text:
\section{Introduction}

\paragraph{}
    The prospect of travelling to other far away astronomical systems has
been a tantalizing thought for many millenia, however its bleak reality has only been realized in the past couple centuries. The vastness of space
is the greatest barrier to interstellar travel. The closest planetary system to Earth is Alpha Centauri at a distance of 4.3 light-years \cite{wilkinson_new_2012}. Using the fastest man-made object, the Parker Space Probe, it would take approximately 6.5 centuries to reach Alpha Centauri \cite{apl_mission_nodate}. This is many times longer than the average human life span. Fortunately, there may exist other methods to manned intersystem travel using more fundamental theoretical processes.

\paragraph{}
    It's well-known that an empty, flat, and non-dynamical spacetime does not permit massive particles from exceeding the speed of light. However, there have been cases in more complex systems of particles exceeding the local speed of light, such as highly energetic massive radiation in a medium giving rise to Cherenkov radiation. In some instances, even spacetime itself can travel faster than the vacuum speed of light. This is the case during the inflationary or dark energy phases of the universe. Such distortions of spacetime manifest as objects travelling faster than light relative to distant observers . This effect can be observed today by measuring the recession speed of distant galaxies and noting they are receeding faster than light away from the earth.

\paragraph{}
    The dynamical nature of spacetime giving rise to superluminal relative speeds may be able to be exploited for interstellar travel. The field equations of general relativity (GR) permit inertial observers to be transported at superluminal rates relative to distance observers. The first solution possessing such features was the Alcubierre spacetime \cite{alcubierre_warp_1994}. This solution describes a region of spacetime in which an observer inside a ``bubble'' could be transported superluminally relative to observers outside the region. This is due to the contraction of spacetime in front of the central observer and a corresponding expansion behind. In theory, this solution permits interstellar travel of a payload on arbitrarily short timescales.

\paragraph{}
    Unfortunately, this solution possesses numerous pathologies that would prevent its construction using realistic matter fields. The most prevalent is the enormous amount of negative energy it requires, several orders
of magnitude more than all the energy content in the observable universe.
Even if one appealed to quantum processes to generate the negative energies, the shear quantity requirement yields this configuration highly unphysical. To generate the energy densities required by the Alcubierre configuration using the Casimir force, the length scales would have to be millions of times smaller than the diameter of a proton. Additionally, the spacetime hosts horizons that would render the soliton uncontrollable \cite{hiscock_quantum_1997}. Other pathologies include subluminal weak energy violations and Planck-scale dimensions \cite{lobo_fundamental_2004, pfenning_unphysical_1997}.

\paragraph{}
    A number of other configurations have been constructed, each with varying goals and properties. The Natario spacetime is another example of a superluminal spacetime \cite{natario_warp_2002}. This solution, by construction, has trivial expansion. The advantage of this configuration is that it preserves volumes, as opposed to the Alcubierre spacetime which dramatically alters them. However, this configuration still comes with many of the same problems that the Alcubierre spacetime hosts. The Broeck configuration aims to reduce the massive amount of negative energy by altering
the geometry of the warping region. They reduce the surface area of the region while maintaining the internal volume. This drastically reduces the
total energy requirements from universal-scale to solar mass-scale. Nonetheless, negative energies are still required in order to generate all previously mentioned spacetimes. In recent years, theoretical research has hinted at possible superluminal configurations generated by purely positive energy densities \cite{lentz_breaking_2020}. This is accomplished by analyzing constraint equations enforced by GR and finding relationships that permit superluminal motion generated by positive energies. This study, and the one presented here, are in contrast to the claimed proof that superluminal motion requires negative energy densities \cite{olum_superluminal_1998}.

\paragraph{}
    Modified theories of gravity provide alternate descriptions of the gravitational force \cite{Heisenberg:2018vsk} that could yield more physically realistic superluminal
solitons. One relevant example is the Debenedictis et al. configuration developed in the Einstein-Cartan theory \cite{debenedictis_energy_2018, cartan_comptes_1922, cartan_manifolds_1986}. In this theory of gravity, the torsion tensor no longer vanishes, resulting in new couplings between the spacetime geometry and matter fields (a similar setup can be constructed in terms of non-metricity \cite{BeltranJimenez:2017tkd, trinitygravity, BeltranJimenez:2018vdo}). An interesting feature of the Einstein-Cartan theory is that deviations from GR only manifest in the presence of matter. The spin of the matter field than appears in the field equations. Debenedictis et al. exploited this coupling to generate the Alcubierre configuration using positive energy densities only. This, however, solves only one pathology of the Alcubierre configuration. It
doesn't solve the horizon problems, causality problems, etc. Nonetheless,
it illustrates the possible advantages of utilizing alternate theories of
gravity to construct more physically realistic superluminal solitonic spacetimes.

\paragraph{}
    With the presence of negative energy densities being one of the main pitfalls of the classical solitonic configurations, the aim of this work is to analyze the weak energy condition at the classical level in the context of superluminal spacetimes. The main question of this work is could a compact superluminal soliton described by the classical equations of general relativity be generated only using positive energy densities? Moreover, the geometric nature of the weak energy condition within a certain subclass of spacetime configurations is investigated, providing insight into how and why the classical configurations necessitate negative energies. A few spacetimes hosting superluminal motion generated by positive energies will also be presented, along with some of the subtleties of the weak energy condition applied to the superluminally transported observer.

\paragraph{}
    This paper is then divided into three main sections. Section 2 will introduce the relevant theoretical tools and their relevance to the superluminal solitonic spacetimes. Section 3 will present the results of this study and its significance. Finally, section 4 will conclude with a summary and discussion on potential future work.

\section{Theory}

\subsection{Background}
\paragraph{}
    Henceforth, the conventions of \cite{gourgoulhon_31_2012} will be adopted, namely Latin indices are assumed to run from 1 to 3, Greek indices run from 0 to 3, and the metric signature is assumed to be $(-,+,+,+)$. The starting point is the decomposition of the Einstein equations in the (3+1)-decomposition. Spacetime is assumed to be globally hyperbolic. This implies the topology is $\Omega \times \mathbb{R}$, where $\Omega$ is a Cauchy surface, since the flow of timelike vector fields intersecting the Cauchy surface provides a homeomorphism between the spacetime $\mathscr{M}$ and $\Omega \times \mathbb{R}$. This allows the spacetime to be foliated by a family of spacelike hypersurfaces, whose extrinsic geometry is described by a normal vector. Since the normal vector is a timelike vector,
it can be thought of as the 4-velocity of an observer. This observer is called an \emph{Eulerian observer}.

\paragraph{}
    The internal geometry of the hypersurfaces is described by the 3-metric $\gamma_{ij}$, which is induced by the pull-back between the spacetime
$\mathscr{M}$ and hypersurface $\Omega$. This metric has an associated Levi-Civita connection and, hence, a corresponding Riemann curvature tensor. This curvature tensor describes the intrinsic curvature of the hypersurface. Moreover, the evolution of the 3-metric along the normal direction gives the extrinsic curvature of the hypersurface as an embedded manifold,
    \begin{equation} \label{def:extrinsiccurvature}
        K_{i j} = - \frac{1}{2} \mathcal{L}_n \gamma_{ij}.
    \end{equation}
    Formally, the extrinsic curvature is defined as the inner product between a tangent vector to the hypersurface and the shape operator. This definition is equivalent to Eq. \eqref{def:extrinsiccurvature}. The Gauss-Codazzi relations are important relations between the Einstein tensor and the intrinsic and extrinsic geometry of the hypersurfaces. They represent
various projections of the curvature tensor of the full spacetime onto the hypersurface and its normal. Their contracted forms can be compactly written using the Einstein tensor as
    \begin{align} \label{eq:gausscodazzi}
        G_{\mu \nu}n^{\mu}n^{\nu} &= \frac{1}{2} \left( \tensor[^\Omega]{\mathscr{R}}{} + \mathscr{K}^2 - K_{ij}K^{ij} \right)\\
        \nonumber
        G_{\mu \nu}n^{\mu}\tensor{\gamma}{^{\nu}_{\alpha}} &= D_{\alpha}\mathscr{K} - D_{\mu}\tensor{K}{^{\mu}_{\alpha}},
    \end{align}
    where $G_{\mu \nu} \coloneqq \tensor[^4]{R}{_{\mu \nu}} - \frac{1}{2}
\tensor[^4]{\mathscr{R}}{} g_{\mu \nu}$ is the Einstein tensor, $n^{\mu}$
is the hypersurface normal vector, $\tensor[^\Omega]{\mathscr{R}}{}$ is the Ricci scalar calculated from the 3-metric, $\mathscr{K}$ is the trace of the extrinsic curvature, and $D_{\alpha}$ is the Levi-Civita connection associated to the 3-metric. Importantly, these relations represent the bilateral projection, resp. mixed projection, of the Einstein tensor onto
the hypersurface normal, resp. hypersurface normal and the hypersurface itself. Adopting the definitions of \cite{wald_general_1984}, the extrinsic curvature trace represents the expansion of a congruence of geodesics passing through the hypersurface,
    \[
        \theta \coloneqq K^{ij}\gamma_{ij} = \mathscr{K}.
    \]

