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japan golf course rankings
Golfers' Choice: Best of Virginia golf courses. Florida golf courses reviewed in 2019: 655 Reviews of Florida golf courses in 2019: 31,496. Best You Can Play, state by state; Top 200 Classic Courses; Top 200 Modern Courses; Top private courses, state by state; Top 30 Campus Courses; Top 50 Casino Courses; Top 200 Resort Golf Courses; Top 200 Residential Courses; Top 50 Mexico & Caribbean Courses It is the second richest women's golf tour in the world. Japan factory will letter your name or Logo etc just for you!! Ranked 17th in the QS University Rankings: Asia 2016, Osaka University is the sixth oldest university in Japan, having originally been founded in 1724. Golf courses that participate in the USGA Handicap System are rated for each set of tees at their course (front tees, middle tees and back tees, for example). 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(For courses with a number preceding the (m) or (c), that is where the course ranks on Golfweek's Best lists for top 200 modern and classic courses in the U.S.) Click to see the 2019 best golf courses in Illinois. 100. The best public golf courses in Alabama that you can play based on your reviews. Each spring, we publish the three lists that are the foundation of our course-ratings program: Golfweek's Best Classic Courses, Golfweek's Best Modern Courses (below) and Golfweek's Best Courses You Can Play.. The best public golf courses in Illinois that you can play based on your reviews. Report Reply. The top 60 available golfers from last season's FedExCup standings, 10 of the best golfers from the Japan Golf Tour and eight sponsor exemptions comprise the 78-man field participating for the $9.75 million prize purse.. Rory McIlroy and Tiger Woods make their 2019-20 season debuts … SOUTH AMERICA Argentina (340 courses) (ranking by Golf Digest affiliate magazine in Argentina) 1.) 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Japan Golf Tour scores, latest results, rankings, player scorecards. In the wake of the release of GOLF's U.S. Top 100 Courses list, a series of my own personal course rankings came to me, as if in a vision. Japan only golf products are considered the best in the world. Click to see the 2019 best golf courses in Tennessee. The members of our course-ratings panel continually evaluate courses and rate them based on our 10 criteria. To accompany our biennial World 100 Greatest Courses list, Golf Digest also publishes a ranking of the best golf courses in every country. ... Japan (2,450 courses) (Top-10 ranking based on World 100 balloting. Our site has japanese second hand golf clubs. For every great course that made GOLF's 2020-21 ranking of the Top 100 Courses in the U.S., dozens of more must-plays were left on the outside … Click here to review a golf course, whether it's your first or your 100th. Then each course is ranked against other courses in its state to produce the final rankings. W e are thrilled by the fact that the main national and international golf course rankings . 63 Tokyo Golf Club (a 1939 layout back on the ranking after a two-year ... C.H. Qualification. Chiba, Japan, and Accordia Golf Narashino Country Club hosts the inaugural ZOZO Championship. shopping cart | Golf Japan - Pro Golf Japan on fujibuy.com : Jack bunny bag for enjoy golfers Embroider your own name. Submit Pending. Follow Japan Golf Tour leaderboard on FlashScore.com. Example: 96.3 Slope Rating® An indication of the relative difficulty of a golf course for players who are not scratch players compared to players who are scratch players.The lowest Slope Rating is 55 and the highest is 155. This allows golf brands to invest in new technologies and testing with the aim to produce golf clubs that actually improve your game with increased distance and accuracy. Golfers' Choice. Golfers' Choice: Best of Virginia golf courses. The origins of golf may be deeply rooted in Europe, but that doesn't mean you won't find some ultra-elite courses to play while you're traveling throughout Asia. The 63rd best university in the world according to the QS World University Rankings® 2018, the Japanese university also …
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2020 japan golf course rankings


German PV equipment manufacturer Singulus has announced a reduction to its financial forecasting for the full year 2017. The company cites delays in a large-scale project for a China-based client as the primary reason for the reduction.
Just a few days after revealing that it expects to post an overall loss for 2017, Singulus has announced a reduction to its expected revenue for the year. The company now expects to see turnover in the range of €90 to 100 million, and an EBIT result between +€2 million and -€3 million.
Singulus was keen to stress that the new figures still represent a significant increase over the previous year, when revenue amounted to €68.8 million. Previously, the company had predicted that this would double, on the assumption that the majority of existing supply contracts could be completed on schedule.
A Chinese customer which had placed a large order for CIGS production equipment from Singulus notified the company that outstanding payments would take place at the end of the year. This meant that the start of construction of the fab would be delayed, and the work will not begin in time contribute to 2017 revenue figures. Lack of further sales also affected the result, however Singulus still hopes to hang on to a positive EBIT for the current year, after posting +€1.1 million for the first half of the year.
Despite the forecast reduction, Singulus remains bullish about the prospects for its solar division. The company states that it expects benefit from a protracted investment cycle for CIGS thin-film production.


It is "official", galilee man (Carlos Goldberg) completed his thru-hike on July 10th, not sure if he beat the previous record or not. You can find his last post on Trailjournals. Congrats and Way to go Carlos!!
excellent but wonder if he enjoyed it.
There's a myth in hiking circles that one must "take their time" to properly enjoy a hike, as if there's only one way to hike -- that's bunk. Some enjoy the feeling they get from pushing themselves. Who has the right to question how someone decides to hike their hike.
He enjoyed it and now has fond memories that he can enjoy anytime.
You go Galilee Man! That's insanely impressive. And anyone who read a few entries in his TJ would know that he obviously enjoyed himself. Some people actually like pushing themselves!
8 days to hike all of Maine? Wow.
Soooo. . . he told you this personally?? . . .
There is no reality, but my own reality; with this certainty I sore above the abyss of uncertainty. Therefore I know the kitty cat is alive and well.
Read the final pages of his journal. The guy tells of the joy of having tested the limits of his body. It's clear he missed most of the things most people enjoy about a thru hike. His hike was obsessed with making miles. His greatest recorded joy was finally getting to sleep each night.
I remember reading something from one of those who competed to be the fastest to complete a supported hike. He told of still having nightmares two years later after his ordeal.
It is also clear that he got to experience a great many things that most people don't get to enjoy on their thru hike. Galilee Man hiked it his way. Good for him.
281 miles in 8 days, or an average of 35 miles per day. In Maine. Roots, rocks, and hills.


text:
\section{Introduction}
\label{Intro}

Since the first detection of gravitational waves (GW) by the advanced Laser Interferometer Gravitational-Wave Observatory (aLIGO), gravitational wave astronomy has moved to the forefront of scientific study~\cite{Abbott:2016blz,Abbott:2016nmj,Abbott:2017vtc,Abbott:2017gyy,Abbott:2017oio,TheLIGOScientific:2017qsa}. These observations have confirmed the existence of gravitational radiation emanating from coalescing compact binaries. The GWs emitted depend sensitively on the orbital evolution of such binaries, and thus, their observation is a prime target for new tests in the \textit{extreme gravity} regime, where the gravitational interaction is simultaneously strong, dynamical and non-linear.

Einstein-\AE{}ther theory (\AE{})~\cite{Jacobson:2000xp} is an ideal model to test with GWs because it encompasses one of the most general ways to break one of General Relativity's (GR) fundamental pillars: local Lorentz invariance. This symmetry is broken through a unit timelike vector field, called the \ae{}ther field, which couples non-minimally to the metric tensor and induces the activation and propagation of scalar, vectorial, and tensorial metric perturbations in compact binary systems~\cite{Jacobson:2007fh,Foster:2005dk,Hansen:2014ewa}. Recent gravitational wave observations have stringently constrained the speed of propagation of tensor modes~\cite{GBM:2017lvd}, but they could not say anything about the other modes, which are only constrained by Solar System and binary pulsar observations much more weakly~\cite{Jacobson:2007fh,Foster:2005dk,Yagi:2013ava}.

Detailed GW tests of \AE{}-theory require the construction of GW models in the theory, which in turn requires an understanding of coalescing binaries. During the inspiral, their trajectory can be modeled as a sequence of osculating Keplerian orbits, with adiabatically changing semi-major axis and orbital eccentricity, within the post-Newtonian (PN) approximation~\cite{Peters:1963ux,Peters:1964zz}. These adiabatic changes are controlled by the rate at which the binary loses orbital energy and angular momentum. In \AE{}-theory, these rates are modified due to the activation of scalar and vectorial tensor perturbations that propagate away from the binary and carry energy and angular momentum away with them~\cite{Foster:2006az,Foster:2007gr}. This, in turn, modifies the chirping rate of GWs, leaving a signature in the GW phase that could be used to constrain the theory if it is found to be absent from the data.

We here study the energy and the angular momentum loss rate of a binary system in \AE{}-theory to, for the first time, derive the rate at which the semi-major axis and the orbital eccentricity decays due to GW emission. We first compute the GW, stress-energy pseudo-tensor (SET) by expanding the field equations to second order in perturbations about a flat background, a method developed by Isaacson~\cite{Isaacson:1967zz,Isaacson:1968zza}. We then use this SET to compute the energy and the angular momentum flux carried by all propagating modes in terms of derivatives of these fields~\cite{Landau:1982dva}. With this at hand, we use a multipolar expansion of the fields to calculate these fluxes in terms of derivatives of multipole moments. Lastly, we use a Keplerian parametrization to present the energy and angular momentum flux as a function of the orbital parameters of the binary. In doing so, we verify the energy flux calculations of~\cite{Yagi:2013ava}, extending them to include the angular momentum flux for the first time. This last result allows us to calculate the rate of decay of the semi-major axis and the orbital eccentricity of the binary.

