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BUILD A STRONG NATION THROUGH THE POLITICS SYSTEM IN DYNASTY WARRIORS 9 EMPIRES, HITTING EUROPE FEBRUARY 15, 2022
KTE Articles
Hertfordshire, 28th October 2021 – It's one thing to defeat an enemy through sheer force. Quite another to defeat them through political manipulation and intrigue. KOEI TECMO Europe and developer Omega Force revealed today even more details behind the political curtain of DYNASTY WARRIORS 9 Empires, a strategic battle experience poised to deliver action both on the battlefield and in the war room, as players vie for control of ancient China. The highly-anticipated title will release across Europe on February 15, 2022 for the Nintendo Switch™, Xbox Series X|S and Xbox One consoles, Windows PC via Steam®, PlayStation®4, and digitally on PlayStation®5*.
DYNASTY WARRIORS 9 Empires adds tactical elements to the 1 vs. 1,000 action of KOEI TECMO's revered DYNASTY WARRIORS series, enabling gamers to use the Politics System to their advantage in order to achieve greatness throughout their quest to conquer the map. In order to strengthen the military through the use of politics, players will be able to execute domestic affairs commands in order to procure the resources necessary for battles, such as gold, food, and troops. Players will also be able to recruit and hire new officers by conducting political commands, stealing valuable officers like Zhang He from a rival kingdom. Different from DW8 Empires, however, is the fact that only officers whom players assign to a certain town can participate in an invasion battle from or a defensive battle at that town, therefore, it will be more effective to recruit as many officers as possible in order to gain an advantage.
Earning the trust of these officers is also vitally important. When players have earned the trust of officers, officers will propose a variety of secret plans while players are preparing for battle. If players use the secret plan an officer suggests, they can further increase the trust of that officer. This trust pays off on the battlefield, as typically during battle, players can only give orders directly to officers who are lower in rank. However, if they have earned enough trust, players can then give orders to officers who are higher in rank. Ally officers will also conduct commands. If players execute the same command of an officer, they can activate a coordination bonus. The higher the trust, the greater the effect, and special conversations can be activated.
In addition, a new strategic element, 'territory stroll', has been implemented, enabling players to explore China while at the same time deepening relationships with officers. By interacting with officers, players will be able to earn their trust, seeing a different side of each character through interactions that include dining and fulfilling special requests. Players will also be able to recruit unaffiliated officers during strolls, and there are special unaffiliated officers that can be recruited only after the player has taken a stroll. While strolling, players will even be able to take photos in the familiar DW9 Photo Mode, allowing fans to designate everything from camera angles and time of day to the weather in every breath-taking shot.
Adding to the heightened look of the characters throughout Photo Mode and beyond is the new ability to layer armour on top of clothing in the character editor. Previously, armour and clothes were of one set, and there were separate informal clothes. However, in DYNASTY WARRIORS 9 Empires, armour can now be placed on top of clothes, meaning that, in battle, officers will wear armour, but depending on the setting, armour can be removed and informal clothes can be seen in special events such as a stroll or a wedding.
KOEI TECMO Europe also revealed that fans of the DYNASTY WARRIORS series will be able to get their hands on a special DYNASTY WARRIORS 9 Empires 20th Anniversary BOX version of the game, exclusively available through the KOEI TECMO Europe Online Store. This must-have anniversary box contains a 20th anniversary character artbook, a pack of 94 character cards with a display stand, the game's soundtrack, and a copy of DYNASTY WARRIORS 9 Empires, all packaged into a Dynasty Warriors themed collector's box. To learn more about this special edition, and future offerings, be sure to sign-up to the KOEI TECMO Europe Online Store mailing list.
For more information on DYNASTY WARRIORS 9 Empires, check out the official site, 'Like' us on www.facebook.com/koeitecmogames, and Follow us on Instagram and Twitter @koeitecmoeurope.
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04/10/2021 HAVE FUN STORMING THE CASTLE! DYNASTY WARRIORS 9 EMPIRES BLITZES EUROPE FEBRUARY 15, 2022
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text:
\section{Introduction}

Many problems in cosmology that are related either to the missing mass in galaxies and clusters
or to the formation of large-scale structures and galaxies  are solved by the
existence of a dark sector, dark matter, and dark energy, dominating the content
of the universe (e.g., Blumenthal et al. 1984, Peebles \& Ratra 2003). The standard hypothesis
 for dark matter is the cold and massive elementary particle (CDM) coming from supersymmetry
(Bertone et al 2005), although there is also a recent revival of warm dark matter models that are
able to reproduce the power spectrum of structures better at galactic scales and below
(Bode et al. 2001). All dark matter models, however, encounter persistent problems at galactic scales,
such as the predicted cusps and abundance of dark matter in galaxies that is too high (e.g.,
Wang \& White 2009, Kennedy et al. 2014, Boylan-Kolchin et al. 2011, 2012).

An alternative to dark matter models that work in Einstein gravity is to assume
that a modification of the gravity could account for the apparent dark sector and, in particular,
the MOdified Newtonian Dynamics (MOND) proposed by Milgrom (1983), which
accounts for the missing mass on galaxy scales very well (see the review by Sanders \& McGaugh
2002 and Famaey \& McGaugh 2012). The fundamental idea is based on the observation
that mass discrepancies mainly occur when the acceleration falls below the critical
value of a$_0 \sim$ 2 10$^{-10}$ m/s$^2$. At low acceleration, the gravitational force
varies as 1/r instead of 1/r$^2$. The outer parts of giant galaxies and dwarf galaxies
should fall entirely into this regime.

In standard dark matter models, bulges in galaxies are thought to be formed mainly
through major or minor mergers (e.g., Toomre 1977, Barnes \& Hernquist 1991,
Naab \& Burkert 2003, Bournaud et al. 2005, 2007a). The time scale of a merger
is short, on the order of 10\% of Hubble time or less, because of the existence of
extended and massive dark halos, which take the orbital angular momentum of baryons away
(Barnes 1988). In modified gravity models and in the absence of halos, the spiral-in of companion
galaxies occur on a much larger time scale, and
the frequency of mergers is low (Tiret \& Combes 2008b). The prediction of the number
and mass of bulges in spiral galaxies could then be a discriminant between models.
 Another way to form bulges occurs in the early universe, when gas-rich disks are unstable
to collapsing into massive clumps, which spiral in and form a bulge and thick disk
(e.g., Noguchi 1999, Bournaud et al. 2007b). Dynamical friction is thought to bring the
clumps inward, faster than their destruction through star formation feedback, and this
could also constrain dark matter models.