     Using co-ordinates adapted to the foliation, the normal vector can be decomposed into a scalar and vector component as $n^{\mu} = (\frac{1}{N}, - \frac{\vec{N}}{N})$. The scalar component $N(t,x,y,z)$, called the
\emph{lapse function}, describes in a sense the spacing of the leaves of the foliation, while the vector component $\vec{N}(t,x,y,z)$, called the \emph{shift vector}, describes the tangential shift of the co-ordinate system between neighboring leaves. The full spacetime metric can then be decomposed in terms of the lapse function, shift vector, and 3-metric as
    \[
        g_{\mu \nu} =
        \begin{bmatrix}
            -N^2 + \vec{N} \cdot \vec{N} & N_j \\
            N_i & \gamma_{ij}.
        \end{bmatrix}
    \]
    Importantly, a shift vector field satisfying $\vec{N} \cdot \vec{N} >
N^2$ is called \emph{superluminal} due to the fact $g(\partial_t, \partial_t) >0$.
\paragraph{}
    In the presence of matter fields, the stress-energy tensor also admits a decomposition in terms of the foliation variables. The complete bilateral projection of the stress-energy tensor onto the hypersurface normal represents the energy density of the matter field, while the complete bilateral projection onto the hypersurface is the mechanical stress. The mixed projection, once onto the hypersurface and once onto the normal, represents the momentum density (or energy flux) of the field.
    \begin{align} \label{def:stressenergyprojection}
        \text{ Energy Density: }& \rho = \mathscr{T}_{\mu \nu}n^{\mu}n^{\nu}\\\nonumber
        \text{ Momentum Density: }& p_{\sigma} = \mathscr{T}_{\mu \nu}n^{\mu}\tensor{\gamma}{^{\nu}_{\sigma}}\\\nonumber
        \text{ Stress Tensor: }& S_{\mu \nu} = \mathscr{T}_{\alpha \beta}\tensor{\gamma}{^{\alpha}_{\mu}}\tensor{\gamma}{^{\beta}_{\nu}}
    \end{align}
    Using the foliation-adapted co-ordinates and the contracted Gauss-Codazzi relations, the Einstein equations decompose under the foliation as
    \begin{align} \label{eq:decomposedeinsteinequation}
        &\left(\partial_t - \mathcal{L}_{\vec{N}}\right) \gamma_{ij} = -2 N K_{ij}\\\nonumber
        &\left(\partial_t - \mathcal{L}_{\vec{N}} \right)K_{ij} = -D_i D_j N + N \Big( \tensor[^{\Omega}]{R}{_{ij}} + \mathscr{K} K_{ij} - 2 K_{ik} \tensor{K}{^k_j} + 4 \pi \big( (\mathcal{S} - \rho) \gamma_{ij} - 2 S_{ij}\big) \Big)\\\nonumber
        &\tensor[^{\Omega}]{\mathscr{R}}{} + \mathscr{K}^2 - K_{ij}K^{ij}
= 16 \pi \rho\\\nonumber
        &D_j \tensor{K}{^{j}_{i}} - D_i \mathscr{K} = 8 \pi p_i,
    \end{align}
    where $S_{ij}$ is the mechanical stress tensor and $\mathcal{S}$ its trace. The third and fourth equations are called the \emph{Hamiltonian constraint} and \emph{momentum constraint}, respectively.

\subsection{Weak Energy Condition}
\paragraph{}
    Investigating the physicality of superluminal spacetime solitons begins with studying the energy conditions enforced on the spacetime. The weakest energy condition one can enforce, aptly named the weak energy condition (WEC), states that
    \[
       \text{WEC:  }  \;\; \mathscr{T}_{\mu \nu} t^{\mu} t^{\nu} \geq 0, \;\;\; \; \;\forall \text{  timelike  } t^{\mu}.
    \]
    Intuitively, this is the statement that the local energy density measured by any observer must be non-negative.
    This implies the Eulerian energy density, calculated from the Hamiltonian constraint, must be positive semi-definite.

\paragraph{}
    The WEC is violated in the Alcubierre configuration. The chosen ansatz is $N=1$, $\gamma_{ij} = \delta_{ij}$, and $\vec{N} = (-v_s f(r_s),0,0)$ with $r_s^2 = x^2 + y^2 + z^2$. The Eulerian energy density is then easily calculated, using Eq. \eqref{def:extrinsiccurvature} and the Hamiltonian constraint, to be
    \[
        \rho = - \frac{1}{8 \pi} \frac{v_s^2 \rho^2}{4 r_s^2} \left(\frac{df}{dr_s} \right)^2,
    \]
    where $v_s$ is the velocity of the warp bubble and $\rho^2 = y^2 + z^2$ the radial cylindrical co-ordinate.
    Indeed, the fact that the weakest energy condition is violated by such a simple example of a superluminal soliton does not bode well for superluminal travel. Note that even at subluminal speeds, when $0<v_s<1$, the energy density is still negative. Similar results hold for the other classical superluminal spacetimes, and indeed it's been shown that a couple of the classical configurations are equivalent, related only by a co-ordinate transformation \cite{bobrick_introducing_2021}. Moreover, it's no surprise the expansion-less Natario configuration violates the WEC. From the
Hamiltonian constraint, if the expansion is zero, the energy density reads $\rho = - K_{ij}K^{ij}$, where intrinsic flatness was assumed. It follows that any configuration attempting to satisfy the WEC must contain a sufficiently large magnitude of expansion, at every spacetime point where
the extrinsic curvature is non-vanishing, so that the Eulerian energy density is non-negative.

\section{Results}
\paragraph{}
Presented in this section is a class of solitonic spacetimes generated by
positive energy densities, alongside a new geometric interpretation of the Eulerian energy distribution. The considered class of spacetimes permit
superluminal transportation of an inertial observer. Several comparisons of the presented configurations can be drawn to previous constructions in
the literature. The most widely used ansatz will also be employed here, namely the shift vector field will be used to fully describe the spacetime. Moreover, potential fields will be introduced to further analyze the constraining equations, similar to the analysis in \cite{lentz_breaking_2020}, albeit without enforcing extra constraints on the metric variables. The presented work appears to be in good agreement with the study performed in \cite{bobrick_introducing_2021}, namely the non-truncation of
the gravitational field leads to positive semi-definite energies, axisymmetric configurations can lead to interesting solitonic configurations, and modifying the geometry of the soliton can lead to a reduction of the energy requirements.

\paragraph{}
There are several advantages to the presented configurations compared to those previously presented in the literature. The foremost advantage is the absence of negative energies, in contrast to the Alcubierre, Natario, and Van Den Broeck configurations among others. The presented solitonic configurations are also tuneable, which is a first of its kind. This means
the central observer can have a variable speed, relative to distant observers. The speed is based upon the geometry of the energy distribution and
not the total energy content, making it highly desirable for interstellar
transportation. The configurations are also highly modifiable due to the geometric interpretation offered by the Hamiltonian constraint. This will
greatly aid any work seeking to minimize the energy requirements.

\subsection{Generalities}
\paragraph{}
    In order to explore the feasibility of constructing a positive-energy
spacetime soliton, the Eulerian energy is investigated in a suitably general ansatz. The shift vector field is taken to be time-independent with no other constraints placed on it. Moreover, the lapse function is taken to be unity, and the induced metric is the identity. The Hamiltonian constraint then reduces to
    \begin{align} \label{eq:WECinansatz}
        16 \pi \rho =& 2 \bigg( \partial_x N_x \partial_y N_y + \partial_x N_x \partial_z N_z + \partial_y N_y \partial_z N_z \bigg)\\
        \nonumber
        &- \frac{1}{2} \bigg( ( \partial_z N_y + \partial_y N_z)^2 + ( \partial_y N_x + \partial_x N_y)^2 + ( \partial_z N_x + \partial_x N_z)^2 \bigg)
    \end{align}
    Some observations are already in order. The first term in the above equation has an indeterminate sign and is quadratic in derivatives of different components. The second term is negative semi-definite and involves linear combinations of derivatives. This explains why some of the previously proposed solitonic configurations exhibit negative energies. Their configurations depend only on a single component of the shift vector. For example, the Alcubierre ansatz reduces the above equation to
    \[
        16 \pi \rho = - \frac{1}{2} \bigg( (\partial_y N_x)^2 + (\partial_z N_x)^2 \bigg).
    \]
    In order to satisfy the WEC, any ansatz must contain at least two non-zero components of the shift vector field.

\paragraph{}
    Eq. \eqref{eq:WECinansatz} does not provide any further information regarding its positivity. One must dive deeper into the internal structure
of the equation to investigate its properties. This can be accomplished by considering a general decomposition of the shift vector field. There are a number of decompositions of vector fields, but the most commonly employed, and the one utilized here, is the Helmholtz decomposition
    \begin{equation}\label{def:Helmholtz}
        \vec{N}(x,y,z) = \vec{\partial}\phi(x,y,z) + \vec{\omega}(x,y,z),
    \end{equation}
    where $\phi$ is a scalar field and $\vec{\omega}$ is a solenoidal field satisfying $\vec{\nabla} \cdot \vec{\omega}=0$. After tedious algebra, the Hamiltonian constraint can be shown to reduce to
    \begin{equation}\label{eq:WECinhelmholtz}
        16 \pi \rho = 2*\bigg( h_1 + h_2 + h_3 \bigg) - 2 \bigg \langle
\mathcal{J}, \mathcal{H} \bigg \rangle_F - \bigg \langle \mathcal{J}, \mathcal{J} \bigg \rangle_F + \frac{1}{2} | \vec{\nabla} \times \vec{\omega}|^2,
    \end{equation}
    where $h_i$ is the i'th second-order principal minor of the Hessian $\mathcal{H}$ of $\phi$, $\mathcal{J}$ is the Jacobian matrix of $\vec{\omega}$, $\vec{\nabla}\times \vec{\omega}$ is the curl of the solenoidal field, and the sesquilinear form $\langle \cdot, \cdot \rangle_F$ is the Frobenius product defined as
    \[
     \left \langle A, B \right \rangle_F = \sum_{i,j} A_{ij}B_{ij}.
    \]
    Importantly, its a positive-definite form, implying the third term in
Eq. \eqref{eq:WECinhelmholtz} is negative definite. The momentum constraint also admits a simple decomposition,
    \[
        16 \pi \vec{p} = \nabla ^2 \vec{\omega} = - \vec{\nabla} \times \vec{\nabla} \times \vec{\omega}.
    \]
    Notably, this implies irrotational fields will always enforce a vanishing momentum density.

\paragraph{}
    The key result of this decomposition is the geometrical interpretation of the energy density in the purely irrotational sector. For shift vector fields described by a single scalar field, $\vec{N} = \vec{\partial}
\phi$, the constraint equations in the (3+1)-decomposition of the Einstein equations reduce to
    \begin{align} \label{eq:WECinirrotationalhelmholtz}
        8 \pi \rho &= h_1 + h_2 + h_3\\\nonumber
        \vec{p} &= 0.
    \end{align}
    The WEC then enforces the constraint
    \[
        h_1 + h_2 + h_3 \geq 0.
    \]
    The scalar component of the shift vector field contributes a geometric term to the Eulerian energy density. The second-order principal minors describe the curvature of the scalar field in the two-dimensional subspaces. Although it's not directly related to the convexity of the entire function, convexity of the two-dimensional subspaces of the scalar field $\phi$ determines the positivity of the Eulerian energy density. Convexity (concavity) of the entire function is indeed a sufficient condition, but it's not necessary. As long as one of the principal minors is sufficiently
large, the other two may be negative while still satisfying the WEC.

\paragraph{}
    Although not evident from Eq. \eqref{eq:WECinhelmholtz}, its a simple
task to show that purely solenoidal shift vector fields have negative semi-definite energy. This follows directly from the Hamiltonian constraint in Eq. \eqref{eq:decomposedeinsteinequation}, noting that $\mathscr{K} =
\vec{\nabla} \cdot \vec{N}$. If the shift vector field were purely solenoidal, then $\vec{\nabla} \cdot \vec{N} = 0$, implying $\rho = - \frac{1}{16 \pi} K_{ij}K^{ij} \leq 0$, as is the case for the Natario spacetime.

