \\
$R1/3-CHI50$    &    50    &  $1.5\times10^{18}$  &  No     \\
$R1/6-CHI50$    &    50    &  $0.75\times10^{18}$  &  No     \\
$R1/6-CHI50-TR$ &    50    &  $0.75\times10^{18}$  &  Yes    \\
\hline
\label{tab:setups}
\end{tabular}
\end{center}
\end{table}
\end{center}

\section{Results}
\label{Results}

\subsection{Evolution of the system}
\label{evol}

We first focus on simulation $R1/3-CHI20$.
Figure \ref{fig:evolhd} shows the 2-D cross-sections through the $(r,~z)$ plane of temperature and density at different evolutionary stages of the $R1/3-CHI20$ simulation. The left panel shows the system $5000$ yr after the beginning of the simulation\footnote{In the following, all the ages will be reckoned from the beginning of our simulations. We remind the reader that our initial condition corresponds to $\sim240$ yr after the SN explosion.}, when the shrapnel interacts with the inter-shock region. Rayleigh-Taylor and Richtmyer-Meshkov instabilities are visible as finger-like structures both in the density and temperature maps. At this stage, the knot is partially eroded by the hydrodynamic instabilities and evolves toward a core-plume structure. The core of the knot, however, is still significantly overdense with respect to the surrounding shocked ejecta. The right panel of Fig. \ref{fig:evolhd} shows the shrapnel at $t=11000$ yr, with its characteristic supersonic bow shock protruding beyond the SNR
main
shock.

\begin{figure}
 \centerline{\hbox{
     \psfig{figure=Smalldens-temp-5000hd.ps,width=3.6cm}
     \psfig{figure=Smalldens-temp-11000hd.ps,width=3.6cm}
     }}
 \centerline{}
 \centerline{}
  \centerline{\hbox{
      \psfig{figure=barra.eps,width=5cm}}}
      \caption{\emph{Left panel:} density (\emph{left}) and temperature (\emph{right}) 2-D cross-sections through the $(r,~z)$ plane showing simulation $R1/3-CHI20$ at $t=5000$ yr. The black$/$blue contours enclose the computational cells consisting of the original ejecta$/$shrapnel material by more than $90\%$. The color bar indicates the logaritmic density scale and the linear temperature scale. \emph{Right panel:} same as left panel, for $t=11000$ yr. }
\label{fig:evolhd}
\end{figure}

 \begin{figure}
  \centerline{\hbox{
      \psfig{figure=dens-2500hd_zoom.ps,width=6cm}}}
 \centerline{}
 \centerline{}
 \centerline{}
      \caption{Density 2-D cross-sections through the $(r,~z)$ plane for model $R1/3-CHI20$ at $t=2500$ yr. The color scale increases linearly between $10^{-22}$ g$/$cm$^{3}$ and $2\times10^{-22}$ g$/$cm$^{3}$. The contours enclose the computational cells consisting of the original shrapnel material by more than $99\%$ (bold line) and $50\%$ (narrow line).}
\label{fig:knotz}
\end{figure}

 \begin{figure}
  \centerline{\hbox{
      \psfig{figure=chi_vs_t_smo.ps,width=\columnwidth}}}
 \caption{Temporal evolution of the shrapnel$/$ejecta density contrast for model $R1/3-CHI20$. The blue horizonthal line marks the beginning of the interaction between the shrapnel and the SNR reverse shock}
\label{fig:chi}
\end{figure}

WC02 found that ejecta knots with density contrast $\chi\le100$ are rapidly fragmented and decelerated in the intershock region and do not even reach the main shock front (these effects being more dramatic for small clumps). Nevertheless, we notice that the value of $\chi$ in WC02 refers to the onset of the interaction between the knot and the reverse shock and that $\chi$ is not constant during the evolution of the system. In the ``free" expansion phase, the density of the shrapnel does not drop down uniformly (as that of the other ejecta does) and the shrapnel undergoes both diffusion and expansion. Figure \ref{fig:knotz} presents a close-up view of the shrapnel density structure at $t=2500$ yr, showing that, while the outer parts of the knot diffuse and mix with the expanding ejecta, its central core remains much denser. The density of the core of the clump drops down much more slowly than that of the spherically expanding ejecta. Therefore, the inhomogeneous rarefaction of the knot makes the density
contrast between the core of the shrapnel and the expanding ejecta higher, and $\chi$ rapidly increases until the shrapnel reaches the reverse shock. We computed $\chi$ during the expansion phases, by calculating the shrapnel density, $\overline{\rho_s}$, as the average of the density in all the computational cells where the shrapnel content is $>90\%$\footnote{These cells are closer to the center of the knot, and are less affected by the diffusion.}. We then divided $\overline{\rho_s}$ by the ejecta density (along the $r$ axis) at the same distance from the origin as the shrapnel center. Figure \ref{fig:chi} shows the evolution of $\chi$ as a function of time for the $R1/3-CHI20$ simulation.  The figure shows that the ejecta knot reaches $\chi> 100$ as it approaches the reverse shock, hence our results are in agreement with those of WC02. Our model shows that a knot that was only 20 times denser than the surrounding ejecta (at the beginnig of the simulations) can reach the SNR main shock without being
fragmented in the intershock region and can produce protrusions that are similar to those actually observed in the Vela SNR.

\subsection{Effects of thermal conduction and radiative cooling}
Figure \ref{fig:evol} shows the 2-D cross-sections through the $(r,~z)$ plane of temperature and density at $t=5000$ yr and $t=11000$ yr for the $R1/3-CHI20-TR$ simulation (same parameters as $R1/3-CHI20$, but including radiative cooling and thermal conduction).
The diffusive thermal conduction completely suppresses the formation and the development of hydrodynamic instabilities and smoothes the temperature and density profiles. This result is in agreement with expectations, as shown below. The characteristic amplitude growth rate, $da/dt$ of a single-mode perturbation of Richtmyer-Meshkov instabilities can be calculated as (see \citealt{ryc60})
\begin{equation}
\frac{da}{dt} = k \Delta v a \overline{A}
\end{equation}
where $k$ is the perturbation wavenumber, $\Delta v$ is the velocity jump at the instability and $\overline{A}=(\rho_1 - \rho_2)/(\rho_1 + \rho_2)$ is the Atwood number. The characteristic time-scale, $\tau_{inst}=a/(da/dt)$, for the growth of the perturbation is therefore
\begin{equation}
\tau_{inst} \approx \frac{l}{2\pi \Delta v \overline{A}}\hspace{0.5cm}[{\rm s}]
\end{equation}
where $l$ is the structure size.
As for the thermal conduction (see \citealt{spi62}),
\begin{equation}
\left(\frac{dE}{dt}\right)_{cond}=\nabla \cdot [\kappa(T)\nabla T]\sim \frac{2}{7}\kappa(T)\frac{T}{l^{2}}
\end{equation}
where $\kappa(T)=5.6\times10^{-7}T^{5/2}$ erg s$^{-1}$ K$^{-1}$ cm$^{-1}$ is the Spitzer's coefficient and $l$ is the characteristic length of temperature variation. therefore, the thermal conduction time-scale is:
\begin{equation}
\tau_{cond}=\frac{7nk}{2(\gamma -1)}\frac{l^{2}}{\kappa(T)}\sim 2.6\times 10^{-9}\frac{nl^{2}}{T^{5/2}}\hspace{0.5cm}[{\rm s}]
\end{equation}

For a characteristic structure with size $l\sim4\times10^{18}$ cm, particle density $n=0.8$ cm$^{-3}$, Atwood number $\overline{A}\sim0.44$, $\Delta v\sim 2\times 10^7$ cm$/$s, $T\sim1.3\times10^7$ K (similar to that shown in Fig. \ref{fig:evolhd}), $\tau_{inst}\sim 1.4\tau_{cond}\sim 2000$ yr. Therefore, the thermal conduction diffusive processes develop faster than the hydrodynamic instabilities and density and temperature inhomogenieties are smoothed out before they can grow.