There is a third main dynamical process able to form bulges in spiral galaxies,
the vertical resonance with a stellar bar (Combes et al. 1990, Kormendy \& Kennicutt 2004).
These are called pseudo-bulges, since they show more rotation, more flattening, and a
radial distribution closer to an exponential than do ``classical" bulges. Bars form at
comparable frequency in MOND and Newtonian models with dark matter (Tiret \& Combes,
2007, 2008a), and pseudo-bulges are expected to form as frequently in the two models.

The goal of the present article is to compare the
formation of bulges in clumpy disks in the frame of dark matter and MOND models, to
probe early bulge formation.
The methods for the simulations are described in Section \ref{simul}, and the galaxy
models used in Section \ref{model}. The results are first presented
for dynamical friction in dissipationless models (Section \ref{stars}),
and then all the phenomena of gas-rich disks forming clumpy galaxies
with star formation and feedback are included  in Section \ref{gas},
and discussed in Section \ref{disc}.
The conclusions of bulge formation in the different models are then summarized in
Section \ref{summary}.

\section{Simulation methods}
\label{simul}

Since the MOND equations are nonlinear, it is not possible to use
normal Poisson solvers, such as the Tree code, but instead the full
differential equations should be solved on a grid.
This is very efficiently done with the multigrid algorithm
(cf. Numerical Recipes, Press et al., 1992, Brada \& Milgrom 1999, Tiret \& Combes 2007,
hereafer TC07).
 Both the MOND simulations and the Newtonian gravity comparison runs
were carried out with the same multigrid method.
For the modified gravity runs, the self-consistent Lagrangian theory AQUAL,
developed by Bekenstein \& Milgrom (1984) was used,
where the Poisson equation is written as

\begin{equation}
\label{eq:mondaqual}
\nabla [ \mu(|\nabla\Phi|/a_0) \nabla\Phi ] = 4 \pi G \rho,
\end{equation}

\noindent where $\mu(x)$ is the interpolation function that is equal to unity at large $x$
(Newtonian regime), and it tends to $x$ when $x <<$ 1 in the MOND regime.
 Various functions have been used in the literature, and for fitting
rotation curves of spiral galaxies, the best one appears to be the standard function
 $\mu(x)= x/(1+x^2)^{1/2}$ (Sanders \& McGaugh 2002), while for the Milky Way, the
best fit is obtained with the so-called "simple" function
 $\mu(x)= x/(1+x)$ (Famaey \& Binney 2005). The values of a$_0$ range between
1 and 2 10$^{-10}$ m/s$^2$, according to the $\mu$ function used: with the simple function,
the MOND regime is reached with an acceleration about one order of magnitude
greater than with the standard function (e.g., Tiret \& Combes 2008a). There are
other uncertain parameters that could influence the choice of the coupled
parameters ($\mu$, a$_0$), such as the unknown fraction of dark baryons
in galaxy disks (Tiret \& Combes 2009) or the impact of the external
field effect (Zhao \& Famaey 2006).

The multigrid method developed in the present work has been described
at length and tested in TC07, in particular the problem of boundary conditions. Equation (\ref{eq:mondaqual}) has been discretized similarly, and
the Gauss-Seidel relaxation with red and black ordering was followed.
If the convergence is very quick with the linear Newtonian Poisson equation,
the analogous MOND equations take a much longer CPU time. Then to be able to run
many more simulations in a given time, I used the quasi linear formulation of MOND,
call QUMOND developed by Milgrom (2010).

This formulation has the advantage of being much easier to solve, since
the interpolation function of a/a$_0$ has been transferred to its inverse equivalent
as a function of a$_N$/a$_0$, with a$_N$ the Newtonian acceleration.
It is a non-relativistic complete theory, derivable from an action,
but the nonlinearity can be reduced to solve the linear Poisson equation several times.
Indeed, the equation to solve is the following:

\begin{equation}
\label{eq:qumond}
\nabla^2 \Phi = \nabla [ \nu(|\nabla\Phi_N|/a_0) \nabla\Phi_N ]
\end{equation}

\noindent where $\Phi$ is the Milgromian potential and $\Phi_N$ the Newtonian one.
Since the normal Poisson equation links $\Phi_N$ and the density $\rho$
by the relation
$\nabla^2 \Phi_N = 4 \pi G \rho$,
equation (\ref{eq:qumond}) can be written as the function of two densities:
$$
\nabla^2 \Phi =  4 \pi G \rho_b + 4 \pi G \rho_{ph}
$$
\noindent where $\rho_b$ is the
 baryonic density, and $\rho_{ph}$ the so-called phantom density,
which is the equivalent of the missing mass within the Newtonian gravity.
Examples of the phantom density distribution are given by L\"ughausen et al. (2013),
it can sometimes (rarely) be negative.
The phantom density can be computed by

\begin{equation}
\label{eq:phantom}
\rho_{ph}= \frac{1}{ 4 \pi G}  \nabla [(\nu -1) \nabla\Phi_N ]
.\end{equation}

The computation of the Milgromian potential therefore can be carried out
in two linear steps. First, the Newtonian potential $\Phi_N$ is computed on the grid
from the baryonic density $\rho_b$, and the phantom density $\rho_{ph}$
is derived on the same grid, through discretization of equation (\ref{eq:phantom})
(see, e.g., Famaey \& McGaugh 2012), in a similar manner to equation
(\ref{eq:mondaqual}). Then the linear Newtonian Poisson solver is used
again, this time with $\rho_b + \rho_{ph}$.
The interpolation function $\nu (a_N/a_0)$ corresponding to the standard
$\mu$ function can easily be computed as
$\nu(y)=\sqrt{0.5+0.5\sqrt{1+4/y^2}}$. The two MOND formulations
AQUAL and QUMOND are
not completely equivalent, since their forces differ by a curl field
(Zhao \& Famaey 2010).
 The two are very close in symmetric systems, however, and in what follows,
the results from the two formulations were checked for similarity.