\subsection{Positive Energy Spacetime Soliton} \label{sec:positivenergywarpdrive}
\paragraph{}
    Using the geometrical interpretation offered by Eq. \eqref{eq:WECinirrotationalhelmholtz}, it's a simple matter to construct, using geometric intuition alone, a positive energy solitonic spacetime. Assume the shift vector field is purely irrotational and let
    \[
        \phi(x,y,z) = -z +
        \begin{cases}
        - \big(\sqrt{x^2 + y^2}\big)^6 - z^2 & -\big(\sqrt{x^2 + y^2}\big)^6 - z^2>z\\
        \big(\sqrt{x^2 + y^2}\big)^6 + z^2 &  \big(\sqrt{x^2 + y^2}\big)^6 + z^2<z\\
        z & \text{else}
        \end{cases}.
    \]
    The shift vector field is then calculated from $\vec{N} = \vec{\partial} \phi$. The scalar field $\phi$ fully describes the spacetime, including the energy density and expansion. See Fig. (\ref{fig:PWSoliton}). The total integrated shift is zero and the magnitude of the shift vector in
the central region $(0,0,0)$ is 1.3, which is superluminal. Moreover, the
energy density approaches zero in the central region, a perfect location for a vehicle. Additionally, the shift vector field portrays the same directionality as the Alcubierre configuration, namely the shift vector field points away from expanding regions and towards contracting regions. It's important to note that the scalar field is not $C^2$-differentiable.
    \begin{figure}
        \begin{subfigure}{0.5\textwidth}
            \centering
            \includegraphics[width=0.75\linewidth]{PW2func-eps-converted-to.pdf}
            \caption{}
            \label{fig:PWslicedfunc}
        \end{subfigure}
        \begin{subfigure}{0.5\textwidth}
            \centering
            \includegraphics[width=0.8\linewidth]{PW2EnergySliced-eps-converted-to.pdf}
            \caption{}
            \label{fig:PWslicedenergy}
        \end{subfigure}
        \begin{subfigure}{0.5\textwidth}
            \centering
            \includegraphics[width=0.85\linewidth]{PW2EnergyFull-eps-converted-to.pdf}
            \caption{}
            \label{fig:PWfullenergy}
        \end{subfigure}
        \begin{subfigure}{0.5\textwidth}
            \centering
            \includegraphics[width=0.75\linewidth]{PW2ExpanFull-eps-converted-to.pdf}
            \caption{}
            \label{fig:PWfullexpan}
        \end{subfigure}
        \begin{subfigure}{0.5\textwidth}
            \centering
            \includegraphics[width=0.7\linewidth]{PW2ShiftVecXZ-eps-converted-to.pdf}
            \caption{}
            \label{fig:PWslicedshift}
        \end{subfigure}
        \begin{subfigure}{0.5\textwidth}
            \centering
            \includegraphics[width=0.83\linewidth]{PW2ShiftVec-eps-converted-to.pdf}
            \caption{}
            \label{fig:PWShift}
        \end{subfigure}
        \caption{Configuration described by a piecewise-defined shift vector potential. Figure \ref{fig:PWslicedenergy} shows the energy density of the configuration in the $y=0$ plane. Note the large discontinuities.
Figure \ref{fig:PWfullenergy} shows a 3D density plot of the energy density. Opacity and color are a proxy for magnitude. The magnitude is maximal
on the outer edge of the toroids and minimal inside. Figure \ref{fig:PWfullexpan} shows a density plot of the volume expansion. The magnitude of the expansion is maximal on the outer face of the toroid and minimal on the inside. Positive expansion is occurring in the positive z region, while
contraction is occurring in the negative z region. Figure \ref{fig:PWslicedshift} is the $y=0$ slice of the shift vector field. In a neighborhood of the origin, the shift vector field is almost purely in the negative z-direction (towards the negative expansion). }
    \label{fig:PWSoliton}
    \end{figure}
\paragraph{}
    One could construct several variations of the above configuration. The key trait is that its energy is purely positive. One could seek to minimize the energy density while maintaining superluminality of the central region by altering the geometry of the scalar field. However, the discontinuities present in the configuration could pose a large problem when attempting to construct such a configuration.

\paragraph{}
    One must be careful when dealing with piecewise functions in spacetime. Cusps, corners, and other discontinuities aren't physical. As suggested by the geometrical nature of Eq. \eqref{eq:WECinirrotationalhelmholtz},
negative energies will manifest if the scalar field $\phi$ has strongly-curved saddle points in any of the three two-dimensional subspaces. One could ``hide'' the saddle points in the discontinuities of the function, such as a corner. Any physically realistic field should be sufficiently smooth, since any physical construction will inevitably possess a certain fall-off in the otherwise geometrical corner. Additionally, the length scale of such a discontinuity is infinitesimally small, way beyond the regime
of classical gravity. One would need a description of the small-scale nature of spacetime to even begin to describe configurations containing scales of this order.

\paragraph{}
    In the interest of constructing a physically interesting superluminal
configuration, an additional smoothness condition is enforced on the spacetime. The shift vector potential field $\phi$ is required to be at least
$C^2$-differentiable. This forces the resulting energy density distribution to be continuous, largely avoiding issues associated to many piecewise
configurations. One such example of a scalar field satisfying this condition is

\begin{comment}
    \begin{align} \label{def:irrotational1potential}
        \phi(x,y,z) = \frac{V}{2 \sqrt{\sigma(x,y,z)}} \Bigg( &\bigg((x^2 + y^2 + z^2)^{\Pi} - r\bigg) Erf\Bigg[ \frac{\bigg((x^2 + y^2 + z^2)^{\Pi} - r\bigg)}{\sqrt{\sigma(x,y,z)}}\Bigg]\\
        \nonumber
        + &\bigg((x^2 + y^2 + z^2)^{\Pi} + r\bigg) Erf\Bigg[ \frac{\bigg((x^2 + y^2 + z^2)^{\Pi} + r\bigg)}{\sqrt{\sigma(x,y,z)}} \Bigg]\\
        \nonumber
        &+ \frac{\sqrt{\sigma(x,y,z)}}{\sqrt{\pi}} \bigg( e^{- \frac{\big((x^2 + y^2 + z^2)^{\Pi} - r\big)^2}{\sigma(x,y,z)}} + e^{ - \frac{\big((x^2 + y^2 + z^2)^{\Pi} + r\big)^2}{\sigma(x,y,z)}} \bigg) \Bigg)\\ \nonumber
        + &z\frac{\sqrt{\pi} V \Pi}{4} \left( \sqrt{\max{\left(\sigma(x,y,z)\right)}} - \sqrt{\min{\left(\sigma(x,y,z)\right)}}\right).
    \end{align}
\end{comment}

  \begin{align} \label{def:irrotational1potential}
     \phi(x,y,z) =& \frac{1}{4}\sqrt{\pi }V\left( 2\left(\rho -\left(x^2+y^2+z^2\right)^{\Pi }\right)\text{Erf}\left(\frac{\rho -\left(x^2+y^2+z^2\right)^{\Pi }}{\sqrt{\sigma (x,y,z)}}\right) \right. \\ \nonumber
     &\left. +2\left(\rho +\left(x^2+y^2+z^2\right)^{\Pi }\right) \text{Erf}\left(\frac{\rho +\left(x^2+y^2+z^2\right)^{\Pi }}{\sqrt{\sigma (x,y,z)}}\right)-4\rho \text{ }\text{Erf}\left(\frac{\rho }{\sqrt{\sigma (x,y,z)}}\right) \right. \\ \nonumber
     & \left. +\frac{2\sqrt{\sigma (x,y,z)}}{\sqrt{\pi}}\left(e^{-\frac{\left(\rho-\left(x^2+y^2+z^2\right)^{\Pi } \right)^2}{\sigma (x,y,z)}}+e^{-\frac{\left(\rho +\left(x^2+y^2+z^2\right)^{\Pi }\right)^2}{\sigma (x,y,z)}}-2e^{-\frac{\rho ^2}{\sigma (x,y,z)}}\right) \right) \\ \nonumber
     & +\frac{1}{4}\sqrt{\pi }V \Pi  z \left( \sqrt{\text{Max}\left(\sigma\left(x,y,z\right)\right)}-\sqrt{\text{Min}\left(\sigma\left(x,y,z\right)\right)}\right)
    \end{align}

    where $\Pi$, $r$, and $V$ are parameters to be specified, $\sigma(x,y,z)>0$ is a Gaussian weight parameter that is allowed to vary spacially, and $\text{Erf}[]$ is the error function. For certain choices of $\sigma(x,y,z)$, this is $C^2$ on the region $\mathbb{R}^3 - 0$ and approaches zero as $\vec{x} \rightarrow \vec{0}$. For example, the choice
    \begin{align*}
        \left(\Pi,r,V, \sigma\right) &=\left(\frac{1}{4}, 6, 10, 1\right)
    \end{align*}
    results in an at least $C^2$-function on $\mathbb{R}^3-0$ and approaches zero as $\vec{x} \rightarrow \vec{0}$. The energy density is everywhere positive and highly localized. Moreover, the total energy density,
    \[
        E_{\text{total}} = \int dx dy dx \rho(x,y,z),
    \]
    is finite. The central region $|\vec{x}|<r$ has asymptotically vanishing shift vector. The only superluminal shift vector is in the exterior region $|\vec{x}|>r$, which approaches Minkowski space at asymptotic infinity. A simple modification to the Gaussian weight parameter results in a configuration possessing superluminal shift in the interior region, Fig. (\ref{fig:irrotsuperluminal}). By increasing the Gaussian
weight parameter in the +z region and decreasing it in the -z region, the
energy density correspondingly increases in the +z region and decreases in the -z region. This results in the gradient of the $\phi$-field increasing in the region $|\vec{x}|<r$, generating a high and level shift. Compare this to the $\sigma(x,y,z) = const.$ case. The $\phi$-field becomes spherically symmetric, resulting in the energy density being uniformly distributed in a spherical shell around the central region $|\vec{x}|<r$. Modifying the central gradient causes the energy density distribution to be highly peaked in the $+z$ region. For the specific choice of parameters
used in Fig. (\ref{fig:irrotsuperluminal}), the central shift magnitude is 1.15, i.e. superluminal.