The evolution of the position of the shrapnel head and the protrusion it produces to the remnant shock front are similar to those obtained without including thermal conduction and radiative cooling. Nevertheless, the shrapnel evolution is remarkably different from that obtained in the pure HD simulations. In particular, as shown by the blue contours in Fig. \ref{fig:evol}, the ejecta knot is elongated along its direction of motion and rapidly assumes a cometary shape, characterized by a prominent tail which is rich in shrapnel material. After $t=11000$ yr, shrapnel material is present at $\sim10$ pc away from the shrapnel head.
Moreover, the shrapnel material is efficiently heated by thermal conduction with the surrounding shocked ejecta. Let $MX_{shra}$ be the mass of the plasma in the computational cells consisting of the original shrapnel material by more than $90\%$ and having a temperature higher than $10^6$ K (and therefore emitting thermal X-rays). Figure \ref{fig:shraX} shows the evolution of $MX_{shra}$ as a function of time for the simulations $R1/3-CHI20-TR$ and $R1/3-CHI20$. When thermal conduction is at work, $\sim90\%$ of the original shrapnel mass is heated up to X-ray emitting temperature at $t=11000$ yr (i.~e., at the age of the Vela SNR), while if thermal conduction in inhibited, only $50\%$ of the original mass has temperature higher than $10^6$ K. Figure \ref{fig:shraX} also shows the amount of X-ray mass beyond the shock front. In the pure HD simulation the hot shrapnel material is all beyond the SNR shock front. In the $R1/3-CHI20-TR$ simulation, only part of the X-ray emitting shrapnel is beyond the shock
front
and there is a significant fraction
of
the ejecta knot material (the shrapnel tail) that is inside the SNR shell and that is expected to emit thermal X-rays (see Sect. \ref{Conclusions}).
\begin{figure}
 \centerline{\hbox{
     \psfig{figure=fig5.ps,width=\columnwidth}
     }}
      \caption{Same as Fig. \ref{fig:evolhd} for model $R1/3-CHI20-TR$.}
\label{fig:evol}
\end{figure}

 \begin{figure}
  \centerline{\hbox{
      \psfig{figure=shra_massx_TRHD.ps,width=\columnwidth,angle=90}}}
 \caption{Temporal evolution of $MX_{shra}$ (mass of the plasma in the computational cells consisting of the original shrapnel material by more than $90\%$ and having a temperature higher than $10^6$ K) for the simulations $R1/3-CHI20-TR$ (blue curves) and $R1/3-CHI20$ (black curves). The dashed lines indicate the part of $MX_{shra}$ that protrudes beyond the SNR shock front.}
\label{fig:shraX}
\end{figure}

We point out that in SNRs the efficiency of thermal conduction can be significantly reduced by the presence of the magnetic field (which is not taken into account in our model). If we assume an organized ambient magnetic field, the thermal conduction is anisotropic, because the conductive coefficient in the direction perpendicular to the field lines is several orders of magnitude lower than that parallel to the field lines, which coincides with the Spitzer's coefficient $\kappa(T)$. The effects of the magnetic-field-oriented thermal conduction in the interaction between shocks and dense clump have been investigated in detail in \citet{obr08}. Because of the high beta of the plasma, the magnetic field lines are expected to envelope the hydrodynamic fingers thus hampering the thermal conduction with the surrounding material.
At the same time, the magnetic field is expected to be trapped at the top of the ejecta clumps, and this yields to an increase of the magnetic pressure and field tension which limits the growth of hydrodynamic instabilities (see O12 and \citealt{snm12}).
The basic physics of the interaction between the ejecta knots and the SNR shocks is similar to that for the interaction of planar  shocks with an interstellar cloud (e.~g. WC02) and it has been shown that, in this case, simulations including thermal conduction in an unmagnetized plasma and pure HD simulations are limiting cases that encompass the results obtained with different configurations of the magnetic field (\citealt{obr08}).
We can then conclude that our simulations provide the two extreme cases that bracket all the possible intermediate scenarios.

\subsection{Effects of the initial conditions}
\label{init}

We study the effects of the initial conditions on the shrapnel evolution with different simulations, as shown in Table \ref{tab:setups}. In particular, we explored two different initial positions of the shrapnel in the ejecta profile ($R_s=1/6~R^{0}_{ej},~1/3~R^{0}_{ej}$) and three different density contrasts ($\chi=10,~20,~50$).

In agreement with WC02, we found that shrapnel formed in the inner ejecta layers (i.~e., those that reach the reverse shock later) produce smaller protrusions.
In particular, an ejecta knot originating at $R_s=1/6~R^{0}_{ej}$, does not even reach the SNR shock in the time spanned by our simulations. Therefore, our model indicates that shrapnel A-F (all protruding well beyond the Vela main shock) originated in more external layers. Left panel of Fig. \ref{fig:chi50} shows the 2-D cross-sections through the $(r,~z)$ plane of temperature and density at the age of the Vela SNR for the $R1/6-CHI50$ simulation. In this case, the knot is well within the intershock region, even though its initial density contrast ($\chi=50$), was higher than that of the $R1/3-CHI20$ run. However, our models of knots originating at $R_s=1/3~R^{0}_{ej}$ clearly show that denser shrapnel produce deeper protrusions and are more stable against the fragmentation and the deceleration induced by the hydrodynamic instabilities in the inter-shock region (as in WC02)\footnote{In our runs, higher values of $\chi$ correspond to smaller values of the shrapnel cross-section (given that the
shrapnel mass is fixed to $1.19\times10^{33}$ g in all our simulations), and this concurs in making the knot a more penetrating bullet.}.
Fig. \ref{fig:chi50}, right panel, shows the 2-D cross-sections through the $(r,~z)$ plane of temperature and density at the age of the Vela SNR for the $R1/3-CHI50$ simulation. As expected, the shrapnel head is much further away from the SNR shell than in the $R1/3-CHI20$ case (shown in the right panel of Fig. \ref{fig:evolhd}). We computed the time evoulution of $\chi$ for the $R1/3-CHI50$ run by following the procedure described in Sect. \ref{evol}. We found that, in this case, the ejecta knot reaches the reverse shock with a very high density contrast ($\chi>1000$, see Fig. \ref{fig:chivst2}), thus producing a very prominent protrusion in the SNR.

\begin{figure}
 \centerline{\hbox{
     \psfig{figure=fig7.ps,width=\columnwidth}}}
      \caption{\emph{Left panel:} density (\emph{left}) and temperature (\emph{right}) 2-D cross-sections through the $(r,~z)$ plane showing simulation $R1/6-CHI50$ at $t=11000$ yr. The black$/$blue contours enclose the computational cells consisting of the original ejecta$/$shrapnel material by more than $90\%$. The color bar indicates the logaritmic density scale and the linear temperature scale. \emph{Right panel:} same as left panel, for simulation $R1/3-CHI50$.}
\label{fig:chi50}
\end{figure}
 \begin{figure}
  \centerline{\hbox{
      \psfig{figure=chi_vs_t_smo50.ps,width=\columnwidth}}}
 \caption{Same as Fig. \ref{fig:chi} for model $R1/3-CHI50$.}
\label{fig:chivst2}
\end{figure}

\begin{figure}
  \centerline{\hbox{
      \psfig{figure=shrapnel_pos2.ps,width=\columnwidth,angle=90}}}
 \caption{Position of the shrapnel head (in units of the shell radius $R_{shell}$) as a function of time for all the simulations listed in Table \ref{tab:setups}. Black curves indicate pure hydrodynamic models, while blue curves indicate simulations including thermal conduction and radiative cooling. Dashed/solid/thick lines indicate $\chi=10/30/50$, respectively. The red diamonds show the projected positions of Shrapnel A-D (\citealt{aet95}) and of the ejecta knots FilE and RegNE (\citealt{mbr08}).}
\label{fig:shrapos}
\end{figure}

Figure \ref{fig:shrapos} shows the position of the shrapnel head (in units of the shell radius) as a function of time for all our simulations. Figure \ref{fig:shrapos} also shows the projected positions of Shrapnel A-D (\citealt{aet95}) and of the ejecta knots FilE and RegNE (\citealt{mbr08}) with respect to the position of the shock front in the Vela SNR. These values were calculated by approximating the Vela SNR as a circular shell with angular radius $211'$ and center with coordinates $\alpha_{J2000}=8^h36^m19.8^s,~\delta_{J2000}=-45^\circ24'45''$.  Models including the effects of radiative cooling and thermal conduction (blue curves in Fig. \ref{fig:shrapos}) do not provide significant differences with respect to pure HD models (black curves) in terms of the shrapnel position.

By considering all the simulations with $R_s=1/3~R^{0}_{ej}$, we find that the position of the head of the knot, $R_h$, after $\sim11000$ yr ranges between $\sim1.1~R_{shell}$ (for $\chi=10$) and $\sim1.4~R_{shell}$ (for $\chi=50$). These values are similar to those observed for Shrapnel B, C, and D.

