text:
\section{Introduction}

A classical problem within the realm of orbital stability studies for theoretical and
observed planets in stellar binary systems is the circular restricted
3-body problem (CR3BP) \citep[e.g.,][]{sze67,roy05}.  The
CR3BP describes the motion of a body of negligible\footnote{Negligible mass means
that although the body's motion is influenced by the gravity of the two massive
primaries, its mass is too low to affect the motions of the primaries.} mass
moving in the gravitational field of the two massive primaries considered here
to be two stars.  The stars move in circular orbits about the center of mass
and their motion is not influenced by the third body, the planet.  Furthermore,
the initial velocity of the planet is assumed in the same direction as the
orbital velocity of its host star, which is usually the more massive of the two
stars.

The study of planetary orbital stability is timely for various astronomical
reasons.  First, although most planets are found in wide binaries,
various cases of planets in binaries with separation distances of less than
30~AU have also been identified \citep[e.g.,][and references therein]{pat02,egg04,egg10}.
Second, many more cases of planets in stellar binary systems are expected to
be discovered noting that binary (and possibly multiple) stellar systems
occur in high frequency in the local Galactic neighbourhood
\citep{duq91,lad06,rag06}.  Moreover, orbital stability studies of
planets around stars, including binary systems, are highly significant in
consideration of ongoing and future planet search missions
\citep[e.g.,][]{cat06,coc09}.

The CR3BP has been studied in detail by \cite{dvo84}, \cite{dvo86}, \cite{rab88},
\cite{smi93}, \cite{pil02}, and \cite{mar07}.  It has also been the focus
of the previous papers in this series.  In Paper~I, \cite{ebe08} obtained the
planetary stability limits using a criterion based on Jacobi's integral and
Jacobi's constant.  The method, also related to the concept of Hill stability
\citep{roy05}, showed that orbital stability can be guaranteed only if the
initial position of the planet lies within a well-defined limit determined by
the mass ratio of the stellar components.  Additionally, the stability criterion
was found to be also related to the borders of the ``zero velocity contour" (ZVC)
and its topology assessed by using a synodic coordinate system regarding the
two stellar components.

In Paper~II, \cite{ebe10} followed another theoretical concept based on the
hodograph eccentricity criterion.  This method relies on an
approach given by differential geometry that analyzes the curvature of the
planetary orbit in the synodic coordinate system.  The centerpiece of this
method is the evaluation of the effective time-dependent eccentricity of the
orbit based on the hodograph in rotating coordinates as well as the calculation
of the mean and median values of the eccentricity distribution.  This approach
has been successful in mapping quasi-periodicity and multi-periodicity
for planets in binary systems.  It has also been tested by comparing
its theoretical predictions with work by \cite{hol99} and \cite{mus05}
in regard to the extent of the region of orbital stability in binary
systems of different mass ratios.

Previously, the work by \cite{ebe10} dealt with the assessment of short-time
orbital stability, encompassing time scales of 10$^3$~yrs or less.  One of the
findings was the identification of a quasi-periodic region in the stellar mass
and distance ($\mu$, $\rho_{0}$) parameter space (see Sect. 2.1).
Due to the relatively short
time scales considered in the previous study, there is a strong motivation to
revisit the onset of orbital instability using longer time scales and different
types of methods.
The focus of this paper is the analysis of orbital stability by Lyapunov
exponents, which are among the most commonly used numerical tools for investigating
chaotic behaviour of different dynamical systems \citep[e.g.,][]{hil94}.  The
exponents have already repeatedly been used in orbital mechanics studies of
the Solar System \citep[e.g.,][]{lis99,mur01}.  For example, \cite{lis99}
discussed the long-term stability of the eight Solar System planets, while also
considering previous studies.  He concluded that the Solar System is most likely
astronomically stable, in the view of the limited life time of the Sun; however,
the orbits of Pluto and of many asteroids may become unstable soon after
the Sun becomes a white dwarf.

The numerical procedure of computing the Lyapunov exponents has been developed by
\cite{wol85} based on previous work by \cite{ben80}.  Hence, the main objective
of the present paper is to establish the Lyapunov
exponent criterion and verify it by performing the power spectra analysis
\citep[e.g.,][]{hil94} as well as by comparing the obtained results to those
presented in Paper I and II.  Our newly established criterion is then used to
investigate the stability of planetary orbits in stellar binary systems (approximated
here as the CR3BP) of different mass and distance ratios.  The methodology of
our study of orbital stability based on the Lyapunov exponent criterion is presented
and discussed in \S2.  Detailed model simulations are described in \S3, and our
conclusions are given in \S4.

\section{Theoretical approach}

\subsection{Basic equations}

In the following, we consider the so-called coplanar
CR3BP \citep[e.g.,][]{sze67,roy05}, which we will define
as follows.  Two stars are in circular motion about their common center of
mass and their masses are much larger than the mass of the planet.  In our
case, the planetary mass is assumed to be $1 \times 10^{-6}$ of the mass
of the star it orbits; also note that the planetary motion is constrained
to the orbital plane of the two stars. Moreover, it is assumed that the
initial velocity of the planet is in the same direction as the orbital
velocity of its host star, which is the more massive of the two stars,
and that the starting position of the planet is to the right of the
primary star (3 o'clock position), along the line joining the binary
components.

Following the conventions described by \cite{ebe08}, we write the
equations of motion in terms of the parameters $\mu$ and $\rho_0$ with
$\mu$ and $\alpha = 1 - \mu$ being related to the ratio of the
two stellar masses $m_1$ and $m_2$ (see below).  Moreover, $R_0$
denotes the initial distance of the planet from its host star, the
more massive of the two stars with mass $m_1$, whereas $D$ denotes
the distance between the two stars, allowing us to define $\rho_0$.
In addition, we use a
rotating reference frame, which also gives rise to Coriolis and
centrifugal forces.  The equations of motion are given as
\begin{eqnarray}
\dot{x} & = & u \\
\dot{y} & = & v \\
\dot{z} & = & w \\
\dot{u} & = & 2v + x -\alpha {x - \mu \over r_{1}^3} -\mu {x + \alpha
\over r_{2}^3} \\
\dot{v} & = & -2u + y -\alpha {y \over r_{1}^3} -\mu {y \over r_{2}^3}               \\
\dot{w} & = & -\alpha {z \over r_{1}^3} -\mu {z \over r_{2}^3}
\end{eqnarray}
where
\begin{eqnarray}
\mu     & = & {m_{2} \over m_{1} + m_{2}} \\
\alpha  & = & 1 - \mu \\
r_{1}^2 & = & \left(x - \mu\right)^2 + y^2 + z^2 \\
r_{2}^2 & = & \left(x + \alpha\right)^2 + y^2 + z^2\\
\rho_0 & = & {R_0 \over D}
\end{eqnarray}

The variables in the above equations describe the position of the planet,
which in essence constitutes a test particle.  Its position is defined in
Cartesian coordinates $\left\{x,\;y,\;z\right\}$.
We denote the time derivative or velocity of a coordinate using the dot
notation $\left\{\dot{x}={\rm dx \over dt}\right\}$.  We also represent
the set of second order differential equations, the equations
of motion, by a set of first order differential equations.  The velocity is
defined by the coordinates $\left\{u,\;v,\;w\right\}$ whose time derivatives
are the accelerations.  By defining the mass ratio and using normalized
coordinates, we can define the distances $\left\{r_{1},\;r_{2}\right\}$ with
reference to the location of the stars in the rotating coordinate system.

We enumerate the co-linear Lagrange points in the synodic frame by the order
of which the ZVC opens.  The point between the stars opens first; therefore,
we denote it as L1.  The point to the left of the star that does not host the
planet opens second; thus, we denote it L2.  The point to the right of the star
hosting the planet opens third and it is denoted L3.  The two Trojan
Lagrange points which are of lesser importance to our study are
L4 and L5 (see Fig.~\ref{fig:convention}).

\subsection{Lyapunov exponents}

A fundamental difference between stable and unstable planetary orbits is that
two nearby trajectories in phase space will diverge as a power law (usually
linear) for the former and exponentially for the latter. The parameter that
is used to measure this rate of divergence is called Lyapunov exponent as it
was originally introduced by \cite{lya07}; see also \cite{bak90}.  A
dynamical system with {\it n} degrees of freedom is represented in {\it 2n}
phase space; thus, to fully determine the stability of the system all {\it 2n}
Lyapunov exponents must be calculated.  The Lyapunov exponents are the most
commonly used tools to determine the onset of chaos and chaotic behaviour of
both dissipative \citep[e.g.,][and references therein]{mus09} and non-dissipative
systems of orbital mechanics \citep[e.g.,][and references therein]{lis99}.  The
positive Lyapunov exponents measure the rate of divergence of neighbouring orbits,
whereas negative exponents measure the convergence rates between stable manifolds.
For dissipative dynamical systems the sum of all Lyapunov exponents is less than $0$
\citep[e.g.,][]{mus09}; however, for Hamiltonian (non-dissipative) systems the sum
is equal to $0$ \citep[e.g.,][]{hil94}.

Specific applications of the Lyapunov exponents to the circular restricted 3-body
problem were discussed by many authors, including \cite{gon81}, \cite{jef83},
\cite{lec92}, \cite{mil92}, \cite{smi93}, \cite{mur01}, and others.
Some of these authors also considered the
so-called Lyapunov time, which measures the $e$-folding time for the divergence
of nearby trajectories. It should be noted that the Lyapunov time is not
well-defined for cases when close encounters between a planet and one of
the stars occur or when the planet is ejected from the system \citep{lis99}.
We shall treat such cases with special caution in this paper.

The previously obtained results clearly show that the Lyapunov exponents can be
calculated for the case of the CR3BP considered in this paper, for which we have
$\textit{2n}=6$.  This requires a state vector for the system containing $6$
elements.  Details about the nature of the state vector are given in Appendix A.
From the equations of motion, the Jacobian \textbf{J} can be determined, which
will be the foundation of how the Lyapunov exponents will be determined.  In
addition, the nature of this Jacobian will elude to certain properties of the
Lyapunov exponents.

For Hamiltonian systems the trace of the Jacobian should equal zero, $Tr\;\textbf{J}=0$.
This requires that the CR3BP should have either all zero diagonal elements or an
even amount of 3 positive/negative diagonal elements.  As a result this forces the
sum of the Lyapunov exponents to be also zero.  Then we should expect some symmetry
in the spectrum of the Lyapunov exponents.  Since this is indeed the case, the Lyapunov
exponent spectra shown in this paper will only present the positive Lyapunov exponents
and omit the negative Lyapunov exponents as they do not give any additional information
about the system.  It is the convention that positive Lyapunov exponents indicate that
both dissipative \citep[e.g.,][]{hil94} and non-dissipative \citep[e.g.,][]{ozo90}
systems are chaotic.  Here the end value of the Lyapunov exponents will be used to make
the distinction between chaotic and non-chaotic orbits.