We find that generically the semi-major axis and the eccentricity decay rate is faster in \AE{}-theory than in GR when dipole emission is present. Figure~\ref*{fig:changes} shows these evolutions for different choices of the $c_{14}$ combination of coupling constants of the theory. All other coupling constants are chosen such that all propagating modes travel at the speed of light, thus satisfying stability and Cherenkov constraints~\cite{Elliott:2005va}, and leaving $c_{14}$ as the only free parameter of the theory that allows us to continuously approach the GR limit~\cite{Barausse:2015frm}. Observe that the evolution of the semi-major axis and the orbital eccentricity becomes faster than in GR (the $c_{14}=0$ case) as the combination of coupling constants $c_{14}$ is increased. Such an increased rate of decay will imprint onto the chirping rate of the emitted GWs, which could be constrained in the future with GW observations.
\begin{figure}
	\centering
	\vspace{0.4cm}
	\includegraphics[width=0.49\textwidth]{cPlotFinal.eps}
	\caption{Temporal evolution of the semi-major axis (a) and the orbital eccentricity (e) of a 1.4$M_\odot$-2$M_\odot$ neutron star binary due to the modified decay rates of the binary's orbital energy and angular momentum. To construct this figure, we modeled the sensitivities with the weak-field expansion of~\cite{Foster:2006az,Yagi:2013ava}, and we used an initial orbital frequency of 10 Hz and an initial orbital eccentricity of 0.9. Observe that the semi-major axis and the orbital eccentricity decay faster than in GR. }
	\label{fig:changes}
\end{figure}

The structure of this paper is as follows.
Section~\ref{sec:EinsteinAether} presents the basics of \AE{}-theory, including how we decomposes the fields of the theory into different propagation modes (Sec.~\ref{sec:FieldDecompositions}).
Section~\ref{sec:SETandLDOT} explains how to derive the SET and how to calculate the angular momentum loss rate.
Section~\ref{sec:BinarySection-AE} specializes the previous results to a binary system in a Keplerian parametrization, calculating the rate of semi-major axis and orbital eccentricity decay.
Section~\ref{sec:Conclusions} concludes and discusses future implications.
In the remainder of this paper, we use the standard $\left(-,+,+,+\right)$ metric signature as described in~\cite{Misner:1974qy}, as well as units in which $c=1$.

\section{Einstein-\AE{}ther Theory}
\label{sec:EinsteinAether}
We begin with a brief introduction to \AE{}-theory, which was developed by Jacobson and Mattingly in 2001 by coupling a Lorentz violating vector field to GR~\cite{Jacobson:2000xp}.  We here follow mostly the presentation~\cite{Foster:2006az}, where the full action of the theory can be written as a sum of a gravitational term and a matter term
\begin{equation}
\label{eq:full-action}
S = S_{\AE{}} + \sum_{A} S_{A}\,,
\end{equation}
for $A$ bodies in the system.

\subsection{Gravitational Action}

The gravitational action in $\AE$-theory is
\begin{align}
\label{eq:EA_Action}
S_{\AE{}} &= \frac{1}{16 \pi G_{\AE}} \int d^4x \sqrt{-g}\left(R \right. \nonumber \\
&\left. - {K^{\alpha \beta}}_{\gamma \epsilon} \, \nabla_\alpha u^\gamma \nabla_\beta u^\epsilon + \lambda \left(u^\alpha u_\alpha +1\right)\right)\,,
\end{align}
where
\begin{align}
\label{eq:EA_Keqn}
{K^{\alpha \beta}}_{\gamma \epsilon} = c_1g^{\alpha \beta}g_{\gamma \epsilon}+c_2{\delta^\alpha}_\gamma{\delta^\beta}_\epsilon + c_3{\delta^\alpha}_\epsilon{\delta^\beta}_\gamma - c_4u^\alpha u^\beta g_{\gamma \epsilon}\,,
\end{align}
$R$ is the Ricci tensor associated with the metric $g_{\alpha \beta}$, and $u^\alpha$ is the unit timelike \ae{}ther field constrained via a Lagrange multiplier $\lambda$.  The coupling constants $c_i$ control the various ways in which the \ae{}ther field couples to the metric.  For future convenience, we introduce the following combinations of $c_i$:
\begin{subequations}
	\begin{align}
		c_{\pm} &= c_1 \pm c_3 \,,\\
		c_{14} &= c_1 + c_4 \,,\\
		c_{123} &= c_1 + c_2 + c_3\,.
	\end{align}
\end{subequations}
The term $G_{\AE}$ in Eq.~\eqref{eq:EA_Action} is the modified gravitational constant which is related to the Newtonian one through the relation~\cite{Carroll:2004ai,Yagi:2013ava}
\begin{equation}
	G_N = \frac{2}{2-c_{14}}G_{\AE{}}\,.
\end{equation}

\subsection{Matter Action}

For compact objects modeled as effective point-particles, the matter action of the $A^{\text{th}}$ particle is given by~\cite{Foster:2007gr}
\begin{subequations}
	\begin{align}
		\label{eq:MatterAction1}
		S_A &= - \int d\tau_A \, \tilde{m}_A(\gamma_A)\, \\
		\label{eq:MatterAction2}
		&= -\tilde{m}_A \int d\tau_A \left[+\sigma_A\left(\gamma_A+1\right) + \frac{1}{2} \sigma_A^\prime \left(\gamma_A+1\right)^2 + \cdots\right]\,,
	\end{align}
\end{subequations}
where $d\tau_A$ is the proper time along the particle's world-line, $\gamma_A = -u_\alpha v_A^\alpha$ with $v_\alpha$ the particle's four-velocity, and $\tilde{m}_A$ is the bare mass, which is related to the particle's active gravitational mass via
\begin{equation}
\label{eq:ActiveGravMass}
	m_A = \left(1+\sigma_A\right)\tilde{m}_A\,.
\end{equation}
We define the $\sigma_A$ and $\sigma_A^\prime$ charges in Eq.~\eqref{eq:MatterAction2} as
\begin{subequations}
	\begin{align}
		\sigma_A &= - \frac{d\,\ln(\tilde{m}_A)}{d \ln(\gamma_A)}|_{\gamma_A = 1}\,, \\
		\sigma_A^\prime &= \sigma_A + \sigma_A^2 + \frac{d^2\,\ln(\tilde{m}_A)}{d \left(\ln(\gamma_A)\right)}|_{\gamma_A = 1}\,,
	\end{align}
\end{subequations}
and relate them to a rescaled sensitivity parameter by~\cite{Yagi:2013ava}
\begin{equation}
\label{eq:sDef}
	s_A = \frac{\sigma_A}{1+\sigma_A}\,.
\end{equation}

\subsection{Field Equations}
\label{sec:FieldEquations}

The variation of the full action in Eq.~\eqref{eq:full-action} with respect to the metric yields the \AE{} modification to the Einstein equations~\cite{Carroll:2004st}
\begin{equation}
\label{eq:FieldEquations}
	G_{\alpha \beta} - S_{\alpha \beta} = 8 \pi \, T_{\alpha \beta}\,,
\end{equation}
where $G_{\alpha \beta}$ is the Einstein tensor, and $S_{\alpha \beta}$ is given by
\begin{align}
\label{eq:S_Tensor}
S_{\alpha \beta} &= \nabla_\gamma \left({K^\gamma}_{(\alpha} u_{\beta)} + K_{(\alpha \beta)} u^\gamma - {K_{(\alpha}}^\gamma u_{\beta)}\right) \nonumber \\
& + c_1 \left(\nabla_\alpha u_\gamma \, \nabla_\beta u^\gamma - \nabla_\gamma u_\alpha \, \nabla^\gamma u_\beta\right) \nonumber \\
& + c_4 \left(u^\gamma  u^\delta \, \nabla_\gamma u_\alpha \, \nabla_\delta u_\beta\right) + \lambda \, u_\alpha u_\beta \nonumber \\
& - \frac{1}{2}g_{\alpha \beta}\left({K^\gamma}_\delta \, \nabla_\gamma u^\delta\right)\,.
\end{align}
with the contracted $K$-tensor
\begin{equation}
\label{eq:Contracted_K}
{K^\alpha}_\gamma = {K^{\alpha \beta}}_{\gamma \delta} \nabla_\beta u^\delta\,.
\end{equation}

The matter stress-energy tensor $T_{\alpha \beta}$ is defined via
\begin{equation}
	\label{eq:MatterSET}
	T_{\alpha \beta} = - \frac{2}{\sqrt{-g}}\frac{\partial S_m}{\partial g^{\alpha \beta}}\,,
\end{equation}
which can be calculated through the matter action in Eq.~\eqref{eq:MatterAction2}:
\begin{align}
	T^{\alpha \beta} &= \sum_A \tilde{m}_A \tilde{\delta}_A \left[\left(1+\sigma_A-\frac{1}{2}\sigma_A^\prime\left(\gamma_A^2-1\right)\right)v_A^\alpha v_A^\beta \right. \nonumber \\
	&\left. - 2 \left(\sigma_A + \sigma_A^\prime\left(\gamma_A+1\right)\right)u^{(\alpha}v_A^{\beta)}\right]\,,
\end{align}
where
\begin{equation}
	\tilde{\delta}_A = \frac{1}{v_A^0 \sqrt{-g}}\delta^3\left(\vec{x} - \vec{x}_A\right)\,
\end{equation}
is short hand for a renormalized Dirac delta function.

The variation of the full action in Eq.~\eqref{eq:full-action} with respect to the \ae{}ther field $u^\alpha$ yields the \ae{}ther field equation
\begin{equation}
	\label{eq:AEtherFE}
	\nabla_\alpha K^{\alpha \beta} = \lambda\,u^\beta + c_4\left(u^\alpha \,\nabla_\alpha u_\gamma\right) \nabla^\beta u^\gamma + 8\pi G_{\AE{}}\Upsilon^\beta\,,
\end{equation}
where
\begin{equation}
	\Upsilon^\alpha = - \sum_A \tilde{m}_A \tilde{\delta}_A \left[\sigma_A+\sigma_A^\prime \left(\gamma_A+1\right)\right]v_A^\alpha\,.
\end{equation}

In addition to the modified Einstein equations and the \ae{}ther field equation, \AE{}-theory also possesses the timelike constraint
\begin{equation}
\label{eq:TimelikeConstraint}
	g_{\alpha \beta} \, u^\alpha u^\beta = -1\,
\end{equation}
which can be derived by varying the full action in Eq.~\eqref{eq:full-action} with respect to the Lagrange multiplier $\lambda$.  With this we can solve Eq.~\eqref{eq:AEtherFE} for $\lambda$ to find
\begin{equation}
	\lambda = 8\pi G_{\AE{}}\Upsilon_\alpha \, u^\alpha+ c_4\left(u^\beta \nabla_\beta u_\gamma\right)\left(\nabla_\alpha u^\gamma\right)u^\alpha - \nabla_\beta K^\beta{}_\alpha\,u^\alpha\,.
\end{equation}

\subsection{Field Decomposition}
\label{sec:FieldDecompositions}

We conclude this section by carrying out an irreducible decomposition of the perturbations of all the fields about a fixed background, as done for example in~\cite{Foster:2006az}. We begin by expanding the metric
\begin{equation}
	g_{\alpha \beta} = \eta_{\alpha \beta} + h_{\alpha \beta}\,,
\end{equation}
about Minkowski spacetime $\eta_{\alpha \beta}$, with $|h_{\alpha \beta}| \ll |\eta_{\alpha \beta}|$\,, and expanding the \ae{}ther field
\begin{equation}
	u^\alpha = t^\alpha + \omega^\alpha\,,
\end{equation}
about $t^\alpha = (-1,0,0,0)$ a timelike background unit vector, with $|\omega^\alpha| \sim \order{h}$.

