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

Many studies have reached the conclusion that superluminous supernovae (SLSNe), i.e., core collapse supernovae (CCSNe) with peak r-band magnitude of $M_{\rm r} < -20$, and luminous supernovae (LSNe) that are CCSNe with $M_{\rm r} =-19$ to $-20$ (see \citealt{Gomezetal2022} for definitions), contain an extra energy source or another ingredient in addition to the explosion itself. We can distinguish between two classes of explanations.

In the first class of explanations the explosion itself is the delayed neutrino mechanism. It seems that the heavily studied delayed neutrino mechanism (\citealt{BetheWilson1985, Hegeretal2003, Janka2012, Nordhausetal2012, Bruennetal2016, Jankaetal2016R, OConnorCouch2018, Mulleretal2019Jittering, BurrowsVartanyan2021, Fujibayashietal2021, Bocciolietal2022, Nakamuraetal2022}; for a recent brief optimistic review of this mechanism see \citealt{Mezzacappa2022}) cannot reach CCSN explosion energies of $E_{\rm SN} \ga 2 \times 10^{51} {~\rm erg}$ (e.g., \citealt{Fryer2006, Fryeretal2012, Papishetal2015a, Sukhboldetal2016, SukhboldWoosley2016, Gogilashvilietal2021}). Many studies of SLSNe and LSNe that take the explosion itself to be by the delayed neutrino mechanism attribute the extra energy of LSNe and SLSNe to a magnetar, i.e., a rapidly rotating magnetized neutron star (e.g., \citealt{Greineretal2015, Metzgeretal2015, Yuetal2017, Marguttietal2018, Nicholletal2017b}).

According to the second class of explanations jets explode most (or even all) CCSNe (for a review see \citealt{Soker2022Rev}). Even if the pre-collapse core is slowly rotating, accretion of material with stochastic angular momentum onto the newly born neutron star leads to the launching of jittering jets (jets with stochastic variation of directions), i.e., the jittering jets explosion mechanism (\citealt{Soker2010, PapishSoker2014Planar, GilkisSoker2015,  Quataertetal2019, Soker2019RAA, Soker2020RAA, ShishkinSoker2021, AntoniQuataert2022, Soker2022a, Soker2022Boosting}). Therefore, according to this class of models jets also explode all LSNe and SLSNe, as well as the CCSNe that accompany gamma ray bursts, as  \cite{Izzoetal2019} also claim from their observation of a gamma ray burst.
Further motivation to consider jet-driven explosions is the problems of magnetar modelling of some SLSNe, e.g., \cite{SokerGilkis2017a} who analysed the magnetar modelling by \cite{Nicholletal2017b}, and LSNe, e.g., \cite{Soker2022LSNe} who analysed the magnetar modelling by \cite{Gomezetal2022}.
Moreover, some studies find that the formation of an energetic magnetar most likely leads to the launching of jets during the explosion and in some cases also after the explosion, and that these jets might carry more energy that the magnetar \citep{Soker2016Magnetar, Soker2017Magnetar, SokerGilkis2017a}; for some possible energy sources of SLSNe see, e.g., \citealt{WangWangDai2019RAA}.)

According to the jittering jets explosion mechanism the jets that explode LSNe and SLSNe keep more or less a fix axis. Namely, the jittering is  small. This requires the pre-collapse core to have fast rotation. For example, a binary companion that spirals-in inside the red supergiant progenitor to a very small orbital separation both spins-up the core and removes the hydrogen-rich envelope to lead eventually to striped-envelope CCSN (CCSN-I), i.e., a type Ib or a type Ic CCSN. The fix axis makes the efficiency of the jet feedback mechanism (for a review see \citealt{Soker2016Rev}) inefficient, namely, the explosion energy will be many times the binding energy of the exploding star. Therefore, the  explosion is very energetic \citep{Gilkisetal2016Super, Soker2017RAA}.

Note that unlike many studies that require the pre-collapse core to have very fast rotation so its specific angular momentum by itself allows the formation of accretion disk around the newly born neutron star or black hole (e.g., \citealt{Khokhlovetal1999, Aloyetal2000, MacFadyenetal2001, Wheeleretal2008, Maedaetal2012, LopezCamaraetal2013, BrombergTchekhovskoy2016,  Nishimuraetal2017, Sobacchietal2017, Grimmettetal2021, Gottliebetal2022, Perleyetal2022}),
in the jittering jets explosion mechanism convective fluctuations in the pre-collapse core can supply additional stochastic angular momentum and therefore the core might have a slower rotation  (e.g., \citealt{GilkisSoker2014, GilkisSoker2016, ShishkinSoker2022}).

\cite{KaplanSoker2020b} proposed a toy model to explain the puzzling light curve of the LSNe SN~2018don. SN~2018don is a hydrogen-poor LSN that has a sharp drop in its light curve \citep{Lunnanetal2020}. It has a long rise time to maximum light relative to other LSNe \citep{Gomezetal2022}.
\cite{KaplanSoker2020b} built simple bipolar ejecta models for jet-driven CCSNe and showed that for an observer in the equatorial plane of the bipolar morphology the light curve has a rapid luminosity decline, and even an abrupt drop. In some cases there is no abrupt drop, but rather a `knee' in the light curve where a rapid drop changes to a moderate drop in luminosity. \cite{Soker2022LSNe} proposes that such a bipolar explosion might explain the `knee' in the light curve of the SLSN SN~2020wnt (for its properties see \citealt{Tinyanontetal2021, Gutierrezetal2022, Tinyanontetal2022}).

\cite{KaplanSoker2020b} did not simulate the bipolar jet-driven explosion, but rather simply assumed that the ejecta has an axisymmetrical structure composed of an equatorial ejecta and faster polar ejecta, each which is a part of a sphere (different spheres), and that it has a uniform effective temperature. In this study we conduct hydrodynamical simulations to simulate the bipolar explosion (section \ref{sec:Bipolar}), and then estimate the light curve, assuming a uniform effective temperature (because we do not calculate radiative transfer) but only if the photosphere is hot (section \ref{sec:Light curve}).
We summarize our study that strengthens the claim that jets power (at least some) LSNe and SLSNe, and more generally most CCSNe (section \ref{sec:Summary}).

\section{The bipolar jet-driven explosion}
\label{sec:Bipolar}
In this section we describe numerical simulations of a jet-driven bipolar CCSN explosion into several different compact bipolar circumstellar matter (CSM) morphologies.

\subsection{The numerical code}
\label{subsec:Numerical}

We use version 4.6.2 of the adaptive-mesh refinement (AMR) hydrodynamical FLASH code \citep{Fryxell2000} in three dimension (3D). We turn off the radiative cooling since the regions we simulate are optically thick.
We include radiation pressure, electrons pressure, and ions pressure as we assume an adiabatic index of $\gamma=5/3$ and $\mu = 0.5$, as we assume a fully ionised pure hydrogen.
We set outflow conditions on all the boundary surfaces of the 3D grid. We use resolution with 7 refinement levels, i.e., the ratio of the length of the sides of the grid to the shortest cell in the grid is $2^{9}$. The finest cell in the grid has a side of $1.05 AU$. We simulate the whole space with a total size of the Cartesian  numerical grid of $(534 AU)^3$, i.e., $(L_x,L_y,L_z) = \pm 267 AU$.
We simulate the entire space, rather than only one half of the symmetry plane $z=0$, to avoid numerical artifacts at the symmetry plane had we simulated only one half of the interaction region. We will present the flow structure in the  entire computational grid to emphasize the bipolar structure that the jets shape and the flow in the equatorial plane.

\subsection{Building the bipolar explosion}
\label{subsec:Explosion}

We build the bipolar explosion by three numerical phases. These might result from a common envelope evolution (CEE) or a grazing envelope evolution (GEE). However, for the present study the only important phase is the general bipolar explosion with dense equatorial CSM gas and fast bipolar outflows.