It is well known that the largest Lyapunov exponent is sufficient to determine the
magnitude of the chaos in a system \citep[e.g.,][]{wol85}.  Therefore, this study
will consider only the effect of the maximum Lyapunov exponent because it will show
the greatest effect of chaos on the system.  This motivates us to also examine how
large the maximum Lyapunov exponent can be before introducing enough chaos to
affect the stability of the CR3BP.

\begin{figure}
\centering
\epsfig{file=16199fg1.eps,width=0.85\linewidth}
\caption{Locations of the Lagrange points L1, L2, L3,
L4, and L5 as used in the CR3BP.  The label P denotes the
primary star and the label S denotes the secondary star.}
\label{fig:convention}

\end{figure}

\begin{table*}
\caption{Errors in the Jacobi constant (JCE) for models of $\mu = 0.3$
at different time intervals.}
\centering
\vspace{0.05in}
\vspace{0.05in}
\begin{tabular}{l c c c c }
\hline
\hline
\noalign{\vspace{0.03in}}
$\rho_0$ & $\rm JCE({\tau \over 4})$ & $\rm JCE({\tau \over 2})$
& $\rm JCE({3\tau \over 4})$ & $\rm JCE({\tau})$ \\
\noalign{\vspace{0.03in}}
\hline
\noalign{\vspace{0.03in}}
 0.355  & 1.0740E$-10$\p* &  2.4747E$-10$\p* &  1.2403E$-10$\p* & 1.8824E$-10$\p*        \\
 0.474  & 1.4498E$-10$\p* &  9.7917E$-11$\p* &  3.7723E$-11$\p* & 1.0067E$-11$\p*        \\
 0.595  & 8.9819E$-13$\p* &  5.2923E$-13$\p* &  5.2001E$-13$\p* & 7.1001E$-06$\p*        \\
\noalign{\vspace{0.05in}} \hline
\end{tabular}
\vspace{0.05in}
\begin{list}{}{}
\item[]Note: $\tau$ denotes the runtime of the simulation.  We show the stable cases
of $\rho_0 = 0.355$ and 0.474 with $\tau = 10^5$ binary orbits as well as the unstable
case of $\rho_0 = 0.595$ with $\tau = 150.64$ binary orbits.
\end{list}
\label{table1}
\end{table*}

\begin{table*}
\caption{Maximum Lyapunov exponent study for the models of $\mu = 0.3$ at different
time intervals.}
\centering
\vspace{0.05in}
\vspace{0.05in}
\begin{tabular}{l c c c c c}
\hline
\hline
\noalign{\vspace{0.03in}}
$\rho_0$ & $\rm MLE\left({\rm 10^2}\right)$ & $\rm MLE\left({\rm 10^3}\right)$
& $\rm MLE\left({\rm 10^4}\right)$ & $e_{\rm median}$ & \rm ZVC  \\
\noalign{\vspace{0.03in}}
\hline
\noalign{\vspace{0.03in}}
 0.20  &  1.1099E$-1$\p*  &  1.1493E$-2$\p*  &  1.1446E$-3$\p* & 0.027 & ...        \\
 0.30  &  1.0322E$-1$\p*  &  1.0103E$-2$\p*  &  1.0691E$-3$\p* & 0.17  & ...        \\
 0.40  &  9.8084E$-2$\p*  &  1.0050E$-2$\p*  &  6.8986E$-4$\p* & 0.58  & L1         \\
 0.474 &  7.7766E$-2$\p*  &  9.4232E$-3$\p*  &  9.2624E$-4$\p* & 0.75  & L1, L2     \\
 0.50  &  8.5390E$-2$\p*  &  9.2048E$-3$\p*  &  7.9830E$-4$\p* & 0.85  & L1, L2     \\
 0.595 &  1.5793E$-1$\p*  &  1.4175E$-1$*    &   ...           & 1.14  & L1, L2, L3 \\
 0.60  &  8.9533E$-1$*    &   ...            &   ...           & 1.10  & L1, L2, L3 \\
\noalign{\vspace{0.05in}}
\hline
\end{tabular}
\vspace{0.05in}
\begin{list}{}{}
\item[]Note: Elements without data indicate simulations that ended due to the energy criterion,
thus representing planetary catastrophes.  Elements with an asterisk (*) indicate that the
simulation ended before the allotted time.  Also, $e_{\rm median}$ represents the median of
the eccentricity distribution obtained for the curvature of the planetary orbits in the
synodic coordinate system (see Paper~II).  The last column indicates the Lagrange point(s)
where the zero-velocity contour (ZVC) is open (see Paper~I).
\end{list}
\label{table2}
\end{table*}

\section{Results and discussion}

We performed simulations for stellar mass ratios from $\mu = 0.0$ to 0.5 in
increments of 0.01.  A Yoshida sixth order symplectic integration scheme was used
\citep[e.g.,][]{yos90}.  As a measure of the precision of the integration scheme, we
note that a time step of $\epsilon = 10^{-4}$~yrs is used for the individual cases.
However, for producing plots of the entire parameter space we adopt a time step of
$\epsilon = 10^{-3}$~yrs as the smaller time step did not noticeably enhance the
quality of the plots.  The order of error in
energy for each time step was $10^{-14}$ and $10^{-10}$, respectively.  We performed
simulations for different time limits, which range from 10 to $10^5$~yrs in increments
of powers of 10.  We also performed case studies with time limits of $10^6$ and $10^7$ yrs,
although we do not expect significant changes to occur at those longer time scales.  By using
different time scales we can estimate when certain phenomena occur and ascertain
how they will affect other regions over longer periods of time.

\begin{figure*} [h]
\centering
\begin{tabular} {ccc}
\epsfig{file=16199fg21.eps,width=0.3\linewidth,height=0.3\linewidth}&
\epsfig{file=16199fg22.eps,width=0.3\linewidth,height=0.3\linewidth}&
\epsfig{file=16199fg23.eps,width=0.3\linewidth,height=0.3\linewidth}\\
\end{tabular}
\caption{Case study for the initial planetary distance ratio
$\rho_0 = 0.355$ with the planetary orbit in the synodic coordinate system, Lyapunov spectrum,
and power spectrum.  The stellar mass ratio is $\mu = 0.3$.}
\label{fig:mu.3rho.355}
\end{figure*}

\begin{figure*} [h]
\centering
\begin{tabular} {ccc}
\epsfig{file=16199fg31.eps,width=0.3\linewidth,height=0.3\linewidth}&
\epsfig{file=16199fg32.eps,width=0.3\linewidth,height=0.3\linewidth}&
\epsfig{file=16199fg33.eps,width=0.3\linewidth,height=0.3\linewidth}\\
\end{tabular}
\caption{Case study for the initial planetary distance ratio
$\rho_0 = 0.474$ with the planetary orbit in the synodic coordinate system, Lyapunov spectrum,
and power spectrum.  The stellar mass ratio is $\mu = 0.3$.}
\label{fig:mu.3rho.474}
\end{figure*}

\begin{figure*} [h]
\centering
\begin{tabular} {ccc}
\epsfig{file=16199fg41.eps,width=0.3\linewidth,height=0.3\linewidth}&
\epsfig{file=16199fg42.eps,width=0.3\linewidth,height=0.3\linewidth}&
\epsfig{file=16199fg43.eps,width=0.3\linewidth,height=0.3\linewidth}\\
\end{tabular}
\caption{Case study for the initial planetary distance ratio
$\rho_0 = 0.595$ with the planetary orbit in the synodic coordinate system, Lyapunov spectrum,
and power spectrum.  The stellar mass ratio is $\mu = 0.3$.}
\label{fig:mu.3rho.595}
\end{figure*}

\begin{figure*} [h]
\centering
\begin{tabular} {ccc}
\epsfig{file=16199fg51.eps,width=0.3\linewidth,height=0.3\linewidth}&
\epsfig{file=16199fg52.eps,width=0.3\linewidth,height=0.3\linewidth}&
\epsfig{file=16199fg53.eps,width=0.3\linewidth,height=0.3\linewidth}\\
\end{tabular}
\caption{Case study for the initial planetary distance ratio
$\rho_0 = 0.290$ with the planetary orbit in the synodic coordinate system, Lyapunov spectrum,
and power spectrum.  The stellar mass ratio is $\mu = 0.5$.}
\label{fig:mu.5rho.29}
\end{figure*}

\begin{figure*} [h]
\centering
\begin{tabular} {ccc}
\epsfig{file=16199fg61.eps,width=0.3\linewidth,height=0.3\linewidth}&
\epsfig{file=16199fg62.eps,width=0.3\linewidth,height=0.3\linewidth}&
\epsfig{file=16199fg63.eps,width=0.3\linewidth,height=0.3\linewidth}\\
\end{tabular}
\caption{Case study for the initial planetary distance ratio
$\rho_0 = 0.370$ with the planetary orbit in the synodic coordinate system, Lyapunov spectrum,
and power spectrum.  The stellar mass ratio is $\mu = 0.5$.}
\label{fig:mu.5rho.37}
\end{figure*}

\begin{figure*} [h]
\centering
\begin{tabular} {ccc}
\epsfig{file=16199fg71.eps,width=0.3\linewidth,height=0.3\linewidth}&
\epsfig{file=16199fg72.eps,width=0.3\linewidth,height=0.3\linewidth}&
\epsfig{file=16199fg73.eps,width=0.3\linewidth,height=0.3\linewidth}\\
\end{tabular}
\caption{Case study for the initial planetary distance ratio
$\rho_0 = 0.400$ with the planetary orbit in the synodic coordinate system, Lyapunov spectrum,
and power spectrum.  The stellar mass ratio is $\mu = 0.5$.}
\label{fig:mu.5rho.40}
\end{figure*}

We display runs for selected initial conditions (i.e., starting distances $\rho_0$
of the planet from the stellar primary) corresponding to $\mu = 0.3$
in Figs.~\ref{fig:mu.3rho.355} to \ref{fig:mu.3rho.595} and to $\mu = 0.5$ in
Figs.~\ref{fig:mu.5rho.29} to \ref{fig:mu.5rho.40}.  In Figs.~\ref{fig:mu.3rho.355}
to \ref{fig:mu.5rho.40}, we first present the planetary orbits in the synodic coordinate
system (X*, Y*).  Secondly in each figure, the Lyapunov spectra of the simulations
are shown using a logarithmic scale for the Y*-axis.  Lastly in each figure, the time
series power spectra of the simulations are shown with their normalized amplitudes.
The power spectra were obtained through the usage of a FFT subroutine in
Matlab$\textsuperscript{\textregistered}$ that uses the X*-component separation distance
as a function of time and converts the output frequencies to periods.
The selected starting distance ratios $\rho_0$ of the planet are 0.355, 0.474, 0.595
for $\mu = 0.3$ and 0.290, 0.370, 0.400 for $\mu = 0.5$.  Note that
$\rho_0$ indicates the relative initial distance of the planet given as $R_0/D$, with
$D = 1$~AU as the distance between the two stars and $R_0$ as the initial distance of
the planet from its host star, the primary star of the binary system.