Next, we perform two more decompositions. We begin with a $3+1$ decomposition of the metric perturbation about a spatial hypersurface normal to the timelike background vector
\begin{equation}
	h^{\alpha \beta} = t^\alpha t^\beta h_{00} + 2 \mathcal{P}^{(\alpha}_i t^{\beta)} h^{0i} + \mathcal{P}^{\alpha}_i \mathcal{P}^\beta_j h^{ij} \,,
	\end{equation}
where $\mathcal{P}^\alpha_i$ is the background spatial projector
	\begin{equation}
	\label{eq:SpatialProjector}
	\mathcal{P}^{\alpha \beta} = \eta^{\alpha \beta} + t^\alpha t^\beta\,.
\end{equation}
We then further decompose the $3+1$-decomposed metric tensor into transverse and longitudinal pieces
\begin{subequations}
	\label{eq:hDecomp}
	\begin{align}
		h^{0i} &= \gamma^i + \partial^i\,\gamma\,,\\
		h^{ij} &= \phi^{ij}_{\mbox{\tiny TT}} + \frac{1}{2}\mathcal{F}_{ij}\left[f\right] + 2 \partial_{(i} \phi_{j)} + \partial_i \partial_j \phi \,,
	\end{align}
\end{subequations}
where $\phi^{ij}_{\mbox{\tiny TT}}$ is a transverse-traceless spatial tensor, $\mathcal{F}_{ij}[f] \equiv \eta_{ij}\,F - \partial_i \, \partial_j f$ with $F=\partial_k \, \partial^k f$, and $\gamma^{i}$ and $\phi^{i}$ are longitudinal so that $\gamma^i{}_{,i}= \phi^i{}_{,i}=0$. We similarly decompose the \ae{}ther field into transverse and longitudinal modes through
\begin{equation}
	\omega^\alpha = t^\alpha \omega_0 + \mathcal{P}^\alpha_i \left(\nu^i + \partial^i \nu \right) \,, \\
\end{equation}
with $\nu^{i}$ longitudinal so that $\nu^i{}_{,i}=0$.

We can simplify the above expressions somewhat as follows. First, we use the timelike constraint on the \ae{}ther field in Eq.~\eqref{eq:TimelikeConstraint} to find
\begin{equation}
	\omega_0 = -\frac{h_{00}}{2}\,,
\end{equation}
to leading order in the metric perturbation. Next, we use the remaining gauge freedom to set
\begin{subequations}
	\begin{align}
	\partial_i \omega^i &= 0 \,, \\
	\partial_i h^{0i}&= 0 \,, \\
	\partial_i \partial_{[j}{h_{k]}}^i &=0 \,,
	\end{align}
\end{subequations}
which grants us $\nu = \gamma = \phi_i =0$ upon simplification.  Through the evaluation of the field equations given in Eq.~\eqref{eq:FieldEquations} and~\eqref{eq:AEtherFE}, we are able to find relations which exist between the various remaining fields.  By looking at the tensor, vector, and scalar modes of the equations separately, we are able to obtain\footnote{For details on the calculation of these relations see~\cite{Foster:2006az,Saffer:2017ywl}.}
\begin{subequations}
	\begin{align}
		\gamma^i &= -c_{+} \, \nu^i \,, \\
		h_{00} &= \frac{1}{c_{14}}\,F\,,\\
		\partial_i \partial^i \phi &= - \frac{1+c_2}{c_{123}}\,F \,.
	\end{align}
\end{subequations}

With these simplifications at hand, one finds that \AE{}-theory only presents 3 non-vanishing perturbations: $\phi^{\mbox{\tiny TT}}_{ij}$, $\nu^i$, and $F$.  These modes propagate as waves about the background spacetime, satisfying modified wave equations in vacuum of the form
\begin{subequations}
	\begin{align}
		\left(\frac{1}{{\text{v}_{\tiny T}}^2}\partial_0^2 - \partial^i\partial_i\right)\phi^{\mbox{\tiny TT}}_{jk} &= 0\,,\\
		\left(\frac{1}{{\text{v}_{\tiny V}}^2}\partial_0^2 - \partial^i\partial_i\right)\nu^k &= 0\,,\\
		\left(\frac{1}{{\text{v}_{\tiny S}}^2}\partial_0^2 - \partial^i\partial_i\right)F &= 0\,,
	\end{align}
\end{subequations}
where the various propagation speeds are given by
\begin{subequations}
	\begin{align}
	{\text{v}_{\tiny T}}^2 &= \frac{1}{1-c_+}\,, \\
	{\text{v}_{\tiny V}}^2 &= \frac{2\,c_1 - c_+c_-}{2 \, c_{14}\left(1-c_+\right)}\,,\\
	{\text{v}_{\tiny S}}^2 &= \frac{c_{123}\left(2-c_{14}\right)}{c_{14}\left(1-c_+\right)\left(2+3c_2+c_+\right)}\,.
	\end{align}
\end{subequations}
The recent coincident electromagnetic and GW observation of a neutron star merger~\cite{GBM:2017lvd} has placed a severe constraint on ${\text{v}_{\tiny T}}$, effectively forcing $c_{+} \lesssim 10^{-15}$, but this observation places no constraint on ${\text{v}_{\tiny V}}$ or on ${\text{v}_{\tiny S}}$.

\section{Angular Momentum Loss Rate}
\label{sec:SETandLDOT}

In this section, we calculate the angular momentum loss rate in \AE{}-theory. We begin with a generic calculation
that leads to a result in terms of derivatives of the decomposed fields. We then specialize these results to an N-body
system and provide the angular momentum loss in terms of derivatives of the multipole moments of the system.
In both cases, we also present previously-derived expressions for the energy loss for the sake of completeness.

\subsection{General Calculation}

The angular momentum loss can be calculated from~\cite{Landau:1982dva,PW}
\begin{equation}
\dot{L}^i \equiv \frac{1}{2} \epsilon^i{}_{jk}\dot{L}^{jk}\,,
\end{equation}
where $\epsilon^i{}_{jk}$ is the Levi-Civita symbol and where we have defined
\begin{equation}
\label{eq:LdotDefinition}
	\dot{L}^{ij} = -2\oint x^{[i}\,\Theta^{j]k} \, dS_k\,,
\end{equation}
with $\Theta^{ij}$ the spatial components of the GW SET.  The latter can be calculated in \AE{}-theory using the techniques outlined in~\cite{Isaacson:1967zz,Isaacson:1968zza,Saffer:2017ywl} by expanding the field equations to second order in the metric perturbation. The resulting expression cannot be simplified directly through Brill-Hartle averaging~\cite{PhysRev.135.B271}, because the integrand of $\dot{L}^{ij}$ is not $\Theta^{ij}$ but $x^{[i}\,\Theta^{j]k}$; one can of course simplify the latter through Bill-Hartle averaging, and we make use of this henceforth.

The resulting expression can be simplified further through the \emph{shortwave approximation}~\cite{Misner:1974qy,PW}. This assumes the observer is in a region far removed from the source of  radiation, such that the observer's local radius of curvature $R_c$ is much larger than the characteristic wavelength of the gravitational radiation, $\lambda_c$.  This  allows us to use $\lambda_c/R_c \ll 1$ as an expansion parameter and simplify partial spatial derivatives on any field $\Phi$ via
\begin{equation}
	\label{eq:ShortwaveApprox}
	\partial_i \Phi = -\frac{N_i}{\text{v}_\Phi} \partial_\tau \Phi + \bar{\partial}_i \Phi\,,
\end{equation}
where $\text{v}_\Phi$ is the speed of the field in question and the special derivative $\bar{\partial}$ operates only on the spatial (typically radial) part of the field's argument. Therefore, terms proportional to  $(\bar{\partial} \partial_\tau \Phi)/\Phi$ are of $\mathcal{O}(\lambda_c/R_c)$.

When we combine this approximation with the properties of the decomposed fields, we can further simplify the resulting expressions. For instance, we have that
\begin{subequations}
	\label{eq:ShortwaveConstraints}
	\begin{align}
	N_i \phi^{ij}_{\mbox{\tiny TT}} = N_i \nu^i &= 0\,,\\
	N_i \partial_\tau \phi^{ij}_{\mbox{\tiny TT}} = N_i \partial_\tau \nu^i &= 0\,,\\
	N_i \bar{\partial}_j \phi^{ik}_{\mbox{\tiny TT}} &= -\frac{{\phi^{{\mbox{\tiny TT}} k}}_{j}}{r}\,,\\
	\bar{\partial}_i N^j &= \frac{^{(3)}\mathcal{P}^j{}_i}{r}\,,
	\end{align}
\end{subequations}
where $^{(3)}\mathcal{P}_{ij} = \delta_{ij} - N_i\,N_j$ is a projector to a hypersurface orthogonal to the wave's propagation vector $N^{i}$, and $r$ is the distance to the source. Clearly the hypersurface orthogonal to $t^{\alpha}$ need not coincide with that orthogonal to $N^{i}$ and thus $^{(3)}\mathcal{P}_{ij} \neq \mathcal{P}_{ij}$.  We are required to utilize the second term in Eq.~\eqref{eq:ShortwaveApprox} in the $\dot{L}^{ij}$ calculation due to the presence of an extra radial term present in Eq.~\eqref{eq:LdotDefinition}.