\subsubsection{The bipolar CSM}
\label{subsubsec:Wind}

We build a bipolar CSM into which the jet-driven explosion occurs. The manner by which we built the CSM is not so important. We expect a CEE or a GEE to form such a bipolar CSM. The explosion then takes place into the bipolar CSM.
Namely, the CSM is formed and shaped, for example, by a precursor where the CCSN progenitor expands few years before the explosion and engulfs a companion that launches jets (e.g., \citealt{McleySoker2014, DanieliSoker2019, Soker2022Rev}).
Core activity of excitation of waves (e.g., \citealt{QuataertShiode2012, ShiodeQuataert2014, Fuller2017, FullerRo2018, WuFuller2022}) or magnetic activity (e.g., \citealt{SokerGilkis2017b}) causes the envelope expansion years to months before explosion.

We set the initial (at $t=0$) grid to have an expanding dense shell of mass $M_{\rm wind}$ from the center to an outer radius of $R_{\rm sh}=10^{15} {~\rm cm} = 67 {~\rm AU}$. An intensive wind due to a CEE/GEE forms this shell. We present the values of this mass in the second column of Table \ref{Table:cases}. In the third column we list the velocity of the wind for each case $v_{\rm wind}$, in the forth column the corresponding mass loss rate of the wind, and in the fifth column we list the total kinetic energy in this wind. The duration of the spherical wind is $3.2(v_{\rm wind}/100 {~\rm km} {~\rm s}^{-1})^{-1} {~\rm yr}$. The density in this shell goes as $\rho_{\rm wind} \propto r^{-2}$.
In the region $r>67 {~\rm AU}$ we have at $t=0$ a low density expanding gas with the same velocity as the wind. The spherical wind that composes the initial condition at $t=0$ is the first phase of our numerical study.
The initial temperature of the simulation box and the jets is $10000{~\rm K}$.
\begin{table*
\centering
\begin{tabular}{|c|c|c|c|c|c|c|}
\hline
Sim. & $M_{\rm wind}$ & $v_{\rm wind}$ & $\dot{M}_{\rm wind}$ & $E_{\rm wind}$ & $M_{\rm jets}$ & $E_{\rm jets}$  \\
           & $M_\odot$ & ${~\rm km\; s^{-1}}$ & $M_\odot {~\rm yr}^{-1}$ & ${~\rm erg}$ & $M_\odot$ & ${~\rm erg}$\\
 \hline
EXP1       & 0.25 & 100 & 0.08 &$2.5 \times 10^{47}$ & $3.3 \times 10^{-5}$ & $8.2 \times 10^{47}$ \\ \hline
EXP2      & 2.5 & 100 & 0.8 &$2.5 \times 10^{48}$  & $3.3 \times 10^{-4}$ & $8.2 \times 10^{48}$\\ \hline
EXP3       & 0.75  &57.7 & 0.24 &$2.5 \times 10^{47}$ & $ 10^{-4}$ & $8.2 \times 10^{47}$\\ \hline
EXP4      & 0.75  &40.8 &0.24 &$1.25 \times 10^{47}$ & $10^{-4}$ & $4.1 \times 10^{47}$\\ \hline

\end{tabular}
\caption{Summary of the CSM properties for the four simulations that we present in the paper. The columns list, from left to right and for each simulation, the name of the simulation, total mass of the spherical wind, the velocity of the wind, the mass loss rate of the wind and the total kinetic energy of this wind.
We start the simulations at $t=0$ by launching two opposite jets into the wind (shell) for 60 days. We list the total mass of these jets that shape the bipolar CSM just before the explosion and their total kinetic energy in the sixth and seventh column, respectively. In all simulations the jet-driven explosion energy that we launch later is $E_{\rm SN} = 2.5\times 10^{51} {~\rm erg}$, and the explosion duration, basically the exploding-jet activity duration, is $3 {~\rm days}$. }
\label{Table:cases}
\end{table*}

At $t=0$ we launch two opposite jets to form a bipolar CSM. The shaping of the CSM by these  jets is the second phase of our numerical study. These jets are active for 60 days in all cases.
To launch the jets we set a fast  outflow, velocity of $V_{\rm j} =  5 \times 10^4 {~\rm km} {~\rm s}^{-1}$ inside two opposite cones, each cone with a length of $r=7 {~\rm AU}$ and a half-opening angle of $\alpha = 40^{\circ}$. The density of the jets inside the cones is $\rho_j (r) = \dot{M}_{\rm jets} / [4\pi r^{2} v_{\rm j} (1-\cos \alpha)]$, where  $\dot{M}_{\rm jets}=M_{\rm jets}/60~{\rm day}$ is the mass loss rate into the jets and $M_{\rm jets}$ is the total mass the two shaping jets carry.
In the sixth and seventh column of Table \ref{Table:cases} we list the combined mass and energy of these jets, respectively, for the four simulations.

During the entire simulation we inject a dense equatorial outflow due to the binary interaction. This equatorial outflow has a half opening angle of $30^{\circ}$ from the equatorial plane, a mass loss rate of $1 M_{\odot} {~\rm yr}^{-1}$, and a velocity of $100 {~\rm km\; s^{-1}}$. During the entire simulation (including the later explosion phase) we inject a mass of $\approx 0.4M_\odot$ in the equatorial outflow.

In Fig. \ref{Fig:time_zero} we present the formation of the bipolar CSM for simulation EXP1. All panels show the density in the meridional plane, i.e., a plane along the jets' axis. The shaping-jets are active for 60 days starting at $t=0$. In the upper, middle, and bottom panels we present the density maps at $t=1$~day, $t=45$~day, and $t=89$~day, respectively.
\begin{figure}
	\centering
	\includegraphics[trim=0.0cm 3.2cm 0.0cm 4.4cm ,clip, scale=0.55]{dens_xz_3_1}
	\caption{The density maps in the meridional plane at three times (as indicated on the panels) during the formation of the bipolar CSM into which we later explode the star. The shaping-jets are active from $t=0$ for 60 days. The density color-bar on the right is in units of $\rm g ~cm^{-3}$. }
	\label{Fig:time_zero}
\end{figure}

\subsubsection{Jet-driven explosion}
\label{subsubsec:ExplosionJets}

The third numerical phase is a second, much more energetic, jet-launching episode. This jet-launching phase is the jet-driven CCSN explosion, as we assume that jets power this CCSN (see section \ref{sec:intro}). We assume that the newly-born neutron star accretes fallback material and launches the jets for three days starting 30 days after we turned off the jets that shaped the CSM (section \ref{subsubsec:Wind}). Namely, we launch the exploding jets during the time period $90 {~\rm days} <t<93 {~\rm days}$.
We launch two opposite jets into two opposite cones each cone with a length of $r=7 {~\rm AU}$ and a half-opening angle of $\alpha = 40^{\circ}$. During these three days we linearly increase the jets' velocity from zero to $100,000 {~\rm km\; s^{-1}}$,
$v_{\rm ej}(t)=100,000 (t-90~{\rm day})/3 {~\rm km\; s^{-1}}$, and we linearly decrease the mass loss rate into the exploding jets from $10 M_{\odot} {~\rm yr}^{-1}$ to zero.
During the explosion we continue to inject the dense equatorial outflow of a half opening angle of $30^{\circ}$ from the equatorial plane, a mass loss rate of $1 M_{\odot} {~\rm yr}^{-1}$, and a velocity of $100 {~\rm km\; s^{-1}}$.

We turn now to analyse the flow properties of the ejecta-CSM interaction, postponing the calculation of the light curve to section \ref{sec:Light curve}.

\subsection{The explosion flow structure}
\label{subsec:ExplosionStructure}

We describe the flow that results from the interaction of the jet-driven ejecta (section \ref{subsubsec:ExplosionJets}) with the bipolar CSM (section \ref{subsubsec:Wind}). We recall that the exploding jets are active for three days from $t=90~{\rm day}$ to $t=93~{\rm day}$. The jets' symmetry axis is along the $z$ axis through the origin.