Shrapnel A, E, and F (Shrapnel E, F are not shown in  Fig. \ref{fig:shrapos}) instead, have $R_h=1.57~R_{shell}$, $R_h=1.88~R_{shell}$, and $R_h=1.91~R_{shell}$, respectively. These values are much larger than those obtained in our simulations. Our results clearly suggest that these large distances from the shell can be produced by ejecta knots originating in outer ejecta layers.
An alternative possibility is that the original density contrast for these shrapnel was $>50$. Nevertheless, Fig. \ref{fig:shrapos} shows that the final position of an ejecta clump is more sensitive to its initial position and depends only weakly on $\chi$. In fact, by varying the initial position of the knot by a factor of two, we found that its final position varies approximately by the same factor, while a variation of the initial density contrast by a factor of five, only determines a 30\% variation in the final position. Therefore it is more likely that Shrapnel A, E, and F were produced at $R_s>1/3~R^{0}_{ej}$.

The two simulations with $R_s=1/6~R^{0}_{ej}$ show that the ejecta knots originating in the inner ejecta layers do not reach the forward shock, even for the highest density contrast ($\chi=50$). The position of the head of the knot predicted by our simulations is in agreement with that observed for FilE (\citealt{mbr08}). X-ray emitting ejecta knots have been observed, in projection, inside the Vela SNR shell (e.~g., RegNE and FilE, \citealt{mbr08}). However, we point out that the actual position of these ``internal'' shrapnel can be well outside the SNR shell, and therefore the values reported in Fig. \ref{fig:shrapos} might be considered as lower limits.

\section{Discussions and conclusions}
\label{Conclusions}

The structure of the ejecta in a SNR contains the imprint of the metal-rich layers inside the progenitor star, and may help to understand the processes occurring in the latest stage of stellar evolution. We performed a set of hydrodynamic simulations to study the evolution of the ejecta knots in the Vela SNR.

\begin{figure}
  \centerline{\hbox{
      \psfig{figure=newfig8a.ps,width=\columnwidth}}}
  \centerline{\hbox{
      \psfig{figure=newfig8b.ps,width=\columnwidth}}}
 \caption{\emph{Upper panel:} Rosat All-Sky Survey image of Vela Shrapnel D in the $0.1-2.4$ keV energy band. The bin-size is $1.5'$ and the image has been smoothed through a convolution with a Gaussian with $\sigma=3$ pixels. North is up and East is to the left. \emph{Lower panel:} Synthesized X-ray emission in the $0.1-2.4$ keV band for the simulation $R1/3-CHI20-TR$ at $t=11000$ yr (see Sect. \ref{Conclusions}).}
\label{fig:shraD}
\end{figure}

We found that moderately overdense clumps (initial density contrast $\chi\sim10$) can produce protrusions in the SNR shell similar to those observed for the Vela shrapnel.
WC02 found that only clumps that reach the reverse shock with density contrast $\chi\ge100$ can reach the main shock front and produce significant protrusions. This criterium is fulfilled in all our simulations. In fact, the (initially) moderately overdense clump experiences diffusion in the ``free" expansion phase, and, while its outer parts mix with the surrounding ejecta, its central core remains much denser. This inhomogeneous rarefaction makes the density contrast between the core of the shrapnel and the expanding ejecta higher as the remnant evolves, and $\chi$ reaches values $\sim100-1000$ at the interaction with the reverse shock.

In particular, a knot with initial $\chi=20$ and $R_s=1/3~R^{0}_{ej}$ (simulations $R1/3-CHI20$ and $R1/3-CHI20-TR$) can explain the observed features associated with the Vela Shrapnel D.
Figure \ref{fig:shraD} shows the the $ROSAT$ All-Sky Survey image of the Vela Shrapnel D in the $0.1-2.4$ keV energy band, compared with a synthesis of the X-ray emission in the $0.1-2.4$ keV band derived from the $R1/3-CHI20-TR$ simulation at $11000$ yr. The synthesized X-ray map has been obtained as in \citet{mro06}: we produced the 3D map of the emission measure and temperature in the cartesian space ($x',~y',~z'$), where the $y'$ axis corresponds to the direction of the line of sight and is perpendicular to the $(r,~z)$ plane. We derived the distribution $EM(x',~z')$ vs. $T(x',~z')$ by considering all the contrbutions along the line of sight, for each $(x',~z')$. We then synthesized the map of the X-ray emission using the MEKAL spectral code (\citealt{mgv85}, \citealt{mlv86}, \citealt{log95}), assuming a distance of $250$ pc, and an interstellar column density $N_{H}=2\times 10^{20}$ cm$^{-2}$. Finally, we degraded the spatial resolution of the synthesized X-ray map to match the resolution of the ROSAT
image and randomized the map by assuming Poisson statistics for the counts in each image bin.

Figure \ref{fig:shraD} shows that the bright X-ray spot at the apex of the shrapnel bow-shock and the enhanced X-ray luminosity at the base of the protrusion can be explained by our model as local enhancements of the plasma emission measure. The overall shape of the observed features is also reproducted by our model. Moreover, the mass of the X-ray emitting shrapnel predicted by our model is in agreement with that measured for Shrapnel D. In fact, it has been estimated that the X-ray emitting mass (considering only the bulge above the Vela SNR bow shock) is $\sim0.1M_\odot$ \citep{kt05} i.~e., the same order of magnitude as that obtained in our simulation (see dashed curves in Fig. \ref{fig:shraX}).
Vela Shrapnel D is therefore consistent with being originated by an ejecta knot 20 times denser than the surrounding ejecta and initially located at $1/3~R^{0}_{ej}$. As shown in Fig. \ref{fig:shrapos}, we found a degeneracy in the space of the initial parameters, and similar results can be obtained also by enhancing/decreasing the density contrast and decreasing/increasing the initial distance of the knot to the explosion center. However, as explained in Section \ref{init}, the final position of the shrapnel is much more sentitive to its initial position in the ejecta profile. In conclusion, according to our model, the original position of Shrapnel D should not differ much from $1/3~R^{0}_{ej}$.

As shown in Sect. \ref{init}, our model suggests that Shrapnel B, C, and D were all originated at $\sim1/3~R^{0}_{ej}$. This conclusion is in agreement with the results of X-ray data analysis that show that Shrapnel B and D have similar abundance patterns (\citealt{kt05}, \citealt{yk09}). The fragment RegNE, which appears inside the Vela shell, has similar abundances as Shrapnel D \citep{mbr08} and its position is compatible with an origin in the same layer where Shrapnel B, C, and D were generated\footnote{In this case, its projected distance from the center of the SNR  must be much smaller than its actual distance.}.

In Sect. \ref{init}, we also pointed out that it is highly unlikely that Shrapnel A originated in the same ejecta layer as Shrapnel D. Indeed, the abundance patterns observed in Shrapnel A are remarkably different from that observed in Shrapnel B and D (\citealt{kt06}), thus suggesting a different location of this knot in the ejecta profile. Nevertheless, the Si:O ratio is much higher in Shrapnel A than in Shrapnel D and this indicates that Shrapnel A comes from a region of the progenitor star below that of the Shrapnel D (e.~g. \citealt{tk06}), at odds with our predictions.
As explained above, an unrealistically high initial $\chi$ is required for an inner shrapnel to overcome outer knots, if we assume that the initial velocity profile of the ejecta increases linearly with their distance from the center. A possible solution for this puzzling result is that the Si burning layer (or part of it) has been ejected with a higher initial velocity, e.~g., as a collimated jet.
It is noteworthy to remark that in other core-collapse SNRs the Si-rich ejecta may show a very peculiar jet-counterjet structure. The  well known case of Cas A has been studied in detail thanks to a very long Chandra observation (\citealt{hlb042}) showing a jet (with a  weaker counterjet structure) composed mainly of Si-rich plasma. \citet{lhr06}  have performed X-ray spectral analysis of several  knots in the jet and concluded that the origin of this  interesting morphology is due to an explosive jet and it is not arising because of an interaction with a cavity or other ISM/CSM peculiar structure. Therefore a jet origin for the Si-rich knots is sound.