\paragraph{}
    This could serve as a method of generating acceleration without violating the continuity equations. One could start with a finite energy distribution highly concentrated and uniformly distributed in a spherical shell around a spacecraft. The energy density is then increased behind the spacecraft and decreased in front, without destroying or creating any additional energy. This increases the shift vector magnitude in the region where the spacecraft is located, transporting it to superluminal speeds relative to faraway observers. This then operates as a tuneable solitonic configuration capable of superluminal speeds. Whether the central vehicle can actually manipulate the energy density in the luminal and superluminal regimes remains in question. The spacetime might still possess some of the other pathologies associated to the classical solitonic configurations,
such as the formation of horizons. Although, there are two important deviations from the classical configurations, namely the absence of negative energies and the exterior region no longer behaving like Minkowski space.
The exterior region of the warp bubble is now Schwarzschild-like and satisfies the prerequisites of Birkoff's theorem only in the case when $\sigma(x,y,z)$ is spherically symmetric, which the spacetime in Fig. (\ref{fig:irrotsuperluminal}) does not. This non-truncation of the gravitational field outside the warping region is likely the reason why negative energies are absent from this configuration, in agreement with \cite{bobrick_introducing_2021}. Interestingly, by increasing the \emph{average} Gaussian weight, the energy density could be reduced without modifying the central
gradient of the $\phi$-field. This could be used to avoid the formation of a black hole due to high energy densities. This configuration is then highly modifiable, thanks to the geometric interpretation of the Eulerian energy. Compared to the
configuration presented in \cite{lentz_breaking_2020}, the shift vector potential in Eq. \eqref{def:irrotational1potential} is more general as it does not assume any relations between the shift vector components. Moreover, as there are no relations between the derivatives of the shift vector
potential, the scalar field can be easily adjusted in any way in order to
optimize the physical construction of the configuration.

\begin{figure}
    \begin{subfigure}{0.5\textwidth}
        \centering
        \includegraphics[width=0.8\linewidth]{IrrotFourFunc-eps-converted-to.pdf}
        \caption{}
        \label{fig:IrrotThreeslicedfunc}
    \end{subfigure}
    \begin{subfigure}{0.5\textwidth}
        \centering
        \includegraphics[width=0.8\linewidth]{IrrotFourEnergyXZ-eps-converted-to.pdf}
        \caption{}
        \label{fig:IrrotThreeSlicedEnergy}
    \end{subfigure}
    \begin{subfigure}{0.5\textwidth}
        \centering
        \includegraphics[width=0.8\linewidth]{IrrotFourEnergyDistribution-eps-converted-to.pdf}
        \caption{}
        \label{fig:IrrotThreeFullEnergy}
    \end{subfigure}
    \begin{subfigure}{0.5\textwidth}
        \centering
        \includegraphics[width=0.8\linewidth]{IrrotFourFullExpansion-eps-converted-to.pdf}
        \caption{}
        \label{fig:IrrotThreeFullExpan}
    \end{subfigure}
    \begin{subfigure}{\textwidth}
        \centering
        \includegraphics[width=0.4\linewidth]{IrrotFourShiftVectorSlice-eps-converted-to.pdf}
        \caption{}
        \label{fig:IrrotThreeFullShift}
    \end{subfigure}
    \caption{Configuration defined from an at least $C^2$-differentiable shift vector potential, shown in Figure \ref{fig:IrrotThreeslicedfunc}. The energy density, Figure \ref{fig:IrrotThreeSlicedEnergy} ($y=0$ slice) and Figure \ref{fig:IrrotThreeFullEnergy} (3D density plot), is highly localized. It has a finite integral over the three-dimensional leaves of the foliation. The expansion, Figure \ref{fig:IrrotThreeFullExpan} (3D density plot), is everywhere non-negative, with greater expansion in the positive z region. Opacity and color in the density plots serve as a proxy for magnitude. The shift vector field, Figure \ref{fig:IrrotThreeFullShift}, is highly radial and asymptotically Minkowskian in the exterior region and highly linear in the interior with a central magnitude of $\sim 1.15$, i.e. superluminal.}
    \label{fig:irrotsuperluminal}
\end{figure}

\paragraph{}
    The ansatz Eq. \eqref{eq:WECinansatz} contains an interesting property related to an O(3) operation. The dynamical equations Eq. \eqref{eq:decomposedeinsteinequation} are not invariant under the total spacial inversion $\vec{N} \rightarrow -\vec{N}$. Additionally, the expansion is not invariant either, since under this operation, $\mathscr{K} \rightarrow -\mathscr{K}$. However, since $\gamma = \mathbbm{1}$, the inversion is equivalent, according to the dynamical equations, to the temporal inversion $t \rightarrow -t$. As expected, the shift vector inversion is equivalent to an inversion of the foliation label, which can be interpreted as ``time running backwards.'' This means that the same static energy distribution can produce two different configurations, one in which spacetime possesses positive expansion and one with negative expansion. It makes sense, then, to consider the strong energy condition (SEC) in this case. In the case of a purely irrotational shift vector field, the geometric side of the SEC, applied to the Eulerian observer, becomes
    \[
        \tensor[^4]{R}{_{\mu \nu}}n^{\mu}n^{\nu} = - \langle \mathcal{H}, \mathcal{H} \rangle_F - \vec{\nabla} \phi \cdot \vec{\nabla}( \nabla^2
\phi),
    \]
    It's interesting that this equation is invariant under the inversion $\phi \rightarrow -\phi$. This means that if the spacetime possessing positive expansion everywhere violates the SEC, then so too will the spacetime obtained by $\phi \rightarrow -\phi$, which possesses negative expansion (contraction) everywhere. In fact, it follows by simple calculations that if
    \[
        \partial_t (\vec{\nabla} \cdot \vec{N}(t,x,y,z))= \partial_t \theta(t,x,y,z) = 0
    \]
    then $\tensor[^4]{R}{_{\mu \nu}}n^{\mu}n^{\nu}$ is invariant under $\vec{N} \rightarrow - \vec{N}$. This means that if the expansion is independent of co-ordinate time, then the geometric side of the SEC, applied to
the Eulerian observer, is invariant under the total inversion $\vec{N} \rightarrow - \vec{N}$. Evidently, the configurations in Fig. (\ref{fig:PWSoliton}) and Fig. (\ref{fig:irrotsuperluminal}) violate the SEC. However,
due to the fact $\vec{p}=0$, the dominant energy condition applied to the Eulerian observer is satisfied.

\subsection{Chronological Protection} \label{sec:chronological}
When studying superluminal motion, one inevitably runs into the problem of generating closed timelike curves (CTCs) and the associated chronological protection conjecture presented in \cite{hawking_chronology_1992}. As discussed, the configurations presented in Sec. \ref{sec:positivenergywarpdrive} admit superluminal inertial observers. This naturally leads to the
question of whether these configurations can be used to generate CTCs or not. It may be that these configurations can be used to violate causality
in the superluminal regime, however there are two possible arguments for reconciliation with the chronological protection conjecture. The first is
that one of the preconditions of the presented configurations is that the
spacetime is globally hyperbolic. This means that the leaves of the foliation are Cauchy surfaces and hence CTCs cannot form. The second is that as the energy distribution is being manipulated from the spherically symmetric distribution into the axi-symmetric distribution (Fig. \ref{fig:irrotsuperluminal}), horizons form preventing manipulation of the energy distribution past the speed of light barrier. In other words, horizon formations prevent the configurations from transporting an inertial observer from the subluminal regime to the superluminal regime. This agrees with the discussion in \cite{bobrick_introducing_2021}. More work will need to be done to analyze the formation of horizons and the evolution from the subluminal to superluminal regimes in the presented configurations.

\subsection{Numerics} \label{sec:numerics}
\paragraph{}
To get a sense of the magnitude of the energy densities in the previous section, Newton's constant and the speed of light are reinserted into the Hamiltonian constraint. With this definition of the units, the energy density becomes
\[
\rho(x,y,z) =\frac{c^4}{16 \pi G} \left[ 2*\bigg( h_1 + h_2 + h_3 \bigg) - 2 \bigg \langle \mathcal{J}, \mathcal{H} \bigg \rangle_F - \bigg \langle \mathcal{J}, \mathcal{J} \bigg \rangle_F + \frac{1}{2} | \vec{\nabla}
\times \vec{\omega}|^2 \right].
\]

\paragraph{}
For the case of an irrotational field, this simplifies, as before, to
\[
 \rho(x,y,z) = \frac{c^4}{8 \pi G} (h_1 + h_2 + h_3).
\]
If $(h_1 + h_2+h_3)$ is order unity, then
\begin{align*}
 \rho(x,y,z) &\approx 4.8 * 10^{42} \text{    $\frac{J}{m^3}$} \\
 &\approx 5.3*10^{25} \text{        $\frac{kg}{m^3}$}.
\end{align*}

\paragraph{}
The maximum value of the energy density for the configuration shown in Fig. \ref{fig:irrotsuperluminal}, as measured by the Eulerian observer, is found to be
\[
\rho_{\text{max}} \approx 5.3*10^{23} \text{   $\frac{kg}{m^3}$}.
\]
This is an astronomical energy density concentrated in a very small region. More than likely, any attempt to construct this specific configuration
will form a black hole. The total energy present on any initial hypersurface can be found to be approximately
\[
 E_{total} \approx 4.5*10^{45} \text{      $J$},
\]
which is still enormous, but quite small in astronomical terms. For comparison, the rest mass energy of the sun is approximately
\[
 E_{\odot} \approx 1.78*10^{47} \text{        $J$}.
\]
Hence, the total energy required to form the configuration of Fig. (\ref{fig:irrotsuperluminal}) is two orders of magnitude smaller than the rest mass energy of the sun. This is a drastic improvement on the energy scales of the classical superluminal solitons and comparable to the configuration in \cite{lentz_breaking_2020}. Moreover, thanks to the geometric interpretation of the Eulerian energy in the considered class of spacetimes, it would be a simple matter to drastically reduce the energy requirements, as discussed in Sec. \ref{sec:positivenergywarpdrive}, and thus avoid
the formation of a black hole.

\section{Conclusion}
\paragraph{}
    The results discussed in the previous sections provide great insight into the properties of the weak energy condition for superluminal solitonic spacetimes. The geometric interpretation of the Eulerian energy density opens new doors for constructing realistic superluminal spacetimes from
feasible energy densities. Numerical techniques could be employed to investigate the nature of the irrotational sector of the Hamiltonian constraint, such as a Finite Element Method for solving the second order partial differential equation. The techniques available during this study could not solve the PDE, owing to its high non-linearity. More than likely, a new PDE solver would need to be constructed specifically for this differential equation. One could also perform other decompositions of the shift vector field to investigate other hidden properties. This may illuminate hidden interpretations that would allow easier construction of a shift vector field composed of irrotational and solenoidal components.

\paragraph{}
    The energy densities discussed in Sec. \ref{sec:numerics} could easily be reduced to more manageable scales by minimizing the curvature of the shift vector potential. One could even utilize computational power to
search for configurations that minimize the energy density while maximizing the central shift vector magnitude. The results of the previous section have translated the complicated and abstract problem of WEC violations in spacetimes containing superluminal motion into a simple geometric one.