\bigskip

\begin{figure}[ht]
\centerline{
\includegraphics[angle=-90,width=4cm]{rotcg-dw.ps}
\includegraphics[angle=-90,width=4cm]{rotc-giant.ps}}
\caption{{\bf Left}: Circular and rotational velocities, together
with the velocity dispersions for the stellar component
in the Newtonian +DM  (top) and MOND (bottom)
initial galaxy models with stars and gas.
{\bf Right}: Same for the giant galaxy model.}
\label{fig:rotc}
\end{figure}

\begin{table*}[ht]
\begin{center}
      \caption[]{Simulation models}
\label{tab:simul}
\begin{tabular}{llrrrrrrrrrrr}
\hline
Model & M$_*$ & r$_*$  & z$_*$ & M$_g$ & r$_g$ & z$_g$ & $\beta_r$ & $\beta_t$ & C$_{star}$ & $\alpha$&  M$_{H}^{(1)}$ & r$_{H}$ \\
     &  10$^9$\msol & kpc & kpc &10$^9$\msol & kpc& kpc &     &     &    &       & 10$^{10}$\msol  &  kpc \\
\hline
dwarf$^{(*)}$ & 5.68 & 5.  &  1.  &  0. & -  & - &  -  & -  &  - &  -  &  7.5  & 12  \\
dwarf & 2.84 & 5.  &  1.  &  2.84 & 5.  & 0.5 &  0.5  & 0.5  &  2 10$^{-4}$ &  1.4  &  7.5  & 12  \\
giant$^{(*)}$ & 56.8 &  5. &  1.  &  0. & -   & -  &  -   & -   &   -  &  -   &  17.6  & 16  \\
giant & 28.4 &  5. &  1.  &  28.4 & 5.  & 0.5 &  0.5  & 0.5  & 2 10$^{-4}$ &  1.4  &  17.6  & 16  \\
\hline
\end{tabular}
\\ $^{(*)}$ These runs are purely stellar
\\ $^{(1)}$ Dark halo mass of the equivalent Newtonian system
\\ The depletion time scale is 5 Gyr, for the homogeneous gas disk
\end{center}
\end{table*}

The grid used in the present work is 257$^3$ in size. The simulation box covers a
$60\ \mathrm{kpc}$ cube, and the spatial resolution is about $230\ \mathrm{pc}$.
 The rest of the simulation code works like a particle-mesh (PM) code.
Up to 0.75 million particles are initially distributed on the grid.
 The density is computed on the grid by a cloud-in-cell (CIC) algorithm,
and once the potential is computed, particles are advanced using a leap-frog
method. For the purpose of distinguishing the various physical mechanisms,
simulations with only stars (and dark matter in the Newtonian equivalent systems) were run, followed by simulations that included gas, star formation,
and feedback. The gas dissipation was taken into account with a sticky-particle
code, as described in Tiret \& Combes (2008a). The rebound parameters
were varied from 0.4 to 1, which essentially affected the amount of
dissipation and the time scales of clump formation. The runs presented in the
following are all with $\beta_r = \beta_t = 0.5$. The variety of results obtained
with a changing gas dissipation does not fundamentally change the conclusions.

Star formation follows a Schmidt law; i.e., the star formation rate (SFR) is proportional
to a power $n$ of the local volumic density with a density threshold.
The exponent $n$ has been taken equal
to 1.4 (Kennicutt 1998). This nonlinear relation means that gas clumps will primarily be the site of star formation. The proportionality factor is selected
to give a depletion time scale for a homogeneous gas disk of 5 Gyr in its initial
state. When clumps form, the consumption time scale is considerably reduced
owing to the higher star formation efficiency in dense clumps.
A continuous mass loss from stars into the gas is taken into account
as in Jungwiert et al (2001). The mass loss by stars
is distributed through the gas on neighboring particles, with a velocity dispersion
to schematize the feedback energy.

\begin{figure}[ht]
\centerline{
\includegraphics[angle=-90,width=4cm]{decay5-dwarf.ps}
\includegraphics[angle=-90,width=4cm]{decay5-giant.ps}}
\caption{{\bf Left}: Decay of the 5 clumps containing globally
25\% of the baryonic disk as a function of time,
in the Newtonian +DM  (top) and MOND (bottom), for
the purely stellar galaxy models.
{\bf Right}: Same for the giant galaxy model.}
\label{fig:decay}
\end{figure}

\section{The model galaxies}
\label{model}

The goal of the present work is to study the formation of bulges
in the early universe, therefore the initial conditions are gas-rich galaxies
with a gas fraction of 50\% of the baryonic mass and no bulge to start with.

The stellar disk follows a Miyamoto-Nagai density profile:

\begin{eqnarray}\label{stdisk}
\rho_{*}(R,Z)&=&\left(\frac{{z_{*}}^2 M_{*}}{4 \pi}\right)\times\nonumber\\&&\frac{r_{*} R^2+(r_{*}+3\sqrt{Z^2+{z_{*}}^2})\left(r_{*}+\sqrt{Z^2+{z_{*}}^2}\right)^2}
{\left[R^2+\left(r_{*}+\sqrt{Z^2+{z_{*}}^2}\right)^2\right]^{5/2}\left(Z^2+{z_*}^2\right)^{3/2}}
\end{eqnarray}

\noindent with mass $M_{*}$ and radial and vertical scale lengths
$r_{*}$ and $z_{*}$, respectively.
The gas disk follows the same distribution with characteristic parameters
 $M_{g}$, $r_{g}$, and $z_{g}$, respectively.
All values of parameters are displayed in Table \ref{tab:simul}.
The simulation resolution ($230$ pc) is barely enough to study the vertical
structure of the gas disk ($500$ pc).
All components are truncated at three times the value of their characteristic scale,
therefore the extent of the disk is initially 15 kpc in radius.

In the equivalent Newtonian galaxies, the dark halo
is modeled as a Plummer sphere with
characteristic mass $M_H$ and characteristic radius
$R_H$. Its density is given by the following analytical
formula:

\begin{equation}\label{halo}
\rho_{H}(R)=\left(\frac{3M_{H}}{4\pi {r_{H}}^3}\right)\left(1+\frac{R^2}{{r_{H}}^2}\right)^{-5/2}
.\end{equation}
The values of these parameters M$_H$ and r$_H$ are selected so that
the Newtonian equivalent model has the same rotation curve as the disk
in the modified dynamics.
The dark matter halo is truncated at 21 kpc, and the halo masses
indicated in Table \ref{tab:simul} are relevant to this radius.