After using all of these simplifications, the end result for $\dot{L}^{ij}$ is
\begin{equation}
\dot{L}^{ij} = \dot{L}^{ij}_{(T)} + \dot{L}^{ij}_{(V)} + \dot{L}^{ij}_{(S)}\,,
\end{equation}
with
\begin{subequations}
	\begin{align}
		\label{eq:FinalTensorLdot}
		\dot{L}^{ij}_{(T)} &= -\frac{1}{8 \pi \, {\text{v}_{\tiny T}} \, G_{\AE{}}} \int r^2 \left[\phi_{\mbox{\tiny TT}}^{a[i} \left(\partial_\tau \phi_{\mbox{\tiny TT}}^{j]}{}_a\right) \right. \nonumber \\
		& \left. - \frac{1}{2}\left(\partial_\tau \phi_{ab}^{\mbox{\tiny TT}}\right)x^{[i} \bar{\partial}^{j]}\phi^{ab}_{\mbox{\tiny TT}}\right] d\Omega\,, \\
		\label{eq:FinalVectorLdot}
		\dot{L}^{ij}_{(V)} &= -\frac{(1-c_+)(2c_1-c_+c_-)}{8 \pi \, {\text{v}_{\tiny V}} \,G_{\AE{}}} \int r^2 \left[\nu^{[i} \left(\partial_\tau \nu^{j]}\right) \right. \nonumber \\
		& \left. - \left(\partial_\tau \nu^a\right)x^{[i} \bar{\partial}^{j]}\nu_a\right] d\Omega\,,\\
		\label{eq:FinalScalarLdot}
		\dot{L}^{ij}_{(S)} &= -\frac{\left(2-c_{14}\right)}{32 \pi \, {\text{v}_{\tiny S}} \, c_{14} G_{\AE{}}} \int r^2 \left(\partial_\tau F\right)x^{[i} \bar{\partial}^{j]}F d\Omega \,.
	\end{align}
\end{subequations}
and the analogous result for the angular momentum loss is
\begin{equation}
\dot{L}^{i} = \dot{L}^{i}_{(T)} + \dot{L}^{i}_{(V)} + \dot{L}^{i}_{(S)}\,,
\end{equation}
with
\begin{subequations}
	\label{eq:AngularMomentomVector}
	\begin{align}
	\dot{L}^i_{(T)} &= -\frac{1}{16 \pi \, {\text{v}_{\tiny T}} G_{\AE{}}} \int r^2 \, \epsilon^i{}_{jk} \left[\phi^{ja}_{\mbox{\tiny TT}} \left(\partial_\tau \phi_{\mbox{\tiny TT}}^k{}_a \right) \right. \nonumber \\
	& \left. -\frac{1}{2}x^j \left(\partial^k \phi^{ab}_{\mbox{\tiny TT}}\right) \left(\partial_\tau \phi_{ab}^{\mbox{\tiny TT}}\right)\right] d\Omega \,, \\
	%
	\dot{L}^i_{(V)} &= -\frac{(1-c_+)(2c_1-c_+c_-)}{16 \pi \, {\text{v}_{\tiny V}} G_{\AE{}}} \int r^2 \, \epsilon^i{}_{jk} \left[\nu^j \left(\partial_\tau \nu^k\right) \right. \nonumber \\
	& \left. - x^j \left(\partial^k \nu^a\right)\left(\partial_\tau \nu_a\right)\right] d\Omega\,, \\
	%
	\dot{L}^i_{(S)} & = -\frac{\left(2-c_{14}\right)}{64 \pi \, {\text{v}_{\tiny S}} c_{14} G_{\AE{}}} \int r^2 \, \epsilon^i{}_{jk} \left[x^j \left(\partial^k F\right)\left(\partial_\tau F\right)\right] d\Omega\,.
	\end{align}
\end{subequations}
Notice that the tensor term in Eq.~\eqref{eq:AngularMomentomVector} matches that given in GR except for the prefactor in front of the integral.  The largest difference between these expressions and those in GR is the presence of the vector and scalar modes, which contribute to the total loss of angular momentum of the system. Even if one sets $c_{+} = 0$ to satisfy the tensor propagation bounds of~\cite{GBM:2017lvd}, the vector and scalar contributions still remain.

For completeness, we show the rate of energy loss in terms of our fields\footnote{See~\cite{Foster:2006az,Yagi:2013ava,Saffer:2017ywl} for a calculation on how $\dot{E}$ was obtained.}
\begin{subequations}
	\label{eq:Edot1}
	\begin{align}
		\dot{E}_{(T)} &= -\frac{1}{32\pi \, {\text{v}_{\tiny T}} G_{\AE{}}} \int r^2 \left(\partial_\tau\phi^{{\mbox{\tiny TT}}}_{ij}\right) \left(\partial_\tau\phi_{{\mbox{\tiny TT}}}^{ij}\right) d\Omega \,,\\
		\dot{E}_{(V)} &= -\frac{(1+c_+)(2c_1-c_+c_-)}{16\pi \, {\text{v}_{\tiny V}} G_{\AE{}}} \int r^2 \left(\partial_\tau \nu_i\right) \left(\partial_\tau \nu^i\right) d\Omega \,, \\
		\dot{E}_{(S)} &= -\frac{(2-c_{14})}{64\pi \, {\text{v}_{\tiny S}} \,c_{14} \, G_{\AE{}}} \int r^2 \left(\partial_\tau F\right)\left(\partial_\tau F\right) d\Omega \,.
	\end{align}
\end{subequations}
It is a curious occurrence that all factors of our coupling constants are identical in the prefactors for both $\dot{L}^i$ and $\dot{E}$ for their respective modes.  We will make further use of Eq.~\eqref{eq:Edot1} below.

\subsection{Specialization to an N-Body System}
\label{sec:BinarySection}

The solution to the \AE{} field equations for a PN binary system were first calculated in~\cite{Foster:2006az} and found to be
\begin{align}
\label{eq:TensorExpansion}
	\phi^{{\mbox{\tiny TT}}}_{ij} &= \frac{2\,G_{\AE{}}}{r} \, \ddot{Q}^{\mbox{\tiny TT}}_{ij}\left(t-\frac{r}{ {\text{v}_{\tiny T}} }\right)\,,
	\\
\label{eq:VectorExpansion}
	\nu^i &= -\frac{2 G_{\AE{}}}{\left(2\,c_1 - c_+c_-\right)r} \nonumber \\
	& \times \left[\frac{1}{v_V}\left(\frac{c_+}{1-c_+} \, \ddot{Q}^i{}_{j}+\ddot{\mathcal{Q}}^i{}_{j} + \mathcal{V}^i{}_{j}\right)N^j - 2 \Sigma^i\right]^{\mbox{\tiny T}}\,,
	\\
    F &= \frac{2\,c_{14} \, G_{\AE{}}}{\left(2 - c_{14}\right)r} \left[3\left(Z-1\right)N^i N^j\ddot{Q}_{ij} + Z\,\ddot{I}^k{}_k \right. \nonumber \\
	& \left. - \frac{1}{c_{14}\,{\text{v}_{\tiny S}}}\left(\ddot{\mathcal{Q}}_{ij} + \frac{1}{3} \,\delta_{ij} \, \ddot{\mathcal{I}}^k{}_k\right)N^iN^j + \frac{2}{c_{14} \, {\text{v}_{\tiny S}}} N^i \,\Sigma_i\right]\,,
\end{align}
where over-head dots stand for partial time derivatives, the superscript T and TT stand for the transverse and the transverse-traceless part (relative to the direction of propagation) of a given object, and we have defined the short-hands
\begin{align}
	Q_{ij} &= I_{ij} - \frac{1}{3}\,\delta_{ij} \, I^k{}_k\,,
	\\
	\mathcal{Q}_{ij} &= \mathcal{I}_{ij} - \frac{1}{3}\,\delta_{ij} \, \mathcal{I}^k{}_k\,.
\end{align}
These shorthands depend on the multipole moments of a system of $A$ bodies
\begin{align}
	I^{ij} &= \sum_A \, m_A x_A^i x^j_A\,,
	\\
	\mathcal{I}^{ij} &= \sum_A \sigma_A\, \tilde{m}_A x_A^i x^j_A\,,
	\\
	\Sigma^i &= - \sum_A \sigma_A \tilde{m}_A \, v^i_A\,,
	\\
	\mathcal{V}^{ij} &= 2 \sum_A \sigma_A \tilde{m}_A \dot{v}_A^{[i}x_A^{j]}\,,
\end{align}
where $x_{A}^{i}$ labels their spatial trajectories and $v^i_A = \dot{x}^i_A$ their orbital velocities,
and we have defined the constants~\cite{Foster:2005dk}
\begin{align}
	Z &= \frac{2\left(1-c_+\right)\left(\alpha_1 - 2\, \alpha_2\right)}{3 \left(2c_+ - c_{14}\right)}
	\\
	\alpha_1 &= - \frac{8\left(c_1 \, c_4 +c_3^2\right)}{2c_1-c_+c_-} \,,
	\\
	\alpha_2 &= \frac{\alpha_1}{2} - \frac{\left(c_1+2c_3-c_4\right)\left(2c_2+c_{123}+c_{14}\right)}{c_{123}\left(2-c_{14}\right)}\,.
\end{align}
All expressions here are to be evaluated at the retarded time $t-r/v$, where $v$ is to be replaced with the propagation velocity of the corresponding mode.