Finally, we investigated the effects of thermal conduction, finding that it determines an efficient ``evaporation" of the ejecta knot and accelerate its mixing with the surrounding medium. Moreover, it affects the shrapnel morphology, producing the formation of a long, metal-rich tail. Enhanced metallicities have been observed in the tails of Shrapnel A, B, and D and the abundance analysis performed on the X-ray spectra clearly suggests an efficient mixing of the ejecta knots with the surrounding medium (\citealt{kt05, kt06}, and \citealt{yk09}). These results are in qualitative agreement with our findings. A quantitative comparison between models and observations requires a forward modeling approach, consisting in the synthesis of the X-ray spectra from the simulations and a detailed comparison between the synthesized observables and the corresponding observations (e.~g., through a spatially resolved spectral analysis, as in \citealt{mro06}, e. g.). Moreover it will also be important for future
models to include some seed magnetic fields in the simulations to study how tangled the field becomes and what this implies for thermal conduction. These further studies are beyond the scope of this paper.

In conclusion, our hydrodynamic modelling of ejecta knots in the Vela SNR allowed us to find that: i) the observed shrapnel can be the results of moderate density inhomogeneities in the early ejecta profile; ii) the evolution of a shrapnel in the SNR is very sensitive to its initial position and depends much less (but does depend) on the initial density contrast; iii) thermal conduction plays an important role and explains the efficient mixing of the ejecta knots observed in X-rays.

\section*{Acknowledgments}
We thank the anonymous referee for their constructive suggestions to improve the paper.
The software used in this work was in part developed by the DOE-supported ASC / Alliance Center for Astrophysical Thermonuclear Flashes at the University of Chicago. The simulations discussed in this paper have been performed on the HPC facility at CINECA, Italy, and on the GRID infrastructure of the COMETA Consortium, Italy.

\bibliographystyle{mn2e}

redpajama_set_name: RedPajamaArXiv


A goodbye note to the border and recipe for my favorite vegetarian burger.
Pakoras are a Ramazan and rainy day staple in Pakistan. You can have them as a roadside snack or with a cup of tea. Here I take a stab at one of my favorite variety - palak pakoray.
Pakistan Eats is a platform for you to discover, celebrate and share Pakistani cuisine.


text:
Q: Surjective ring homomorphism from $M_n(R)$ to $M_n(R/I)$ where $R$ is a ring and $I$ is an ideal for R? I'm looking for such a surjective homomorphism. I was thinking of starting from the canonical surjection from $R$ to $R/I$ and induce one but somehow I get stuck... Can you help me?
Thank you very much!

A: If $n > 0$, we have a functor $M_n : \operatorname{Ring} \to \operatorname{Ring}$ where $M_n(R)$ is the ring of $n \times n$ matrices with entries in $R$. If $f : R \to S$ is a ring homomorphism, then $M_n(f) : M_n(R) \to M_n(S)$ is a ring homomorphism defined by $$M_n(f)\Bigg( \begin{bmatrix} a_{11} & \cdots & a_{1n} \\ \vdots &  & \vdots \\ a_{n1} & \cdots & a_{nn}\end{bmatrix}\Bigg) =  \begin{bmatrix} f(a_{11}) & \cdots & f(a_{1n}) \\ \vdots &  & \vdots \\ f(a_{n1}) & \cdots & f(a_{nn})\end{bmatrix}.$$
In our specific case, we let $R$ be a ring and $I$ an ideal, so we can consider the ring $R/I$ and the quotient homomorphism: $f : R \to R/I$ defined by $f(r) = \overline r = r + I$. Notice that our homormorphism is clearly surjective.
Let's pick an arbitrary element in $M_n(R/I)$: $$\begin{bmatrix} \overline {a_{11}} & \cdots &\overline{ a_{1n}} \\ \vdots &  & \vdots \\ \overline{a_{n1}} & \cdots & \overline{a_{nn}}\end{bmatrix} = \begin{bmatrix} a_{11} + I & \cdots & a_{1n} + I \\ \vdots &  & \vdots \\ a_{n1} + I & \cdots & a_{nn} + I\end{bmatrix}$$ where we can choose the obvious representatives: for $\overline{a_{ij}}$ we pick $a_{ij} \in R$ and notice that $f(a_{ij}) = \overline{a_{ij}} = a_{ij} + I$.
It should be clear that $$\begin{bmatrix} a_{11} & \cdots & a_{1n} \\ \vdots &  & \vdots \\ a_{n1} & \cdots & a_{nn}\end{bmatrix}$$ is an element such that $$M_n(f)\Bigg(\begin{bmatrix} a_{11} & \cdots & a_{1n} \\ \vdots &  & \vdots \\ a_{n1} & \cdots & a_{nn}\end{bmatrix}\Bigg) = \begin{bmatrix} \overline {a_{11}} & \cdots &\overline{ a_{1n}} \\ \vdots &  & \vdots \\ \overline{a_{n1}} & \cdots & \overline{a_{nn}}\end{bmatrix}.$$
Hence the surjective homomorphism you requested should be $M_n(f)$ where $f$ is the canonical quotient map.

redpajama_set_name: RedPajamaStackExchange


Series Manifesto: Instead of ignoring the pain following the disclosure of our spouse's sexual sin, we choose to use our trauma as a catalyst for growth, digging deeply into God's Word in search of spiritual healing and transformation.
This is the fourth in a five-part miniseries on Colossians 1:10-12.
So far in this multi-part, in-depth examination of Colossians 1:10-12, we addressed how we all need to get our worth from God. Next, we discussed having the right motives for bearing fruit for God. Last time, we focused on how we can know God intimately. This time, we're going to explore how we can patiently endure our spouse's sexual addiction recovery—and our own recovery from codependency—by relying on God's strength rather than our own.
A friend of mine passed away last year after a 10-year out-and-out war with the cancer that finally won over her body. But it could never rob her of her spirit and spiritual strength. Everyone who visited Janet with the goal to encourage her walked away full. That's because Janet overflowed with strength she got directly from "His glorious might".
Our spouse's sexual sin and our corresponding codependency can feel like an emotional cancer. Life is moving forward with all our dreams intact and then BAM! the devastating news of the condition of our marriage stops us in our tracks. We're paralyzed in a kind of dazed denial. We know if someone doesn't aggressively pursue "treatment", our relationship is dead.
Within weeks of my separation, I was ready to face the fact that my husband wasn't the only one who was broken and needing recovery. Every day seemed like an eternity with God cutting away at my codependency with a hot scalpel. I felt as empty, weak, and sick as a chemo patient.
I had nothing left. There was no one else to turn to for strength but God.
I expected Russ to be over his immoral pursuits in six months, tops. I mean, he was a Christian, and we had three kids and 19 years invested in our marriage. When the first anniversary of our separation rolled around and Russ was further away than ever, I began to wonder if I could really put up with it any longer. I pondered divorce countless times.
The words were like…well, magic. More than a balm, they were a well for me to drink from and find refreshment. The Psalm was a reminder of where the real power in this world resides. They words were my strength. But they were also my challenge.
I didn't necessarily believe my husband could change—he was so deeply in sin—but did I really believe that God could change him?
Wasn't I a "Christian"? Wasn't the whole tenant of my faith based on Christ's resurrection? Didn't I believe that Jesus raised the widow's son from the dead (Luke 7:11-17)? Hadn't he called Jairus' daughter from her mortal sleep (Mark 5:21-43)? Hadn't he restored Mary and Martha's dead brother to them (Luke 11:17-44)? Hadn't Jesus himself created life from death (John 1:3)? So if God could raise Jesus from the dead, surely he had the power to resurrect my spiritually dead husband and restore my marriage?
About this time, a friend recommended the book Don't Call It Love. The author, Dr. Patrick Carns, shared the results of his sexual addiction recovery research. He found out it takes the average sexual addict five years—yes, you read that right, five years—of active and deliberate recovery before there is stability.
Surely this was a typo, I thought. Five years? How the heck was I supposed to wait five years?
I wanted to act. I wanted to do something. Isn't that what women today did? They didn't sit back and take crap from their wayward spouses.
Truth is, sometimes it takes more strength to be still than it does to act. I didn't have that strength myself. It took supernatural strength to sit tight for four years and wait on God to act on my behalf.
And boy, did He ever act.
We're actually in our seventh year of recovery and I must say this end of the road is much better than the beginning. The years of support groups and counseling were inestimable and irreplaceable, but they could never have been enough without God.
Through my patient endurance, I've learned something invaluable. That God is faithful. I mean, really faithful.
No, he doesn't always act in my timeframe, but I guess as the omnipotent, omniscient, and omnipresent creator of the world, he probably knows better than I do anyway.
Question: Have you ever wondered why God is taking so long to act on your behalf? Where are you getting your strength to patiently endure?
Just what I needed! 🙂 Thanks!