Using the method of Lyapunov exponents, we are able to verify and extend the methods
described by \cite{ebe08} and \cite{ebe10}.  Absolute orbital stability can
be more rigorously shown through the Lyapunov exponent method.  It occurs when
$\rho_0 < \rho_0^{\left(1\right)}$, where $\rho_0^{\left(1\right)}$ represents the point
at which the initial condition results in a ZVC that opens at L1.  For larger values of
$\rho_0$, stability is not guaranteed due the behaviour discussed by \cite{ebe08};
this result is also consistent with our Lyapunov exponent criterion for orbital
stability.

\begin{table*}
\caption{Maximum Lyapunov exponent study for the models of $\mu = 0.5$ at different
time intervals.}
\centering
\vspace{0.05in}
\vspace{0.05in}
\begin{tabular}{l c c c c c}
\hline
\hline
\noalign{\vspace{0.03in}}
$\rho_0$ & $\rm MLE\left({\rm 10^2}\right)$ & $\rm MLE\left({\rm 10^3}\right)$
& $\rm MLE\left({\rm 10^4}\right)$ & $e_{\rm median}$ & \rm ZVC  \\
\noalign{\vspace{0.03in}}
\hline
\noalign{\vspace{0.03in}}
 0.25  & 8.7189E$-2$\p* &  1.1353E$-2$\p* &  1.0009E$-3$\p* & 0.20  & ...        \\
 0.29  & 1.0647E$-1$\p* &  9.5469E$-3$\p* &  9.9141E$-4$\p* & 0.45  & L1         \\
 0.30  & 7.6275E$+0$*   &   ...           &   ...           & 0.67  & L1         \\
 0.35  & 5.2937E$+0$*   &   ...           &   ...           & 0.82  & L1         \\
 0.37  & 6.1946E$+0$*   &   ...           &   ...           & 0.98  & L1         \\
 0.40  & 1.0675E$-1$\p* &  9.6613E$-3$\p* &  8.8900E$-4$\p* & 0.71  & L1         \\
 0.43  & 2.8614E$-1$\p* &  2.9420E$-1$*   &   ...           & 0.87  & L1         \\
 0.50  & 7.9684E$-1$*   &   ...           &   ...           & 0.089 & L1, L2, L3 \\
\noalign{\vspace{0.05in}} \hline
\end{tabular}
\vspace{0.05in}
\begin{list}{}{}
\item[]Note: Elements without data indicate simulations that ended due to the
energy criterion, thus representing planetary catastrophes.  Elements with an
asterisk (*) indicate that the simulation ended before the allotted time.
Also, $e_{\rm median}$ represents the median of the eccentricity distribution
obtained for the curvature of the planetary orbits in the synodic coordinate system
(see Paper~II).  The last column indicates the Lagrange point(s) where the
zero-velocity contour (ZVC) is open (see Paper~I).
\end{list}
\label{table3}
\end{table*}

In this paper, the main criterion for orbital stability is the Lyapunov exponent
criterion, which is based on the maximum Lyapunov exponent.  From a
theoretical point of view, an orbit is stable when all Lyapunov exponents are
exactly zero.  Obviously, this `perfect' criterion for orbital stability will
be very difficult to reach numerically because it would require an infinite
simulation time.  Based on our finite simulation times, we obtain 3 positive and
3 negative Lyapunov exponents, and their sum becomes close to zero within the
limits of our numerical simulations.  Hence, in order to determine orbital
stability numerically, we must look at the values of the three positive
Lyapunov exponents at the beginning and at the end of our simulations.  By
comparing these values, we determine whether the exponents decrease in
time, and if so what is the rate of their decrease, or whether they stay
approximately constant in time.

Using this information, we are able to identify the maximum Lyapunov exponent
and adopt it as our primary indicator of orbital stability.  We classify an
orbit as stable if the initial value of the maximum Lyapunov exponent is below
a certain threshold and if it decreases at a `reasonable rate' (see below);
otherwise, the orbit is classified as unstable.  In our plots of Lyapunov
spectra (see the second panels in Figs.~\ref{fig:mu.3rho.355} to
\ref{fig:mu.5rho.40}), we present all three positive Lyapunov exponents
to show their values and study how they change in time.

In addition to the Lyapunov exponent criterion for orbital stability, we also
use the so-called orbital energy criterion, which requires that the kinetic
energy should not exceed twice the value of the potential energy.  This is evaluated
in our numerical simulations during each time step.  A failure of this criterion
would imply a break in conservation of the Jacobi constant as detailed by
\cite{sze67} and shown numerically in Table~\ref{table1}.  It should also be
noted that the cases presented in Table \ref{table1} are also presented in
Figs.~\ref{fig:mu.3rho.355} to \ref{fig:mu.3rho.595}.
There are two important points associated with this criterion.
First, our systems are Hamiltonian, which means that their energy must be
conserved.  On the other hand, the fact that the energy conservation of the
planet may be broken because we are neglecting the effects of the third mass
on the larger masses has already been discussed by \cite{sze67}.  Second,
even if the energy is only approximately conserved in our numerical simulations,
we still request that the Jacobi constant remains constant, which is a required
stability condition for CR3BP.  To be consistent with this criterion (see also
Paper I), we stop our numerical simulation once changes (even small) in
the Jacobi constant occur; such cases are depicted in Tables~\ref{table2} and
\ref{table3}.

Alike in the previous paper by \cite{ebe08}, we are able to identify the same
regions of orbital stability, instability, and domains of quasi-periodic orbital
stability.  A key difference, however, is that the orbit diagrams depicted in
Figs.~\ref{fig:mu.3rho.355} to \ref{fig:mu.5rho.40} have been simulated for $10^5$
years, whereas the corresponding figures in the previous paper have been simulated
for only $10^3$ years.  The power spectra are shown to indicate how we determined
the region of quasi-periodic orbital stability including the correct magnitude.

We begin by classifying Figs. \ref{fig:mu.3rho.355}, \ref{fig:mu.3rho.474},
\ref{fig:mu.5rho.29}, and \ref{fig:mu.5rho.40} as stable candidate
configurations.  Three of the cases
show similar behaviour in the maximum Lyapunov exponent as shown in Figs.~\ref{fig:mu.3rho.474}b,
\ref{fig:mu.5rho.29}b, and \ref{fig:mu.5rho.40}b.  These Lyapunov spectra have a common trend
by starting at a maximum
value on the order of $10^{-1}$ and converging, albeit slowly, to smaller orders of ten.
Figure~\ref{fig:mu.3rho.474} shows a somewhat different behaviour compared to the other cases in
its class of stable candidates.  This case establishes a quasi-periodic orbit, which illustrates
a $\left(3:1\right)$ resonance in the power spectrum and reveals the same trend of
stability in the Lyapunov exponent spectrum.  Figure~\ref{fig:mu.3rho.355} shows an additional
variance in behaviour due to the elevated nature of the maximum Lyapunov exponent.
This shows that a limited amount of chaos exists in the system while remaining stable
for the full simulation time.  This case also demonstrates a $\left(4:1\right)$ resonance
in the power spectrum.

In contrast, Fig.~\ref{fig:mu.3rho.595} demonstrates a case of instability.
The Lyapunov spectrum shows a different nature than that of the preceding cases.
In Fig.~\ref{fig:mu.3rho.595}b it begins at a maximum value greater than 1 and converges
to a value between $10^{-1}$ and 1.  By establishing the preceding cases as stable cases,
we can contrast the final values of the corresponding maximum Lyapunov exponents.  In the
unstable case of Fig.~\ref{fig:mu.3rho.595}b, it is two orders of magnitude greater than
in the stable cases of Figs.~\ref{fig:mu.3rho.474}b, \ref{fig:mu.5rho.29}b, and
\ref{fig:mu.5rho.40}b.  However, in comparison with Fig.~\ref{fig:mu.3rho.355}b we find
only a difference of one order of magnitude.

Figure~\ref{fig:mu.5rho.37} has been examined in a similar manner.  Having already classified
Fig.~\ref{fig:mu.5rho.29} and \ref{fig:mu.5rho.40} as stable configurations, we emphasize
that they reveal similar trends in the maximum Lyapunov exponent as given by Fig.~\ref{fig:mu.3rho.474}.
However, Fig.~\ref{fig:mu.5rho.37} shows a
different orbit diagram and is described by a maximum Lyapunov exponent that gives the
outcome of instability.  This case conveys a much noisier power spectrum along with a maximum
Lyapunov exponent on the order of 1 or greater.  Finer detail is illustrated in Table~\ref{table1}
and Table~\ref{table2}.  Particularly Table~\ref{table2} shows a boundary in the maximum
Lyapunov exponent where values near 0.1 and smaller for the first 100 years tend toward stability.

Figure~\ref{fig:contour} conveys the bigger picture for the overall parameter space.
It represents contour plots of the maximum Lyapunov exponent with respect to the
($\mu$, $\rho_{0}$) parameter space in linear and logarithmic scale.
The crosses depict initial conditions for runs that prematurely ended due to the orbital energy criterion.
This demonstrates where the regions of instability occur as reflected by the respective colour coded scale
of the maximum Lyapunov exponent.  Comparing Fig.~\ref{fig:contour} (left) to the previous result by
\cite{ebe08}, it can be seen that the main regions of stability remain the same.  Other noteworthy
features include that the instability islands present near $\rho_0 = 0.4$ have grown as the
simulation time has been increased as well as the existence of a plateau near $\rho_0 = 0.48$.
The colour scale in Fig.~\ref{fig:contour} (left) has a maximum colour of dark red at a maximum
Lyapunov exponent of 0.15.
Some regions appear to be coloured black; however, this does not correspond to the adopted
colour scale as it is caused by the finite contour line width due to the close proximity of
the lines.  Therefore, the plateau has a peak value of a maximum Lyapunov exponent near 0.15.
Considering the diagrams in Fig.~\ref{fig:mu.3rho.474}, we conclude that a region of
quasi-periodicity exists on this plateau.