With this at hand, we may utilize the Brill-Hartle averaging scheme~\cite{PhysRev.135.B271} and write the angular momentum loss rate as
\begin{widetext}
\begin{align}
\dot{L}^{i}_{(T)} &= -\frac{2 \, G_{\AE{}}}{5 \, {\text{v}_{\tiny T}}} \, \epsilon^i{}_{jk}\avg{\ddot{Q}^{ja} \, \dddot{Q}^k{}_a}\,.
	\\
\label{eq:LdotVector}
	\dot{L}^{i}_{(V)} &= -\frac{4 \, c_{14} \, c_+^2 \, G_{\AE{}}}{5 \left(2\,c_1-c_+c_-\right)^2 {\text{v}_{\tiny V}}} \epsilon^i{}_{jk} \avg{\ddot{Q}^{ja}\dddot{Q}^k{}_a} - \frac{2 \, c_+\,G_{\AE{}}}{5 \left(2c_1 - c_+c_-\right){\text{v}_{\tiny V}}^3} \epsilon^i{}_{jk} \avg{ \ddot{\mathcal{Q}}^{ja}\dddot{Q}^k{}_a +\ddot{Q}^{ja}\dddot{\mathcal{Q}}^k{}_a } \nonumber \\
	& - \frac{2 \left(1-c_+\right)G_{\AE{}}}{5\left(2c_1 - c_+c_-\right) {\text{v}_{\tiny V}}^3} \epsilon^i{}_{jk} \avg{\ddot{\mathcal{Q}}^{ja}\dddot{\mathcal{Q}}^k{}_a} - \frac{2 \left(1-c_+\right)G_{\AE{}}}{3\left(2c_1 - c_+c_-\right) {\text{v}_{\tiny V}}^3} \epsilon^i{}_{jk} \avg{ \mathcal{V}^{ja}\dot{\mathcal{V}}^k{}_a} - \frac{8 \left(1-c_+\right) G_{\AE{}}}{3 \left(2c_1-c_+c_-\right) {\text{v}_{\tiny V}}} \epsilon^i{}_{jk} \avg{\Sigma^j \dot{\Sigma}^k} \,,
	\\
	\label{eq:LdotScalar}
	\dot{L}^i_{(S)} &= -\frac{3 \, c_{14} \, G_{\AE{}}}{5\left(2-c_{14}\right){\text{v}_{\tiny S}}}\left(Z-1\right)^2 \epsilon^i{}_{jk} \avg{\ddot{Q}^{ja}\dddot{Q}^k{}_a} + \frac{2 \, G_{\AE{}}}{5\left(2-c_{14}\right) {\text{v}_{\tiny S}}^3} \left(Z-1\right)\epsilon^i{}_{jk}\avg{ \ddot{\mathcal{Q}}^{ja}\dddot{Q}^k{}_a + \ddot{Q}^{ja} \dddot{\mathcal{Q}}^k{}_a} \nonumber \\
	& - \frac{4 \, G_{\AE{}}}{15 \left(2-c_{14}\right) c_{14} \, {\text{v}_{\tiny S}}^5} \epsilon^i{}_{jk} \avg{\ddot{\mathcal{Q}}^{ja} \dddot{\mathcal{Q}}^k{}_a} - \frac{2 \, G_{\AE{}}}{3 \left(2-c_{14}\right)c_{14} \, {\text{v}_{\tiny S}}^3} \epsilon^i{}_{jk} \avg{\Sigma^j \dot{\Sigma}^k}\,.
	\end{align}
The above expressions can be combined and simplified to write the total angular momentum loss as follows
\begin{align}
\label{eq:LdotFinal}
	\dot{L}^i &= -G_{\AE{}} \, \epsilon^i{}_{jk} \avg{\frac{2\, \mathcal{A}_1 }{5}\, \ddot{Q}^{ja}\dddot{Q}^k{}_a + \frac{\mathcal{A}_2}{5}\left( \ddot{\mathcal{Q}}^{ja}\dddot{Q}^k{}_a + \ddot{Q}^{ja} \dddot{\mathcal{Q}}^k{}_a\right)+ \frac{2 \, \mathcal{A}_3}{5} \, \ddot{\mathcal{Q}}^{ja} \dddot{\mathcal{Q}}^k{}_a + \mathcal{C} \, \Sigma^k \, \dot{\Sigma}^k +2 \, \mathcal{D} \, \mathcal{V}^{ja}\dot{\mathcal{V}}^k{}_a}\,,
\end{align}
\end{widetext}
where we have introduced the new constants
\begin{subequations}
	\label{eq:constants}
	\begin{align}
		\mathcal{A}_1 &\equiv \frac{1}{{\text{v}_{\tiny T}}} + \frac{2 \, c_{14} \, c_+^2}{\left(2c_1 - c_+c_-\right) {\text{v}_{\tiny V}}}+\frac{3\,c_{14}\left(Z-1\right)^2}{2\left(2-c_{14}\right){\text{v}_{\tiny S}}}\,, \\
		\mathcal{A}_2 &\equiv \frac{2 \, c_+}{\left(2c_1-c_+c_-\right){\text{v}_{\tiny V}}^3} - \frac{2\left(Z-1\right)}{\left(2-c_{14}\right){\text{v}_{\tiny S}}^3}\,, \\
		\mathcal{A}_3 &\equiv \frac{1}{2\, c_{14} \, {\text{v}_{\tiny V}}^5} + \frac{2}{3\,c_{14}\left(2-c_{14}\right){\text{v}_{\tiny S}}^5}\,, \\
		\mathcal{C} &\equiv \frac{4}{3\,c_{14} (2-c_{14}){\text{v}_{\tiny S}}^3} + \frac{4}{3\,c_{14}\,{\text{v}_{\tiny V}}^3}\,, \\
		\mathcal{D} &\equiv \frac{1}{6 \, c_{14} \, {\text{v}_{\tiny V}}^5}\,.
	\end{align}
\end{subequations}
The first term in the $\mathcal{A}_1$ quantity represents the GR term (with the modified propagation velocity).  All other terms lead to deviations away from GR due to contributions of the \ae{}ther field.  As with the discussion above, in the limit $c_+ \to 0$ the contributions of the additional modes of propagation persist.

For completeness, we also present here the energy loss for an N-Body system, computed e.g. in~\cite{Yagi:2013ava}
\begin{align}
\label{eq:Edot2}
	\dot{E} &= - G_{\AE{}}\avg{\frac{\mathcal{A}_1}{5}\, \dddot{Q}^{ij} \dddot{Q}_{ij} + \frac{\mathcal{A}_2}{5} \, \dddot{\mathcal{Q}}^{ij}\dddot{Q}_{ij} + \frac{\mathcal{A}_3}{5} \, \dddot{\mathcal{Q}}^{ij} \dddot{\mathcal{Q}}_{ij} \right. \nonumber \\
	& \left. + \, \mathcal{B}_1 \dddot{I} \dddot{I} + \mathcal{B}_2 \dddot{\mathcal{I}} \dddot{I} + \mathcal{B}_3 \dddot{\mathcal{I}}\dddot{\mathcal{I}} + \mathcal{C} \dot{\Sigma}^i \dot{\Sigma}_i + \mathcal{D} \dot{\mathcal{V}}^{ij}\dot{\mathcal{V}}_{ij}}\,,
\end{align}
where
\begin{subequations}
	\begin{align}
		\mathcal{B}_1 &\equiv \frac{c_{14} \, Z^2}{4\,(2-c_{14})\, {\text{v}_{\tiny S}}}\,, \\
		\mathcal{B}_2 &\equiv \frac{Z}{3\,(c_{14}-2) {\text{v}_{\tiny S}}^3}\,,\\
		\mathcal{B}_3 &\equiv \frac{1}{9\,c_{14}\,(2-c_{14}){\text{v}_{\tiny S}}^5}\,.
	\end{align}
\end{subequations}
This result is important for use in the following section.  As with the $\dot{L}^i$ term, the deviations away from the GR result for $\dot{E}$ are due to the presence of the alternative modes whose velocities are unbounded.

\section{Binary Dynamics in \AE{}-theory}
\label{sec:BinarySection-AE}

We now specialize the discussion further by considering a non-spinning binary system with active gravitational masses $m_{1}$ and $m_{2}$ in an elliptical orbit of separation $\vec{r}_{12} = \vec{r}_{1} - \vec{r}_{2}$, as shown schematically in Fig.~\ref{fig:binary}.  Observe that the orbital plane is chosen here to coincide with the $x$-$y$ plane, so that the orbital angular momentum is along the $z$-axis.
\begin{figure}
	\centering
	\vspace{0.3cm}
	\includegraphics[width=0.3\textwidth]{Binary.png}
	\caption{Example of Binary System Used}
	\label{fig:binary}
\end{figure}

Neglecting radiation-reaction, such an orbit can still be described through Keplerian ellipses in \AE{}-theory~\cite{Foster:2007gr,Yagi:2013ava}.
\begin{align}
		r_{12} &= \frac{a(1-e^2)}{1 + e \cos(\varphi)}\,,
\end{align}
where the azimuthal angle evolves according to
\begin{align}
	\dot{\varphi} &= \frac{1}{r_{12}^2}\sqrt{\mathcal{G}\,M\,a\,(1-e^2)}\,,
\end{align}
and where $a$ is the semi-major axis, $e$ is the orbital eccentricity, $M=m_1+m_2$ is the total mass and we have defined
\begin{align}
	\mathcal{G} &\equiv \frac{G_N}{(1+\sigma_1)(1+\sigma_2)}\,.
\end{align}
Without radiation-reaction, the semi-major axis $a$ and the orbital eccentricity $e$ are constants, while $\phi$ is a function of time. The binary's energy and angular momentum are then also constant, and related to the semi-major axis and the eccentricity via
\begin{subequations}
	\label{eq:EandL}
	\begin{align}
		E &= - \frac{\mathcal{G} \, m_1 \,m_2}{2a}\,,\\
		L^2 &= \frac{\mathcal{G} \, m_1^2 \, m_2^2}{M} \, a(1-e^2)\,.
	\end{align}
\end{subequations}

Once we include radiation-reaction, the energy and angular momentum are no longer constant, as we found in the previous section. Instead, for a binary system,  Eqs.~\eqref{eq:Edot2} and~\eqref{eq:LdotFinal} are given by
\begin{align}
\label{eq:Edot3}
	\dot{E} &= - \frac{\mathcal{C} \, G_{\AE{}}^2 \, \mathcal{G}^2\left(2-e^2-e^4\right)S_-^2 \, M^4\, \eta^2 }{2\left(1-e^2\right)^{7/2}a^4} \nonumber \\
	&- \frac{G_{\AE{}} \, \mathcal{G}^3 \, M^5 \, \eta^2}{30 \left(1-e^2\right)^{7/2}a^5} \nonumber \\
	&\times \left[2\left(96+292e^2+37e^4\right)\left(\mathcal{A}_1 + \mathcal{S}\mathcal{A}_2 + \mathcal{S}^2\mathcal{A}_3\right) \nonumber \right. \\
	&\left. + 15e^2\left(4+e^2\right)\left(\mathcal{B}_1 + \mathcal{S}\mathcal{B}_2 + \mathcal{S}^2\mathcal{B}_3\right)\right]\,,
\end{align}
and
\begin{align}
\label{eq:Ldot3}
	\dot{L}^i &= -\frac{\mathcal{C} \, G_{\AE{}} \, \mathcal{G}^{3/2} \, S_-^2 \, M^{7/2} \, \eta^2}{\left(1-e^2\right) a^{5/2}} \nonumber \\
	&- \frac{4\left(8+7e^2\right)G_{\AE{}} \, \mathcal{G}^{5/2} \, M^{9/2}\, \eta^2}{5\left(1-e^2\right)^2 a^{7/2}}\left(\mathcal{A}_1 + \mathcal{S}\mathcal{A}_2 + \mathcal{S}^2\mathcal{A}_3\right)
\end{align}
where we introduced the symmetric mass ratio $\eta=m_1m_2/M^2$, the mass-weighted symmetric sensitivity $\mathcal{S}=m_1s_2/M+m_2s_1/M$, and the anti-symmetric sensitivity $S_-=s_1-s_2$.