\paragraph{}
    These results are extremely exciting. They shed new light on physically-realistic superluminal warp drives and brightens the future of manned interstellar travel.

\section*{Acknowledgements}
LH is supported by funding from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation programme grant agreement No 801781 and by the Swiss National Science Foundation grant 179740.

 \begin{comment}

\begin{appendices}
\section{Problem with Insufficiently Smooth Configurations} \label{sec:problemfunc}

\paragraph{}
    An illustration of the ability of discontinuities to hide negative energy densities is offered by the following construction. Consider the function describing the shift vector potential
    \small
    \begin{align*}
        \phi(x,y,z) = &- \tanh{\Bigg[3\Bigg( -1 + \Bigg(\sqrt{\Big(\frac{x}{\sqrt{2}} - \frac{y}{\sqrt{2}}\Big)^2} + \sqrt{\Big( \frac{\sqrt{3}x}{2\sqrt{2}} + \frac{\sqrt{3}y}{2 \sqrt{2}} + \frac{z}{2}\Big)^2} + \sqrt{\Big( \frac{x}{2 \sqrt{2}} + \frac{y}{2 \sqrt{2}} - \frac{\sqrt{3}z}{2}\Big)^2} \Bigg) \Bigg) \Bigg]}\\
        &+ \tanh{\Bigg[3\Bigg( 1 + \Bigg(\sqrt{\Big(\frac{x}{\sqrt{2}} - \frac{y}{\sqrt{2}}\Big)^2} + \sqrt{\Big( \frac{\sqrt{3}x}{2\sqrt{2}} + \frac{\sqrt{3}y}{2 \sqrt{2}} + \frac{z}{2}\Big)^2} + \sqrt{\Big( \frac{x}{2
\sqrt{2}} + \frac{y}{2 \sqrt{2}} - \frac{\sqrt{3}z}{2}\Big)^2} \Bigg) \Bigg) \Bigg]}.
    \end{align*}
    \normalsize
    See Fig. \ref{fig:discontinuitiesproblem}. This function was constructed by rotating a function parameterized by the $L_1$-norm of $(x,y,z)$. It turns out the energy of this configuration, calculated from Eq. \eqref{eq:WECinhelmholtz}, is zero.
    \begin{figure}[H]
            \begin{subfigure}{0.5\textwidth}
            \centering
            \includegraphics[width=\linewidth]{ProblemfunctionNOEnergy}
            \caption{}
            \label{fig:discontinuitiesproblemfunctionslice}
        \end{subfigure}
        \begin{subfigure}{0.5\textwidth}
            \centering
            \includegraphics[width=\linewidth]{ProblemfunctionNOEnergy2}
            \caption{}
            \label{fig:discontinuitiesproblem3D}
        \end{subfigure}
        \caption{Configuration specified by the $L_1$-norm of $(x,y,z)$. Figure \ref{fig:discontinuitiesproblemfunctionslice} is the $y=0$ slice
of the function, showing the perfect corners in the function thanks to the absolute value in the $L_1$-norm. Figure \ref{fig:discontinuitiesproblem3D} is a 3D density plot showing the full 3-dimensional extent of the function. Opacity of the plot serves as a proxy for the magnitude. Note, the faces of the diamond shape are flat, implying the corners are mathematical corners.}
        \label{fig:discontinuitiesproblem}
    \end{figure}
    The corners apparent in Fig. \ref{fig:discontinuitiesproblem} are indeed geometric corners, owing to the absolute values in the definition of $\phi$. One can see this by calculating the gradient of $\phi$ and observing its step-like nature. However, any attempt to construct such a configuration will inevitably smooth the corners. This can be represented by a small deviation from the $L_1$-norm,\footnote{Though not exactly, since this will also change other aspects of the function and it wont even get rid of the step-like character of the gradient. But it is sufficient for the present considerations. Smoothing the corners while maintaining other properties of the function would be much more complicated. The present method only serves as a simple example.} such as
    \small
    \begin{align*}
        \phi(x,y,z) = &- \tanh{\Bigg[3\Bigg( -1 + \Bigg(\Big(\frac{x}{\sqrt{2}} - \frac{y}{\sqrt{2}}\Big)^{1+\epsilon} + \Big( \frac{\sqrt{3}x}{2\sqrt{2}} + \frac{\sqrt{3}y}{2 \sqrt{2}} + \frac{z}{2}\Big)^{1+\epsilon}
+ \Big( \frac{x}{2 \sqrt{2}} + \frac{y}{2 \sqrt{2}} - \frac{\sqrt{3}z}{2}\Big)^{1+\epsilon} \Bigg)^{\frac{1}{1+\epsilon}} \Bigg) \Bigg]}\\
        &+ \tanh{\Bigg[3\Bigg( 1 + \Bigg(\Big(\frac{x}{\sqrt{2}} - \frac{y}{\sqrt{2}}\Big)^{1+\epsilon} + \Big( \frac{\sqrt{3}x}{2\sqrt{2}} + \frac{\sqrt{3}y}{2 \sqrt{2}} + \frac{z}{2}\Big)^{1+\epsilon} + \Big( \frac{x}{2 \sqrt{2}} + \frac{y}{2 \sqrt{2}} - \frac{\sqrt{3}z}{2}\Big)^{1+\epsilon} \Bigg)^{\frac{1}{1+\epsilon}} \Bigg) \Bigg]},
    \end{align*}
    \normalsize
    which is again a rotated form of a $L_{1+\epsilon}$-normed function. The Hamiltonian constraint calculated from this function possesses negative energy densities (Fig. \ref{fig:discontinuitiesproblemNegenergies}).
    \begin{figure}[H]
        \begin{subfigure}{0.5\textwidth}
            \centering
            \includegraphics[width=0.9\linewidth]{ProblemFunctionNegXZ}
            \caption{}
        \end{subfigure}
        \begin{subfigure}{0.5\textwidth}
            \centering
            \includegraphics[width=0.8\linewidth]{ProblemFunctionNeg}
            \caption{}
            \label{fig:discontinuitiesproblemNegenergies3D}
        \end{subfigure}
        \begin{subfigure}{\textwidth}
            \centering
            \includegraphics[width=0.45\linewidth]{ProblemEnergyNegXZ}
            \caption{}
            \label{fig:discontinuitiesproblemNegenergiesENN}
        \end{subfigure}
        \caption{Configuration specified by a shift vector potential parameterized by the $L_{1+\epsilon}$-norm of $(x,y,z)$. Negative energies manifest due to the rounding of the corners of the function. Figure \ref{fig:discontinuitiesproblemNegenergies3D} is a 3D density plot of the scalar
field $\phi$, showing its full three-dimensional extent. The opacity serves as a proxy for the magnitude of the function. Figure \ref{fig:discontinuitiesproblemNegenergiesENN} shows the $y=0$ slice of the energy density of the configuration, showing the presence of negative energy densities.}
        \label{fig:discontinuitiesproblemNegenergies}
    \end{figure}

\paragraph{}
    One must be very careful when constructing physically realistic solitons using a decomposition such as Eq. \eqref{def:Helmholtz}. Discontinuities can easily hide negative energies that would otherwise be \emph{required} when attempting to construct the configuration using realistic matter distributions.

\end{appendices}
\end{comment}

\newpage
\phantomsection
\addcontentsline{toc}{section}{References}
\printbibliography

\end{document}

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Handmade RAIN of Western WA: Belated birthdays and happy new year!
Since I was traveling over the holidays, I missed a handful of EtsyRain birthdays!
December 28th was the birthday of two of our members, Colleen of BCharmer and David of Nastrovia Handmade Gifts. Colleen's shop features a variety of sewn goods, while David's shop (which he shares with his wife) contains woodworking and jewelry.
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Happy Birthday Everyone! Happy New Years Everyone! And I'm super happy you included our calendar picture! Happy THANK YOUS!


The United Kingdom Chevening Secretariat is accepting applications for 2017/2018 Chevening Scholarships from 8 August until 8 November 2016, announced the British Embassy in Buenos Aires. Chevening Scholarships are awarded to individuals with demonstrable leadership potential who also have strong academic backgrounds.
Several sustainable mining projects supported by the British Embassy's 2016 Prosperity Fund and Newton-Picarte science and innovation fund were discussed at a workshop held at the British Embassy in late July.
Argentina is organizing a major business and investment forum next month, September 12/15, in Buenos Aires and more than 1,500 world business leaders and representatives of government and economic institutions are scheduled to attend the event, probably the largest in recent times in Latin America.
Guatemalan government makes a call to Apple asking to rename iconic ringtone.
The movement made up of artists and local authorities has now 7000 signatures of support. The " Marimba " ringtone is the classic iPhone ringtone and probably one of the most recognizable ringtones in the world. What most people around the globe don't know is that the Marimba is the national instrument of Guatemala and one of it's national symbols.


Click on play button to listen high quality(320 Kbps) mp3 of "Toni Braxton - I Wish (Audio)". This audio song duration is 3:05 minutes. This song is sing by Toni Braxton. You can download Toni Braxton - I Wish (Audio) high quality audio by clicking on "Download Mp3" button.


text:
Shan, Pan and Eschborn, Ulrich. Nabokov's Lolita in China: Its Reception and the Rise of Popular Literature. 2016
Shan, Pan and Eschborn, Ulrich
Nabokov's Lolita in China: Its Reception and the Rise of Popular Literature
The article by Pan Shan (Peking University) and Ulrich Eschborn (Beijing Institute of Technology), "Nabokov's Lolita in China: Its Reception and the Rise of Popular Literature," analyzes the connections between the rise of popular culture in mainland China and the publication history of Lolita, which was first published there in Chinese in 1989. In the first section, we explain that, in the decade after the Cultural Revolution, publishers used the more market-oriented and more liberal climate to profit economically by publishing translations of previously forbidden Western books. The second part of the article compares a passage from Wang Shuo's popular novel Fierce Animals (1991) to the passage from Lolita in which Humbert Humbert first encounters Lolita. This comparison reveals striking parallels and serves as an example of how Nabokov's novel figures as one element in the tremendous rise of Chinese popular culture.
Thank you for all the… 19 hours 2 minutes ago

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text:
Q: Rails Minitest undefined method `greater_than_or_equal_to' for #I want to use ShouldaMatchers gem inside of Minitest to check simple model validation:
class Portfolio < ApplicationRecord
  validates :share_ratio, numericality: { greater_than_or_equal_to: 0, less_than_or_equal_to: 100 }
end

To do so I've got a Minitest:
require 'test_helper'

class PortfolioTest < ActiveSupport::TestCase
  context 'validations' do
    should validate_numericality_of(:share_ratio).greater_than_or_equal_to(0)
    should validate_numericality_of(:share_ratio).is_less_than_or_equal_to(100)
  end
end

But I'm getting an error:

class:PortfolioTest': undefined method `greater_than_or_equal_to' for #Shoulda::Matchers::ActiveModel::ValidateNumericalityOfMatcher:0x00007fba91da3ce0 (NoMethodError)

#Gemfile:
  gem 'shoulda', '~> 4.0'
  gem 'shoulda-matchers', '~> 4.0'

I tried to change validation inside of the model:
validates_numericality_of :share_ratio, greater_than_or_equal_to: 0, less_than_or_equal_to: 100

But error is the same.