The stability of these galaxy models is controlled initially through a
Toomre parameter for the stellar disk of $Q_{\mathrm{star}}=1.5$ and
for the gas component, $Q_{\mathrm{gas}}=1.1$.
The initial rotation curves of the model galaxies are shown in Fig.\ref{fig:rotc}.
 To avoid artificial initial relaxation of the disks, particles are
advanced during a typical rotation period in the frozen initial potential,
computed with the multigrid potential solver. No gas dissipation or star formation
are included in this relaxation phase.

\section{Results}
\label{res}
  To isolate the main physical parameters, purely stellar models
are run first, although they do not correspond to the reality of galaxies in
the early universe.  They are compared to analogous simulations,
where half of the baryonic mass is gas, which emphasizes the role of dissipation,
star formation, and feedback.

\begin{center}
\begin{table}[ht]
      \caption[]{Estimate of decay time scales for Newton+dark matter models}
\label{tab:decay}
\begin{tabular}{lrr}
\hline
Model & 5 clumps$^{(1)}$ & 3 clumps$^{(2)}$  \\
\hline
dwarf & 1.4$\pm$0.2    & 0.7$\pm$0.12 \\
giant  & 0.5$\pm$0.07  & 0.2$\pm$0.04 \\
\hline
\end{tabular}
\\ $^{(1)}$ Each clump has a mass of 5\% of the baryonic mass
\\ $^{(2)}$ Each clump has a mass of 10\% of the baryonic mass
\\ Decay time scales are in Gyr
\end{table}
\end{center}

\subsection{Dissipationless models}
\label{stars}

  Two extreme mass models, dwarf and giant galaxies, were run with the
same characteristic scales, but with masses that are different by an order of magnitude
(see Table \ref{tab:simul}). To quantify the effects of dynamical friction,
initial clumps were simulated by massive particles, in two options:
either five clumps in all containing 25\% of the disk mass or
three clumps containing 30\% of the disk mass were distributed randomly
with the same initial velocity distribution as the rest of particles.

In total, eight types of runs were carried out with two mass models, with two types of clumps,
and for the two gravity models. For each type of run, ten different random realizations
of the initial conditions were used, to average out the results.
The decay of the clumps through dynamical friction is illustrated
in some of these runs in Figure \ref{fig:decay}.
 An estimate of the decay time scale (time for the clumps to fall
from their initial radius to the central region at 1-2kpc where their
orbit reaches a stationary state)
is obtained through averaging of these clump orbits,
and is gathered in Table \ref{tab:decay} for the Newton+DM runs.
All realizations of a given run type
are averaged out, with all orbits that are selected randomly. This procedure
looks more realistic than launching a given clump alone at an external radius,
since the dynamical effects of all the clumps interfere in the deformations
they impact on the dark halo and other particles in the disk.
This interference of several clumps can reduce and sometimes increase the dynamical friction effect
(Weinberg 1989). Also the decay time scales depend on the launching radius,
and in the same run, the clumps starting at smaller radii have a shorter
decay time scale.

Although these final averaged values have relative error bars of 10\% to 20\%, they are
compatible in their mass and density dependency with the Chandrasekhar
formula for dynamical friction (Chandrasekhar 1943). The decay time
is predicted to be inversely proportional to the clump mass, for a
given background distribution, and with the present assumptions on
radii and mass ratios between clumps and disk, roughly inversely
proportional to the square root of the total host mass. It is only
an approximation of course, since many other parameters enter into account,
such as the initial velocity of the clump and the dark and baryonic radial mass
distributions.
It was not possible to measure the
corresponding values in the MOND models, because of weak dynamical friction.

\begin{figure}[ht]
\centerline{
\includegraphics[angle=-0,width=8cm]{qclump-3pl.ps}}
\caption{All baryons (left) and gas (right) surface densities of the dwarf
clumpy galaxy, simulated with MOND gravity, at epochs 0.5, 1, and 2 Gyr.
Each panel is 60 kpc in size. The color scale is logarithmic
and is the same for all plots.}
\label{fig:qclump}
\end{figure}

\begin{figure}[ht]
\centerline{
\includegraphics[angle=-0,width=8cm]{qclump2-3pl.ps}}
\caption{All baryons (left) and gas (right) surface densities of the giant
clumpy galaxy, simulated with MOND gravity, at epochs 0.5, 1, and 2 Gyr.
Each panel is 60 kpc  in size. The color scale is logarithmic
and is the same for all plots.}
\label{fig:qclump2}
\end{figure}

\begin{figure}[ht]
\centerline{
\includegraphics[angle=-90,width=8cm]{sfr.ps}}
\caption{Evolution of the star formation rate (black line, left scale) and the
remaining amount of gas (red lines and middle scale) in the giant galaxy,
with MOND (left), and Newtonian dynamics (right). }
\label{fig:sfrate}
\end{figure}

\subsection{Models with gas, star formation, and feedback}
\label{gas}
Figures \ref{fig:qclump},  \ref{fig:qclump2}, and \ref{fig:newtg2}
show the evolution of the gas and total baryonic component of some
models with gas. The disks are highly unstable to clump formation
owing to the high gas fraction of 50\% and the absence of a bulge. Control runs
with only stars were relatively stable, but they formed a strong bar,
after 500 Myr for the MOND disks and more than 2 Gyr for the Newtonian ones.
 The mass in clumps increases at the beginning with the gravitational
instability due to the gas dissipation and large gas fraction. But these overdense
regions are very efficient at forming stars, and the gas fraction in clumps decreases,
as does the global gas fraction. Figure \ref{fig:sfrate} shows the evolution
of the star formation rate (SFR) with time and the corresponding consumption of the gas.
 Since the SFR law adopted is nonlinear, the formation of dense clumps
leads to intense starbursts with an episodic character, which consume
the gas much more quickly than  the analogous quiescent, almost homogeneous disk galaxy,
which was used to calibrate depletion time.

 In the absence of external gas accretion and replenishment of the gas content,
the disk becomes more
stable. Through both the star formation feedback and the gravitational shear
on the stellar clumps, the mass fraction in clumps slowly decreases.
The dynamical friction due to the dark halo on the clumps is, however, fast
enough to bring the clumps towards the center and build a bulge in the
Newtonian runs. In the MOND models, the stellar fragments are maintained in
the disk, because of  the weaker dynamical friction from the disk.