The above expressions shown in Eqs.~\eqref{eq:Edot3} and~\eqref{eq:Ldot3} do not contain angle-brackets because we have explicitly carried out the orbit averaging. By the latter, we mean specifically
\begin{equation}
\label{eq:averaging1}
	\avg{X(t)} = \frac{1}{P}\int_0^{P} X(t)\,dt\,,
\end{equation}
for any quantity $X(t)$ with $P$ the orbital period. This integral can of course be rewritten in terms of the orbital angle ($\varphi$ in Fig.~\ref{fig:binary}), as
\begin{equation}
	\avg{X(\varphi)} = \frac{\left(1-e^2\right)^{3/2}}{2\pi} \int_0^{2\pi} \frac{X(\varphi)}{\left(1+e\cos(\varphi)\right)^2}\,d \varphi\,.
\end{equation}
where we have used
\begin{equation}
\frac{d \varphi}{d t} = \sqrt{\frac{G_{\AE{}} \, M}{a^3}} \left(1-e^2\right)^{-3/2} \left(1+e\cos\left(\varphi\right)\right)^2\,.
\end{equation}

We can now combine the above equations with the time derivative of Eq.~\eqref{eq:EandL} to find how the semi-major axis and the orbital eccentricity evolve. We find that
\begin{widetext}
\begin{align}
\label{eq:adot}
	\dot{a} &= -\frac{\mathcal{C}\,G_{\AE{}} \, \mathcal{G} \, S_-^2 \, M^2\,\eta}{a^2} \, \text{h}_1(e)
	- \frac{G_{\AE{}} \, \mathcal{G}^2\,M^3\,\eta}{15\,a^3}\left[2\left(\mathcal{A}_1 + \mathcal{S}\mathcal{A}_2 + \mathcal{S}^2\mathcal{A}_3\right) \text{f}_1(e)
	+ 15\left(\mathcal{B}_1 + \mathcal{S}\mathcal{B}_2 + \mathcal{S}^2\mathcal{B}_3\right) \text{g}_1(e)\right]\,,
	\\
	\label{eq:edot}
	\dot{e} &= -\frac{\mathcal{C} \,G_{\AE{}} \, \mathcal{G} \, S_-^2 M^2 \, \eta}{a^3}\,\text{h}_2(e) - \frac{G_{\AE{}} \, \mathcal{G}^2 \, M^3 \, \eta}{30 \, a^4} \left[2\left(\mathcal{A}_1 + \mathcal{S}\mathcal{A}_2 + \mathcal{S}^2\mathcal{A}_3\right)\text{f}_2(e) + 15\left(\mathcal{B}_1 + \mathcal{S}\mathcal{B}_2 + \mathcal{S}^2\mathcal{B}_3\right) \text{g}_2(e)\right]\,.
\end{align}
\end{widetext}
The above expressions depend on certain enhancement factors that are only functions of eccentricity, namely
\begin{subequations}
	\begin{align}
		\text{f}_1(e) &\equiv \frac{96 + 292 e^2 + 37 e^4}{(1 - e^2)^{7/2}}\,,\\
		\text{g}_1(e) &\equiv \frac{e^2 (4 + e^2)}{(1 - e^2)^{7/2}}\,,\\
		\text{h}_1(e) &\equiv \frac{2+e^2}{(1-e^2)^{5/2}}\,, \\
		%
		\text{f}_2(e) &\equiv  \frac{e\left(304 + 121\,e^2\right)}{(1-e^2)^{5/2}}\,,\\
		\text{g}_2(e) &\equiv \frac{e\left(4+e^2\right)}{(1-e^2)^{5/2}}\,, \\
		\text{h}_2(e) &\equiv \frac{3\,e}{2(1-e^2)^{3/2}} \,,\\
	\end{align}
\end{subequations}
The evolution of the semi-major axis and the orbital eccentricity is clearly faster than in GR due to the dipole term proportional to ${\cal{C}}$.  As was shown earlier, $\mathcal{C}$ is produced by terms that come from the vector and scalar modes of propagation. Therefore, it is these additional propagation modes that are responsible for the contribution to the dipole term in the decay rates, and the latter is thus not affected by bounds on the propagation speed of the tensor mode.

Figure~\ref{fig:changes} shows the temporal evolution of the semi-major axis and the orbital eccentricity for a neutron star binary in the inspiral. This evolution was obtained by numerically solving Eqs.~\eqref{eq:adot} and~\eqref{eq:edot} for a binary with masses $m_{1}=1.365 M_{\odot}$ and $m_{2}=2.040 M_{\odot}$. The sensitivities are modeled through a weak-field expansion of~\cite{Foster:2006az} with stellar radii $R_{1}=12.214$km and $R_{2}=11.966$km and are given by
\begin{equation}
	s_A = \left(\alpha_1 - \frac{2}{3} \, \alpha_2\right)\frac{m_A}{R_A}\,.
\end{equation}
This approximation suffices to roughly model the temporal evolution of the semi-major axis and the orbital eccentricity. A proper GW model in \AE{}-theory, however, ought to employ the strong-field representation of the sensitivities found in~\cite{Yagi:2013ava}.

\section{Conclusion and Future}
\label{sec:Conclusions}

We have here calculated the rate of change of the orbital angular momentum due to GW emission in \AE{}-theory, accounting for all modes of propagation. This calculation, together with the energy flux of~\cite{Foster:2006az,Yagi:2013ava}, allowed us to compute the rate of change of a binary's semi-major axis and its orbital eccentricity. We found that these quantities decay much more rapidly than in GR due to the emission of dipole radiation by the vector and scalar modes of the theory. These modifications persist even when one forces the tensor modes to propagate at the speed of light, thus by-passing the recent GW bounds of~\cite{GBM:2017lvd}.

One could use these results in a variety of ways. One possibility is to construct a leading order GR deviation model for the GWs emitted in the inspiral of eccentric compact binaries. This model could be based on the recent work of~\cite{Moore:2018kvz}, which built a model in GR that is valid for binaries with arbitrary eccentricity. Alternatively, one could work in a small-eccentricity expansion, as suggested in~\cite{Yunes:2009yz}, or in a large-eccentricity expansion, as suggested in~\cite{Loutrel:2017fgu,Loutrel:2014vja}. Such a model could then be used to inspiral a model-independent parameterization of modified GW models, as done for quasi-circular inspirals through the parameterized post-Einsteinian framework~\cite{Yunes:2009ke}. With this at hand, one could use future GW observations by advanced LIGO, or by third generation GW detectors or space-based detectors~\cite{Audley:2017drz}, to place interesting constraints on \AE{}-theory.

Another possibility for future work is to revisit the strong-field sensitivity calculations of~\cite{Yagi:2013ava} and repeat the computation of binary pulsar constraints in light of the recent tensor propagation speed constraints of~\cite{GBM:2017lvd}. The results on the \AE{} constraints found in~\cite{Yagi:2013ava} are not valid any longer because that work made certain assumptions regarding the magnitude of the coupling constants, which is violated by the constraints in~\cite{GBM:2017lvd}. Once this work is repeated, however, one could redo the computation of binary pulsar constraints using not only binaries with very small eccentricity, but also much more eccentric ones. Such an extension would require the use of the angular momentum flux calculated in this paper.

\section{Acknowledgments}
\label{ackno}

N.Y and A.S.~acknowledge support through the NSF CAREER grant PHY-1250636 and NASA grants NNX16AB98G and 80NSSC17M0041.

redpajama_set_name: RedPajamaArXiv


text:
MINOTAURUS – Insolubilis
MINOTAURUS have been active since 1994, delivering a unique mixture of Folk, Metal and an unmistakeable dash of originality. Until today, they could look back on eight releases, each of them displaying clear development factors from one to the next, something that has always been recognised by their growing fan base. The development goes a step further with "Insolubilis", their new album in a new, extended line-up. MINOTAURUS work under the motto "create new and keep the tried and tested", which, considering the band's long history, shows wisdom and farsightedness. It is exactly in the realm of Folk Metal, one in which fans orientate themselves explicitly to bands, credibility in an important asset. In the band's own discography the album, "Insolubilis" is an absolute reference point and is certain to carry the band yet further forwards with giant steps. Like the half man, half bull, mythological creature which gave the band its name, MINOTAURUS is pawing the ground, about to charge.
Their fifth long-player, "Insolubilis" took the band once again to the Empire Studios in Bensheim, with Rolf Munkes. Eleven new songs packed into a varied package, offer an impressive mixture of melodies and subjects. With lots of phantasy and humour the tracks transport the listener along an exciting journey to historical and mythological places, visiting sailors and mermaids, witches and ghosts, heroes, kings, princesses and priests, yes, even the legendary minotaur itself, through graveyards, pirate ships, forests, campfires, army camps, ruins and valleys.
Overall the album is harder and the song-writing is clearly more mature. Besides guitar duels so typical of the band, one hears Celtic harps, tin whistle, Tinwhistle, wooden flutes and even a curtal, the forerunner of the bassoon. The Folk influence has been honed and rounds off the overall impression beautifully. Multivocal song lines as well as several very catchy tracks also belong to the order of the day. With their fifth long player, MINOTAURUS has proved that there is still a lot of potential within them. "Insolubilis" confirms this with no doubt whatsoever.
Preacher Show Me The Way
Only A Dream
Cemeterery
Poison Rose
Shelter Of The Witch
Bonfire Brothers
The Haunted Palace
Insolubilis
Mature, dynamic, heavy: that is the 2016 MINOTAURUS sound!
Produced by Rolf Munkes (Empire, Crematory, ex-Majesty, Tour guitarist for Tony Martin etc…) in the Empire Studios.
Ancient Epic Metal.
High quality back catalogue with excellent reviews.
Band: MINOTAURUS
Release: 11. November 2016
Genre: Ancient Epic Metal
Tags: 2016, Ancient Epic Metal, MINOTAURUS

redpajama_set_name: RedPajamaCommonCrawl


Pesticide-free can be used on areas that come directly into contact with skin.
Natural, safe, odourless, does not stain completely pesticide free.
Oa2ki is a crawling insect control product produced from fossilised diatoms. Diatomaceous earth consists of fossilized remains of diatoms, a type of hard-shelled algae. It is used as a mechanical insecticide in areas where pesticides cannot be used i.e. where animals / livestock are present.
The powder causes loss of moisture by dessication of the insects cuticle and subsequent death. Oa2ki is extremely popular with poultry keepers for the control of red mite, it can also be applied directly to mattresses, bedding and soft furnishings for the control of bed bugs.
Apply dust as required to areas that insects live or frequent.
To treat dogs and cats apply 1-2 grams, depending on the animal size.
Product can be added to bird cages of pet birds as a bird bath.