In Figs. \ref{Fig:dens}, \ref{Fig:vel} and \ref{Fig:temp} we present the density, velocity, and temperature maps, respectively, in the meridional plane at four times as the insets indicate in the panels.
\begin{figure}[ht!]
	\centering
	\includegraphics[trim=0.1cm 0.8cm 0.0cm 1.0cm ,clip, scale=0.44]{dens_xz_2_2_3.png}
	\caption{Density maps in the meridional plane at four times all after explosion, as indicated on the panels. Time is measured from the onset of the jets that shape the CSM. The exploding jets are active from $t=90~{\rm day}$ to $t=93~{\rm day}$. The logarithm of the density in units of $\rm g ~cm^{-3}$ is according to the color-bar. }
	\label{Fig:dens}
\end{figure}
\begin{figure}[ht!]
	\centering
	\includegraphics[trim=0.1cm 0.8cm 0.0cm 1.0cm ,clip, scale=0.44]{vtot_vec_xz_2_2_3.png}
	\caption{Similar to Fig. \ref{Fig:dens} but showing the velocity maps. The direction is according the arrows and the logarithm of the velocity magnitude in units of $\rm cm ~s^{-1}$ is according to the color-bar.  }
	\label{Fig:vel}
\end{figure}
\begin{figure}[ht!]
	\centering
	\includegraphics[trim=0.1cm 0.8cm 0.0cm 1.0cm ,clip, scale=0.44]{temp_xz_2_2_3.png}
	\caption{Similar to Fig. \ref{Fig:dens} but showing the temperature maps. The color-bar gives the logarithm of the temperature in K. }
	\label{Fig:temp}
\end{figure}

As expected, the jet-driven explosion into a bipolar CSM forms a highly non-spherical bipolar explosion. The faster expansion along and near the polar direction has implications to the light curve (e.g., \citealt{KaplanSoker2020b}). The first one is that the inflated polar lobes imply that at early times an equatorial observer sees a larger photosphere than a polar observer. Later, because of the faster expansion of the lobes the photosphere of the lobes retreats faster. This implies that the photosphere area that an equatorial observer sees decreases faster than that of a polar observer.

The outcome is a rapid, and even abrupt, drop in the light curve for an equatorial observer, as \cite{KaplanSoker2020b} noticed with their toy model. We next demonstrate this behaviour of the lightcurve with our more sophisticated model of bipolar explosions.

\section{The lightcurves}
\label{sec:Light curve}

\subsection{Assumption and scheme}
\label{subsec:setup}

Our first assumption is that the ejecta and CSM radiates as a black body with a uniform temperature. To calculate the luminosity we need therefore to find the effective photosphere area that an observer sees. Since the morphology is, up to instabilities, axi-symmetric, we only vary the angle of the observer from the symmetry axis $\theta$ (i.e., $\theta=0$ for a polar observer and $\theta=90^\circ$ for an equatorial observer).

For a given observation angle $\theta$ we follow many lines parallel to the line of sight that cover the entire nebula (ejecta + CSM) and find the point in the nebula along each line  where the optical depth from infinity is
\begin{equation}
\tau = \int^{\infty}_{R_{ph}} \kappa \rho_{\rm H} dl = 2/3,
\label{eq:tauph}
\end{equation}
where $dl$ is a length element along the line of sight. We take the density $\rho_{\rm H}(x,y,z)$ from the hydrodynamical simulations (section \ref{sec:Bipolar}), and we assume a constant opacity $\kappa$.
To these we supply two conditions. First we take only points that are in the half space closer to the observer. Namely, we take a plane perpendicular to the line of sight and through the explosion site, and consider only points with $\tau=2/3$ that are between this plane and the observer. Points in the other half of space will radiate away from the observer. Secondly, we assume that cool areas, as the hydrodynamical results give, will further cool and will not contribute to the luminosity in the visible and near IR. Therefore, in calculating the photosphere area we consider only photospheric points with a temperature of
\begin{equation}
T_{\rm H}>T_{\rm H,c}=15,000 {~\rm K},
\label{eq:ConditionThc}
\end{equation}
where the temperature is from the hydrodynamical simulations.  The value of $T_{\rm H,c}$ is a parameter of our calculations that we must use because we do not include radiative transfer. Changing the value of $T_{\rm H,c}$ within the reasonable range of  $T_{\rm H,c} \la 20,000 {~\rm K}$ changes the lightcurve quantitatively in a small manner, but not its qualitative behavior. The later is the goal of our present study.

The above calculation gives us the cross section of the photosphere on the plane of the sky, i.e., the effective photospheric area $A_{\rm ef,ph}$ based on the hydrodynamical simulations and our assumptions.
To estimate the total explosion luminosity we assume that because of radiative cooling the photosphere temperature is much lower than what the hydrodynamical simulations give, and it is as observed in many CCSNe. We take $T_{\rm ef,ph}=8000 {~\rm K}$, but note it might be higher or a little lower and non-uniform.
The luminosity is then
\begin{equation}
L=4 A_{\rm ef,ph} \sigma T^4_{\rm ef,ph},
\label{eq:Luminosity}
\end{equation}
where $\sigma$ is Stefan–Boltzmann constant. In this study we adopt
$T_{\rm ef,ph}=8000 {~\rm K}$ Later we compare to observations and calculate the absolute r-band magnitude as $m_r=4.64-2.5\log(L/L_\odot)$.

We note that due to numerical limitation in simulating the very inner ejecta regions our results at late times are less accurate.

\subsection{Results}
\label{subsec:REsultsLightCurve}

In presenting the lightcurves we recall that we set $t=0$ when we start to shape the bipolar CSM inside  which the jet-driven explosion occurs. The jet-driven explosion itself takes place during the time period  $90 {~\rm days} <t<93 {~\rm days}$. Namely, the explosion time is $t=90 {~\rm days}$.

Before we present our results we point out again the limitations of our simple scheme to calculate the lightcurve. (1) One limitation of the hydrodynamical simulations is that we could not follow the very inner regions of the ejecta. As a result of that the light curves at late times are less accurate and can even be qualitatively wrong, e.g., a large increase of luminosity with time at late times.  (2) Another limitation of our lightcurve calculation is that we do not follow radiative transfer. As a result of that we do not have the correct temperature in the outer regions and cannot calculate the opacity at each point. We therefore take a uniform opacity in the grid and constant in time. (3) Also, in calculating the relevant area of the photosphere, $A_{\rm ef,ph}$, we avoid low temperature regions with $T<T_{\rm H,c}$ (equation \ref{eq:ConditionThc}), where $T_{\rm H,c}$ is a parameter of our calculations. (4) We take a uniform photosphere temperature $T_{\rm ef,ph}$ that does not evolve in time. It reality it does evolve with time.

In Fig. \ref{Fig:EXP1opacities} we present the lightcurves (r-band magnitude) of case EXP1 for observers at four angles (measured from the polar direction), and for three opacities of $\kappa=0.06$, $0.1$, and $0.2 {~\rm cm}^2 {~\rm g}^{-1}$, from top to bottom panel, respectively.  As expected, the higher the opacity is the longer the broad luminosity peak is. Namely, with increasing opacity the abrupt drop in the lightcurve occurs later.
\begin{figure}[htb!]
\includegraphics[trim=0.2cm 0.0cm 0.0cm 1.4cm ,clip, scale=0.33]{mag_t_AU_0.06_T_15e3_regular.png}
\includegraphics[trim=0.2cm 0.0cm 0.0cm 1.4cm ,clip, scale=0.33]{mag_t_AU_0.1_T_15e3_regular.png}
\includegraphics[trim=0.2cm 0.0cm 0.0cm 1.4cm ,clip, scale=0.33]{mag_t_AU_0.2_T_15e3_regular.png}
	\caption{Our calculated lightcurves for the case EXP1 for observers at four different angles relative to the symmetry (polar) axis. The upper, middle, and lower panels are for opacities of $\kappa=0.06$, $0.1$, and $0.2  {~\rm cm}^2 {~\rm g}^{-1}$, respectively, that we use in calculating the photosphere (equation \ref{eq:tauph}). We note the rapid decline in the light curve for observers that are not close to the polar axis. }
\label{Fig:EXP1opacities}
\end{figure}