A: You got one of them right, but not the other.
should validate_numericality_of(:share_ratio).is_greater_than_or_equal_to(0)
should validate_numericality_of(:share_ratio).is_less_than_or_equal_to(100)

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text:
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Whale Day
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By: Julian Barnes
Narrated by: Saul Reichlin
In the summer of 1885, three Frenchmen arrived in London for a few days' shopping. One was a Prince, one was a Count, and the third was a commoner with an Italian name, who four years earlier had been the subject of one of John Singer Sargent's greatest portraits. The three men's lives play out against the backdrop of the Belle Epoque in Paris. The beautiful age of glamour and pleasure more often showed its ugly side: hysterical, narcissistic, decadent and violent, a time of rampant prejudice and blood-and-soil nativism, with more parallels to our own age than we might imagine.
Spellbound from start to finish- fascinating.
The Lost Spells
By: Robert Macfarlane, Jackie Morris
Narrated by: Robert Macfarlane, Yrsa Daley-Ward, Johnny Flynn, and others
An audio treasure, a new collection of 'spells' - acrostic poetry and artwork - by writer Robert Macfarlane and artist Jackie Morris. Captivatingly read, calling to forest, field, riverbank, ocean and also to the heart, these 'spells' summon back what is often lost from sight and care. From Jay to Jackdaw, Oak to Barn Owl, Silver Birch to Grey Seal, they evoke the special spirit of each plant and creature. Above all, they celebrate a sense of wonder at nature's power to amaze, console and bring joy.
Stop and listen.
By Vicki Jordan on 22-11-20
By: Maggie O'Farrell
Narrated by: Daisy Donovan
On a summer's day in 1596, a young girl in Stratford-upon-Avon takes to her bed with a fever. Her twin brother, Hamnet, searches everywhere for help. Why is nobody at home? Their mother, Agnes, is over a mile away, in the garden where she grows medicinal herbs. Their father is working in London. Neither parent knows that one of the children will not survive the week.
Narrator fights writing and wins (sadly)
By Leaf Green on 20-07-20
By: Richard Osman
Narrated by: Lesley Manville, Richard Osman, Marian Keyes
In a peaceful retirement village, four unlikely friends meet up once a week to investigate unsolved killings. But when a local property developer shows up dead, 'The Thursday Murder Club' finds themselves in the middle of their first live case. The four friends, Elizabeth, Joyce, Ibrahim and Ron, might be octogenarians, but they still have a few tricks up their sleeves. Can our unorthodox but brilliant gang catch the killer, before it's too late?
Oh WHAT a disappointment!
By mollyeyre on 03-09-20
How Fungi Make Our Worlds, Change Our Minds and Shape Our Futures
By: Merlin Sheldrake
Narrated by: Merlin Sheldrake
Neither plant nor animal, it is found throughout the earth, the air and our bodies. It can be microscopic, yet also accounts for the largest organisms ever recorded, living for millennia and weighing tens of thousands of tonnes. Its ability to digest rock enabled the first life on land, it can survive unprotected in space and it thrives amidst nuclear radiation. In this captivating adventure, Merlin Sheldrake explores the spectacular and neglected world of fungi: endlessly surprising organisms that sustain nearly all living systems.
Willingly entangled
By Paul on 17-11-20
By: Barack Obama
Narrated by: Barack Obama
5 out of 5 stars 2,855
In the stirring, highly anticipated first volume of his presidential memoirs, Barack Obama tells the story of his improbable odyssey from young man searching for his identity to leader of the free world, describing in strikingly personal detail both his political education and the landmark moments of the first term of his historic presidency - a time of dramatic transformation and turmoil.
Dropping a classic
By jesse on 17-11-20
The Return of Nature to a British Farm
By: Isabella Tree
Narrated by: Isabella Tree
Forced to accept that intensive farming on the heavy clay of their land at Knepp was economically unsustainable, Isabella Tree and her husband, Charlie Burrell, made a spectacular leap of faith: they decided to step back and let nature take over. Thanks to the introduction of free-roaming cattle, ponies, pigs and deer - proxies of the large animals that once roamed Britain - the 3,500 acre project has seen extraordinary increases in wildlife numbers and diversity in little over a decade.
Correction...
By n.bennett on 28-06-20
Why I'm No Longer Talking to White People About Race
By: Reni Eddo-Lodge
Narrated by: Reni Eddo-Lodge
In February 2014, Reni Eddo-Lodge posted an impassioned argument on her blog about her deep-seated frustration with the way discussions of race and racism in Britain were constantly being shut down by those who weren't affected by it. She gave the post the title 'Why I'm No Longer Talking to White People About Race'. Her sharp, fiercely intelligent words hit a nerve, and the post went viral, spawning a huge number of comments from people desperate to speak up about their own similar experiences.
cherry picked science to fulfill a narrative
By Dan norman on 03-04-20
A new collection from Billy Collins, former US poet laureate and "America's favorite poet" (The Wall Street Journal).
Billy Collins' new collection brings together more than 50 poems and showcases his deft mixing of the playful and the serious that has made him one of our country's most celebrated and widely known poets. Here are poems that leap with whimsy and imagination, yet stay grounded in the familiar, common things of everyday experience.
Collins takes us for a walk with an impossibly ancient dog, discovers the original way to eat a banana, meets an Irish spider, and even invites us to his own funeral. Sensitive to the wonders of being alive as well as the thrill of mortality, Whale Day builds on and amplifies Collins' reputation as one of America's most interesting and durable poets.
©2020 Billy Collins (P)2020 Random House Audio
Aimless Love
Dueling Anthologists at the 92nd Street Y
Billy Collins Live
What listeners say about Whale Day
Maggie Hess
To be read in the voice of Billy Collins
I have considered Billy Collins among the best writers ever since I first came across his poetry, which happened to be a poem he read on Prairie Home Companion about a Lanyard. I myself have long considered myself a poet, and I often wondered, regarding Collins, how he got to the superior collected quality you find in Whale Day and the rest of his works. "It is something about his voice," I considered quietly to myself, not realizing the irony in my words until later. Now I think I have found just what it is about his writing that carries so strongly in voice, because I imagine one day, long ago, when Billy Collins looked down at his own shoes and said to himself "If I want to be a poet, I am going to have to transform my literal voice into something that better fits what I do wish to have as my poetry." So on that day, age 13, when his voice finally had begun changing to something screechy and juvenile naturally on his own, Collins began the artful embodiment of the style of speech that you hear in this wonderful book today, or maybe you haven't read this yet, in which case let me describe it. The narrating voice of Billy Collins puts true poetry, deep emotional moments of love and trembling, to a vocalization that I personally have described as monotone. But it is in the contrast from his totally relatable writing to this droll yet sensitive tone, that so exquisitely and beautifully captures all that I value in poetry.


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Abertay student proves child's toy can be hacked
An Abertay student has carried out ground-breaking hacking work showing how an innocent child's toy could be transformed into an offensive 'talking Chucky' doll.
Ethical Hacking fourth year student Cheryl Torano spoke of the project she carried out as it was revealed that parents in Germany have been told to destroy the 'Cayla' doll because of its security risks.
The warning over Cayla – a doll that reads stories and can respond to a user's question through an app – was issued by the Federal Network Agency, which oversees telecommunications.
Researchers there say Cayla's smart technology can reveal personal data. But Abertay student Cheryl's project went a stage further and showed how hacking into the talking doll was 'frighteningly easy'.
The 32-year-old transformed Cayla from an 'angelic' child's doll into a 'swearing and offensive' toy.
Cheryl said, 'We downloaded the doll's app using free software that anyone can access. We then extracted the files from the doll and decoded it.
"It was in English on a Word document, which exposed the password. Then we were in… It couldn't have been easier.
"We turned Cayla back into a working doll – but this time she was a talking Chucky doll. Her stories went from being nice and gentle to being vulgar and offensive. Suddenly Cayla was swearing like a trooper in her sweet, little voice.
"The one thing that was meant to be secure in this doll was that it could not use inappropriate language. We proved that wasn't the case far too easily.
"We contacted the doll's manufacturers (Genesis Toys) and they said they were aware of its vulnerabilities and would update the software. But this doll is out there now. I'm not surprised to see sanctions being taken like in Germany today.
Cyber security firm Pen Test Partners were the first to hack a Cayla doll in 2014.
For her project, Cheryl uses a different method known as reverse engineering to gain access to the toy.
"Cheryl says, as a mother of two children – Jessica, 13, and Stewie, 5 – she was even more aware of the potential dangers posed by toys.
"It was unbelievably easy. Anyone sitting in their house could effectively spy on your child through a doll.
"This is why I want to make cyber security my career. Seeing how easy hacking into Cayla was makes me want to protect people.
"Dr Natalie Coull, Ethical Hacking lecturer at Abertay, said, 'The big problem is that a lot of these issues arise with toy manufacturers who have not really had to consider cyber security before.
"But now, the likes of baby monitors and talking dolls are risks and are perhaps not tested enough before being sold and used.
"The reality of the Internet of Things (IoT) is just around the corner: an era in which all manner of devices will be online, collecting data about daily life.
"Internet-enabled toasters, fitness watches and even toothbrushes are available with high-tech features that offer an improved user experience. However, these devices can also be misused and attacked. Misuse of these devices has the potential to bring the internet to its knees."


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A feisty new hour about facing the future named after my fourth favouriteHot Chip song (and a beautby Phoebe Bridgers).
Mock the Week, Live at The Apollo, As Yet Untitled, Live from The BBC and Fighting Talk.
Last year, John Hastings was hit by a car and broke his arm. He then became homeless (his choice) with a long distancegirlfriend (her choice) and now has a lot of thoughts on pigeons and bicycles (your choice). A tale of displacement, death and denial (don't worry, there are jokes too).
Comedy Central, BBC Seann Walsh's Late NightComedy Spectacular.
***** (Mirror). ***** (BroadwayBaby.com). **** (Fest). **** (Herald). **** (ThreeWeeks). **** (Melbourne Herald Sun).