To offer the most high quality resources, This We Affirm has partnered with The Convergence Music Project, Darkwood Brew and The Worship Design Studio. For $8.99 a month for individuals and $10.99 a month for churches, you can draw on resources from each site. Subscriptions options are available in both monthly and yearly packages.
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text:
World Neighbours 28 Mar 2019 'No terror camp ...
World, Neighbours
'No terror camps exist on 22 locations shared by India,' says Pak on Pulwama
Published Mar 28, 2019, 11:46 am IST
Updated Mar 28, 2019, 11:52 am IST
'While 54 detained individuals are being investigated, no details linking them to Pulwama have been found so far,' it said.
It said that in consistent with its commitment to cooperate, Pakistan on Wednesday shared 'preliminary findings' of its investigations with India along with a set of questions. (Photo: PTI)
Islamabad: Pakistan on Thursday said it has examined 22 "pin locations" shared by India but found no terror camps and claimed that there are no links to nail 54 people detained in connection with the Pulwama terror attack as it shared the "preliminary findings" with New Delhi.
Pakistan is willing to allow visits, on request, to these locations, the Foreign Office (FO) said in a statement. "While 54 detained individuals are being investigated, no details linking them to Pulwama have been found so far," it said.
"Similarly, the 22 pin locations shared by India have been examined. No such camps exist. Pakistan is willing to allow visits, on request, to these locations," the FO said.
It said that in consistent with its commitment to cooperate, Pakistan on Wednesday shared "preliminary findings" of its investigations with India along with a set of questions.
"Subsequently, the diplomatic corps in Islamabad was briefed as well," the FO said. India handed over the dossier to the Acting High Commissioner of Pakistan in New Delhi on February 27 with specific details of Pakistan-based terror group Jaish-e-Mohammed (JeM)'s complicity in the Pulwama attack that killed 40 CRPF personnel on February 14 and the presence of JeM terror camps and its leadership in Pakistan. The FO said soon after receiving the dossier, Pakistan constituted an investigation team, detained a number of people for investigation and initiated work on the technical aspects of social media content, a main basis of the Indian documents.
The Indian dossier contains 91 pages and six parts, out of which only part two and three pertain to the Pulwama attack, it said.
"Other parts are generalised allegations. Pakistan is focusing on those parts which relate to Pulwama incident," it said. The FO claimed that during the course of investigations, all aspects of the information provided by India have been thoroughly examined including the "confessional" video of Adil Dar, "claim" of responsibility for the attack, Whatsapp and Telegram numbers used to share videos and messages in support of the Pulwama attack, list of 90 individuals suspected of belonging to a proscribed organisation and 22 pin locations of alleged training camps.
Service Providers have been requested for data including relevant details of activities and contacts of the GSM (Global System for Mobile communications) number provided by India, it said.
A request for assistance from Whatsapp has also been made to the US government, it said, adding that the said additional information and documents from India would be essential to continue the process of investigations.
"Pakistan remains committed to taking this process to its logical conclusion," the FO added. Tensions between India and Pakistan escalated after the suicide bomber of JeM killed 40 CRPF personnel in Jammu and Kashmir's Pulwama district on February 14.
India launched a counter-terror operation against a JeM training camp in Balakot. The next day, Pakistan Air Force retaliated and downed a MiG-21 in an aerial combat and captured its pilot, who was handed over to India on March 1.
Tags: pulwama attack, jem, crpf jawans, balakot air srike
Location: Pakistan, Islamabad
More From Neighbours
China begins once-a-decade census of world's largest population
Pakistan on FATF's 'Enhanced Follow-up' list for meagre progress on terror financing
Bangladeshi floating hospital treats flood-ravaged community
Mumbai attack mastermind and LeT commander Lakhvi gets 5-year jail term
Pak court asks Sharif to appear before it to avoid being declared proclaimed offender

redpajama_set_name: RedPajamaCommonCrawl


This page displays sold house prices for Gallowgate Lane in Leeds.
Gallowgate Lane in Weeton, Leeds consists predominantly of detached houses. Properties on Gallowgate Lane typically have values around £850,000 - £1,150,000, but larger detached houses can command upwards of £1,150,000.
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text:
Q: Clang AST Dump is missing nodes I need to analyze bodies of a few functions/methods in a C++ source file using clang's AST. My goal is to find all accesses to members of the method's class.
When running clang --std=c++20 $includes -Xclang -ast-dump /path/to/src.cpp, the AST is printed but missing some parts of my function bodies. $include contains all relevant include paths of the project.
The C++ code (excerpt):
654 void BehaviorPathPlannerNode::onRoute(const HADMapRoute::ConstSharedPtr msg)
655 {
656   std::lock_guard<std::mutex> lock(mutex_pd_);
657   const bool is_first_time = !(planner_data_->route_handler->isHandlerReady());
658
659   planner_data_->route_handler->setRoute(*msg);
660
661   // Reset behavior tree when new route is received,
662   // so that the each modules do not have to care about the "route jump".
663   if (!is_first_time) {
664     RCLCPP_DEBUG(get_logger(), "new route is received. reset behavior tree.");
665     bt_manager_->resetBehaviorTree();
666   }
667 }

The corresponding part of the clang AST (excerpt):
| |-CXXMethodDecl 0x1136e310 parent 0x11322b48 <line:654:1, line:667:1> line:654:31 invalid onRoute 'void (const int)
'
| | |-ParmVarDecl 0x1136e278 <col:39, col:73> col:73 invalid msg 'const int'
| | `-CompoundStmt 0x1136fd78 <line:655:1, line:667:1>
| |   |-DeclStmt 0x1136e668 <line:656:3, col:46>
| |   | `-VarDecl 0x1136e5b0 <col:3, col:45> col:31 lock 'std::lock_guard<std::mutex>':'std::lock_guard<std::mutex>'
 callinit destroyed
| |   |   `-CXXConstructExpr 0x1136e638 <col:31, col:45> 'std::lock_guard<std::mutex>':'std::lock_guard<std::mutex>'
 'void (std::lock_guard<std::mutex>::mutex_type &)'
| |   |     `-MemberExpr 0x1136e538 <col:36> 'std::mutex':'std::mutex' lvalue ->mutex_pd_ 0x11324028
| |   |       `-CXXThisExpr 0x1136e528 <col:36> 'behavior_path_planner::BehaviorPathPlannerNode *' implicit this
| |   |-DeclStmt 0x1136e710 <line:657:3, col:79>
| |   | `-VarDecl 0x1136e698 <col:3, col:14> col:14 used is_first_time 'const bool'
| |   `-IfStmt 0x1136fd60 <line:663:3, line:666:3>
| |     |-UnaryOperator 0x1136e788 <line:663:7, col:8> 'bool' prefix '!' cannot overflow
| |     | `-ImplicitCastExpr 0x1136e770 <col:8> 'bool' <LValueToRValue>
| |     |   `-DeclRefExpr 0x1136e738 <col:8> 'const bool' lvalue Var 0x1136e698 'is_first_time'
 'const bool'
| |     `-CompoundStmt 0x1136fd48 <col:23, line:666:3>
| |       `-DoStmt 0x1136fd18 </opt/ros/galactic/include/rclcpp/logging.hpp:94:3, line:103:13>

The statement in line 659 is skipped.
In general (as far as I could observe), statements like method calls and assignments that are not part of a declaration or if/for/... condition are not appearing in the AST.
Thanks for helping!