Another way to extend the light curve is to increase the mass of the CSM and/or reduce its velocity. In Fig. \ref{Fig:MassiveCases} we present the lightcurves of cases EXP2, EXP3, and EXP4 which have larger masses and EXP3 and EXP4 have also lower velocities (Table \ref{Table:cases}). These lightcurves show that a more massive CSM can prolong the wide peak up to $\simeq 80 {~\rm days}$ for the parameters we use.
\begin{figure}[htb!]
	\includegraphics[trim=0.2cm 0.0cm 0.0cm 1.4cm ,clip, scale=0.33]{mag_t_AU_0.1_T_15e3_halfE.png}
    \includegraphics[trim=0.2cm 0.0cm 0.0cm 1.4cm ,clip, scale=0.33]{mag_t_AU_0.1_T_15e3_x3M.png}
	\includegraphics[trim=0.2cm 0.0cm 0.0cm 1.4cm ,clip, scale=0.33]{mag_t_AU_0.1_T_15e3_halfE_x3M.png}
	\caption{ The lightcurves for the cases EXP2, EXP3, and EXP4, all for an opacity of $\kappa=0.1  {~\rm cm}^2 {~\rm g}^{-1}$. }
	\label{Fig:MassiveCases}
\end{figure}

Our main result is that the lightcurve for an observer that is not too close to the polar direction might have an abrupt drop.
This is similar to the results of \cite{KaplanSoker2020b} who built a bipolar explosion toy model. We went beyond the toy model by conducting hydrodynamical simulations of jet-driven supernova explosion into a bipolar CSM (section \ref{sec:Bipolar}) and used the bipolar ejecta-CSM regions to calculate the luminosity as we explained in section \ref{subsec:setup}. Despite the limitation of our scheme, the qualitative results are robust. Exact fittings of specific cases will require more accurate calculations, in particular the inclusion of radiative transfer and a more systematic search of the (large) parameter space. Nonetheless, as we show next we can qualitatively explain the light curve of SN 2018don.

\subsection{The case of SN 2018don}
\label{subsec:2018don}
Below we compare our results with the lightcurve of  SN 2018don \citep{Lunnanetal2020} as \cite{KaplanSoker2020b} did.
The most similar lightcurve shapes to the shape of the lightcurve of SN 2018don are the lightcurves at $\theta=30^\circ$, $\theta=50^\circ$ and $\theta=80^\circ$ in EXP1 with $\kappa=0.1  {~\rm cm}^2 {~\rm g}^{-1}$ that we present in the middle panel of Fig. \ref{Fig:EXP1opacities}.
However, the wide peak duration in these lightcurves is much  shorter than that of SN 2018don. We can prolong the wide peak duration by increasing the CSM mass, e.g., four times longer in the lower panel of Fig. \ref{Fig:MassiveCases}. However, the shapes of the lightcurves of the cases with larger masses (the three cases that we present in Fig. \ref{Fig:MassiveCases}) are not as similar to the light curve of SN 2018don. To obtain the same shape as in the middle panel of Fig. \ref{Fig:EXP1opacities} (case EXP1 with $\kappa=0.1 {~\rm cm}^2 {~\rm g}^{-1}$) and with a longer wide peak we will have to conduct a very extensive search of the parameter space.
For example, we will have to modify also the explosion properties, which are the same in all cases here. Namely, we will have to  change in a systematic way the properties of the exploding jets, like their opening angle, energy, and duration. We also will have to consider a CSM that might be lighter in mass and that does not contain a hydrogen-rich gas. These additions are beyond our specific goal here. In future studies that will include also radiative transfer we will scan the parameter space.

Our goal here is to present the possibility of bipolar explosions to account for lightcurves with an abrupt drop. We therefore take the lightcurves from the middle panel of Fig. \ref{Fig:EXP1opacities} and simply multiply the duration by 4 (we stretch and shift the time). We then shift the curves in time to match the zero time in the observations of SN2018don. We present our comparison in Fig. \ref{Fig:KaplanSoker}. We also note that \cite{Lunnanetal2020} estimate the maximum luminosity of SN~2018don to be $-20.1$~mag according to the extinction.
\begin{figure}[htb!]
	\centering
	\includegraphics[width=0.5\textwidth]{mag_SN2018DON_Sim_0.1_T_15e3_regular.png}
\caption{The green and red points are the lightcurves of SN 2018don in the g-band and r-band, respectively, as
reported by \citep{Lunnanetal2020}. The four lines are based on our calculated lightcurves for the case EXP1 at four observer angles, measured from the symmetry(polar) axis as indicated in the inset, but that we stretched in time by a factor of 4. Namely, these are the four lines of the middle panel of Fig. \ref{Fig:EXP1opacities} stretched in time by a factor of 4. This figure demonstrates that we can reproduce the lightcurve shape for observers at $\theta \ga 30^\circ$, i.e., observers that are not close to the polar axis. To reproduce the correct timescale we have to take more massive nebula as we demonstrate in Fig. \ref{Fig:MassiveCases}.
	}

	\label{Fig:KaplanSoker}
\end{figure}

Our conclusion from Fig. \ref{Fig:KaplanSoker} is that when we observe bipolar supernova explosions from directions that are not too close to the polar directions, the exact angle depends on the morphologies of the bipolar CSM and of the jet-driven bipolar explosion, we might have an abrupt drop in the lightcurve.
Specific fitting of each observed lightcurve will require an extensive search of the parameter space of both the bipolar CSM, like its composition (adding hydrogen-poor gas) and other morphologies, and that of the jet-driven bipolar explosion, like other explosion energies and other jets' opening angles.

\section{Summary}
\label{sec:Summary}

We conducted hydrodynamical simulations of bipolar CCSN explosions and used a simple scheme to calculate the expected lightcurves. The explosion is applicable mainly (but not only) to stripped-envelope CCSNe according to the following scenario (section \ref{sec:Bipolar}).

A companion, main sequence, neutron star or a black hole, interacts with a red supergiant star and enters a CEE with the red supergiant. The initial interaction leads to a several-years long enhanced mass loss rate by the red supergiant to all directions. In addition, the CEE that lasts weeks to months leads to an even higher mass loss rate in the equatorial plane, and at the onset of the CEE, and/or during the CEE, and/or at the exit from the CEE, the companion launches relatively weak jets that shape the CSM to possess a bipolar structure. The companion spirals-in to close distances to the core, or even merges with the core, and therefore it spins-up the core. Shortly after that the core of the red supergiant explodes. Because of the rapid pre-collapse rotation the explosion is driven by jets that have more or less a constant axis.

We conducted four different cases of bipolar CSM hydrodynamical simulations by varying the properties of the spherical wind and/or those of the shaping jets (Table \ref{Table:cases}; section \ref{subsubsec:Wind}). We present the formation of the bipolar CSM in the case EXP1 in Fig. \ref{Fig:time_zero}. The time $t=0$ corresponds to the time when we start launching the shaping jets into the dense spherical wind (shell) to form the bipolar CSM.

We then set the explosion by launching two energetic jets for three days starting at $t=9 0~{\rm day}$ (section \ref{subsubsec:ExplosionJets}). We launch both the shaping jets and the exploding jets (in each phase two opposite jets) along the $z$-axis. We present the evolution of the ejecta-CSM interaction for case EXP1 at four times in Figs.
\ref{Fig:dens}-\ref{Fig:temp}.

From the bipolar structure we calculate the projected area of the photosphere on the plane of the sky, $A_{\rm ef,ph}$, for an observer at an angle $\theta$ to the polar direction by applying conditions (\ref{eq:tauph}) and (\ref{eq:ConditionThc}), as we explain in section \ref{subsec:setup}. We then calculate the luminosity and r-band magnitude as function of time by equation (\ref{eq:Luminosity}). We present the different lightcurves in Figs. \ref{Fig:EXP1opacities} and \ref{Fig:MassiveCases}.