Figure~\ref{fig:contour} (right), the contour plot in logarithmic scale, is shown to display
some of the finer details pertaining to structure inside the stability regions.  The blue-green
coloured regions demonstrate areas of possible stable chaos that are hidden in
Fig.~\ref{fig:contour} (left).  Some other smaller contours are also produced in the stability region,
but the colour coding in general shows little change, which is partially due to the chosen spacing
between contours.  The average difference in height between these levels is $-0.15$; on the
logarithmic scale, it indicates a change by a factor of $1.41$ in the maximum Lyapunov exponent.

Inspecting Fig.~\ref{fig:contour} also allows a comparison with previous results, particularly
results of Paper~I.  There it was shown that absolute orbital stability occurs when
$\rho_0 < \rho_0^{\left(1\right)}$, where $\rho_0^{\left(1\right)}$ represents the point at
which due to the initial condition the ZVC opens at L1.  This condition is represented by the
line of C$_1$ in Fig.~\ref{fig:contour}.  It is evident that the Lyapunov exponent
criterion is almost perfectly consistent with this condition.  Additionally, as discussed in
Paper~I and references therein, no stability can be expected if $\rho_0 > \rho_0^{\left(3\right)}$
because now the ZVC is open at L1, L2, and L3.  This finding is also almost perfectly reflected
through the behaviour of the maximum Lyapunov exponent as a orbital stability criterion.  Both
panels of Fig.~\ref{fig:contour} show no stability regions on the right side of C$_3$, which is
reflective of the opening of the ZVC at Lagrange points L1, L2, and L3.

\section{Conclusions}

We present a detailed case study of the CR3BP with analyses through the usage of the Lyapunov
exponents.  We are able to characterize stability limits based on the value of the maximum
Lyapunov exponent at the end of each simulation.  Cases where the maximum Lyapunov exponent
exceeds a value of 0.15 indicate that the planet will experience an event that causes the orbital
velocity to decrease.  These events include intersecting a Lagrange point or the ZVC. After
such an event, the planet will experience a series of near misses (or collisions) with one of the stars in the
binary system leading to overall instability.  Chaos theory and the concept of Lyapunov time
prevent us from predicting exactly when the planet will be ejected.  Using the Lyapunov time as
a measure of the length of predictive time, we can show that this relationship is proportional
to the inverse of the maximum Lyapunov exponent.  Using our critical value of 0.15, the unstable
systems will lose predictability within $(0.15)^{-1} = 6\frac{2}{3}$ years or less.  After that
time, it is unknown when the planet will be ejected as this could take many multiples
of the Lyapunov time to occur.

The method also shows evidence of a region of quasi-periodicity.  This is a region where the
maximum Lyapunov exponent remains near the critical value without exceeding that value.  This
is shown for cases simulated for $10^5$ years.  Based on this time scale, we can conclude that
our quasi-periodic plateau represents a region of stable or quasi-stable chaos.  This is due
to the Lyapunov times being much less than the simulation run time.  The chaos is shown through
the value of the maximum Lyapunov exponent, whereas the stability is shown through the motion
of the planet over longer time scales.  The lack of near miss events and encounters with regions of
decreasing velocity prohibits the planet from becoming orbitally unstable.

Comparisons to previously established criteria for stability show that our results are consistent
with previously obtained stability limits \citep[e.g.,][]{hol99,mus05,cun07,ebe08,ebe10}.
In \cite{ebe08}, Paper~I, the onset of instability was related to the topology of the ZVC,
whereas in \cite{ebe10}, Paper~II, it was shown that the onset of orbital instability occurs when
the median of the effective eccentricity distribution exceeds unity.  Both results are consistent
with the findings of Paper~III, i.e., the inspection of the maximum Lyapunov exponent.
However, the latter offers the advantage to link the study of orbital instability for the
CR3BP (and any subsequent generalization, if available) to chaos theory, including the
evaluation of different types of chaos.

Although our results have been obtained for the special case of the CR3BP, we expect that
it may also be possible to augment our findings to planets in generalized stellar
binary systems.  Desired generalizations should include studies of the
elliptical restricted 3-body problem (ER3BP) \citep[e.g.,][]{pil02,sze08}
as well as of planets on inclined orbits \citep{dvo07}, noting that especially
the former have important applications to real existing systems in consideration of the
identified stellar and planetary orbital parameters \citep{egg10}.

\begin{figure*}
\centering
\begin{tabular} {ll}
\epsfig{file=16199fg81.eps,width=0.577\linewidth,height=0.375\linewidth}&
\epsfig{file=16199fg82.eps,width=0.375\linewidth,height=0.375\linewidth}\\
\end{tabular}
\caption{We depict the maximum Lyapunov exponent (colour coded) for various mass ratios
$\mu$ and initial conditions $\rho_0$ using a \emph{linear} scale (left) or a
\emph{logarithmic} scale (right) where $-n$ corresponds to $10^{-n}$.  The crosses denote
cases where the simulation was terminated due to the planet being captured by one of the
stars or being ejected from the system. The green, red, and black curves represent the
initial conditions that cause the ZVC to open at L1, L2, and L3, respectively.}
\label{fig:contour}
\end{figure*}

\begin{acknowledgements}

This work has been supported by the U.S. Department of Education under GAANN
Grant No. P200A090284 (B.~Q. and J.~E.), the Alexander von Humboldt Foundation
(Z.~E.~M.) and the SETI institute (M.~C.).

\end{acknowledgements}

\section*{Appendix A}

\subsection*{Basic concepts and definitions}

From stability analysis we can use a Jacobian matrix to show how a state vector $\textbf{x}$
evolves in time (see \citealt{tso92} for details).  The governing equations are
\[\dot{\textbf{x}} = \textbf{J} \cdot \textbf{x}\]
\[\textbf{J} = \left(\begin{array}{ccc}
{\partial f_{1} \over \partial x_{1}} & \ldots & {\partial f_{n} \over \partial x_{1}} \\
\vdots & \ddots &\vdots \\
{\partial f_{1} \over \partial x_{n}} & \ldots & {\partial f_{n} \over \partial x_{n}}
\end{array}\right)\]
This differential equation has a general solution, which is
$\textbf{x}\left(t\right) = e^{\textbf{J}t}\:\textbf{x}\left(0\right)$.  Assuming $\textbf{J}$ has distinct eigenvalues,
we can find a matrix $\textit{U}$ to diagonalize $\textbf{J}$ to form a diagonal matrix
$\textit{D}$ such as
\[\textit{U}^{-1}\:\textbf{J}\:\textit{U} = \textit{D}\]
By rewriting the above equation we obtain the more useful form given as
\[\textbf{J} = \textit{U}\: \textit{D}\: \textit{U}^{-1}\]
Using the multiplication theorem, we can develop relations to obtain the eigenvalues of $\textbf{J}$
yielding
\[\det\:\textbf{J} = \left(\det\:\textit{U}\right)\left(\det\: \textit{D}\right)\left(\det\:
\textit{U}^{-1}\right) = \det\:\textit{D}\]
\[=\lambda_{1}\lambda_{2}\cdots\lambda_{n}\]
Furthermore, we find
\[Tr\:\textbf{J} = Tr\: \textit{D} = \lambda_{1} + \lambda_{2} + \ldots + \lambda_{n}\]
This can be generalized from $\textbf{J}$ to a function $f\left(\textbf{J}\right)$ such as
\[\det \: f\left(\textbf{J}\right) = f\left(\lambda_{1}\right)f\left(\lambda_{2}\right)\cdots f\left(\lambda_{n}\right)\]
\[Tr\: f\left(\textbf{J}\right) = f\left(\lambda_{1}\right) + f\left(\lambda_{2}\right) + \cdots + f\left(\lambda_{n}\right)\]
From our general solution, we can assume $f\left(\textbf{J}\right) = e^{\textbf{J}t}$.
Therefore, we find
\[\det\: e^{\textbf{J}t} = e^{\left(\lambda_{1} + \lambda_{2} + \ldots + \lambda_{n}\right)t} = e^{\left(Tr\:\textbf{J}\right)t}\]
A volume of perturbations in phase space will be conserved if $\left|\det\: e^{\left(Tr\:
\textbf{J}\right)t}\right| = 1$ or $Tr\:\textbf{J}=0$ for Hamiltonian systems.  A dissipative system
will have $\left|\det\: e^{\left(Tr\:\textbf{J}\right)t}\right|<1$ or $Tr\:\textbf{J}<0$.
The eigenvalues $\lambda_{1},\lambda_{2},\cdots,\lambda_{n}$ are the Lyapunov exponents of
the flow or the logarithms of eigenvalues of $\textbf{J}$.

\subsection*{Numerical determination of Lyapunov exponents}

From these equations we can define 6 dimensional tangent vectors $\textbf{x}_{i}$ and their
derivatives $\dot{\textbf{x}}_{i}$ where $i=1,\ldots,6$ as
\[\textbf{x}_{i} = \left\{x_{i}, y_{i}, z_{i}, u_{i}, v_{i}, w_{i}\right\}^T \]
\[\dot{\textbf{x}}_{i} = \left\{u_{i}, v_{i}, w_{i}, \dot{u}_{i}, \dot{v}_{i},
\dot{w}_{i}\right\}^T \]
Also we can define a Jacobian matrix, $\textbf{J}$, given as
\[\textbf{J} = \left(\begin{array}{cccccc}
	0 & 0 & 0& 1 & 0 & 0\\
	0 & 0 & 0& 0 & 1 & 0\\
	0 & 0 & 0& 0 & 0 & 1\\
	{\partial \dot{u} \over \partial x} & {\partial \dot{u} \over \partial y} & {\partial \dot{u}
\over \partial z}& 0 & 2 & 0\\
	{\partial \dot{v} \over \partial x} & {\partial \dot{v} \over \partial y} & {\partial \dot{v}
	\over \partial z}& -2 & 0 & 0\\
	{\partial \dot{w} \over \partial x} & {\partial \dot{w} \over \partial y} & {\partial \dot{w}
	\over \partial z}& 0 & 0 & 0\\
\end{array}\right)\]

\subsection*{Wolf method}
Now we describe the scheme by which \cite{wol85} determine the Lyapunov spectrum
and its application to the CR3BP.  The Wolf method follows a basic algorithm.  The first step
is to initialize a state vector of 6 elements.  Then, the tangent vectors need to be initialized
to some value.  We choose to have all tangent vectors to be unit vectors for simplicity.
This means that the elements $\left\{x_{1},\:y_{2},\:z_{3},\:u_{4},\:v_{5},\:w_{6}\right\} = 1$
and all other elements will be equal to zero.