There are many photo studios in Singapore that will provide your best photos for passport requirement. One such studio that brings affordability to the masses with fast and reliable Quick snap Digital Passport Photography is Instant Glamour. This shop is ideal for CV photos, Driving licenses, ICs, name cards, Travel VISAs, Company Cards, Corporate Profiles, Professional Photos, Resume Photos and Student Passes.


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MIGRANT LIFE STORY / JAPAN
23 Mar MIGRANT LIFE STORY / JAPAN
Jasmine (fictitious name), 50 years old, a single parent divorced from a Japanese man, has two children. The elder is a girl 16 years old, in the 4th year of junior high school, and the younger a boy 13 years old, a grade 6 student; both are graduating this coming April, 2020.
Jasmine is a native of Pampanga City, Philippines. She was the third child in the family. She decided to come to Japan because she broke up with her long-time boyfriend. She applied as a "Talent Entertainer", obtained a tourist visa for 3 months and renewed it for another 3 months. When it expired, she needed to go back to the Philippines because Japan would not allow her to renew her visa.
After two months in the Philippines she re-applied to her talent agency, but her visa was denied by immigration. She begged the agency, promising to accept a 50% reduction in her salary if they would help her return to Japan. Her agency suggested that if she really wanted to go back to Japan, she should use a different name, as that would make it easier to process the papers; she agreed to that arrangement. The agency handled the process; immigration approved her working visa for Japan as an entertainer under the falsified name.
When her visa was reaching the date of expiration, the agency advised her to look for a Japanese man to marry or have a "fixed" marriage (marriage for the sole purpose of obtaining immigration benefits), in order to get a permanent visa. In the bar where she was working, she had a regular customer who wanted to marry her, so they got married.
At the beginning they were happy couple, although she realized that her husband was an alcoholic. After they had lived together for almost a year she became pregnant, which made life more difficult because she had to stop working. Her husband always came home drunk; whenever they had an argument, he would hit her. After giving birth to their first child (daughter), Jasmine discovered that her husband was not only an alcoholic but also a drug addict. Often they would quarrel, and he would beat her. Jasmine did not know what to do; she just cried and felt sorry for herself.
When she and her daughter had the opportunity to go on a vacation to the Philippines, Jasmine secretly planned to separate from him, so she bought a one-way ticket. Her husband thought they would stay there for only 2 weeks. After two weeks she didn't return to Japan. Her husband called her repeatedly, telling her to return. After five months her husband went to fetch them, promising not to hurt her again. For the sake of their daughter they reconciled, and together they returned to Japan.
After a few months, her husband fell back into his old vices. She regretted her decision and often just wanted to give up. However, she felt sorry for her daughter, and asked herself what kind future they would have if she were to separate from him. She did not want her child to experience – as she herself had experienced – having a broken family. For the sake of her child's future she stayed, hoping that one day her husband might change.
Time passed, her husband never changed; the domestic violence continued until they had a second child. Then one day, unable to bear it any longer, Jasmine went to the police to seek help. During the interrogation the police discovered that she was using false name. They arrested her and detained her for almost 3 months. The police brought her children to a Child Care Institution while Jasmine was in prison. The immigration officer wanted to deport her, but she refused to leave without her children. Jasmine really fought for her right to take care of her children. She told immigration that she would not leave her children no matter what happened; it was her right as a mother. The government provided her with a lawyer, and the Filipino Community helped her until she obtained a divorce from her husband.
Now Jasmine is an active volunteer in KALAKASAN, an NGO for women's empowerment in which I collaborate.
Sr Dhay Marqueses, aci


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Melissa Barber
After graduating with a degree in European languages, Melissa followed her parents move from Sydney to Orange in 1989. She found herself starting a painting career from the attic of an antique woolshed on their farm. Teaching herself to use oil and gouache, she began to make a living making portraits. With Radio National and Seventies Music for company in the serene rolling hillside, she developed a number of uniquely disparate styles, devoured artistic biographies for sustenance and determined to pursue a career as an artist.
With nowhere to promote her work locally, Melissa moved to Canowindra 60 kms away and opened a gallery and café combined – The Gallery Koolabah Cafe. It was a hit - with cuisine rustique, REAL cakes, and her own paintings hanging in the gallery. Four years later, no longer able to meet the demands of both cooking and painting, the café closed it's doors and reopened as The Melissa Barber Galleries. At the beginning of her career Melissa was an entirely independent, self-taught and self-made artist – hanging her own works in her own gallery. Since then her profile has rocketed. She has been exhibited throughout Australia and the States and hangs in private collections in the UK, Europe and the States.
Now in 2015, a Mother as well as full time artist, Melissa exhibits from the beautifully restored nineteenth century cottage which is her home in Canowindra.
Melissa Barber The Candidate Wanrong
oil on linen 91 x 52 cm $7900
Melissa Barber The Beginning of The End
oil on linen 122 x 122cm $ 9500
Melissa Barber Glisten IX
acrylic on canvas w x h cm $ 4950
Melissa Barber Glisten VII


and I was not ashamed.
As expected, I found this assignment very strange to begin with. The idea of taking words out of a cohesive sentence to create a completely new meaning was really hard for me. I also read the entire original page to begin with, and I think this made the task harder because it was more difficult to isolate the individual words once I had a story associated with them.
I finally decided on the words that I did because they form a twisted, but comprehensible sentence. Although there was a lot of space to be creative, I was also limited by the layout of the page. For example, some of my original plans did not work because the words jumped all over the page and it was impossible to follow. Although my poem is quite basic, I find it quite powerful, and logical to follow.
After deciding on my words, I also found it hard to come up with a picture that complemented the meaning of my new poem. In the end, I decided to focus my picture on the final line of the poem "I will not be ashamed." and tried to capture someone standing tall and proud. I used watercolor paint to create the visual. I haven't really worked with any paints before, so this was a new skill for me, but I really liked it. I can't explain why I chose the colors that I did, or why I chose to splatter the paint. it just looked bare until I added more color, and so I just kept experimenting until I was happy.
Overall, this was a challenging, but enjoyable task.
between her sweater and coat.
There was time, couple of hours, a few minutes to feed her.
I used a page from the short story "Lie Down with Lions". I used lead pencils to create a blackout poem and then I went over it with a set of childrens' Crayola brush pens from CVS and water to get a soft watercolor-like effect. I then created a collage with famous stolen paintings and the old illustrations from the book itself.
In looking at the words I saw singular images and word combinations that I liked and I started to pair them together. "morning kept isolated" was one of my favorites that jumped out at me immediately. The next one was the idea of carrying sunlight underneath a coat, and the ending image of someone eating time and letting the minutes and hours feed her. I didn't set out to write this poem based on personal experience, but by letting the words on the page jump out at me in no particular sequence I think I captured a mood that feels familiar. The final product is something that emerged out of a little homesickness, and the fact that I was missing Lake Michigan and the feeling of eating lunch on the beach in the middle of January with friends. Everything looks dead in Chicago in the winter, the only thing that makes the whole scene come alive is the movement of frigid January air. Surreal or abstract art always evokes a feeling in me more than it does a complex message, but it has the potential to be equally powerful.


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Deadline Extended! Renew Membership by April 17
Philadelphia Bar Association members now have until Monday, April 17 to renew and save fifteen dollars by avoiding a late fee.
Renew today and take advantage of our many new member-only benefits including 6 FREE CLE CREDITS and access to high-quality, low-cost CLE throughout the year!
Tonight: YLD Running Group Meet-Up
Join the Young Lawyers Division Running Group tonight for a joint run with Young Involved Philadelphia's Running Club. Meet at 6:30 pm at Philadelphia Runner, 1601 Sansom St., Philadelphia. All running levels are welcome and no one runs alone. Drinks afterward at the Field House, 1150 Filbert St., Philadelphia (across from Reading Terminal Market). Contact Catelyn McDonough and Jordan Strokovsky for more details.
2017 Jewish Law Day April 6
The 35th annual Jewish Law Day will occur this year on Thursday, April 6 at 5 p.m. at the Jewish Federation Building at 21st and Arch streets. The event is titled "Examining Modern Questions on Israel, Campus Free Speech, and Boycott Movements through the Lens of Jewish Values." This year's speaker, Professor Eugene Kontorovich, has written and spoken extensively about Israel and about the BDS movement…READ MORE
DIPC Law Student Series: Making the Most of Summer Internship April 10
Hosted by the Diversity in the Profession Committee, Hispanic Bar Association and National Bar Association Women Lawyers Division, Philadelphia Chapter
Get a head start on the summer internship and speak with lawyers about unstated and stated expectations during your summer employment!
Come learn what employers are looking for, and what they may or may not be telling you that could affect your employability…READ MORE
Individual Registration Open for Striking Injustice: The Bar Abides Fundraiser April 27
Back by popular demand, the Young Lawyers Division is again hosting its "Striking Injustice: The Bar Abides" fundraiser to benefit the Philadelphia Bar Foundation. Mark your calendars for a fun evening of bowling and beyond…READ MORE
Lyon-Philadelphia Bar Association Relationship 20th Anniversary April 20-22
Join the Philadelphia Bar Association for the Lyon-Philadelphia Bar Association 20th Anniversary Conference & Networking Reception on April 20-22, 2017, a unique networking, educational and cultural gathering celebrating 20 years of the successful "twinning" relationship between the Philadelphia and Lyon bar associations, exemplified by the annual exchange of lawyer interns between the two cities…READ MORE
Chancellor's Forum With Area Law Deans, Moderated by YLD Chair Matt Olesh April 25
The 12,000-member Philadelphia Bar Association will host a panel of deans from six area law schools at a Chancellor's Forum moderated by Young Lawyers Division Chair Matthew S. Olesh on Tuesday, April 25, 2017 from 4 - 5:30 p.m…READ MORE
April Compliance Month is Here!
FREE Philadelphia Bar Association CLE April 17
CLE - Litigation Lessons From the VW Emissions Scandal
Second FREE CLE of 2017 for Philadelphia Bar Association Members in good standing.
Hosted by the Professional Responsibility Committee, the Business Law Section's Business Litigation Committee and the Young Lawyers Division
What ethics and practical lessons can be learned from this case?
The Volkswagen emissions cheating scandal went as far as the in-house legal department. The pitfalls encountered by counsel there confront all litigators…READ MORE
CLE - Executive Orders At-A-Glance April 4
Hosted by the Young Lawyers Division and the Diversity in the Profession Committee
An executive order is a signed, written, and published directive from the President of the United States that manages operations of the federal government. But what is it and what isn't it?
Since January 20, 2017, President Trump has enacted 17 executive orders. While these orders have varied in content from succession within the Department of Justice to the review of the Clean Water Rule, the President's two orders concerning immigration have garnered particular interest…READ MORE
CLE - The Forensic Fruits of a Labor (& Employment) Client April 5
Hosted by the Cybersecurity Committee of the Business Law Section
Digital forensics came about nearly twenty-five years ago as society moved into a digital age. Since that time, the field has greatly matured through evolving technology. With the advent of laptops, smart phones, dense storage systems, GPS, social media networks and the Internet of Things, digital forensics has continually reinvented its tools and
techniques to remain on the cutting edge of technological advances…READ MORE
CLE - Ethical Implications of Elder Investment Fraud & Finance April 6
Co-hosted by the Pennsylvania Department of Banking and Securities, American Bar Association Commission on Law and Aging, Investor Protection Trust, Investor Protection Institute, the First Judicial District of Pennsylvania and Philadelphia Bar Association
Elder Investment Fraud and Financial Exploitation (EIFFE): Ethical Traps for Lawyers and Navigating the Challenges of Diminished Financial Capacity
As demonstrated by the sensational Brooke Astor case and other less notorious examples, a lawyer who is ignorant of elder investment fraud and financial exploitation (EIFFE) and of the signs of diminished financial capacity may fail to protect the client from harm or unwittingly participate in the client's victimization…READ MORE
CLE - Termination Following a Work Injury April 7
Following an on-the-job injury, there are many aspects of the relationship between the employer and employee that suddenly change. In this CLE program, hosted by the Workers' Compensation Section, claimant and defense counsel will examine issues to consider regarding termination from employment following a work injury…READ MORE
Tonight: HBAPA In-House Counsel Panel April 4
Please join the Hispanic Bar Association of Pennsylvania on April 4 at 6 p.m. for a discussion with in-house counsel concerning the path to securing an in-house position, the benefits and challenges of the job, and successful networking and business development strategies. This is a free event…READ MORE
Reception and CLE Sponsored by The Lawyers' Club of Philadelphia May 15
The reception on May 15, 2017 will be attended by the judges of the Philadelphia Court of Common Pleas and the Philadelphia Municipal Court. Hon. Idee Fox will be honored at the reception for her service to the Philadelphia Court system for her work in both Family Court and in the Trial Court Civil Division…READ MORE
Pennsylvanians for Modern Courts Young Friends Committee
Pennsylvanians for Modern Courts (PMC) is proud to announce its new Young Friends Committee: an advisory group of young professionals helping PMC to educate Pennsylvania's citizens about the judicial system and to find common sense solutions for modernizing the Commonwealth's judicial system. PMC is a statewide nonprofit, nonpartisan organization that also advocates for equal access to justice and greater judicial independence. For more information…READ MORE
New Member Benefits from 1-800-GO-ANSWER!, Orangetheory Fitness, PAR-Recycle Works, Office Depot, Lenovo, the Philadelphia Business Journal and More
Visit Member Benefits for full details on all exclusive member benefits of the Philadelphia Bar Association.