Our new results confirm the results of \cite{KaplanSoker2020b} that the lightcurve of an equatorial observer of a bipolar CCSN might have a rapid, and even an abrupt, drop. \cite{KaplanSoker2020b} used a bipolar toy model. We here calculated the lightcurves from bipolar explosions that we built with 3D hydrodynamical simulations that we base on a CEE scenario. In that respect our calculation are more realistic. However, since we did not include radiative transfer we had to assume a uniform and constant opacity in equation (\ref{eq:tauph}), a minimum temperature $T_{\rm H,c}$ (equation \ref{eq:ConditionThc}) from the hydrodynamical simulations for a photosphere area element to be included in the effective projected area $A_{\rm ef,ph}$, and a photospheric temperature $T_{\rm ef,ph}$ in the calculation of the luminosity (equation \ref{eq:Luminosity}).
All the values that we assume are within a very reasonable range of possible parameters of CCSNe. Due to numerical limitations we could not follow in details the inner regions of the ejecta, and for that our lightcurves at late times is not accurate.

Like \cite{KaplanSoker2020b} we try to fit the lightcurve of the hydrogen-poor SN 2018don. The lightcurves shapes that best fit the light curves are those of case EXP1 (Fig. \ref{Fig:EXP1opacities}). However, these lightcurves evolve too rapidly. We showed that by increasing the mass in the CSM and/or reducing its velocity we can prolong the lightcurve (Fig. \ref{Fig:MassiveCases}). Because of the numerical difficulties we could not obtain lightcurves with similar shapes to that of SN2018do. For that, we simply took the lightcurve from the middle panel of Fig. \ref{Fig:EXP1opacities} and stretched the time by a factor of 4. In order to fit the lightcurve of SN2018 we will have to make an extensive search of the parameter space, including changing the properties of the exploding jets and compositions of the CSM and ejecta, something we did not do here.

Let us place our results within a broader scope. It is our view that modelling lightcurves with the neutrino-driven explosion mechanism and then adding a magnetar and ejecta-CSM interaction cannot explain a large fraction of LSNe and SLSNe (for a review of this see \citealt{Soker2022Rev}). Therefore, jets explode these CCSNe, and possibly also most regular CCSNe (section \ref{sec:intro}).
Our study strengthens the claim that jet-driven explosions can account for some properties of LSNe and SLSNe, and by that our study supports the call for a paradigm shift from neutrino-driven CCSN explosion mechanisms to the jittering jets explosion mechanism.

\section*{Acknowledgments}

This research was supported by the Amnon Pazy Research Foundation.
AM acknowledges support from the R\&D Authority in Ariel University.
Numerical simulations presented in this work were per-formed on the Hive computer cluster at the University of Haifa.

redpajama_set_name: RedPajamaArXiv


text:
Q: Print the exmpp Packet to Raw XML string How to print the Packet type to raw XML string ? In the example https://github.com/processone/exmpp/blob/master/examples/echo_client.erl the echo_packet(MySession, Packet) -> function takes the parameter Packet which is of xmlel record type. As mentioned in the post https://stackoverflow.com/a/31020654/579689 tried the function xml:element_to_binary/1 but it did not work.
When i tried to print using the following expression
io:format("Received Presence stanza:~n~p~n~n", [xml:element_to_binary({xmlel,<<"message">>,[{<<"xml:lang">>,<<"en">>},{<<"type">>,<<"chat">>},{<<"to">>,<<"x">>},{<<"id">>,<<"aaf6a">>}],[{xmlcdata,<<"\n">>},{xmlel,<<"body">>,[],[{xmlcdata,<<"wewe">>}]},{xmlcdata,<<"\n">>},{xmlel,<<"active">>,[{<<"xmlns">>,<<"http://jabber.org/protocol/chatstates">>}],[]},{xmlcdata,<<"\n">>},{xmlel,<<"time">>,[{<<"xmlns">>,<<"urn:server-time">>},{<<"stamp">>,"2015-06-23T22:48:24Z"}],[]}]})]).

received following error
=ERROR REPORT==== 12-Oct-2015::09:06:01 ===
Error in process <0.30.0> with exit value: {undef,[{xml,element_to_binary,[{xmlel,<<7 bytes>>,[{<<8 bytes>>,<<2 bytes>>},{<<4 bytes>>,<<4 bytes>>},{<<2 bytes>>,<<1 byte>>},{<<2 bytes>>,<<5 bytes>>}],[{xmlcdata,<<1 byte>>},{xmlel,<<4 bytes>>,[],[{xmlcdata,<<4 bytes>>}]},{xmlcdata,<<1 byte>>},{xmlel,<<6 bytes>>,[{<<5 bytes>>,<<37 bytes>>}],[]},{xmlcdata,<<1 byte>>},{xmlel,<<4 bytes>>,[{<<5 bytes>>,<<15 bytes>>},{<<5 bytes>>,"2015-06-23T22:48:24Z"}],[]}]}],[]},{echo_client,loop,1,[{file,"../examples/ech...

A: Error {undef,[{xml,element_to_binary,[list of N args]}]} tells you that function xml:element_to_binary/N is undefined.
Looking through xml module of the project you may try element_to_string instead of element_to_binary.
However from the point of efficiency exmpp_xml:document_to_iolist/1 will suit you better

redpajama_set_name: RedPajamaStackExchange


A young boy comes home from school in a bad mood. His father asks him, "What's wrong, son?" The kid tells his dad that he's upset because another kid has been teasing him and calling him gay. The father says, "Punch him in the face next time he does that. I bet he'll stop." The kid replies, "Yeah, but he's so cute!"
A boy came into class late one day and his teacher asked him why he was late. The boy replied "Sorry sir, I was doing push-ups on Abbey Lane." The teacher excused him and he sat down.
Five minutes later, another boy came in and the teacher asked him why he was late. He replied, "Sorry I'm late, I was doing push-ups on Abbey Lane."
Another five minutes later, a girl walks into class, late. The teacher says "I suppose you were doing push-ups on Abbey Lane too." The girl replied, "No sir, I am Abbey Lane."
A fifth grader looked downcast, so her teacher asked, "What's the problem, Carol? I hope it's not homework again."
"Well, uh, yes, it is." replied Carol. "I was stupid and made my homework paper into a paper airplane."
"Carol, you're right, that wasn't a very bright thing to do," said the teacher, "but this once I'll let you just unfold the paper and hand it in."
"Oh, but that won't work," said Carol, looking even sadder. "You see, the plane was hijacked."


text:
/**
 * Created by Jonathan on 12/14/16.
 */
export class KeyRequest {
	constructor(public profileId: number, public publicKeyX: string) {}
}

redpajama_set_name: RedPajamaGithub


text:
Porphyrosoma episphaeria är en svampart som beskrevs av Pat. 1928. Porphyrosoma episphaeria ingår i släktet Porphyrosoma, ordningen köttkärnsvampar, klassen Sordariomycetes, divisionen sporsäcksvampar och riket svampar.   Inga underarter finns listade i Catalogue of Life.

Källor

Köttkärnsvampar
episphaeria

redpajama_set_name: RedPajamaWikipedia


With a Core Board, it is possible to keep the body in motion.
The Danish designer Henrik Christensen has designed this beautiful Core Board that makes ergonomics look elegant and simplistic. Many people remain static during a work day at their desk, and even with a height-adjustable desk, you may still lack dynamic movement throughout the day.
With a Core Board, it is possible to keep the body in motion and avoid these static positions, as it rock sideways, forward, and backwards, keeping the whole body moving. This is a great combination of ergonomics and environmental awareness.
Core Boards are manufactured in solid, Danish oak.


text:
De Grande Motte is een 3653 meter hoge berg in het Franse departement Savoie. De berg behoort tot de Vanoise, deel van de Grajische Alpen.

Op 250 meter van de top begint het zomerskigebied van Tignes.

De eerste beklimming vond plaats in 1864.

Er bevindt zich een kabelbaan op deze berg.