The next step consists of a loop that will use a standard
integrator akin to the Runge-Kutta schemes to determine how the state and tangent vectors will
change within a time step.  This will continue for an adequate number of steps so that the tangent
vectors become oriented along the flow.  When this has been accomplished, it is necessary
to perform a Gram-Schmidt Renormalization (GSR) to orthogonalize the tangent space.  Thereafter,
we take the logarithm of the length of each tangent vector to obtain the Lyapunov exponents.
We then continue the loop.

\subsection*{Procedure}

We use the first tangent vector, $\textbf{x}_{1}$, to define the basis for the GSR process.
Thus, the first step consists in normalizing this vector.  With the vectors of
the new orthonormal set of tangent vectors, denoted by primes ($\prime$), we find
\[\begin{array}{l}
\textbf{x}_1^{'} = {\textbf{x}_1 \over \left\|\textbf{x}_{1}\right\|} \\
\textbf{x}_2^{'} = {\textbf{x}_2 - \left\langle\textbf{x}_2,\:\textbf{x}_1^{'} \right\rangle
\textbf{x}_1^{'} \over \left\|\textbf{x}_2 - \left\langle\textbf{x}_2,\:\textbf{x}_1^{'}
\right\rangle \textbf{x}_1^{'}\right\|} \\
\vdots \\
\textbf{x}_6^{'} = {\textbf{x}_6 - \left\langle\textbf{x}_6,\:\textbf{x}_5^{'} \right\rangle
\textbf{x}_5^{'} - \ldots -\left\langle\textbf{x}_6,\:\textbf{x}_1^{'} \right\rangle
\textbf{x}_1^{'} \over \left\|\textbf{x}_6 - \left\langle\textbf{x}_6,\:\textbf{x}_5^{'}
\right\rangle \textbf{x}_5^{'} - \ldots -\left\langle\textbf{x}_6,\:\textbf{x}_1^{'}
\right\rangle \textbf{x}_1^{'}\right\|} \\
\end{array} \]
From this new set of tangent vectors, the Lyapunov exponents will be calculated considering the
lengths of each vector.  Therefore, we find
\[\lambda_i = {1\over \tau}\left[\lambda_{i-1} + \log\left\|\textbf{x}_i - \sum_{j=1}^{i}
{\left\langle \textbf{x}_i,\:\textbf{x}_{j-1}^{'}\right\rangle\textbf{x}_{j-1}^{'}}\right\|
\right]\] $\ \rm where\:\lambda_{o}=\textbf{x}_{o}^{'}=0$.

redpajama_set_name: RedPajamaArXiv


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text:
How Hollywood hitched a ride on 'Galaxy'
By Stephen Humphries Staff writer of The Christian Science Monitor
Twenty-seven years ago, Douglas Adams wrote a BBC radio series about Arthur Dent, an Englishman who has barely gotten out of bed when Earth is destroyed by extraterrestrials to make way for an interstellar freeway.
Fortunately, Dent escapes by stowing away on a passing spaceship. Unfortunately, Dent happens to be clad in pajamas and a bathrobe at the time. And so the last surviving member of the human race is stuck traveling across the universe dressed as if he's on his way to a slumber party.
Thus begins "The Hitchhiker's Guide to the Galaxy," a quirky sci-fi comedy that went on to become a bestselling book (which spawned four sequels) as well as a popular BBC television series. Now, after two decades in development limbo, "The Hitchhiker's Guide to the Galaxy" has finally made it to the big screen. The movie, released Friday, stands to introduce a whole new generation to the writings of its creator, who died in 2001, and deepen the book's already considerable impact on pop culture.
"Douglas Adams was a genius," says humorist Dave Barry via e-mail. "He's the only writer ever who could begin a book with the destruction of the planet Earth and having you LAUGHING OUT LOUD about it."
No doubt about it, "Hitchhiker's" is a tad unusual. During Dent's interplanetary odyssey, he not only meets a two-headed humanoid and a manic-depressive robot, but also inadvertently stumbles across "the answer to the ultimate question of life, the universe, and everything." (The answer, as it happens, is the number 42.) Even stranger events transpire, including a scene in which a whale materializes in space and finds itself contemplating ontological questions as it plummets toward a planet below.
"He'd always wanted ... to write comedy mixed with science fiction, which nobody had done at that time," says Shaye Areheart, Adams's editor at Harmony Books. "He had spent a number of months traveling around Europe with his guitar [and] with a copy of a book called 'The Hitchhiker's Guide to Europe.' As legend goes, one night in either Austria, Spain, or Greece - it was told in different ways at different times - he was lying under a night sky looking up at the stars and planets and said to himself, 'Somebody should write 'A Hitchhiker's Guide to the Universe.' "
Adams's books are filled with outlandish episodes that reflect his love of Monty Python, the comedy troupe he befriended during the 1970s. What holds these surreal sketches together is understated British humor, often expressed through the story's eponymous book-shaped guide, a computer repository for all knowledge and wisdom that Dent consults during his journey. Adams (who was as tall as an NBA forward) never stooped to cheap gags or scatological jokes. Profoundly influenced by literary humorist P.G. Wodehouse, Adams's greatest talent was his witty wordplay.
"The delights of 'Hitchhiker' are the delights of watching Douglas create these absolutely memorable sentences," says Neil Gaiman, the bestselling fantasy novelist and author of "Don't Panic: The Hitchhiker's Guide to the Galaxy Companion."
" 'The spaceships hung in the air in exactly the way that bricks don't,' is a sentence that is perfectly constructed to create a laugh. And to create a laugh in its imagery. If you get anyone who's read 'Hitchhiker' books into a conversation, they'll actually start quoting lines, mostly very, very accurately."
As a result, much of the author's jargon has entered the popular lexicon. The phrase "life, the universe, and everything" has become commonplace, while the number 42 has a cosmic significance wholly unsuspected by the earliest mathematician to discover the six and seven times tables.
The influence of "Hitchhiker's," which has sold 20 million copies, can be seen in everything from Radiohead's breakout single, "Paranoid Android," to BabelFish, the language-translation software named after the mysterious creature Dent inserts in his ear to help him decipher what aliens are saying. In 2003, BBC television polled hundreds of thousands of British readers about their top 100 books of all time. "The Hitchhiker's Guide to the Galaxy" came in fourth, narrowly edging out Harry Potter.
Adams's quest to write something memorable was both his strength and weakness. The author crafted his novels with the meticulous precision of someone setting up a line of dominos along the Great Wall of China - each and every word was carefully selected to give sentences the perfect weight and equilibrium. Not surprisingly, he found the process so painful and daunting that he tended to procrastinate rather than face the blank page. As Adams himself once put it, "I love deadlines. I love the whooshing noise they make as they go by." (Sonny Mehta, Adams's editor at Pan, came up with a novel solution: He once locked the author in a hotel room until he finished writing a book.)
Unfortunately, Adams's sluggish work habits stalled production of the movie. During the '90s, he diverted his attention to devising innovative computer games, and in 1994 he even played guitar on stage with Pink Floyd. Though several big-name producers had expressed interest in Adams's drafts over the decades, the writer struggled to adapt his sci-fi comedy into a workable screenplay. Yet his enthusiasm for the project never waned, and he even went as far as relocating his family to California following a deal with Disney in the late 1990s.
After Adams's untimely passing, however, it seemed the film would never be made. Yet the producers persevered. They hired Karey Kirkpatrick, writer of "Chicken Run," to rework the problematic script. Mr. Kirkpatrick went back to the original radio plays and read the books. He was also given access to Adams's computer hard drive so that he could see earlier drafts of the screenplay.
"I've always said that the book is a very long setup: You meet the characters and then you go right to the end," says Kirkpatrick. "The book is sort of missing its middle, or the 'second act' if you're using film-structure jargon."
Kirkpatrick amplified a romantic plot in which an attractive galactic hitchhiker falls for Dent (even if he is dressed like Hugh Hefner). The writer also worked on a new character, a cult leader named Humma Kavula (played by John Malkovich in the film), that Adams had invented.
For Adams, the most important element of the script was his philosophical ideas, says Nick Webb, author of "Wish You Were Here: The Official Biography of Douglas Adams." "He was one of the first people who really thought about what information technology could do for us," says Mr. Webb, noting that Adams came up with the idea of the guide long before the Internet and PDAs arrived.
Strip away Adams's comic riffs about planets with pink oceans and the universal utility of the common bath towel, and one also discovers a subtext in the book about the vastness of infinity and mankind's place in it. As Mr. Gaiman puts it, "the delight of the universe Douglas was creating ... was taking all the small human concerns and then painting them on an intergalactic scale ... and realizing that they're still small human concerns."
For his part, Kirkpatrick admits that the script had to lose some of the book's sharp observations, since they didn't translate well to film. But, he says, the movie was careful not to compromise the book's tone or idiosyncrasies.
The film was directed by a British team professionally known as Hammer & Tongs (real names: Garth Jennings and Nick Goldsmith), who set about the daunting challenge of making a science-fiction comedy for audiences who aren't used to science-fiction comedies, at least not the type without Will Smith. "Hitchhiker" boasts good actors but no big-name stars - it's anyone's guess how it will fare.
"I've seen 'Hitchhiker's' and I would say it's better than most stuff you're going to see out there," concludes Kirkpatrick. "I'm very hopeful that people will find it. It's definitely not going to be criticized for being like other things out there."
Douglas Adams: The hitchhiker's guide to humor and science
42 facts about Douglas Adams
Detective stories by 'Hitchhiker's Guide to the Galaxy' author set to become TV series
https://www.csmonitor.com/2005/0429/p12s01-almo.html