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Townsend reveals reason he joined Palace and how it became 'home'
Speaking with Premier League Productions last week, Andros Townsend opened up on his experiences as a youngster with Tottenham Hotspur, revealed some of the key reasons behind joining Crystal Palace and explained why the club can now be called 'home'.
Typically honest, Townsend recalled the story behind his first major experience of football's unpredictable nature. With a smile, the winger explained:
Wilf Zaha and Andros Townsend are key Fantasy Premier League midfield choices from Crystal Palace
"Within a couple months, I'd made my debut for Tottenham in the FA Cup v Charlton, scored, got Man of the Match, went on loan to Watford, didn't play and got sent back after three weeks because I wasn't integrating with the group well!
"That just shows you, in a month period, how you can have the biggest high of scoring for your boyhood club and then getting sent back from a loan a month later. Football for me - not only for me, but for any footballer who makes it as a professional – is full of ups and downs, and that was a brief example of one of them.
"Maybe as a youngster when you do make your debut for your club, your parent club, maybe you get carried away, maybe think you've made it and then need a little reality check and I got that at Watford. It gave me the inspiration to go back to Spurs and knuckle down in training.
"I then went to Millwall and had a successful end to the season. You need reality checks every now and then to keep you motivated."
Townsend's early years are often cited as one of the most successful examples of the loan system, with the now-29-year-old's nine spells leading to him becoming a regular for Spurs and earning 13 England caps.
Today he reflects on a tough, educational period, but says he remembers those founding years fondly:
"It was all a part of the process. Every loan I went on, there was a reason to it. It was a stepping stone from the last one and the long-term goal was of course to play in the first-team at Spurs, which I accomplished.
"I look on each loan with fond memories, I learnt a lot from each loan – whether it be successful or unsuccessful. They made the player [I am] and got me to where I am today."
Where he is today, of course, is Crystal Palace, with Townsend joining the Eagles over four years ago. He reflected on that July 2016 move to explain the inspiration behind it, revealing how Wilfried Zaha and Yannick Bolasie played a part:
"I remember at the time thinking of the wingers they already had: Wilf Zaha and Yannick Bolasie, seeing how they'd progressed at Palace, seeing how much the fans loved them, seeing how the manager at the time got the best out of them.
"I remember thinking: 'I want that to be me, I want to take my career to another level. If I do what I do best, the fans will take to me and I can make this place my home.'
Andros Townsend reflects on Crystal Palace's Manchester United win and Wilfried Zaha's performance
"[Since then,] there have been a lot of ups and downs. I've had a lot of moments where I've been out of form but I've had moments where I've been in form, scored a lot of goals – some good goals, memorable goals – some memorable performances, big upsets against big sides. I'm in my fifth season now - it's a place I can definitely call home."
Finding 'home' after so long at Spurs and so many moves across the country can't be an easy task, however, and it takes some work to find comfort in the fleeting career of a top-flight player.
"I'm settled with a great group of players here," Townsend continued. "The manager's been a big part of that, having known me from his England days and when he joined Palace he was intent on getting the best out of me; not only offensively but defensively as well. He's turned me into a more all-round player and I thank him for that.
"I've had five seasons here, played 150 games for the club now so it means a lot to me. If there is a time when I do move on, it's still a club I'll be first to look at their results, first to cheer them on.
"But hopefully I've got a good few more years at the club and we can have many more memories together and eventually break into that top 10, which everyone – the players, the staff, the fans – all deserve and all want."
To hear more from Andros on his views of recent matches, life at Palace and more, head over to Palace TV by clicking here or 'Palace TV' within the app!
READ NEXT: Vote for Crystal Palace's W88 Player of the Month
Andros Townsend


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8 health benefits of iced tea
Driving sustainability mainstream
Melissa Breyer MelissaBreyer
© Fedorovacz
From soothing stress to providing weird minerals you didn't know you need, iced tea provides more than just a refreshing boost.
After water, tea is the most frequently consumed beverage in the world. Which make sense; tea goes hand in hand with images of Asia, the United Kingdom, India, Russia. But how about here in the old United States of America? It might not seem like we have a booming tea culture, but the fact is that on any given day, more than half of the American population drinks tea. But here's the twist: 85 percent of that tea is served on the rocks.
While heavily sweetened iced tea can't really be considered a health food, iced tea in general is a super salubrious quaff. Regardless of the temperature it is served at, tea is chock full of good things. There has been much research done, and compelling conclusions that tea can reduce the risk of heart disease, and possibly even help prevent a number of others. In warmer weather, having your tea iced is a great way to reap the benefits all year. And not only that, if you use loose leaf tea to brew your own, it's a virtually zero-waste beverage; no cans, no bottles, hurray.
Whether black, green, white or oolong – all of which come from the same plant, just processed differently – all teas do a body good. Here are a few of the ways in which they do so (with the caveat that you aren't drinking tea swimming in sugar).
1. Keeps you hydrated
Dehydration sucks, so to speak. Hydration is good. The Harvard School of Public Health lists tea as a great source of hydration. Despite the common myth that caffeine dehydrates the body, there is ample evidence that such is not the case.
2. Boosts your antioxidants
Everything is all about the antioxidants these days, we can't seem to escape the heaping of accolades on these plant compounds that fight cell-damaging free radicals in the body. But if they really prove to be as beneficial as science seems to think they are, then we should be scarfing them down as frequently as possible. And on that note, by some accounts, tea has about eight to 10 times the polyphenol antioxidants found in fruits and vegetables.
3. Offers a superior swap for sugary soda
A 12-ounce can of regular cola contains 39 grams of total sugar, which is about 9 1/2 teaspoons of sugar and 140 calories. Twelve ounces of unsweetened iced tea has 0 teaspoons of sugar and 2 calories.
4. May help your teeth
Some research has shown that drinking tea may help prevent tooth loss; tea changes the pH in your mouth, which may prevent cavities. At the very least, it appears not to harm tooth enamel like some beverages do.
5. Could fight cancer
The Tea Association of the USA explains that more than 3,000 published research studies exist that evaluate the role tea and tea compounds, such as epigallocatechin gallate (EGCG), may play in cancers of various sites. The effects apply to a number of different cancers and are linked to varying degrees of significant success.
6. Provides a surprise source of manganese
OK so maybe you don't go around wondering how you can get more manganese in your diet, but hey, it can't hurt. An 8-ounce glass of brewed black iced tea provides 520 micrograms of manganese, which is 35 percent of the recommended daily intake for women and 23 percent for men. According to SF Gate, manganese promotes healthy wound healing, helps maintain the strength of your bones and supports your metabolism.
7. Chills the nerves
A British study found that people who drank tea were able to de-stress more quickly than those who didn't. As well, during the study the tea drinkers – who drank black tea four times a day for six weeks – had lower levels of the stress hormone cortisol in their blood after a stressful event, compared with a control group who drank a placebo.
8. Helps your heart
"There's a lot of literature out there on tea and heart health," says Anna Ardine, clinical nutrition manager at Magee-Womens Hospital of the University of Pittsburgh Medical Center. "This is a health effect for which there is the strongest evidence."
In fact, reports Today.com, a comprehensive review study found a nearly 20 percent reduction in the risk of heart attack and a 35 percent reduced risk of stroke among those who drank one to three cups of green tea daily. "Those who drank four or more cups of green tea daily had a 32 percent reduction in the risk of having a heart attack and lower levels of LDL cholesterol."
You can make iced tea by brewing tea traditionally and then adding ice or allowing it to cool, or you can make sun tea. You can use any type of true tea – or herb tea. You can toss in citrus, fruits, herbs or spices when you steep it for additional flavor. Go crazy! Mix things up; add lemon, mint and ginger to black tea; peaches and lime to white tea; raspberries and orange slices go beautifully with Earl Gray. Have a tea free-for-all, have fun ... and reap the many benefits along the way.
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