Berg in de Franse Alpen
Geografie van Savoie
Drieduizender
Champagny-en-Vanoise


text:
Next Step, US Dept. of Defense
Ryan Gutierrez, a Forensic Science Ph.D. student was recently awarded the Department of Defense Science, Mathematics and Research for Transformation (SMART) Scholarship.
This prestigious award provides students with a unique opportunity to pursue a STEM degree and begin a rewarding career with the U.S. Department of Defense upon graduation. Benefits include full tuition, an annual stipend, book and health insurance allowance, a summer internship and a guaranteed position with the Department of Defense upon graduation. Through the program, Gutierrez will have the chance to begin a full-time career with the Defense Forensic Science Center in Forest Park, Ga.
"This type of achievement proves our students are leaving here with a competitive edge and are prepared to address current needs of the forensic science community," said Sarah Kerrigan, chair of the Department of Forensic Science and director of the Institute for Forensic Research, Training, and Innovation.
After applying for the scholarship, based on a professor's recommendation, Gutierrez visited the Georgia lab and was excited to see many familiar instruments from his research work at SHSU.
"Their lab is state-of-the-art, high-tech, a lot of what we have here actually," Gutierrez said. "It felt like putting familiar gloves on. It's a relief knowing whenever I'm done here that I have a quality experience waiting for me."
Gutierrez is another testament to the cutting-edge research SHSU forensic science students are pursuing. His research focuses on new techniques to recover genetic information from rootless hair shafts. The bulb, or root, contains the best quality DNA, Gutierrez explained. He chose to pursue this avenue of research because of the challenges presented.
"The goal of a PhD is to contribute to the body of knowledge of science and that's what he's doing," said Bobby LaRue, associate professor and Gutierrez's dissertation chair. "Ryan deserves the credit for all the work he is doing and I enjoy mentoring students like him who are driven."
A Game Changing Gift
Transforming Health
Leading the Way in School Safety
Giving Voice to New Music
Answers from Ashes, Dust and Dirt
Gift Leads to Cancer Research
Criminology, Psychology Come Together for Brain Research
Student Becomes the Master
Making Waves in Math and Climate Research
© 2022 Sam Houston State University. All rights reserved. Last Modified: Tue Apr 14 15:28:36 CDT 2020

redpajama_set_name: RedPajamaCommonCrawl


When I rented the film An Education, I expected it to kind of be like a moderner day version of Pride and Prejudice from the 1960s. Although it ended up being nothing like my favorite classic, it definitely touched on several important issues throughout the movie. It served as a reminder that you are your most important thing. People will come and go but you always have to live with yourself, so it's important, especially as women, to be self-supporting and create our own successes.
The movie is about Jenny, a mature and intelligent 16-year-old schoolgirl, who falls in love with an older man, David. As they continue to see each other, Jenny becomes enthralled with his world full of art, music, gambling, traveling and culture. As a young woman who was focused and adamant on going to Oxford to study English, she begins to doubt the point of her education as she thinks of a prospective life with David full of fun and leisure.
Unfortunately, all that glitters ain't gold, and Jenny shortly discovers after dropping out of school upon accepting David's marriage proposal that David is in fact already legally married to another woman. Jenny's attraction to the (seemingly) glamorous life and belief that she could take the easy way out by marrying David instead of constantly challenging herself at Oxford quickly comes back to slap her on the behind. After persuading her schoolmaster to allow her to come back to school, Jenny bulldozes through another year with regained unyielding focus and ends up being accepted into Oxford after all.
""I feel old, but not wise."" While I understand why she feels like a fool for not being able to see through David's facade, I do believe that the experience ended up molding her in a positive way.
come back with a new sense of determination, purpose and self-worth. She undoubtedly learned from her experience running with an adult crowd living on lies. It also goes to show that, even though one may be intellectually equal or superior to another who is older age wise, it's one's experiences and life lessons that are just as important in getting on in the world as unscathed as possible.
I actually really enjoyed this movie. It wasn't corny or unimaginable; it is realistic even by today's standards. Originally I pitied Jenny for losing her virginity to a man who was a liar and cheater, but then I realized that Jenny's biggest mistake was throwing away her previous desire to go to Oxford when she thought she could live an easy life off David. Luckily, Jenny's pride didn't get in the way of her seeking the help of her former English teacher to assist in persuading the schoolmaster to grant her permission to come back and finish high school. It was refreshing to see her own up to her mistake and bounce back from it. I also found it admirable that Jenny surprisingly handled everything with grace. Instead of giving up or sinking into depression, she truly acted as an adult and took responsibility for her actions.
Besides going on some fun trips this past winter, I also got a good taste of the arts in NYC. I went to a really cool contemporary art fair, a concert at Madison Square Garden, and I saw three really great Broadway shows:Elephant Man, You Can't Take it With You, and Constellations.
The art fair I went to was called PULSE. Kevin and I were invited by C24 Gallery in New York because we worked with them to get our Nick Gentry pieces. I didn't really know what the PULSE fair was all about, but Kevin and I were free one of the eveningsof the fair, so we figured we'd check it out. As their fair guide pamphlets states, the [Pulse] fair cultivates a supportive environment for its international community of galleries and provides a platform for their growth and expansion in the contemporary art market. From its inception [ten years ago], PULSE has presented thoughtfully-curated exhibitions and ever-evolving programming that reflect the fair's commitment to making the visitor experience a dynamic one.
I think the description of the PULSE art fair is spot on. I saw a lot of different works of art, all cool in their own way. Some of my favorite pieces included a collage made using stickers like the ones I used to collect for my sticker book when I was a kid by Beijing artist Ye Hongxing,an x-ray-looking photo of an airplane and a motorcycle, a weird but cool painting of emojis, eerie but beautiful pictures of destroyed and abandoned buildings in Italy that were once great (which reminded me a lot of the pictures from Andrew Moore's Detroit Disassembled exhibit that I went to at the Queens Museum a few years ago), and of course some of Nick Gentry's newer work using film strips.
My absolute favorite piece at the fair was by a Turkish artist I was unfamiliar with, Irfan Onurmen, who makes his art out of tulle. It was unlike anything I've seen before. It's just amazing at what he can create using the same material as a ballerina's tutu. I love that good art can make you feel alive, and I felt a good electric vibe in the air while walking around checking out vastly different pieces. Art is good if it makes you feel something, and I left the fair feeling inspired.
In addition to seeing some art, I also saw a few good shows on Broadway this winter. I saw ElephantMan starring Bradley Cooper who plays a disfigured man and he was amazing in it. I recently saw another more serious show, Constellations, starring Jake Gyllenhaal and Ruth Wilson about the possibility of so many different outcomes in ones life. New York Times writer, Ben Brantley says it best in his review Constellations is about, among other things, how inevitably fraught and imperfect communication is, even with people closest to you.
Jake was great in Constellations, but Ruth really took the stage. She was amazing. She is also in the new hit show on Showtime, The Affair. Another equally as good but much more light-hearted show I saw on Broadway was You Can't Take It With You. It was a comedic play about an unconventional family. I originally wanted to see it because it got pretty good reviews and because Rose Byrne was in it, but by the time I was finally able to see it, she wasn't in it anymore. Luckily the storyline is so good and all of the characters are so quirky and entertaining that I don't think it was necessary to have any really famous actors in it.
Lastly, I saw my first concert at Madison Square Garden. Kev and I saw Maroon 5. Even though our seats were pretty bad, we still had a great time, and Maroon 5 was super good live. It makes me want to see more live music.
Last month I went on the most amazing trip of my life. I have traveled quite a bit, but my trip to Australia was unlike any other I've ever been on. It was also the furthest I've ever traveled.
Kev and I flew from NYC to LA on Thursday evening, then from LA to Brisbane and finallyfrom Brisbane to Cairns. After a very long day of traveling and a big time change, we finally landed in Australia on Saturday morning. It was a 23 hour flight. Luckily I had a few sleeping pills, so the flight was surprisingly pretty easy. What wasn't as easy was adjusting to the time difference.
On Sunday we relaxed and walked around the Cairns esplanade, and then on Monday we went on a rainforest tour with Wait-a-While Rainforest Sightseeing Tours where we got to see a lot of cool trees and animals.
The rainforest tour was an awesome land trip before the sea portion of our trip. The morning after our rainforest excursion, we boarded the Spirit of Freedom live aboard boat to go scuba diving on the Great Barrier Reef. We did eleven dives in only two and a half days…I'm not kidding. It was physically exhausting but such an amazing experience. Kev and I even got advanced open water diving certified.
The last leg of our Australia trip was spent in Sydney. We stayed at the beautiful Westin and spent one full day shopping and walking all over the city, seeing iconic spots like theSydney Opera House and the Sydney Harbour Bridge, and grabbing dinner with one of Kev's former co-workers. On our last day we met up with another friend to go on a beautiful scenic 10k walkto Manly Beach followed by an equally as amazing evening seeing Dirty Dancing the Musical.


text:
Paradactylodon es un género de anfibios caudados de la familia Hynobiidae. Se distribuyen por el norte de Irán y de Afganistán.