The evolution of the stellar surface density $\Sigma$ as a function of time
is shown in Fig. \ref{fig:prof-ens2} for the giant galaxy in the Newtonian model
and in Fig. \ref{fig:prof-ens2} in the MOND gravity.
Initially, there is an exponential distribution in the disk, while a second component is
progressively accumulated toward the center in the
clumpy galaxy with dark matter. An edge-on view reveals that
there is indeed a small spheroid in the center, along with a thick disk (Fig.
\ref{fig:edge}). This initial bulge formation due to massive clumps
has been discussed widely in the literature (Noguchi 1999, Immeli et al. 2004,
Bournaud et al 2007b, Elmegreen et al. 2008), along with the formation of a thick
disk from star formation
in a turbulent gas disk (Bournaud et al. 2009).
 We show that this rapid and early bulge formation does not occur
in the MOND gravity model. The disk remains clumpy until 2~Gyr, as revealed
by Fig. \ref{fig:prof-ens2}. This is the natural consequence of a much
longer dynamical friction time scale.

\begin{figure}[ht]
\centerline{
\includegraphics[angle=-0,width=8cm]{newtg2-3pl.ps}}
\caption{All baryons (left) and gas (right) surface densities of the giant
clumpy galaxy, simulated with Newtonian+DM gravity, at epochs 0.5, 1, and 2 Gyr.
Each panel is 60 kpc in size. The color scale is logarithmic
and the same for all plots.}
\label{fig:newtg2}
\end{figure}

The mass fraction in clumps was monitored as a function of time,
in the same manner as described by Bournaud et al. (2007b).  The surface
density of the baryonic component was computed at each snapshot.
It was first smoothed at a resolution of 700 pc to reduce noise, and
the azimutal average surface density $\Sigma$(r) computed at each radius.
When the local surface density was higher than three times $\Sigma$(r), it was considered
to belong to a clump. When plotted together, these regions do correspond
to the main clumps seen in the maps. There is no ambiguity with spiral arms,
since the clumps are dominating the global spiral structure (see Fig. \ref{fig:qclump}).
 The number of clumps found by this method is typically 10 to 20. The fraction of the disk
mass in clumps can reach at the maximum of the starburst of the order of 30\%.
Figure \ref{fig:clumpf} displays the clump mass fraction evolution for the giant
model galaxy. It is remarkable that in the MOND regime, the disk galaxy remains
highly clumpy, while in the Newtonian gravity with a massive dark matter halo,
the clumps are driven toward the center, and the disk becomes more homogeneous
after some last starbursts have consumed the remaining gas.

\begin{figure}[ht]
\centerline{
\includegraphics[angle=-90,width=8cm]{prof-ens2.ps}}
\caption{Stellar profile of the giant galaxy in the Newtonian dynamics,
at various epochs (0, 0.5, 1, and 2 Gyr). A bulge is building
alongside the exponential disk.}
\label{fig:prof-ens2}
\end{figure}

\begin{figure}[ht]
\centerline{
\includegraphics[angle=-90,width=8cm]{prof-qclump2.ps}}
\caption{Same as Fig. \ref{fig:prof-ens2} for the MOND model.}
\label{fig:prof-qclump2}
\end{figure}

\subsection{Dynamical friction}
\label{DF}

The different dynamical friction efficiency in the two gravity models
is the key to understanding the morphology of clumpy galaxies in the early universe
and the bulge formation. The main phenomenon at the origin of the drag on the
clumps is the deformation or wake
that a massive body imprints on the background distribution of particles. When the
bodies have low mass with respect to the total system, their wake is a
small perturbation, and the process can be handled analytically. However,
with massive bodies, it is not an intuitive process to
derive the actual effect of the friction,
especially when the massive bodies are numerous, and their wakes interfere.
They can perturb the system significantly, so that it cannot be considered
as an infinite reservoir of energy and angular momentum.

Results that may look controversial at first glance have been claimed in the literature.
A perturbation study by Ciotti \& Binney (2004) concludes that dynamical friction is stronger
in MOND. They consider only very low-mass
bodies, like star clusters, with a negligible effect on the full stellar
background, and adopt an impulse approximation
for deflection or orbits and linear summation of effects. For the Newtonian model with dark matter, they
consider the dark matter halo as a rigid
background that does not participate in the dynamical friction. They find that
the two-body relaxation time is shorter for disks in the MOND regime
and extrapolate these results to the dynamical friction
time, obtained for test particles in the local formula of Chandrasekhar (1943).
The consequences would be that globular clusters should spiral inwards
to the center in dwarf galaxies on a few dynamical time scales,
as well as galaxies in groups and in clusters. Simulations
by Nipoti et al. (2008) confirm these findings in the context of
 tiny perturbations:
the massive bodies subject to the friction, either globular clusters or a
rigid bar, have to contain less than 5\% of the baryonic mass, so that particles
in the stellar background absorbing the energy and angular momentum are
not significantly perturbed.
In realistic systems though, Nipoti et al. (2007) find that the merging time scales
 for spherical systems are significantly longer in MOND than in Newtonian gravity
with dark matter, and Tiret \& Combes (2007) found that bars keep their pattern speed
constant in MOND, while they are strongly slowed down in the Newtonian equivalent
system with a dark matter halo.