text:
Play Area Association
A family co-op since 1973
About Our Activities
PAA Neighborhood Surverys
Kids' Enrichment Classes
PAA Class Registration Procedure and Policies
Play And Learn co-op
About Play And Learn (PAL)
PAL Policies
PAL Curriculum
PAL Separation Guidelines
PAL Teacher (Ms. Liz)/ TA (Ms. Aartie)
[Member Area]
The PAA play areas are accessible through the lobby of Payson House, 435 East 70th Street. The play areas are reserved for use only by members and require a key for entry that is given to members annually with their dues payment. For liability reasons, only PAA members are permitted in these play areas at all times.
The Playroom
The Playroom is an indoor play area with a climbing structure and many toys and books. The floor consists of carpeting and soft foam playmats.
Rules for the Playroom:
1) Eating is NOT allowed in the playroom.
2) NO SHOES ON THE MATS.
3) Do not dispose of soiled diapers in the bathroom trashcan. Please take them with you.
Woodchips is an outdoor play area containing a large climbing structure, a water table (with a hose to fill it), a playhouse, and toys such as ride-in cars and toddler basketball hoops. There is also a picnic table and benches. The floor of the "Woodchips" play area presumably used to be covered in woodchips. It now has soft, rubber, outdoor matting but has retained the nickname.
Rules for Woodchips:
1) Keep gates closed and do not block them. They are fire escapes and must be kept free of locks and blockades.
2) Please dispose of any garbage in the trashcans before you leave and replace lids securely.
3) No glass.
4) No dogs.
Guidelines for Parties at Woodchip:
Only 1 party can be reserved per day, and parties cannot be reserved on the same day that PAA parties and community-building activities are planned in the outdoor space, e.g. June Ice Cream Social, August Caffeine and Conversation.
Members may not exclude other children from Woodchips during a party, as Woodchips is a shared space for all our children to enjoy. ***The table at Woodchips will be exclusively reserved for your party with a special sign. Please check with the Payson doormen for a party packet before setting up.
Parties may be reserved for a maximum of 1.5 hours: Mon-Fri from 6pm- 7:30pm; 2 hours Sat-Sun 10:30am – 7:30pm
Parties held in the outdoor PAA play space must be kept to a maximum of 10 children. If members would like to hold a birthday party or celebration with more guests, we suggest you do so at one of the nearby parks or playgrounds, particularly those with picnic tables and bathrooms:
John Jay Park: FDR drive from East 76-78th Streets: picnic tables, fully-equipped playground, water sprinklers, bathrooms.
St. Catherine's Park: 1st Ave between 67th/68th Streets: picnic tables, fully-equipped playground, water sprinklers, bathrooms.
Carl Schurz Park: East End Av To East River, E 84th St To E 90th St: fully-equipped playground, green grass on which to picnic, room to roam or ride scooters / bicycles along the East River, a pair of restrooms.
Arthur Ross Pinetum Playground, Central Park: picnic tables, open space to roam, swings, fairly close to a bathroom.
Billy Johnson Playground, Central Park: East 67th Street and 5th Ave: A picnic table and green grass on which to picnic, giant sandbox and swings, water sprinklers, a giant granite slide, fairly close to a bathroom.
Hecksher Playground, Central Park: 61st-63rd Street, mid park: picnic tables, fully-equipped playground, water sprinklers, bathrooms, and the bonus of Umpire Rock to climb.
PAA members must contact parties@paanyc.org at least 5 days in advance to see if they can reserve a date and time for a birthday party.
The outdoor PAA play space must be cleaned up after the party. Families who violate this rule will be fined $200 per offense in accordance with PAA policy. Woodchips must be cleaned up after parties – all trash should be collected and put into self-supplied trash bags. Once the trash is collected, please notify the front desk and they will ask building staff to bring the garbage to the appropriate place.
If a family asks to have more than two parties/year in Woodchips, the request will be reviewed by the Board as we want to make sure that Woodchips is available to as many PAA members as possible
If you notice any broken toys, structures in need of maintenance, or anyone in blatant disregard of the rules, please contact the Playroom/Woodchips Chair immediately at playroom@paanyc.org.
© 2023 Play Area Association | All rights reserved Contact Us


text:
#TechTop3 – Our top three tech stories of the week
By LondonOctober 10, 2014EU insight
By the London Technology Team
Political parties continue to fight over Communications Data Bill
The unedifying fight between the UK's three main political parties over the abandoned Communications Data Bill has continued this week, with the battle rumbling on throughout the Liberal Democrat Party Conference. This latest round of hostility was triggered last week by the Home Secretary, Theresa May, who launched a scathing attack on her coalition partners during her speech at the Conservative Party Conference, making the incredible claim that the abandonment of the Communications Data Bill had effectively resulted in children's lives being put at risk. Most importantly, May promised that, if elected with a majority, the Conservative Party would re-introduce the Bill. May's insults prompted demands for an apology by the Deputy Prime Minister, Nick Clegg.
As explained by Rowena Mason in the Guardian, this week, speaking at a fringe event at the Liberal Democrat Party Conference in Glasgow, Julian Huppert MP (the Liberal Democrats' Home Affairs Spokesman), stated that the Labour Party is just as likely to re-introduce the Bill as the Conservative Party. The Communications Data Bill, known by many as the Snoopers' Charter, would have required mobile network operators and internet service providers to retain records of users' internet browsing history, internet gaming, mobile messaging, and voice calls for 12 months, and its abandonment in 2013 was welcomed by many civil liberties campaigners.
Furthermore, Huppert pledged that if in Government as part of a coalition, the Lib Dems would once again veto the Communications Data Bill or any similar legislation. This point was reiterated by Clegg in his keynote speech, with the Deputy Prime Minister stating that the "Communications Data Bill was disproportionate, disempowering — we blocked it once and we'd do it again".
Excellent articles on this and last week's news can be found in the Independent and the Guardian.
Online battlegrounds
The last few weeks have seen fierce debate over the UK's role in the coordinated airstrike campaign against Isis targets in Iraq and Syria. However, away from discussions about military solutions, greater prominence has been given to navigating the online battlegrounds of the Isis threat. European security officials, including the Home Office's James Brokenshire MP, convened in Luxembourg to examine options for countering online radicalism. The European Commission had called on major global technology companies to join security ministers from across the continent to discuss how to combat the online threat.
Representatives from Google, Facebook, Twitter and Microsoft were amongst those from industry that attended the high level meeting, tasked with halting the spread of jihadist propaganda and diluting Isis efforts to use social media as a recruitment tool. This is not new; large tech firms have long advised Government's and supra-national bodies on cyber terror threats, but typically on an adhoc basis. However, as The Times' technology correspondent, James Dean, perceptively noted in an article this week, the European Commission's effective codification of this relationship is a reflection of the perceived severity of the Isis threat, and recognition of their skill in spreading their message online.
Cyber-attacks, extremist propaganda and the use of social media to recruit vulnerable young people are simply modern incarnations of age-old tools of war. However – with the recent spate of Isis beheadings in mind – of particular concern is the capacity of the digital sphere to circumvent traditional physical barriers to unwanted content. The new breed of digital tools used by those wishing to spread hate are tremendously efficient and we are yet to develop the digital barriers needed to protect some of the most vulnerable in society from their insidious influence.
A third of children have their own tablets
Ofcom have published new research that one in three children have their own tablet computer. This presents new challenges for parents, politicians and the tech industry as well as reflects wider changes. More kids have tablets, but this is at the expense of TVs, which fewer children have compared to 2009.
With concerns over inappropriate content, it is not surprising to see that 84% of parents surveyed directly supervise their kids online and 82% have set rules for browsing. Over half of respondents also said they use software to mitigate online risks, which comes a year after the major ISPs started offering and majorly marketing free parental controls to their customers and overall, 9/10 parents took some sort of action to mitigate online risks. Away from parental controls, these actions include time limits on things like social media, using anti-virus software and passwords on devices.
Away from content, the tech industry has suffered quite a bit of pressure over bills too. Many 'free' games offer the option to pay for extra content, which has led to some big bills for parents as kids unwittingly bought this content without knowing it was being paid for with real money. Apple and Google, who process the payments, have worked on making this harder to do, but it faced serious pressure from regulators across the world to add in extra barriers. Another issue is so called 'bill-shock' when youngsters go over their data limits, or use 3/4g abroad, not knowing this is substantially more expensive than at home.
Children and technology has always been contentious. When TVs and games consoles become more ubiquitous, campaigners and parent groups were just as worried about the impact on children. What would happen to children's academic performance? Will they go to bed on time, and is it healthy to spend more time inside and not doing any exercise? These are not new concerns, but as tablets become even more popular and affordable, the number of people using them will only grow.
Ofcom's research can be viewed here.
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PI Brussel's Matti Van Hecke nominated as PACE's newest Board member December 12, 2022
PI announces acquisition of its UK business by global marketing & communications agency Clarity October 25, 2022


Everything Lady Serena Parker thought she knew about her own life has just proved a lie. Now, only one man can lead her to the truth: Moonlight Square's most mysterious resident, the enigmatic and solitary Azrael, Duke of Rivenwood. He alone can give her the answers she seeks...but at what price?
When shocking family secrets emerge, they turn Lady Serena Parker's world upside-down, sending the bold, raven-haired beauty on a quest to find answers. Ironically, her search soon points her right across the street, to the home of her most mysterious neighbor in Moonlight Square—the elusive and solitary Azrael, Duke of Rivenwood.