Wales produced a repeat of their Cardiff comeback to deny Gordon Strachan a winning start to his competitive Scotland managerial career.
Scotland started poorly but led through Grant Hanley's first-half header.
Wales' Gareth Bale had to be taken off, but Aaron Ramsey equalised from the spot as Robert Snodgrass was sent off.
And with the Scots reeling, Hal Robson-Kanu rose unchallenged to head home the winning goal for Wales, who had Ramsey sent off in injury time.
The victory lifts Wales up to third place in Group A but the Scots find themselves adrift at the bottom with no wins and just two points from five games.
The match ended in a similar fashion to Wales' as Chris Coleman's side came from behind to strike two late goals after Scotland needlessly conceded a penalty.
27 mins: James Morrison gives Scotland the lead.
Steven Fletcher doubles Scotland's advantage but it's incorrectly disallowed.
81 mins: Gareth Bale equalises from the spot for Wales after Shaun Maloney's foul.
89 mins: Bale scores a wonder-goal to secure all three points.
Their comeback on this occasion was all the more impressive given Bale's withdrawal at half-time.
Coleman's side played the better football for large swathes of the game, but Strachan will be bitterly disappointed that having clawed their way into a winning position, it was surrendered.
Wales certainly came out the blocks quicker and almost caught the Scots flat-footed as they threatened to take the lead inside a minute.
Ponderous defending allowed Ramsey the opportunity to power in a drive, which Hanley did superbly to block and a soft-looking free kick given against Craig Bellamy, with Allan McGregor grounded, brought an immediate end to the danger.
But there was a less welcome respite for the Scots moments later, as Steven Fletcher crumbled in agony following an innocuous aerial challenge with Ben Davies and had to be replaced by Kenny Miller.
Hanley epitomised the nervousness seemingly coursing through the Scotland side as he misjudged a ball back to McGregor and only just managed to atone by heading clear.
Almost quarter of the game had passed before Scotland fashioned a chance. Chris Burke's deep cross found Miller, but the striker's header flew over.
Burke, who had excelled in Strachan's first game in charge against Estonia, twice blew chances to pick out well-placed team-mates in front of goal, with too many Scots passes finding Welsh feet.
Bellamy and Bale were denied in quick succession by the bravery and quick reactions of McGregor, but Scotland were gradually finding their way into the game.
And though Boaz Myhill was untested by two more Miller headers, he was motionless as the Scots took the lead in first-half injury time.
Mulgrew curled a corner from the right to the back post and Hanley, brilliantly freeing himself from the shackles of Sam Ricketts, headed into the net from just a few yards.
Scotland emerged after the break a far brighter side than the one that had started the game, no doubt buoyed by the goal and the non-appearance of Bale for the second period.
Their initiative was almost rewarded by a beautifully struck Snodgrass effort, which thudded back off Myhill's post.
But this Wales side is not one to feel sorry for itself and though penalty claims for a handball by Hanley were hopeful, they were denied an equaliser when the referee Antony Gautier deemed McGregor had been fouled before substitute Andy King - on the park seconds before - swept into the net.
The game was turned on its head in a three-minute spell, starting with a foul by Snodgrass on Chris Gunter that brought him a second yellow card and - after a delay - a correctly-awarded penalty to Wales.
Ramsey hammered it in off the crossbar and with the Scots dazed, they were punished again as King floated in a cross from the right for Robson-Kanu to head emphatically past McGregor.
Scotland failed to threaten an equaliser, though James McArthur was cynically hauled down by Ramsey in the dying seconds, leading to the Welshman seeing a straight red.
Sadly for Scotland, Shaun Maloney blasted the free kick from 22 yards well over and Wales were left to take the acclaim of their fans.


Most films are conceived as a work solely for entertainment value. Movies are just something to watch, laugh at, intrigue, mystify, or frighten the viewer. Some movies do however every once in a while deliver a message that hits you dead smack in the face but none truly affect the viewers way of life. Enter Fat, Sick and Nearly Dead. Since watching this movie I have changed my lifestyle and improved upon not only my own health but others around me also. How did I come to watch this film? One day my friend at work Andy says to me "You gotta watch this movie dude. It has changed my way of life. Watch this trailer on YouTube and tell me what you think." After watching the trailer for Fat Sick and Nearly dead I was determined to check out the full film. I had recently watched Food Inc on netflix and discovered this gem was available in the instant queue also.
So, what's the film about? Joe Cross is the creator, narrator, and test subject in this masterful documentary. He is a successful businessman from Australia who has neglected his health, is overweight (300+lbs), suffers from breakouts of hives that he has to take a lot of medication for, and one day decides enough is enough. Joe does research on "Juicing" which is a highly popular dietary supplement to ones nutrition however, Joe pushes juicing to the extreme by doing a 60 day fast solely on juice. Juicing is not the use of steroids instead; this form of juicing involves drinking 4, 16oz glasses of vegetables and one fruit a day. We are not talking about V-8 processed juice here but fresh vegetables and fruits. My usual mixture will include kale spinach, sweet potatoes, celery, cilantro, ginger, tomato, carrots, beet, and a granny smith apple. The greener the better they say. All this goes into a Breville juicer, which produces pulp as waste and the purest form of highly nutritious juice from the vegetables and fruit. The amount of vegetables I use would be impossible to consume even if I ate the portion I juiced for 2 days straight for 3 meals a day. I will tell you after drinking my concoction I feel energized and revived. I no longer have the occasional acne breakouts I used to. I honestly feel better since I started juicing. My last physical has also resulted in lower blood pressure and cholesterol. Personally I feel that all the sicknesses and illness that are presently rampant in the world today which, were not as prevalent prior to mass consumption are from the highly processed foods that we eat, and juicing is a step to give your body back what it needs. Just like the early man analogy in the film we once had to chase our food (exercise) and eat what was available to us at that time ie. nuts, fruits and vegetation and did not have the convenience of going to the store or fast food restaurant to buy everything we need.
O.K. Back to the film. From beginning to end this film keeps the viewer infactuated with Joe's progress as he journeys across the U.S. interviewing people along the way and spreading the benefits of Juicing and, speaking with them about eating habits and what they eat. What keeps the film authentic is that Joe is just like every one of us. Joe is a person that loves to eat, drink, and may exercise here and there. Through the film we see Joe as he is sometimes teased by food (even just the scent of it) but maintains on his fast. The greatest part of Joe's journey is when he runs into 430 Lb Phil Staples at a truck stop in Arizona. Joe discovers that Phil has the same rare autoimmune disease that he has. Joe explains to Phil the health benefits of juicing and the amount of weight he has lost. Joe also explains to Phil he no longer has to take his costly medication because his own body has healed itself naturally from juicing. Joe then lets Phil sample a cup and gives Phil a business card and tells him to give him a call if he has any questions. (Joe is just that type of guy, very friendly and shows genuine cares about people he speaks with.) After Joe returns to Australia six months later he receives a poignant call from Phil asking for his help and Joe comes to the rescue. I won't give too much away but Phil completely turns his life around and shares the benefits of juicing to others.
All in all I highly recommend watching this film. This movie is very motivating and after watching, it may encourage you to try juicing yourself. I have yet to try a complete juice fast but instead drink a juice in the morning for breakfast, a regular lunch, and a juice at night. I will soon attempt a 10 day fast and will keep you guys updated. The juicer I bought is the Breville Ikon 900 watt juicer which is the best money I have spent to improve the lives of everyone in my household. If you have a farmers market available in your area I recommend buying from there instead of the super market which will be more expensive. Also go to www.jointhereboot.com for all your information on juicing from Joe and his gang.


Gentlemen's Day returns to Royal Windsor Racecourse on Saturday 29 June with MINISTRY OF SOUND and an incredible line-up, featuring TIM CULLEN, FULL INTENTION and a headline DJ set from BASEMENT JAXX!
The famous Best Dressed Gent Competition returns again this year with some incredible prizes to be won. Could you be the best dressed? Let's see your finest attire and don't forget to visit our Best Dressed Station for the chance to win.
Windsormania was one of our brand new to 2018 themes and is returning this year on Sunday 30 June for even more fantastic family fun and thrills! There will be a huge selection of entertainment and attractions on offer including a spectacular free funfair for the children and the best news is, all of the entertainment on the day is free!
As well as all this entertainment, there will also be seven thrilling races for both the adults and children to enjoy.
Last year we had a selection of the countries best tribute acts, including One Direction, Katy Perry and Pink! This year, it's going to be even better with two of the countries fantastic tribute acts. But who could it be? Please stay tuned and check back regularly to find out who will be performing LIVE!
Ronnie Scott's world famous jazz club - Live after racing!
What better way to end our 3 day festival than with our famous Monday Night Racing for Ronnie Scott's Jazz Club Live! Ronnie Scott's are the perfect accompaniment to Monday Night Racing!
Start July with a great night of competitive racing and dance the night away with the greatest jazz and funk sounds in town.


Fantastic Garden Apartment perfect for holiday rental in Riviera del sol. This proper has two bedrooms and two bathrooms with a fully equipt kitchen and utility area. There is a spacious lounge and dining area which leads onto the terrace and private garden. There is a barbeque on the terrace for guests to use . There is also a underground garage space and a lift. The communal swimming pool is fantastic and also has a small pool for children, a perfect place to enjoy with family and friends.