The main conclusion of these apparently different claims is that
the dynamical friction time scale is greater in MOND for satellite
galaxy interactions and for stellar bars, since
galaxies are not embedded in extended and massive spheroids of dark matter particles, which are
able to accept the orbital angular momentum.
Although the impact of very small fluctuations could be greater in MOND
than in Newtonian dynamics, the effect saturates quickly when the perturbation
is no longer infinitesimal. In contrast, the equivalent Newtonian system
with dark matter has shorter dynamical time scales, and common satellites and bars
are slowed down in a few rotation times.
The present results extend these conclusions for clumpy galaxies,
which are typical of high-redshift systems, where the total clump mass fraction
can reach 30\% of the disk mass, with individual clumps of 10$^8$-10$^9$\msol.
The typical time scale for the clumps to be driven to the center and form
the bulge in the Newtonian model with dark matter
is about 1~Gyr for the giant galaxy and 3~Gyr for the dwarf.
For the MOND model, the dynamical friction is not efficient enough to form
a bulge before the clumps are destroyed or reduced by the star formation feedback
and the tidal and shear forces.

\begin{figure}[ht]
\centerline{
\includegraphics[angle=-0,width=8cm]{edge.ps}}
\caption{Evolution of the edge-on morphology of the giant galaxy,
in the Newtonian gravity model with gas and star formation.}
\label{fig:edge}
\end{figure}

\begin{figure}[ht]
\centerline{
\includegraphics[angle=-90,width=8cm]{clumpf.ps}}
\caption{Evolution of the clump mass fraction (see text for the definition) for
the giant galaxy, in the MOND gravity (left) and
in the Newtonian gravity (right).}
\label{fig:clumpf}
\end{figure}

\section{Discussion}
\label{disc}

The present simulations are based on the simple model of sticky particles for the gas physics
and dissipative character. Previous works have used different methods, either sticky particles
(Noguchi 1999, Immeli et al 2004, Bournaud et al 2007a, Elmegreen et al 2008), AMR
hydro-code (Dekel et al 2009, Ceverino et al. 2010, Behrendt et al. 2014) ,
or Tree-SPH code (Hopkins et al. 2012).
The results are very similar, as far as the instability of the early galaxies is concerned.
 Massive clumps are formed, reproducing clumpy galaxies at high redshift. The importance
of the bulge formation is variable according to the stellar feedback adopted. Clumps
are driven to the center through dynamical friction in less than 1 Gyr for massive
galaxies of $\sim$ 7 10$^{10}$ \msol\, in baryons, but extreme supernovae feedback could
significantly reduce the mass of clumps ending in the bulge (Hopkins et al. 2012).
The bulge in all cases has a stabilizing influence on the disk, and after the clumpy phase,
the disk remains quite homogeneous, even in the case of abundant external gas accretion
(Ceverino et al 2010).
We have tried several degrees of dissipation, and the variation
of the collisional parameters $\beta$ between 0.3 and 0.7 did not have a strong influence on
the results, confirming the conclusions of Bournaud et al. (2007a).
The essential point is to have sufficient dissipation in the gas to allow its collapse
into dense clumps and to enhance the star formation rate through a nonlinear
Schmidt law.

It is also necessary to check that the spatial resolution of the simulations
is not perturbing the main conclusions. The 257$^3$ grid means a resolution of 230~pc
for the potential solver, it is always lower than the Jeans scales.
From initial conditions, it is possible to predict the range in sizes and
masses of clumps in the unstable disks (but see Behrendt et al. 2014).
The Jeans length in an axisymmetric disk is $\lambda_{J}= \sigma_g^2/(G \Sigma)$,
where $\sigma_g$ is the gas velocity dispersion, and
 $\Sigma$  the disk's surface density.  These range from 0.5 to 1~kpc in the dwarf
galaxy model and from 1.4 to 2~kpc for the giant. The corresponding ranges in mass
of the clumps are M$_{J}= \pi \sigma_g^4/(G^2 \Sigma)$,
between 10$^6$-10$^8$\msol\, for the dwarf galaxy, and
10$^8$-10$^9$\msol\, for the giant model.
A higher resolution simulation with 513$^3$ grid has been run for the dwarf galaxy
model, increasing the number of particles to six million. The clump mass fraction
is plotted in Fig. \ref{fig:clumpf-dwarf}. In general, the evolution is similar,
with the clump fraction determined with the smoothing length adapted
to a factor-2 higher spatial resolution.

\begin{figure}[ht]
\centerline{
\includegraphics[angle=-90,width=8cm]{clumpf-dwarf.ps}}
\caption{Evolution of the clump mass fraction for
the dwarf galaxy in the MOND gravity (left) and
in the Newtonian gravity (right). The high-resolution run with a 513$^3$ grid
and 8 times the number of particles is plotted in red.}
\label{fig:clumpf-dwarf}
\end{figure}

Another interesting issue is the stability of the considered disks to
large-scale waves, although small-scale fragmentation is dominant.
The critical wavelength $\lambda_{crit}$ above which disks should be stabilized
by differential rotation, even without pressure (dispersion) terms,
indicating that the self-gravity scale is
$\lambda_{crit} = 4 \pi^2 G \Sigma /\kappa$, where $\kappa$ is the epicyclic frequency. It ranges from 1-3~kpc in the dwarf galaxy and from 2-6~kpc for the giant. The role of
the dark matter halo is proportionally much higher in the dwarf.
The X-Toomre parameter, X = $\lambda/\lambda_{crit}$, where $\lambda\sim 2\pi r$
controls the self-gravitating response of the disk through
the swing amplifier; waves develop more efficiently when X$\sim$ 2
(Toomre 1981). In the present galaxy models, a
central region always exists where X $\sim$ 1-2.

\section{Summary}
\label{summary}

Simulations have been carried out of the dynamical processes occurring
early in the universe, in galaxies that are very rich in gas, and corresponding
to the clumpy galaxies observed at high redshift (e.g.,
Elmegreen \& Elmegreen 2005, Elmegreen 2007). Previous works have established that
bulge formation is rapid in those galaxies through dynamical friction driving
the clumps to coalesce in the galaxy centers (Noguchi 1999, Bournaud et al. 2007b,
Elmegreen et al 2008). The present work explores the analogous phenomena
in modified gravity (MOND, Milgrom 1983). A multigrid code is used to solve
the nonlinear equations, both from the original AQUAL Lagrangian (Bekenstein
\& Milgrom 1984) and the QUMOND solution, recently developed by Milgrom (2010).
 Both appear to give similar results, and most runs were performed in the
faster method of QUMOND.
For each galaxy model, the corresponding rotation curve is first computed in
MOND, and then an equivalent Newtonian system is built with a dark matter
halo added, in order to get exactly the same rotation curve as in
Tiret \& Combes (2007, 2008a).
The efficiency of dynamical friction was first compared between the two gravity models,
with academic purely stellar runs, where an ensemble of clumps were
randomly distributed initially with 20-30\% of the baryonic mass.
 A series of such simulations show that clumps should spiral inwards to the center
in the Newtonian galaxies in about 1~Gyr or less, while the clumps remain orbiting
in the disk for more than 2-3 Gyr in the MOND regime.