Especies
Según ASW:
 Paradactylodon gorganensis (Clergue-Gazeau & Thorn, 1979)
 Paradactylodon mustersi (Smith, 1940)
 Paradactylodon persicus (Eiselt & Steiner, 1970)

Referencias

 Risch, 1984 : Brève diagnose de Paradactylodon, genre nouveau d'urodèle de l'Iran (Amphibia, Caudata, Hynobiidae). Alytes, Paris, vol. 3, p. 44-46.

Enlaces externos

Hynobiidae
Anfibios de Asia


text:
dogtired
Posts posted by dogtired
Robert Plant and Glastonbury 2010.
Posted October 30, 2009 · Edited October 30, 2009 by dogtired
On the subject of Amy Winehouse, I just have to ask why you people think it's so terrible that she's an "Alcoholic druggie," but that same thing is perfectly fine for other musicians. You do realize that most musicians - including our own dear Zeppelin - are or were alcoholics and drug addicts, don't you?
Interesting compassion for someone exhibiting such socially unnacceptable behavior. And the analogy is so true.
Surprisingly refreshing.
Consistency is the key however.
Have You Ever.........?
in Ramble On
HYE had an ostrich burger?
No but Furr burgers are at the top of the menu!
Have you ever eaten a foot long weenie?
Where did Halloween come from?
A cauldron of elixir to cast evil spells or maybe it's a love potion #9, #9, #9, #9, #9?
HE HE HE HE!
HE HE HE indeed!
What do you call Led Zeppelin's 4th album?
in Led Zeppelin Master Forum
I call it "The first album I waited in line outside the record store for several hours on the first day of release to buy!"
Or "The one before Houses of the Holy".
What on earth is that witch stirring?
Wolfgang's concert vault
in Led Zep Live
Although these concerts are available on bootleg, I'm hoping that the Zeppelin camp will move towards an official release with maximum sound quality, new photos, liner notes, etc.. And if there is also video of any of these concerts in this fault that would be obviously an incredible release.
Hopefully we'll hear something
Nice to be wishful, but it ain't gonna happen.
What's the Last Concert You Attended?
in Other Bands / Music
The Ron Artis Family Band,
in Haleiwa Hawaii, my favorite surf town. They're SO FUNKY!!
http://www.ronartis.com/
http://www.youtube.com/profile?user=ronartis#g/u
What are your opinions on Walking into Clarksdale?
in Pre / Post-Zeppelin Forum
Look at what Albini did to Nirvana. Nevermind sounded incredible thanks to Butch Vig. Cobain then decides to bring in Albini for the next record and it sounded like complete shit! What a huge mistake that was.
I have a feeling it was Plants idea to bring in Albini, but Page should never have let that happen.
Personally, I can't listen to WITC, primarily because of the vocals, they're just awful sounding to me.
And yes, the songs sound 'much' better live.
Major dissapointment.
If you're talking about "In Utero", I think that sounds fine. Better than the mastering on Physical Graffiti, IMO.
And as far as tunes from WIC sounding better live, maybe, but they played second fiddle to the Zeppelin numbers in concert in 1998. The sets could've done without them and I wouldn't have missed a thing.
Stealth mode can't hide you, dear.
Oh my, and I hardly know you!
Dear me.
If Keith Moon hadn't uttered Led Zeppelin
Wacko Jacko...or The League of Extraordinary Gentlemen...
Robert Fripp is such an ordinary gentleman. Humble too.
We might have never had John Bonham if not for Moonie's errant suggestion. That had to have disappointed Jimmy with his lead balloon remark. " I'll show you Keith!! I'll get the better drummer in Bonzo and show you what heights we can achieve! Ha! And for you Entwistle, I'll also find a better bassist and you can stay with that twit Pete! " Roger that!
Doesn't it have something to do with The Addams Family or The Munsters?
But I'll put my money on Milton.
I stay in stealth mode most of the time too; what's the big deal? It's an available feature so why not use it? I use it on Facebook too.
Come to think of it, maybe you girls are right. Stealth mode and hiding might be a great idea for message boards.
Understanding all the stalking and such going on, I suppose that's a prudent option.
I'm gonna hide now and try it.
If you can't beat 'em, join 'em.
So to speak.
Adam Lambert - Time for Miracles
WHOOOoopsie.
Dayum!!!!!
He's a good lookin' woman!
Untill People in the Business actually Come Out and Condem these Alcholic Drug-Abuser Cretins then we are all going to have to watch their Antics on TV and in the Papers.
You must long for the 80s BIGDAN. It's been done! Remember the old MTV commercials?
Some more comedy,
http://video.google.com/videosearch?hl=en&source=hp&q=r+a+d+rockers+against+drugs&um=1&ie=UTF-8&ei=ElDoSqGhDY3SM_rLpaEI&sa=X&oi=video_result_group&ct=title&resnum=4&ved=0CBsQqwQwAw#
Sure it's hypocritical to downgrade Amy for her activities when other band's personel have been involved in far more heinous antics.
The difference here is (crazed bands on the road) - The Doors, The Who, The Rolling Stones, Led Zeppelin, ALL these bands and musicians are GREAT MUSIC and Amy Winehouse's music SUCKS!!
There's no hypocrisy there. I can't stand her music and that makes her antics all the more revolting! BLEEEEEEEECCCCKKKKKKKKK!!!!!!!!!!!!!!!!!!!
Great thread. I hope to see more people getting their disgust out!
No, it's not weird In the past when that function was on I DID have a few pests who did just that.
Oh yeah.....I've got SO much to hide.
Regardless I answered your question as to why I do.
If it bothers you tough.
Having people watch other's moves IS weird. And on a posting forum to feel some kind of threat or whatever to have the need to "hide" IS weird too.
Does it bother me? No, but it IS a curiosity. And yes, you did answer me but the fascination still is there. It's just a message board for chrissakes!
I guess sunglasses are needed by some, even at night.
Sniper...
Ok well the reason I "hide" is because the new board here has the function that "tells where you are" all the time. I just don't like people knowing where I am ALL the time.
Plus I like to look and snoop at profiles anono.
K?
Yeah, being able to "fire away" without being "seen". As in your profile viewing anonymity. Do you really believe people watch your forum moves? That's weird for sure.
I've just noticed posts by several members here and hardly, if ever, see them "online". I suppose if you have something to hide it's a good decoy of sorts. I promise I won't be watching your moves or any others for that matter. Who'd care?
Then again, it is post 911.
More of a curiosity than a "Pet Peeve", but,
Why do people choose to be "hidden", yet post while hiding?
I guess it's about being a drive-by sniper, than just a reconnaissance scout.
I'm still curious.
To end Zeppelin
Based on 30 years of words and actions from JP and Robert, it certainly isn't a stretch to assume that Robert was the driving force behind the breakup...regardless of the Press release.
Since you include "assume", others may or may not feel that way, but it qualifies YOUR opinion on the matter and that makes it valid. You didn't say Robert WAS the driving force, but assumed.
That's reasonable.
And from another thread about Robert's assumed distancing,
I don't want to rain on anybody's parade but I don't think the o2 performance is going to be officially released anytime soon. Obviously Jimmy, Robert, and JPJ would have to agree to release it and IMHO I just don't see Robert being onboard with it. Look at it this way...would Robert want to release, and immortalize, what is likely to be the last Zeppelin performance and while a great concert to many showcases his reduced vocal range and capacity? He's obviously going to want to release his best work recorded when Zep was at the peak of their playing ability and his vocal range was intact. That's pretty much what they did with their last DVD...compiled the best they had and put it out. Robert believes, and one would have to agree, that he sang Zeppelin best when he was a young man and that's where he wants to leave it and as much as I would like to see an O2 DVD, and new material, and a tour I understand his point.
Why are you assuming it's Robert who is the one vetoing an official release of the concert? We have no idea what's behind their decision not to release it and it's pointless to speculate or point fingers with no concrete facts behind it.
Look at davidscott's post again. He explains his feelings on the matter very clearly, even as disputed as it may be. He's also made an assumption and in other threads posters are speculating on reasons for Led Zeppelin's breakup and their reluctance to reform for ongoing tours etc. There's nothing wrong with wondering and posting opinions and as I see it, many are explained and qualified from one's own opinion!
What Made You Un-Happy Today ?
Thanks, dogtired! I don't have his email address. I looked it up here, but it is "private". You wouldn't have it would you?
No, I'm sorry I don't. Try dzldoc, I read where he's in close contact with him.
Hi ImPLANTed! I'm glad. I just hope (as Buck'EYE'doc' said), that nothing bad has happened to him. I PM'd him twice, no response. (This is not like him)
Would you consider ZeppFanForever a man of honor? If so, maybe he's sticking to his guns and not returning to the forum and as such would not be able to answer his PM's.
Try email.
I don't remember precisely when he sold those rights, but it was circa '81-'83. He may have been cashing out in anticipation of his Spring 1983 divorce but I'm not going to get into that here.
While it's true a full-fledged Led Zeppelin reunion at any time would stimulate back catalog sales, the big money to be made would come from touring.
That would be right Steve, I see now. Unlike the old days where touring basically encouraged record sales as the main income producer for bands. No doubt it was Peter Grant's negotiating with promoters to get, what?, 90% of the gate for "Led Zeppelin".
I think you meant death knell. Anyway, I wouldn't say he "needed" the money, I'd say he wanted it to launch his solo career at the height of New Wave music era.
HaHa! It's a hybrid!
The worst of both worlds.
http://www.urbandictionary.com/define.php?term=Death+Nail
And it looks like you somewhat qualify my choice of "needing" in that you say he "wanted it to launch his solo career...". So the extra funding might have been the reasoning. Hmmm.
Still, no matter, no wonder he didn't seem to care for re-unions on a mass scale. No income from catalog sales!
I have no idea what happened but the concerts they had by Led Zeppelin are very common bootlegs and easily obtainable.
No great loss on Wolfgang's archives considering they were lossy files anyway.
Robert Plant sold his rights to sales of the Led Zeppelin back catalog at the onset of his solo career circa 1981.
Was that because he needed the money or was leaving Led Zeppelin in the past? Seems like a death nail to me. Or was it because he thought Zeppelin had no ongoing legacy? Strange indeed.
I see it as an event that signaled "The Party's Over", for Robert anyway.