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Pilot (No Ordinary Family)
Title: Pilot (No Ordinary Family)
Subject: Tom Amandes, Pilot (television episode)
No Ordinary Family episode
David Semel
Teleplay by
Jon Harmon Feldman
Greg Berlanti &
September 28, 2010 (2010-09-28)
— Next →
"No Ordinary Marriage"
List of No Ordinary Family episodes
"Pilot" (also known as "No Ordinary Pilot") is the first episode of the ABC series No Ordinary Family. The episode's teleplay was written by Jon Harmon Feldman, from a story by Greg Berlanti and Feldman. David Semel directed the episode, which was originally broadcast on September 28, 2010.
3.1 Ratings and viewership
3.2 Critical reception
An average, ordinary family, the Powells have been growing apart steadily thanks to Stephanie Powell's (Julie Benz) successful career as a research scientist and their kids becoming teenagers. Jim Powell (Michael Chiklis) is the only one who seems to notice. During a family vacation research trip (which Jim forced his family to take), the plane they are in crashes into a lake during a storm. The family safely returns home, but doesn't seem to be any closer to each other. Eventually, Jim, Stephanie, Daphne (Kay Panabaker) and JJ (Jimmy Bennett) discover that they have superpowers. Jim attempts to use his newly discovered invulnerability and strength to stop crime, but ends up being shot and injured by high calibre bullets. He eventually ends up revealing his newfound powers to his wife, who has discovered that she has superspeed. They eventually reconcile and have a heart to heart talk, finally admitting that their marriage needs help. Meanwhile their daughter faces normal teenager issues, which are worsened with the arrival of her telepathy, enabling her to learn that her boyfriend is cheating on her. Initially distraught, she eventually accepts her new power. Meanwhile, JJ, who prior to the crash had a learning disability, suddenly becomes a genius. The episode ends with the family spending more time together, playing and Jim and Steph visiting a marriage counselor.
Part of the episode "Pilot" was filmed on location at the Amazon River.
Ratings and viewership
A total of 10.70 million American viewers watched the pilot episode, placing third in its timeslot and first in family viewing.[1][2] The episode was also watched by 2.07 million Canadian viewers, placing eleventh for that week.[3]
The episode received mixed reviews from Zap2it.[4] Chris Carabott of IGN gave the episode a 7.5 out of 10, stating "the show has a whimsical flair that's not hard to appreciate."[5] Tim Goodman of the San Francisco Chronicle said, "There's lot of promise here, of drama, action, comedy, etc, all wrapped up in a family-friendly series."[6] Review aggregator Metacritic gave the series a score of 65 out of 100, indicating generally favorable reviews based on 28 professional critics.[7] Alessandra Stanley from The New York Times gave an average review, praising the fact that the show offers "calmer, more restrained fantasy about paranormal prowess" by combining shows like Heroes and Lost with the wholesome fantasy of Disney's The Incredibles and The Swiss Family Robinson, but concluded her review by saying that "it's not clear whether this series—a hybrid of family drama and graphic novel—can sustain interest once the premise is fully established".[8]
Tom Amandes
Abraham Lincoln, JAG (TV series), Numbers (TV series), Scandal (TV series), Richmond, Illinois


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According to the US National Highway Traffic Safety Administration (NHTSA), General Motors is recalling 12,626 units of the 2013 Cadillac XTS model due to improper rear seat head restraints.
"The rear seat head restraints may not lock in the upright position after being folded forward," said NHTSA. "If the head restraint is at its lowest position and it falls forward, it will not meet the height required by the standard. In the event of a vehicle crash, the lowered head restraint may increase the occupant's risk of neck injury." The affected vehicles were made between 12 Oct 2011 and 30 Aug 2012.
To GM's credit, the automaker discovered the problem themselves. The single piece rear headrest design looks classy and unique but is sadly lacking in its functionality.
The Cadillac XTS is a full-size luxury car that is meant to be a replacement for the STS and DTS. The XTS proved to be a popular model. For the first 10 months of 2012, the XTS is already the 4th best-selling car in the states.


What's the most recognizable Racing Livery? What paint job tells you the Team sponsor by seeing the color combo from a mile away? Even without reading any text…. I'd think Red Bull, Coca Cola, Marlboro, Rothmans, Martini, Gulf, Falken, Tic Tac, Yagermeister… maybe a few others would make the list. But since Hot Wheels is a kid brand, most of the cigarette and booze sponsors get excluded from making it into mainline cars. So of the remaining teams we're left with instantly recognizable paint jobs, and I'm going to start adding them to my collection.
Thanks to all the detailed work HWCOLLECTORSNEWS.COM put into their web site it can be used as a shopping catalog for desirable cars… past and present. I'm happy to say that many of the abovementioned cars are already in my collection. And the rest I'll be on the lookout for on eBay to be sure I can add them to my wall.
There are of course others in each of these series, none large than the amazing Gulf Racing variety.
But it's important to remember that collecting anything requires patience. Especially with something like Hot Wheels where new surprises come out every year. So I'll be adding my additions as I accumulate them over the years.
Update…. after sleeping on it I realized there were more iconic liveries that I should have definitely included in my "look out for" list.


Have you ever wondered if there is a cheapest time of the day to put a load of washing on? Well the answer is yes, there is. Energy is most expensive when demand is at its highest, so using more during these times every day could significantly increase your energy bills.
But, thanks to new software developed by conservation charity WWF (World Wide Fund for Nature) and the National Grid, you can find out when energy is in high demand and when demand is low (and therefore at its cheapest rate). The best part is that you can get this information up to two days in advance, meaning you can schedule your wash accordingly.
The software looks at weather information from the Met Office and historical data from the National Grid to predict energy demand. It breaks the day down into two-hour segments. It can also show when renewable energy sources are active, letting those households conscious about the environment use energy at the best times for wind and solar power.
While the software has been developed, there aren't yet any apps that have tapped into its power. The National Grid is expecting energy corporations to create their own or add the functionality to already existing apps.
However, there are already similar initiatives available. Some suppliers have started offering 'time of use' tariffs for those households using smart meters. You get rewarded with cheaper rates for using energy when demand is low. Green Energy UK and British Gas both offer tariffs which charge less for energy used overnight.
This software could soon become main stream and change the way people use energy. This follows reports from the National Grid of "the greenest summer ever", where 52% of electricity demand was filled by renewable resources.
Anything that helps the environment and simultaneously saves people money is alright with us.