text:
LocationsCurrently selected
IowaCurrently selected
30 Years of Providing Care and Compassion in Iowa
News and EventsCurrently selected
Wednesday, Jan 5, 2022
Establishing a comfortable work relationship is one of the most important factors for consultants working with families dealing with issues. For Boys Town's Livie Gordon, it made the difference in helping a family come together and find solutions for its problems.
Livie is a Family-Centered Services Specialist for Boys Town in Sioux City, Iowa. She began providing services for a family this past February with a 15-year-old son and 7-year-old daughter. Services began after their daughter unfortunately ended up between mom and dad during a physical altercation. Tensions were already high after their son was removed from the home and placed with relatives due to alleged sexual abuse concerns he had with another child in the community.
The parents were not getting along, argued often and the home atmosphere was very tense.
Livie was able to develop a positive working relationship with the family very early on. Originally, she was not their primary service provider, but covered one day of services with them and made a positive impression.
The family stated they felt comfortable working with Livie. She was able to get mom, dad, and the daughter into counseling services right away and she introduced a safety plan with them. She also taught the family various communication skills, helped them work through difficult situations and taught parenting skills from Common Sense Parenting®.
Livie made a difference.
The family never needed to use their safety plan and they never had another incident of domestic violence. They reported being able to the use the skills Livie had taught them, such as giving space to one another when having a disagreement and using healthy communication skills when they were both calm and ready to talk.
Additionally, there were issues between the family and the relatives caring for their 15-year-old son. The boy was unhappy while he was there and asked to return home before going to placement. They asked Livie if their case could remain open so she could support them in having their son home with them. Livie and the family advocated to the DHS worker to keep the case open until the son's placement was available and DHS agreed.
The worker returned the child to the parent's home and Livie continued to provide services to the family. The son struggled with listening, following through, and staying on task and they often reached out to Livie for assistance in how to deal with these behaviors. When Livie would arrive at the family home, all of the family members were seated at the table and ready to work on whatever skill Livie was teaching that appointment. There were no incidents with the son while he was home and the parents did not have major arguments or disagreements between one another. Their case has now closed successfully.
Stay Connected with Boys Town Iowa
1702 West Broadway, Suite 17
P:712-302-7900
For information about working at Boys Town Iowa, visit our Careers site.
Additional Links Charity Accreditation Research Annual Report National Journal Residential Advocacy Planned Giving Corporate Support How to Give Trade Life Boys Town Gift Shop BoysTownHospital.org BoysTownPress.org BoysTownAdmissions.org BoysTownTraining.org


text:
define([
    'app/applets/allergyEiE/applet',
    'hbs!app/applets/allergy_grid/details/detailsFooterTemplate',
    'hbs!app/applets/allergy_grid/list/expirationCellTemplate',
    'app/applets/allergy_grid/modal/modalView',
    'app/applets/allergy_grid/util',
    'hbs!app/applets/allergy_grid/list/severityTemplate',
    'hbs!app/applets/allergy_grid/list/summaryItemViewTemplate',
    'hbs!app/applets/allergy_grid/list/summaryViewTemplate',
    'hbs!app/applets/allergy_grid/list/siteTemplate',
    'hbs!app/applets/allergy_grid/list/commentTemplate'
], function(EnteredInError, detailsFooterTemplate, expirationCellTemplate,
    ModalView, Util, severityTemplate, summaryItemViewTemplate, summaryViewTemplate, siteTemplate, commentTemplate) {
    'use strict';
    //Data Grid Columns
    var summaryColumns = [{
        name: 'summary',
        label: 'Allergen Name',
        cell: 'string',
        hoverTip: 'allergies_allergenName'
    }, {
        name: 'reaction',
        label: 'Reaction',
        cell: 'string',
        hoverTip: 'allergies_reaction'
    }, {
        name: 'acuityName',
        label: 'Severity',
        cell: 'handlebars',
        template: severityTemplate,
        hoverTip: 'allergies_severity'
    }];

    var fullScreenColumns =
        summaryColumns.concat([{
            name: 'drugClassesNames',
            label: 'Drug Class',
            cell: 'string',
            hoverTip: 'allergies_drugClass'
        }, {
            name: 'originatorName',
            label: 'Entered By',
            cell: 'string',
            hoverTip: 'allergies_enteredBy'
        }, {
            name: 'facilityName',
            label: 'Facility',
            cell: 'string',
            hoverTip: 'allergies_facility'
                //template: siteTemplate

        }, {
            name: '',
            cell: 'handlebars',
            template: commentTemplate
        }]);

    fullScreenColumns.splice(1, 0, {
        name: 'standardizedName',
        label: 'Standardized Allergen',
        cell: 'string',
        hoverTip: 'allergies_standardizedAllergen'
    });

    var viewParseModel = {
        parse: function(response) {

            if (response.products) {
                response = ADK.utils.extract(response, response.products[0], {
                    name: 'name'
                });
            }

            if (response.observations) {
                response = ADK.utils.extract(response, response.observations[0], {
                    acuityName: 'severity',
                    observed: 'date'
                });
                response = Util.getAcuityName(response);
                response.observedDate = ADK.utils.formatDate(response.observed, "MM/DD/YYYY - HH:mm");
            }

            response = Util.getDrugClasses(response);
            if (response.entered) {
                response.originatedFormatted = ADK.utils.formatDate(response.entered, "MM/DD/YYYY - HH:mm");
            }
            //response = Util.getComments(response);

            response = Util.getReactions(response);
            response = Util.getFacilityColor(response);
            response = Util.getStandardizedName(response);
            response = Util.getSeverityCss(response);
            response = Util.getCommentBubble(response);
            //response = Util.getOriginatedFormatted(response);
            return response;
        }
    };

    //Collection fetchOptions
    var fetchOptions = {
        resourceTitle: 'patient-record-allergy',
        viewModel: viewParseModel,
        criteria: {
            filter: 'ne(removed, true)'
        },
        cache: false,
        pageable: false
    };
    var defaultConfiguration = {
        fetchOptions: {
            resourceTitle: 'patient-record-allergy',
            viewModel: viewParseModel,
            criteria: {
                filter: 'ne(removed, true)'
            },
            cache: false,
            pageable: false
        }
    };
    var gistModel = [{
        id: 'name',
        field: 'summary'
    }, {
        id: 'severity',
        field: 'severityCss'
    }];

    var _super;
    var gridView;

    var showModal = function(model, event) {
        //event.preventDefault();
        var view = new ModalView({
            model: model
        });

        // ORIGINAL REMOVED: Will McVay, Team Saturn
        // Need to augment with a footer view that offers option to close
        // detail view or mark Entered in Error.
        var modalOptions = [{
            title: Util.getModalTitle(model)
        }];
        // New version includes custom footer view with an "Entered in Error" button
        // that invokes the allergyEiE applet as a modal and passes in the reaction data.
        // WRM/Saturn
        var siteCode = ADK.UserService.getUserSession().get('site'),
            pidSiteCode = model.get('pid') ? model.get('pid').split(';')[0] : '';

        modalOptions[1] = {
            title: Util.getModalTitle(model),
            footerView: Backbone.Marionette.ItemView.extend({
                template: detailsFooterTemplate,
                onRender: function() {},
                events: {
                    'click #error': 'enteredInError'
                },
                enteredInError: function(event) {
                    var allergyEnteredInErrorChannel = ADK.Messaging.getChannel('allergyEiE');
                    allergyEnteredInErrorChannel.trigger('allergyEiE:clicked', event, model, gridView);
                },
                templateHelpers: function() {
                    if (ADK.UserService.hasPermission('remove-patient-allergy') && pidSiteCode === siteCode) {
                        return {
                            data: true
                        };
                    } else {
                        return {
                            data: false
                        };
                    }
                }
            }),
            callShow: true
        };

        ADK.showModal(view, modalOptions[1]);
    };

    var AllergySummaryItemView = Backbone.Marionette.ItemView.extend({
        tagName: 'div',
        className: 'summaryItem',
        attributes: function() {
            return {
                'tabindex': '0'
            };
        },
        template: summaryItemViewTemplate,
        events: {
            'click span': function(e) {
                showModal(this.model, e);
            }
        }
    });

    var AllergySummaryView = Backbone.Marionette.CompositeView.extend({
        initialize: function(options) {
            this.collection = options.collection;
            this.maximizeScreen = options.appletConfig.maximizeScreen;
        },
        template: summaryViewTemplate,
        childView: AllergySummaryItemView,
        childViewContainer: '.allergyBubbleView',
        events: {
            'click a.seeAll': function(event) {
                event.preventDefault();
                ADK.Navigation.navigate(this.maximizeScreen);
            }
        },
        onRender: function() {
            if (this.collection.length > 0) {
                // this.$el.find('.allergyBubbleView')
                //     .after('
See All >>
');
            } else {
                this.$el.find('.allergyBubbleView')
                    .after('
No Records Found
');
            }
        }

    });

    var GridApplet = ADK.Applets.BaseGridApplet;
    var AppletLayoutView = GridApplet.extend({
        className: 'app-size',
        initialize: function(options) {
            _super = GridApplet.prototype;
            var dataGridOptions = {};
            dataGridOptions.enableModal = true;
            dataGridOptions.filterEnabled = true;
            dataGridOptions.tblRowSelector = '#data-grid-allergy_grid tbody tr';
            if (this.columnsViewType === "summary") {
                dataGridOptions.columns = summaryColumns;
                dataGridOptions.filterFields = ["summary"];
                dataGridOptions.gistView = false;
                dataGridOptions.appletConfiguration = defaultConfiguration;
            } else {
                fetchOptions.pageable = true;
                dataGridOptions.columns = fullScreenColumns;
                dataGridOptions.gistView = false;
                dataGridOptions.appletConfiguration = defaultConfiguration;
            }
            fetchOptions.onSuccess = function() {
                dataGridOptions.collection.reset(dataGridOptions.collection.models);
            };

            dataGridOptions.collection = ADK.PatientRecordService.fetchCollection(fetchOptions);

            if (ADK.UserService.hasPermission('add-patient-allergy') && ADK.PatientRecordService.isPatientInPrimaryVista()) {
                dataGridOptions.onClickAdd = function(event) {
                    var addAllergyChannel = ADK.Messaging.getChannel('addAllergy');
                    addAllergyChannel.trigger('addAllergy:clicked', event, gridView);
                };
            }

            dataGridOptions.collection.on('sync', function() {
                //dataGridOptions.collection.comparator = 'acuityName';
                dataGridOptions.collection.comparator = function(a, b) {
                    var acuityNameA = a.get('acuityName') || '';
                    var acuityNameB = b.get('acuityName') || '';
                    if (acuityNameB.localeCompare(acuityNameA) !== 0) {
                        return acuityNameB.localeCompare(acuityNameA);
                    } else {
                        var enteredA = a.get('entered') || '';
                        var enteredB = b.get('entered') || '';
                        return enteredB.localeCompare(enteredA);
                    }
                };
                dataGridOptions.collection.sort();
            });
            //Row click event handler
            dataGridOptions.onClickRow = showModal;

            this.dataGridOptions = dataGridOptions;
            gridView = this;
            _super.initialize.apply(this, arguments);
        },
        onRender: function() {
            _super.onRender.apply(this, arguments);
        }
    });