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Attorney Group for Alabama / Lawsuits / Alabama Dangerous Drug Attorney / Alabama Abilify Lawsuit
Alabama Abilify Lawsuit
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Abilify, also known as aripiprazole, is an antipsychotic medication. Lawsuits allege that the drug causes compulsive gambling, resulting in severe financial consequences. Affected patients and their families may be eligible to pursue compensation with the help of an Alabama Abilify lawsuit attorney.
For more information, contact Attorney Group for Alabama today. Our consultations are free, confidential and without any obligation on your part. We can help answer your questions, and if you choose to pursue a claim we can connect you with an affiliated attorney who can assist you throughout the legal process.
The time you have to pursue a claim is limited. Contact us for more information.Get Help Now.
What is Abilify?
Abilify is a prescription antipsychotic medication used to treat symptoms of psychotic disorders such as schizophrenia and bipolar disorder. In some cases, Abilify may be used as an add-on medication to treat major depressive disorder in adults. Abilify may also be used to treat symptoms of autistic disorder, including aggression, mood swings, temper tantrums, and self-injury.
How Does Abilify Work?
Abilify belongs to a class of drugs known as atypical antipsychotics. Most atypical antipsychotics work by blocking dopamine and serotonin receptors, however, Abilify works somewhat differently. Instead of blocking chemical receptors, Abilify works by stimulating or inhibiting dopamine receptors to help keep them balanced.
Abilify Side Effects
Common side effects of Abilify include:
Difficulty speaking
Uncontrollable movements of the body
In rare cases, the following side effects may develop in patients who use Abilify as prescribed to treat their condition:
Increased sweating
Severe muscle stiffness
Abilify and Compulsive Gambling
In 2012, the European Medicines Agency (EMA) requested that the product information for prescription Abilify be updated to include warnings about compulsive gambling. According to the EMA, post-marketing reports of pathological gambling have been reported among patients who were prescribed Abilify, regardless of any prior history of compulsive gambling and those patients.
In addition to the request made by the EMA, Canadian regulators issued an update for product labels of Abilify advising patients of an increased risk of compulsive behaviors, including pathological gambling and hypersexuality. Based on reports of pathological gambling in Canada and an additional eighteen international reports, a Canadian Safety Review published in November 2015 concluded that there was a connection between Abilify and certain pathological behaviors, including compulsive gambling.
Although warnings have been issued in Europe and Canada, product labeling in the United States does not mention that pathological gambling has been reported in patients who were prescribed Abilify. Abilify compulsive gambling lawsuits filed in California and Minnesota allege that the drug makers had a duty to provide adequate warnings and instructions regarding the potential risks associated with compulsive disorders.
Other Abilify Risks
According to the U.S. Food and Drug Administration (FDA), antipsychotic drugs such as Abilify have been associated with several severe, sometimes life-threatening conditions. Prescription information issued by the FDA notes the following warnings and precautions:
Elderly patients who suffer from dementia-related psychosis are at an increased risk of death when treated with antipsychotic drugs such as Abilify
In clinical studies of dementia-related psychosis, there was an increased risk of cerebrovascular adverse events, including stroke and brief, stroke-like events
Children and adults with major depressive disorder may experience worsening of their depression and should be monitored for unusual changes in behavior
A potentially fatal neurological disorder known as Neuroleptic Malignant Syndrome (NMS) may occur with the administration of antipsychotic drugs, including Abilify
Patients treated with antipsychotic medications may develop tardive dyskinesia, a potentially irreversible condition that affects the nervous system
Atypical antipsychotic drugs—including Abilify—have been associated with metabolic changes that include hyperglycemia, dyslipidemia, and body weight gain.
Other risks possibly associated with the use of Abilify include orthostatic hypotension (low blood pressure); leukopenia, neutropenia, and agranulocytosis (lowered white blood count); seizures; motor impairment; elevation in core body temperature; suicide; and dysphagia (difficulty swallowing).
How An Alabama Abilify Lawsuit Can Help
Drug manufacturers have a duty to ensure their products are accompanied by full and accurate instructions and warnings to guide prescribing doctors and other health care providers in making treatment decisions. If a drug maker fails to fulfill this duty, it could be held liable in lawsuits for injuries and damages that may result.
When patients suffer from severe side effects from a dangerous or defective drug, they may be entitled to compensation for their injuries and damages. The types of losses that can be recovered include:
Economic Losses
Medical and other treatment expenses
Pain, suffering, and mental anguish
Loss of income or ability to work
If the conduct of a drug company in manufacturing and selling drug is found to be highly reckless, punitive damages may be awarded to punish the company and deter similar conduct in the future.
Patients who have suffered loss as a result of compulsive gambling or other compulsive behaviors are encouraged to speak with an Alabama Abilify lawsuit attorney to learn more about their rights and remedies.
For more information, contact Attorney Group for Alabama.
When you contact us, an attorney will follow up with you to speak with you about your case or answer questions that you might have. There is no cost or obligation to speak with us, and any information you provide will be kept confidential.
Please note that the law limits the time you have to pursue a claim or file a lawsuit for an injury. If you think you have a case, you should not delay taking action.
Attorney Group for Alabama
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