The most realistic simulations include gas dissipation, star formation, and feedback.
Disks are initially composed of 50\% stars and 50\% gas.
Rapid fragmentation occurs in these unstable disks, and clumpy galaxies that are
similar to what is observed at high redshift are formed in both gravity models.
This clumpy morphology lasts less than 1~Gyr in the giant galaxy model
of baryonic mass 5.7 10$^{10}$ \msol and 3 Gyr in the dwarf galaxy, with
ten times less mass. Clumps are driven inwards by
dynamical friction, and form a spheroidal bulge.
This is very compatible with previous works.
However, in the MOND gravity model, the clumps remain in the disk for
a much longer time, are eventually destroyed or reduced by stellar
feedback and shear, and have no time to fall in the center to form a bulge.
 The lower bulge formation efficiency in MOND is more in line with
the large number of observed bulgeless galaxies today (Kormendy et al. 2010).

Fisher \& Drory (2011) also find that the galaxies that contain either a pseudo-bulge or no bulge
represent more than 80\% of galaxies above a stellar mass of 10$^9$\msol\, in the
local volume of 11 Mpc radius.
This is difficult to explain in the standard Newton plus dark matter models.
Weinzirl et al. (2009) compare the observations of the bulge mass and frequency in present-day
galaxies with the predictions of the CDM model. Massive galaxies can have less than 20\%
of their baryonic mass in a bulge if they experience mergers only before z=4. But
 galaxies having later mergers and larger fractions of their mass in a bulge are
 about 30 times more abundant in CDM simulations than observed.
Zavala et al. (2012) and Avila-Reese et al (2014) revisit the CDM predictions, with
semi-enpirical recipes and an analytical treatment to follow the transfer of stellar
masses to bulges after a merger. They assign the stars coming from merging satellites to
the classical bulges and stars coming from the primary during the merger to pseudo-bulges.
But they do not consider the pseudo-bulges formed by secular evolution of bars.
They then claim to form less classical bulges, since there is now only one path to form them.
Also the result depends on the adopted evolution of the stellar-to-halo mass relation, the mass assembly
in their models resembling more a monolithic scenario than a hierarchical one.
In any case, there are still problems explaining the large fraction of bulgeless galaxies
observed locally.

In the framework of MOND, classical bulges are hardly formed in early times in the
clumpy phase of galaxy formation, when gas is dominating the surface density of galaxy disks.
They can form later through hierarchical merging with a frequency that is
smaller than what occurs in the analogous Newtonian systems with dark matter.
Pseudo-bulges, however, form with equivalent frequency through secular evolution
by vertical resonances with bars.  It is therefore expected that the relative frequency
of pseudo-bulges is higher in MOND. More quantitative statements will require
many more simulations with a cosmological context.

\begin{acknowledgements}
 I warmly thank the referee, Stacy McGaugh, for constructive comments and suggestions.
The idea of this work came when Eija Laurikainen asked me to write a review article on
bulge formation with MOND.
The European Research Council
for the Advanced Grant Program Number 267399-Momentum
is acknowledged. Most simulations have been run on the cluster
provided by this ERC grant.
\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


Palmetto Football Talk | View topic - Westwood Antics! Is It A Blythewood Thing?
Westwood Antics! Is It A Blythewood Thing?
Chippy-ness gone awry! This year with Westwood. L.Y. with Ridge View. They both have really good athletes that suit up for them. But, dang you can count on them having a bunch of "trash talk and unsportsman like antics too"!
If they had "just played football" they had a good chance of beating The Stallions! But, no, they hung in tough in the 1st qtr after SP went up 13-0(missed PAT). The QB Green had a nice game! #8 seemed like their best player; although #1 is the kid signed to South Carolina. Both good - both very much could stand to go out and just focus on football during the game too! Be pumped! Be edgy! But, be smart for crying out loud.
I can't tell you how in the world #1 is supposedly better than #8. 8 was the punter, WR and "Bail Out WR Target"! And the kid just kept making play after play against really good defense. He was just better. The defense was there; can't really fault the Stallions on that. Kid just made plays!
This is one I hope Coach Herron turns into the SCHSL regarding the officials. They let way too much go. In fact, had they gained control of the game earlier, it may not have "almost" gotten out of hand.
Lots of jawing! Lots of Personal fouls that really ended up motivating the Stallions! So, thank you for that bit of what you did.
End of the game as SP is running out the clock. #1 is on the Stallions sideline dancing. Jawing with Stallions players. Hand gestures trying to be a complete (I don't know what) as he could possibly be. I guess he was proud of the fact, "they played us close"!
Just really not classy at all. Especially considering the fact you were down two TD's.
I see Westwood winning a bunch more games than they lose. But, composure had better grab hold of that team or they will keep imploding. Yeah, imploding. Did I mention they had a 21-20 lead starting the 4th qtr?
Ridgeview L.Y. same thing - was playing well and then got to jawing! Taken completely out of their game! When they got down early and was in comeback mode; they was just playing football and was hanging tough!
Some never learn I guess!
"WHEN YOU'RE EVERYBODY'S SUPER BOWL"! I guess folks get way way way more animated!
Re: Westwood Antics! Is It A Blythewood Thing?
…….….. listening to a fan of another team who was off tonight leaving the stadium when he said, "they were trying to do what South Pointe do to people"!
He went on to say, "out South Pointe; South Pointe"!
Laughable! Some of BC South Pointe teams maybe had that rap! Coach Herron doesn't like that non-sense. And, has little tolerance for it.
I'm all for bully the bully! Except make sure you have a bully on your hand and not a "sleeping giant"!
Does Blythewood trash talk too, or is it just the other two schools?
Saw Westwood play the last couple of years. Always the same deal. Their performance never matches their talent. Undisciplined. Seems like the coaches just let it go in an attempt to build the kids confidence in some misguided attempt to create some type of swag. Westwood could be a good team if they would find somebody to instill some discipline. Plenty of talent there.
@region2 - you must be Nostradamus! You kind of predicted what was going to happen exactly how it went down!
Man, them and RV could be real good teams w/o all the antics! If they just shut up and played ball! Coach Herron does not play that - but the kids on the roster have to fight everything in them "not to go there" b/c coach doesn't! When some team gets to bumping the gums too much - they tend to just play with more intensity! They "do talk back too" if you get the right Stallions player. But mostly, they about playing harder and trying to let the scoreboard talk for them!
According to the Beaufort players, YES. Far too much for a team that talented.
I do not know where they got the Refs for the South Pointe vs Westwood game, but it seems to me that they were scrapping the bottom of the barrel with that bunch of Zebras.
WS2 - Agreed! In particular the line judges were awful. The missed offensive P.I. was maybe the worst most blatantly missed call I have ever seen! And they ended up scoring later after having gained a 1st down on that pass. No holding calls on them and they were routinely holding Rontarious Aldridge.
I have heard fans from other teams who are the "favorite" complain about the same thing! Some of these refs come in seemingly trying to "level the playing field"! Help the David out versus the goliath if you will. But, dang that's wrong! Those kids worked their butts off too! Why should they have to face adversity they shouldn't have to worry about just to satisfy some sense of "fairness"! Last night, WW was bigger than SP. They looked very much the part of an undefeated team physically! I hate that underdog ref bias!
Underdog Ref Bias. . . . . . now trending on twitter! B/C I swear that's what I saw last night. Check my post since my time on PFT. - . not a complainer about calls normally but that crew was apparently straight from Blythewood. Probably live off of Killian Road. They conversed with the Redhawks coaches during timeouts. Before the half ended. During a long injury timeout. Never with the SP coaches. Just blatant.
Both Westwood and Ridge View seem much more interested in recreating a high school version of 'the U" from the 80's than focusing on winning football games. Usually implodes on them both in the long run. Suppose they think faking some type of swag will intimidate someone. Only people it intimidates are the cupcakes they would beat anyway. Doesn't faze the good teams.
"FAKE SWAG" is the worst! Be confident b/c you have prepared for the game. Don't bump gums off left and right and not backing it up on the scoreboard! I guess WW came in unbeaten and wanted to "show they wasn't scared or intimidated"! Best way to do that is --- not talk about it ----- but show it!
Region2 your right - 80's Miami Hurricanes thuggish stuff is weak!
p.s. I was really disappointed in Coach Parks team last year! The pre-game speech to must have been all week getting those kids to almost wanting to start a fight ( not football ) from the very beginning of the game. I thought he was of a different sort; but was wrong! Kind of surprised me honestly!