    // expose detail view through messaging
    var searchAppletChannel = ADK.Messaging.getChannel("allergy_grid");
    searchAppletChannel.on('getDetailView', function(params) {
        showModal(params.model);
    });
    var channel = ADK.Messaging.getChannel('allergy_grid');
    channel.reply('detailView', function(params) {
        var fetchOptions = {
            criteria: {
                "uid": params.uid
            },
            patient: new Backbone.Model({
                icn: params.patient.icn,
                pid: params.patient.pid
            }),
            resourceTitle: 'patient-record-allergy',
            viewModel: viewParseModel
        };

        var response = $.Deferred();

        var data = ADK.PatientRecordService.fetchCollection(fetchOptions),
            pidSiteCode,
            detailModel;
        data.on('sync', function() {
            detailModel = data.first();
            var siteCode = ADK.UserService.getUserSession().get('site'),
                pidSiteCode = detailModel.get('pid') ? detailModel.get('pid').split(';')[0] : '';
            response.resolve({
                view: new ModalView({
                    model: detailModel
                }),
                title: Util.getModalTitle(detailModel),
                modalSize: "medium",
                footerView: Backbone.Marionette.ItemView.extend({
                    template: detailsFooterTemplate,
                    onRender: function() {},
                    events: {
                        'click #error': 'enteredInError'
                    },
                    enteredInError: function(event) {
                        var allergyEnteredInErrorChannel = ADK.Messaging.getChannel('allergyEiE');
                        allergyEnteredInErrorChannel.trigger('allergyEiE:clicked', event, model, gridView);
                    },
                    templateHelpers: function() {
                        if (ADK.UserService.hasPermission('remove-patient-allergy') && pidSiteCode === siteCode) {
                            return {
                                data: true
                            };
                        } else {
                            return {
                                data: false
                            };
                        }
                    }
                })
            });
        }, this);

        return response.promise();
    });

    var GistView = ADK.AppletViews.PillsGistView.extend({
        className: 'app-size',
        initialize: function(options) {
            var self = this;
            this._super = ADK.AppletViews.PillsGistView.prototype;
            fetchOptions.onSuccess = function() {
                self.appletOptions.collection.reset(self.appletOptions.collection.models);
            };
            this.appletOptions = {
                filterFields: ["summary"],
                gistModel: gistModel,
                collection: ADK.PatientRecordService.fetchCollection(fetchOptions)
            };
            this._super.initialize.apply(this, arguments);
        }
    });

    var applet = {
        id: 'allergy_grid',
        viewTypes: [{
            type: 'gist',
            view: GistView,
            chromeEnabled: true
        }, {
            type: 'summary',
            view: AppletLayoutView.extend({
                columnsViewType: "summary"
            }),
            chromeEnabled: true
        }, {
            type: 'expanded',
            view: AppletLayoutView.extend({
                columnsViewType: "expanded"
            }),
            chromeEnabled: true
        }],
        defaultViewType: "summary"
    };

    return applet;
});

redpajama_set_name: RedPajamaGithub


St. Odile's Church, often called "Saint Old's", is a small Catholic church located in the suburb of Pescodside along the northern border with Dulston. The church was built in 1924 and is considered a "heritage church" among the residents of Pescodside, as it is one of the oldest churches in the suburb, if not all east Malton. While this church has seen its fair share of fire and brimstone preachers most never last long as zombies often eat the loudest humans they find first.
Noted NecroTech scientist, Caleb Usher, stayed at St. Odile's Church for a brief period while locked out of the Waish Building in late December 2005. Survivors noted him standing in the doorway shaking his fist at the adjacent NecroTech facility and yelling that they let him back in. Caleb's departure from the church was attributed to him regaining access to the Waish Building.
At one time another frequent survivor at the church was a man by the name of Shepherd Taylor. Back in March of 2006 he was noted to have spent many days at St. Odile's, making minor repairs and tidying up. The good Shepherd administered first-aid to any needy survivor, regardless of denomination, and having been trained by local NecroTech employees in the use of their equipment he, as he put it, applied "a dose of Lazarus" to any zombies who wandered into the area. When not out on supply runs, he was often cleaning up the church. Of course these days have since passed and no one has seen Shepherd in a long while.
The church is only interested in providing shelter to the injured and lower level survivors. All the clergy ask for in return is that survivors assist with the barricades should they ever drop below Very Strongly. While the clergy frown upon over-barricading they do see the need to protect themselves and their flock when under zombie siege, but ask that barricades be lowered after the danger has passed in keeping with an open door policy.
He restoreth my soul, he leadeth me in the paths of righteousness for his name's sake.
The church, not being a resource building or home to any known group, does not have any affiliates. Even so, survivors staying there can seek assistance from Pegrum Place PD (93,9) should a zombie mob ever attack the building.
Barricades are to be kept at Very Strongly (VS+2) during times when zombie numbers are fewer than 5 within a 2x2 block grid. Should zombie numbers rise above this or reports of nearby resources buildings being overrun be confirmed, then barricades will be raised to Extremely Heavily.
At this time Free Running is essential to entering and departing the church. May God have mercy on those poor souls left trapped outside during such a time of strife.
February 24th, 2010 - Rumors say, some people saw a ghost of crocodile on the top of building.
September 24th, 2008 - The Electric Light Torchestra recon reported that St. Odile's Church, while ruined, was empty of zombies. Survivors could, in a pinch, reclaim and rebarricade the building.
September 14th, 2008 - The Electric Light Torchestra recon reported that the church was in ruins. At this time there were 1 zombie inside and 4 zombies outside.
March 30th, 2006 - Due to the acts of a bored murderer, Shepherd Taylor has departed the city. It appears that the survivor StinkeyBrains made it part of his daily routine to kill the good Shepherd. Even with constant revivals at the local NecroTech building he could only do so much before deciding that his efforts were being wasted.
March 10th, 2006 - Caleb Usher confirms that he performs daily "medical visits" on his way to the Waish Building each morning. His intentions are clearly to heal any and all injured survivors found inside the church with the more than ample supply of first-aid kits at his disposal. While Caleb does not encourage survivors to stay at the church for long he does deem it a safe location for low-level survivors seeking shelter off the streets, as its security has been vigilantly maintained by veteran survivor, Shepherd Taylor.


text:
'The Disappearance of My Mother' is All About Appearances
Former fashion icon Benedetta Barzini reluctantly receives the documentary treatment courtesy of her filmmaker son.
NANOF
Benedetta Barzini does not want to be the subject of a documentary. But her son, director Beniamino Barrese, insists on making a film about her. Yeah, it's basically Tell Them Who You Are and Mistaken for Strangers all over again, at least at first. The easiest idea that there is in documentary is to make a film about your parent or other close relative, especially if they were famous. But it's also one of the hardest ideas to get right. Having a parent who is combative during the process, not even merely reluctant, can be problematic on many levels.
Barrese's film, his feature directorial debut, is called The Disappearance of My Mother. The meaning of the title is a mystery for much of the film, even while he explains early on with some opening titles that his mother has said she is leaving and never coming back. Where is she going? Is she dying? Planning to take her own life? Simply moving away and becoming a recluse? Regardless, he really wants to record her one last time. Benedetta finally agrees because, as she says, better to hurt herself than him.
What ensues can sometimes be painful for the audience, as well, in an uncomfortable but still engrossing fashion. Benedetta constantly asks her son to stop filming and swears at him for doing so at awkward times, like when she's sleeping. Even her old friend, Lauren Hutton, berates Barrese about having his camera in their faces as they're trying to reconnect (he retreats behind some plants). For Benedetta, though, there's something to her objections. She was a model long ago, the first to grace the cover of Vogue Italia and a regular at Warhol's Factory, but she later became a feminist and Marxist critic of her own profession and, apparently, of images in general.
As a filmmaker, Barrese is now the one who is all about images, and that creates a dramatic dynamic and conflict between him and his mother. They have a dysfunction, yet also a bond, that is probably unhealthy. There are moments in his documentary where Barrese is filming his mother changing or going to the bathroom. And he comes off as having an obsession with her, the way he lingers on her with his lens, the way he includes a casting session to find young models to re-create Benedetta's work of half a century ago… But he's just a young man curious about his aging mother, who'd had him late in life and never told him of, let alone talked about her glamorous past.
And she just wants her son to be present, not behind a camera. She can be cruel but she definitely loves her baby boy — when she cooperates and plays along it comes off as a total surprise. A psychoanalyst could probably have a field day reviewing The Disappearance of My Mother. For me, I just found Benedetta to be an extraordinarily interesting woman and am inspired to read more about her complicated beliefs about modeling (she is shown returning to that world for various unclarified appearances) and her theories about media and gender and more (the class we see her teaching at the University of Milan as a professor of fashion and anthropology looks incredible).
And by the end, I came to appreciate the battle between mother and son, even enjoying it like some kind of intense sporting match, though it's hard to ignore the fact that, all the while, I'm on her side and ironically that means I'm technically against the very documentary that is making me aware of my own dilemma. Who doesn't love a good paradoxical film viewing experience?
As for the feeling of not getting to know enough about Benedetta or Beniamino or their family history, well, another point for her, because she believes images and films are lies that can't possibly capture a real person. Oh, and don't you dare walk out of this film feeling depressed, though that's certainly a possible effect. Stay for the post-credits scene to understand why.
Tags:Benedetta BarziniBeniamino BarreseDocumentaryfashionLauren HuttonmodelphotographySundance 2019Tell Them Who You AreThe Disappearance of My Mother
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Christopher Campbell(Editor in Chief)
Christopher Campbell is the founding editor of Nonfics.