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Category Archives: Hot Peppers
Hot Peppers, Uncategorized
"Hot" New Habanero Varietal Is Heatless
February 25, 2017 javava2012	Leave a comment
The shishito — another mild pepper varietal popularized by Noah Robbins.
Just as you've never heard anyone say they drink sweet tea just for the sugar, it's highly unlikely you've every heard someone say they eat Habanero peppers just for their wonderful taste. That's about to change.
A guy who clearly got bit by a 'crazy-as-a-fox' bug has found a way to consistently breed the heat out of the Habanero, leaving a "tangy, sweet, melon-like flavor," Ark Foods CEO Noah Robbins told Munchies.vice. Robbins' company, which has farms in New York, North Carolina and Florida, specializes in what he calls "interesting" vegetables, such as that mild, tasty Habanero and the shishito pepper, a sweet Asian variety.
Robbins first encountered the heat-free Habanero at a farmers' market in New York City. The seller didn't have many available, but Noah was so impressed with the different eating sensation – "you keep expecting heat, but it doesn't come," he told Munchies – so he picked up a few to generate enough seeds for some experimenting. It took about three years to come up with the one he now marketing, in a limited way across the country.
He notes on his company's website that "the newest (and cutest) member" of the Ark Foods family is the cucamelon.
"They're strikingly similar looking to tiny watermelons, with the tangy, fresh taste of a cucumber. Delicious, refreshing, and tart," the web site says.
Never let it be said that there's nothing new under the sun!
HabanerosHot Peppers
Cajun, Hot Pepper Health Risk, Hot Peppers, Research, Science, Scoville Heat Units Scale
Hot Pepper Causes 2.5cm Rip In Man's Esophagus
October 22, 2016 javava2012	Leave a comment
Louisiana pepper breeder/grower Tony Primeaux handles some hot ones. (Photo: Lee Celano/The Daily Advertiser via AP)
A 47-year-old man recently attempted a rather silly, super-spicy feat – eating a hamburger covered with a ghost pepper puree. The ghost pepper measures a scary 1 million units on the Scoville heat unit (SHU) scale, a per-mass measure of capsaicin, the chemical compound that makes some peppers spicy-hot.
By way of comparison, a bell pepper measures 0 on that scale. A jalapeno comes in at between 3,500-10,000 units; a Serrano and a Peperoncino score in the range of 10,000-30,000 units, and both Cayenne and Tabasco peppers range from 30,000-50,000 units – about as high as most people care to experience.
(Police pepper spray, by the way, comes it at around 5 million SHU.)
(I thought my mouth was on fire once when I took a bite out of an Habanero, AKA Scotch Bonnet chili – 100,000 -350,000 heat units – I'd found on sale at a London street market. I'd been told, simply, "It's a hot pepper." I said, "Oh, I love hot peppers." This one was not to love!
(As quickly as I could, I went into a pub and ordered a pint of beer, as beer is rumored to cut the effect of heat in food, or peppers. Alternatively, the beer may just make you forget about the pepper's burning sensation!)
An article in The Washington Post said that peppers that pass the 1 million SHU mark are called superhot. "As a rule they are reddish and puckered, as though one of Satan's internal organs had prolapsed. To daredevil eaters of a certain stripe, the superhot peppers exist only to challenge.
"When consumed, ghost peppers and other superhots provoke extreme reactions," The Post article said.
"Your body thinks it's going to die," as Louisiana pepper grower Ronald (Tony) Primeaux told the AP in October. "You're not going to die."
The Washington Post's Tim Carman described eating a pea-sized chunk of the pepper, sans seeds, in 2012. "It was as if my head had become a wood-burning oven, lighting up my tongue and the interior of my skull," he wrote. "Milk provided little relief, until the burn began to subside on its own about 10 minutes later."
Primeaux, who hopes to claim the world's hottest pepper title through cultivating his Louisiana Creeper variety, said, "When you put one of these in your mouth, it's a whole 'nother ballgame," in his interview with the AP. "A bear is chasing you. You've just been in a car wreck. You just got caught speeding, and a cop is giving you a ticket."
Pepper breeder/grower Tony Primeaux with some of his plants. (Photo: Lee Celano/The Daily Advertiser via AP)
That truly seemed to be the sensation experienced by the unnamed 47-year-old reported on in The Journal of Emergency Medicine. For him, "ingesting the pepper burger was less a bear chase and closer to an attack," The Post article said.
As physicians at the University of California at San Francisco reported in the case study reported on in The Journal of Emergency Medicine article, he consumed the burger and attempted to quench the heat in his mouth with six glasses of water. When that failed the man began to vomit, which gave way to abdominal pain. He dialed emergency help.
At the emergency department, he received Maalox and painkillers. After his condition worsened, doctors moved him to the operating room, where they discovered a "2.5-cm tear in the distal esophagus," about one inch, as the case report authors noted. The force of the vomiting and retching led to a rare diagnosis of Boerhaave's syndrome; these spontaneous tears in the esophagus can be fatal if they are not diagnosed and treated.
"The rupture was as a result of the forceful vomiting and retching," said UC San Francisco clinical fellow and study author Ann Arens, in an email to The Washington Post, "as a result of eating the hamburger with the ghost pepper puree."
In this case, surgeons were able to repair the man's throat. "He remained intubated until hospital day 14, began tolerating liquids on hospital day 17," they wrote, "and was discharged home with a gastric tube in place on hospital day 23."
The researchers concluded the case study with a warning.
"Food challenges have become common among social media, including the infamous cinnamon challenge," they wrote, referencing the spice fad that was popular in early 2012. (When eating a heaping spoonful of cinnamon went wrong, it led to emergency calls and at least one collapsed lung.)
"When people ask me whether it is safe to try the 'spicy food challenges' I generally take a Nancy Reagan stance," said Arens, "and say 'Just Say No.' But if you really just can't help yourself, I would recommend just starting with a taste."
Crazy Food-Eating EventsHot Pepper Health RiskPepper-BreedingScoville Heat Unit Scale


Thank you for the excellent tile-work on our new home!
We had Berry Ceramic tile every inch of flooring in our home. They cleaned up another contractor's mess and left us with absolutely beautiful floors, shower/tub and backsplash tiles. They are professional, and work very hard to do the job the right way. We really struggled to get a genuine pro tile company, but found it with this company!


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Joint Coordination Center opens in Istanbul to oversee grain export agreement
CNNJuly 27, 2022
Military delegations of Turkey, Russia and Ukraine, United nations (UN) sit at the opening of the Joint Coordination Centre (JCC) for Ukrainian grain exports in Istanbul on july 27, 2022. - Turkey formally opened a joint coordination centre for Ukrainian grain exports under a UN-backed deal aimed at resuming shipments for the first time since Russia's February invasion of its neighbour. (Photo by OZAN KOSE / AFP) (Photo by OZAN KOSE/AFP via Getty Images)
The Joint Coordination Center, which will oversee the export of Ukrainian grain, has opened in Istanbul.
In an address at the National Defense University, Turkish Defense Minister Hulusi Akar said the center "has a special meaning for the whole world and will work for purely humanitarian purposes."
The coordination center was one of the key creations of the grain deal agreed between Russia and Ukraine under the auspices of the UN and Turkey.
As part of the deal signed Friday, grain ships will navigate through safe corridors in the Black Sea and then pass through the Bosphorus strait — an important shipping corridor in northwest Turkey — in order to reach global markets.
According to Akar, the deal "signed by the parties will be valid for 120 days and will continue unless the parties request termination."
He told journalists and officials that "the preparation and planning of the first grain-laden ships to leave the Ukrainian ports continues."
"The duty of the center is to provide safe sea transportation of grain and similar food products to be exported from Ukraine from the ports of Odesa, Chornomorsk and Yuzhny," the minister added during an opening ceremony at the university.
Russia, Ukraine, the UN and Turkey will each send five representatives, including a mixture of civilian and military representatives, according to Akar.
"We believe that the works to be carried out through the Joint Coordination Center will make significant contributions to overcoming the food crisis affecting the whole world, especially to lowering prices," the minister continued.
Akar stressed that the officials working at the center "are aware that the eyes of the world are on them," outlining Turkey's hope that the center "will make maximum contributions to humanitarian needs and peace through collective and successful work."
CNN's Yusuf Gezer in Istanbul contributed reporting to this post.
Chornomorsk exported from Ukraine Food products Opening ceremony ports of Odesa Russia the minister transportation of grain Turkey Ukraine UN university Yuzhny
"We have freedom, give us wings to protect it": Zelensky repeats call for fighter jets
Dramatic photos show the moment an 8-year-old survivor was rescued and reunited with his mother
Earthquakes moved Turkey 3 meters toward west: geologist
Egyptian Foreign Ministry: 2 Egyptian victims found dead in Turkey


The Project Management Professional (PMP)® is the most important industry-recognized certification for project managers. The PMP certification is not industry-specific, it is a global certification attesting to the candidates ability to speak to, understand, and apply the PMP principles. As a PMP, you can work in virtually any industry, with any methodology and in any location.
CompTIA provides premier, vendor-neutral certifications to help IT professionals stay ahead of the information technology curve curve. It validates expert knowledge in the latest technology trends and the ability to work with an extensive variety of existing and emerging technologies.
Microsoft has been providing certifications since the early-1990s. I received my first MCP certification in 1994 when I passed the Microsoft DOS exam. The required exams for my 1995 MCSE certification were: DOS, Windows for Workgroups 3.11, NT Workstation 3.1, NT Server 3.1, SQL Server or Microsoft Mail 3.2, and TCP/IP. I also completed the Microsoft Certified Trainer (MCT) certification around the same time.
I kept my certifications current until 2006, when I moved into a full-time project management role.
Back in the day Cisco offered five certifications: CCNA, CCDA, CCNP, CCDP. and CCIE. They still offer the same certifications today, but each one has at least five specialization areas to choose from. I completed these certifications to compliment my Microsoft knowledge. It proved helpful when teaching Microsoft engineering classes as well as during various consulting projects.


We can provide technical assistance for things such as simple networking and computer setups. We can help with installations and basic IT services. We can help you design and develop a website such as this one. We can do detailed spreadsheets and simple graphic design. We are a tech-saavy company so that you don't have to be.