text:
CMT Lands Broadcast Rights for 'Skyville Live' All-Star Concert Specials
Chris Willman
CMT announced Wednesday that it has acquired exclusive broadcast rights for "Skyville Live," an all-star concert series bringing together artists from the rock and pop worlds as well as the country and America that are the cable channel's bread-and-butter.
The Viacom network will premiere the series with the Jan. 19 broadcast of "Skyville Live: Kris Kristofferson & Friends," which has the venerable singer-actor joined by Jason Isbell, Brandy Clark, Lady A and Raul Malo of the Mavericks. Second up on the agenda Feb. 17 will be "Midnight Train to Georgia: Gladys Knight & Guests," with the R&B-pop legend bringing in Martina McBride and Estelle.
Jennifer Nettles to Receive First 'Equal Play Award' From CMT Awards for Women's Advocacy (EXCLUSIVE)
Dennis Hopper's Legendary 'Last Movie' Finally Gets a Soundtrack Album, Five Decades Later, Via Record Store Day
CMT Lands Kenny Chesney, Tim McGraw, Avril Lavigne, Sheryl Crow and Dozens More for Day-Long Benefit Livestream
Among the hour-long specials coming up down the pike as part of the series is a salute to Gregg Allman, including the late frontman of the Allman Brothers Band himself. Allman died in May 2017, so that is a bit of a tipoff to the vintage of the shows, which began airing in 2015 as a digital-only series. Episodes previously aired only on Verizon's Go90 and the Skyville Live website as one-time-only livestream presentations. CMT is editing those longer webcasts down to an hour each and repackaging them for their television debuts, in partnership with Believe Entertainment Group.
"Live music is the heart and soul of CMT and we're so excited to bring this concert series to television," said Margaret Comeaux, VP of production, music & events for CMT. "From Kris Kristofferson, Graham Nash and the late Gregg Allman to Gladys Knight, Emmylou Harris and Cyndi Lauper, 'Skyville Live' showcases some of the greatest names in music, making it an excellent addition to CMT's expansive live music library."
Beyond the Kristofferson, Knight and Allman salutes, "Skyville Live" specials earmarked for later in 2021 include shows featuring Cyndi Lauper, Graham Nash, Emmylou Harris and a salute to Jerry Lee Lewis.
The shows were all captured in a private club-type warehouse setting in Nashville with an intimate audience of about 250, and were the brainchild of Skyville Music co-owner Wally Wilson, who started the all-star jams before cameras were in place and sought to bring the chummy shows to a wide audience.
"Skyville Live" bears at least fleeting resemblance to CMT's flagship music series, "CMT Crossroads," which has country stars joined by their contemporaries from other genres. But "Skyville Line" doesn't have the same genre-crossing high concept — the lineups are only partly anchored by country artists, and some of the specials have stars joined by unlikely guests from disparate other genres while others, like the Kristofferson salute, skew closer to an honoree's core format.
In 2016, the webcasts caught the attention of industry blogger Bob Lefsetz, who lamented the lack of wider distribution for the digital series — "No one's ever heard of it" — and heralded tChris Stapleton's version of "Whipping Post" on the Allman special. Lefsetz enthused, "This is better than any Grammy performance, better than almost all of the Kennedy Center Honors. You get the feeling you're at a rehearsal of people who did not get the memo, who did not hear that all the money is in banking and tech, who think pushing limits based on their talents is everything in life. Screw those Grammy moments, faux greatness that leaves us with the blahs. Rather on "Skyville Live" it's all about focusing on playing as opposed to image, after all music is something you HEAR first and foremost. It's about a great tune, with great musicians locking on to it, all in service to the song."
Use RM35m hall construction allocation for Johor healthcare facilities instead, Kluang MP says
Blue Monday is the third Monday in January and said to be the most depressing day of the year.
Ivory Coast defender Willy Boly conceded a penalty, created a goal, and scored for Wolves in a 3-2 defeat by West Brom at the weekend in the English Premier League.


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These procedures are a predictable way to cover unsightly, sensitive, or exposed root surfaces and to prevent future gum recession. If you are unhappy with the appearance of short unsightly teeth this can be greatly improved by a combination of periodontal procedures by Dr. DiVincenzo and Associates and cosmetic dentistry by your dentist. For more information about cosmetic periodontal surgery or to schedule a consultation appointment, call our office in Jersey City and Bayonne, NJ at Jersey City Office Phone Number 201-216-9191.


On Monday, I found myself in a room of 1,000 fellow Catholics who share a similar mindset. We were many, but, from what one could see, one in our pro-God, pro-family, pro-love, pro-life mentality of heart.
The banquet was a fundraiser for Real Presence Radio, our local Catholic radio station — part of a modern-day treasure of the Catholic world. Every day, this ministry is changing lives. "People are thirsting for the truth," as we were reminded that evening. And it's true.
Our keynote speaker for the evening was Catholic media rock star Teresa Tomeo, award-winning television journalist who left secular media after a profound conversion back to her Catholic faith, and has become a beloved national Catholic radio host. Looking out into the vast crowd, Teresa, who hails from the Detroit area, said ours was the biggest such fundraiser she'd ever keynoted. Impressive for our humble state!
As anyone who listens to Teresa's morning radio show, "Catholic Connection," knows, she loves discussing pro-life issues, especially as they're portrayed in the culture and mainstream media — her former stomping grounds.
Teresa spoke on this topic at a luncheon earlier in the day, too, during her talk, "Bringing America Back to Life," and in that presentation, she broached the topic of a new report by NARAL, an organization known for its abortion-rights clamoring, titled, "The Insidious Power of the Anti-Choice Movement." The report, which details its magnified glance at the pro-life movement (from the outside at least), seems something of a frantic scramble to try to figure out how in the world we've made the gains we have, painting us as sinister and conniving. I patterned my title here after their own choice of words for their report: "The Preposterous Claims of the Anti-Life Movement." Because that is exactly what this report is.
Teresa wove part of the report into her evening talk as well, reading out loud on stage the report summary. And as she did, the chuckles began. "This (anti-choice) movement — funded by secret foundations injecting millions into this work — is slowly chipping away at abortion access across the country," she read. At the word "secret," Teresa paused momentarily for emphasis, and the crowd collectively laughed.
We laughed because these claims are laughable. When you confront something utterly ridiculous, and you know it (in part because you are living that life and understand it from the inside out), and when you see the irony in all its glory, it's a lot like responding to a cartoon. Though the underlying matter is quite serious, the portrayal of those of us working to turn the ship of death of around can't help but release our gasps as giggles.
NARAL includes this visual in its report; a graphic showing the covert operations of my tribe. Take a look at their map. I can just imagine the discussions that ensued as they drew up this baby.
There in blue, you'll find my type of "operative" — the dreaded "protesters." Yes, we are part of this "insidious" game. And right under that, you'll find the violet-colored "Fake Health Centers;" places like FirstChoice Clinic here in Fargo, where scared young women and men come to have ultrasounds, receive education and counseling, connect with a variety of resources, and find loving companions to walk with them in their pregnancy journeys.
Now, let's just think about the idea of the "fake health center" for a moment. On the one hand you have abortion facilities which claim to be all about healthcare, but which exist primarily to end the lives of human beings, yet call themselves clinics. The one in Fargo goes by the name of Red River Women's Clinic. The dictionary definition of a clinic is: "An establishment or hospital department where outpatients are given medical treatment or advice, especially of a specialist nature." "Medical treatment," you'd think, would have the end of helping people live, not helping them die.
So which are the real fake health centers?
Teresa likened this whole scenario to the Biblical story of David and Goliath. On one side we've got little David stepping out mightily despite understated strength and weapons — that's us pro-lifers. Then you've got Goliath, a larger than life ogre who has all the weapons and money at his disposal — that's the abortion industry.
"…demand dignity for every person in this great nation." I'm hearing the song, "Isn't it ironic?" resounding.
Yes, these are real words. This is the inside of THEIR end game.
As for the NARAL report, others have noticed it, too. Here's a great take on the document by Eric Metaxas and Anne Morse, with some encouragement and resources linked at the end.
Now then, I double-dog dare you pro-lifers: keep at it. Keep your spy glasses and black cloaks within reach, continue meeting in your caves with only a candle to light the table, where you plot your next move. Keep speaking in code — you never know who's watching! And don't forget your most powerful, super-duper secret weapon of all: prayer.
It's only been a year since I held a book to which I helped contribute in my hands, but 12 years have passed since I opened a box containing one of my children's books.
Well, this week it happened again, and I couldn't be more thrilled!
After the publication of my first two children's books in 2005, a third came into view, but the publishing company didn't (they sank altogether from what I know), so that third book never happened. Perplexed by the changes in the publishing industry at that time and how best to navigate those new waters, I turned my attention elsewhere. Though I loved writing for — and speaking to — children, other kinds of writing seemed to be calling to me as well. I continued doing some school visits, but it wasn't a full-time gig by any means, though always a pleasure.
Mainly, I forged ahead with where the Spirit led. And in these past years it's certainly led me to some wonderfully interesting places, but never could it erase my earliest love and the hours I spent diving into the world of children's literature. So when I received a tap from Sterling Publishing a few summers ago, asking if I'd be interested in auditioning for another book based on the great state of North Dakota, I jumped, happily and excitedly.
I remember being super busy during the time the audition piece was due, but I found a way to work it in. I knew that having a chance to write another children's book would be pure blessing — an unexpected gift. I knew it would be wonderful to work on another children's book about North Dakota in particular, so I waited to see if I'd be given the chance. And then the news came, and the journey commenced. I can now say that the experience of putting together this work has exceeded my expectations. It was a total joy!
Well, there were a few interesting bumps along the way, too, and I think that just makes the whole story even more interesting. I look forward to sharing more soon. For now, the link is already up on Amazon, and pre-orders are available. It would be great for this book to be given a nice jump start and have orders in wait. If you love North Dakota, children, or just want to learn about our humble, but fascinating, state, please consider it. You'll have them before the holidays since official release is in early October, so the timing couldn't be better.
Soon, I'll give you more of the inside scoop on how this book was fashioned. There's much to share. I can't wait!
Q4U: What have you held in your hands lately that felt particularly good?
Our third day in Chicago brought bright skies and Lake Michigan in all her glory, as seen — at least for a brief time — through the vantage point of the Ferris wheel at the Navy Pier.
But first, we had to get there, and the free trolley we discovered the night before provided a way.
we happened to see a bus dressed in a certain ice-cream advertisement. I suppose I paid special attention because I happen to be a fan of this ice cream. It brings me back to Grandma's house, where this special treat always awaited in my growing up years.
But wait, did you catch this little cutie peeking out the window? I think that secret sight made my morning before it had really begun.
Upon reaching the pier, we discovered that a special exhibition was being shown the week of our visit, featuring the Rolling Stones. And so these famous lips, in various forms and creative fashion, appeared throughout our gander along the way.
The garden, the colored tops of the carousel and other rides….
Upon our return, we split up, and some of us stopped in to gaze at the cute shops directly across the street from the Embassy Suites, our temporary abode.
My girl and I decided to pause for a shared afternoon treat — a S'mores dessert and some tea.
It would be our last supper, in a sense, or the dinner before things almost fell apart, as you'll soon see.
Q4U: What is your top choice of ethnic food when given lots of choices? What's your favorite ethnic dish?