To cultivate love of the Holy Eucharist, devotion to the Blessed Virgin Mary, and unswerving loyalty to the Holy Father and the Magisterium (the teaching authority) of the Catholic Church.
To prepare members to share the gift of Christ's truth and love, as found in its fullness in the teachings and practice of the Catholic Church, through the Apostolate of Catechesis.
If you are interested in pursuing membership, we suggest you begin by reading Cardinal Burke's essay, Re-Christianize America, which explains Father Hardon's vision for the Apostolate.
For Father Hardon, the work which God had given him was to be carried out with every ounce of his energy and at every moment of his life.
Father Hardon had been teaching the Missionaries of Charity since the beginning of his association with Mother Teresa, and the teaching trip to the motherhouse in Calcutta had been a yearly event.
With our Holy Father, our beloved founder, Father John A. Hardon, S.J., understood that, if our world is to be saved, which is indeed the mission of the Church, the faith must be taught and lived with the enthusiasm and the energy of the first Christians.
If you sense that the Holy Spirit might be calling you to become a Marian Catechist, please read about the doctrinal and spiritual formation of Marian Catechists.
I write to all those who have been associated with the Marian Catechist Apostolate since its foundation by the beloved Servant of God Father John A. Hardon, S.J., and to those who have come to know the Marian Catechist Apostolate since his death on December 30, 2000.
Over the years, as I met with Father Hardon we thoroughly discussed the essential elements of the Marian Catechist Apostolate, and I began to promote the use of his courses for the training of teachers in the Diocese of La Crosse, and to encourage catechists to become Consecrated Marian Catechists. When he became gravely ill, Father Hardon asked me to assume the direction of the Marian Catechists upon his death.
In the Marian Catechist Manual (available from the Marian Catechist Bookstore), Father Hardon sets forth plainly the origin, purposes and activities of Marian Catechists. The Marian Catechist Manual is the vademecum, the handbook, for all Marian Catechists. If you have any questions regarding the status and activities of the Apostolate, please consult this helpful guide.
In the future, God willing, the International Office of the Marian Catechist Apostolate will be located at the Father John Anthony Hardon Center at the Shrine of Our Lady of Guadalupe in La Crosse, Wisconsin. The Shrine will fittingly house this Center at which Marian Catechists can gather for private study and reflection, spiritual and doctrinal courses, and spiritual retreats. The Center will be dedicated to the memory of Father Hardon and will house the Archive and Guild of the Servant of God. For now, however, the International Office is temporarily located in the lower level of the Pilgrim Center at the Shrine of Our Lady of Guadalupe in La Crosse.
I invite you to give yourself to the service of Christ as either an Active or a ContemplativeConsecrated Marian Catechist. Those who are unable to complete the doctrinal studies and/or the spiritual practices are invited to participate in the work of the Apostolate as Associate members.
If you have not already done so, I ask you to register officially through the International Office in order that you may receive the special graces which come from participation in the Apostolate. Registration also makes it possible to share important information and makes it easier to organize meetings and retreats. To register, simply fill out and mail an application form, or send us your name and address and we will mail you information along with an application. Anyone who wishes to identify him or herself as a Marian Catechist is required to register.Finally, in accord with Father Hardon's directives, the Marian Catechist Apostolate practices the counsel of poverty. Therefore, the Marian Catechist Apostolate welcomes donations. I ask for your generosity in helping to provide for the material needs of the Apostolate.
Please keep the Apostolate and me in your prayers. Be assured that I pray each day for all members of the Marian Catechist Apostolate. May Almighty God—Father, Son and Holy Spirit—bless you, your home and your apostolate of catechesis.
I confide you and your intentions to the all-loving intercession of the Mother of God, Our Lady of Guadalupe, Mother of America and Star of the New Evangelization.


We want you to love your new Sonnet + Rose bag.
So if you have any concerns or queries about your order, please email us at sonnetandrose@gmail.com.
Please keep in mind that a refund or exchange needs to be requested within 30 days of receiving your order.


Part of the fun of flyball is your dog earning titles. For each race the team completes successfully the dogs earn points. The points are awarded per heat and in an average racing day one team races ~30 heats.


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Melbourne Symphony Orchestra Pty Ltd
Melbourne Symphony Orchestra Pty Ltd is a large-scale charity established in 1997. Their main activity is registered as culture and arts primarily serving general community in australia.
An arts leader, the Melbourne Symphony Orchestra (MSO) is recognised as a national icon and ambassador for the arts and contributes significantly to the social and intrinsic value of Victorias cultural economy. Australias oldest professional orchestra, MSO works to improve the quality and vibrancy of our creative economy through the delivery of an annual season of performance, education and broader community engagement. Through the generous support of government funding partners, corporate sponsorship, trusts and foundations, bequests and individual donations, the MSO evolves to inspire and engage audiences across Victoria, Australia and internationally by making orchestral music available to everyone. In 2019, the MSO engaged more than 5 million people through digital and broadcast channels, live in concert, at festivals and free events, on tour, via workshops and in schools. Together with its vast calendar of concert performances 172 performances, including 20 world premieres and 61 Australian works performed - the MSO delivers an extensive youth and education program in Melbourne and across regional Victoria, as well as an extensive emerging talent program to develop Australias next generation of musicians. MSO programs such as Adopt a Musician, Cybec 21st Century Young Composers Program, SnareDrum Award, Cybec Assistant Conductor and Young Composer programs champion Australias emerging artists and many of these could not exist without philanthropic support. The MSO and its Chorus of 171 volunteers performed 29 performances, including 2 regional performances in 2019. Our Sidney Myer Music Bowl concert series is celebrated as an annual gift to the 25,000 people who attend each year, and Secret Symphonies for young audiences are also valued highlights. The MSOs extensive education and community programs continue to provide opportunities for people of all ages to discover, explore, and learn more about music through performance, workshops, online experiences and resources. Thanks to the generosity of our donors, these highly-valued programs engaged close to 25,000 students, teachers and families in 2019.The Pizzicato Effect continued as the MSOs flagship community music program to inspire enhanced social, emotional and educational engagement through musical accomplishments. Thanks to continued support of trusts and foundations and private donations, the MSO provided 70 students (12 different cultures/14 different languages) from 28 schools in Melbournes City of Hume with 893 free instrumental lessons across the year. Education Week, an annual program of concerts and activities including workshops and performances tailored towards primary/secondary school students and families is similarly supported by MSO donors and engaged close to 15,000 people in 2019. Of those, 25% were able to access the program through sponsored school initiatives.
Total employee expenses: $18,757,264 (50% of revenue).
Average full-time equivalent salary: $100,846.
Melbourne Symphony Orchestra Pty Ltd has seen an average annual growth of 4% in revenue versus a 4% p.a. increase in expenses.
As of 2019, Melbourne Symphony Orchestra Pty Ltd has a debt-to-equity (D/E) ratio of 0.67. This is considered slightly riskier than average within the charity space.
Daniel Gorog
Michael Ullmer
Possibly also represents: THE TRUSTEE FOR THE BUSINESS WORKING WITH EDUCATION FUND.
Sophie Galaise
Possibly also represents: Symphony Services Australia Limited.
Oliver Carton
Possibly also represents: The Good Foundation.
Diane Jameson
David Li
Helen Silver
Possibly also represents: Victorian Arts Centre Trust.
Lorraine Hook
Margaret Jackson
Possibly also represents: The Trustee For The Foundation For Imaging Research, The Trestle Trust, Barefoot to Boots Foundation, Barefoot to Boots Limited, Burns Support Foundation Inc, University Of Divinity.
Andrew Dudgeon
Possibly also represents: American Australian Association Limited.
David Sedgwick
Possibly also represents: QUEEN'S COLLEGE MELBOURNE LTD.
David Krasnostein
Possibly also represents: National Breast Cancer Foundation, Nafsika Stamoulis Hellenic Museum Limited.
Hyon-ju Newman
Melbourne Youth Music Incorporated
We brought young Victorian musicians together to access specialist resources, equipment and expertise beyond what is available in schools. We undertoo…
Personal Injury Education Foundation Limited
PIEFs purpose is to strengthen personal injury and disability management industry capability to deliver social and economic value and community outcom…
Spiritual Health Association Limited
We developed national Guidelines for Quality Spiritual Care in Health to ensure safe and high quality spiritual care services are delivered in health …
La Trobe Lifeskills Recreation And Work Inc
La Trobe Lifeskills Recreation and Work Inc. provided support and education to people with disability within the North East Melbourne and the Loddon M…
Melbourne City Mission
Melbourne City Mission is a leading community support organisation working alongside people to live the life they aspire to, their way, providing a br…
Endorsed
Donations can be claimed as a tax deduction. (Fund name: MELBOURNE SYMPHONY ORCHESTRA FUND).
120-130 Southbank Bvd
A private Australian company is not listed on the stock exchange and is not included in the description of Australian public company or cooperative.
education, music, australia's, melbourne, symphony, symphony orchestra, orchestra, vic, concert, Southbank


Aberdeen, an international asset management company based in the UK, was in need of several video animations to help educate consumers on their value proposition and current capabilities. The videos would be integrated into their overall marketing mix with executions online, at trade shows, and in rich media advertisements.
We started with hand-drawn storyboards to define the message and flow.
Each video has a clear message paired with simple, yet beautiful graphics.
"These projects were a lot of fun.


This is your day and the food that is served is an incredibly important element in making it unique and special. We are delighted to offer you an excellent choice of menus - whether it's a simple finger buffet, a spit roast or a formal wedding breakfast.
For parties of up to 120 guests, a marquee is attached adjacent to the Cyder House. The Cyder House is fully licensed offering a superb range of selected wines and a bar as well as being fully licensed for entertainment. It is ideal for smaller receptions or for celebration meals building up to your big day. Catering is provided by our in-house catering team. Catering will be quoted according to your requirements.
For weddings of up to 48 guests, the atmospheric fifteenth century Cyder House offers a truly unique and intimate setting for your evening celebrations. Our menu emphasises bistro-style cooking, with seasonal produce from the estate. This includes game – pheasant and venison are specialities – and traditionally-reared Owlpen beef. We try and use as much of the produce of Owlpen's Elizabethan kitchen garden, set just below the restaurant. Owlpen's cellars offer a good selection of reasonably-priced wines, especially from the French and Spanish regions. However, we are very happy to source other wines you may particularly like.


The UAE is making the best use of information and communications technology (ICT) to further its economic growth out of all the countries in the Middle East and North Africa (MENA).
According to the Global Information Technology Report - a study conducted by the World Economic Forum and INSEAD, an international graduate business school - the UAE ranks first among 14 MENA countries for the second consecutive year and 23rd among 133 countries across the world, Gulf News reported.
The study analysed the link between ICT readiness and economic growth, with Sweden coming top of the global ranking.
Commenting on the UAE's strong performance, Soumitra Dutta, a professor of business and technology at INSEAD, and co-editor of the report, told the news provider: "The ranking confirms the positive impacts of the investments that the UAE has made in supporting technology excellence over the last years. Now the UAE has to build on this, and further prepare its economy for the knowledge economy."
According to economic minister Sultan Bin Saeed Al Mansouri, economic growth in the UAE will more than double to 3.2 per cent this year.


Gah, wish I could help you out.
Check out Feng's site. He has a tutorial on marker rendering.
while ive read just about everywhere that you should buy 30 50 70 or 20 40 60 im finding that in the lighter colors using 20 30 40 60 80 is better for me ! maybe just a individual thing last but not least if your using colors remeber you can use difrent percentages of grey over your colors to get nice chroma effects !
Could use Pilot hi tech fine pen.
or a Pentel pens but there heavier blacks.
Layout pads one that i can see thru.
line first, so many styles.
then higher values like 8 9 10 tend to be real dark.
in the eyes of the buyer.
do it like the nike ad says.