text:
Reference | FYI
Loopholes let records pertaining to Abe's scandals slip through the cracks
Former education ministry bureaucrat Kihei Maekawa has pointed to the existence of documents alluding to Cabinet Office pressure in the approval of a new university veterinary department that benefited a friend of Prime Minister Shinzo Abe. | KYODO
by Reiji Yoshida
The Cabinet of Prime Minister Shinzo Abe is in crisis, stung by scandals that have bitten into his public approval ratings in recent weeks.
At a glance, these scandals look like separate events with little connecting them. But experts say they have one grave problem in common: an apparent violation of the Public Records and Archives Management Act.
How have government documents been mismanaged in the scandals? Why are they important? What measures are experts proposing to improve the situation?
Following are questions and answers about the government document management law and apparent violations in recent scandals:
What role do government documents play in the recent scandals hitting the Abe administration?
Expert say the scandals have all involved apparent violations of — or use of a loophole in — the Public Records and Archives Management Act.
Enacted in 2009 and implemented in 2011, the act obliges the government to prepare, register and preserve "administrative documents" so citizens can later look into how a government decision was made.
In some of the scandals, the government has been blamed for discarding key records by taking advantage of an apparent loophole in the law. In others, the government refused to investigate state papers leaked to the media, insisting they are not "administrative documents" covered by the public record act and don't need to be disclosed.
"It has become clear that the government is managing administrative documents in a very sloppy way," said Hajime Sebata, a lecturer of modern Japanese history at Nagano Prefectural College.
"Rather, it regards only documents that officials consider are necessary for themselves as public documents," said Sebata, who is familiar with the history of the government's document management policy and wrote a book about it in 2011.
The government doesn't "understand why the information disclosure law and the public record and archive management law were enacted," he said.
Why is compliance with the Public Records and Archives Management Act important?
The law was enacted after a number of government scandals involving the loss of official records, including the pension premium payments of millions of people that came to light in 2007.
Until the enactment of the law, the government was not obliged to prepare, manage or preserve administrative documents.
Document management was separately decided by each ministry, and many historical documents — including those concerning secret diplomatic arrangements with other countries — were lost or at best later discovered among papers in the private possession of former bureaucrats and politicians.
Together with the 1999 information disclosure law, citizens for the first time won a public system guaranteeing the preservation of, and access to, government documents detailing the processes of administrative actions.
"I sometimes go to America and see public archives and records. I was stunned to see the massive amount of documents there" compared with the small volume of historical government records preserved in Japan, Sebata said.
"The foundation of democracy lies in the use of sovereign power by the nation based on unrestricted access to accurate information and sound judgments by the people on it," declares the preface of a 2008 final report by a government expert panel on public document management.
How has Abe's government allegedly mishandled government documents?
In the Moritomo Gakuen scandal, the Finance Ministry sold a plot of land in Toyonaka, Osaka Prefecture, to the school operator in June last year at a whopping 86 percent discount.
During Diet sessions, Finance Ministry officials claimed they had discarded all of the records detailing the negotiations with Moritomo Gakuen. This thwarted an investigation by opposition lawmakers.
The public records law obliges the government to prepare, register and preserve administrative papers for between one and 30 years, depending on their degree of importance.
However, each ministry is authorized to judge the degree of importance of each paper. If a ministry judges that documents don't fall into the category of "historical public records and archives" it can set the preservation period at less than one year. The Finance Ministry has been criticized for taking advantage of this loophole and quickly discarding the records pertaining to Moritomo Gakuen.
Kazuhiro Nakamoto, president of the Japan Federation of Bar Associations, released a statement April 28 pointing out that the loophole allows government entities to interpret the public records law "in an arbitrary manner" and quickly throw out official papers.
The JFBA also called on the government to keep all electronic data files of government documents for a certain period of time. It said specialized archivists, not a government agency, should be allowed to decide which papers are to be discarded.
The Kake Gakuen scandal also involved an alleged violation of the public records law.
Abe's government has been accused of favoring the Okayama-based school operator in a special deregulation project to open a new veterinary department at a university — the first anywhere in Japan in 52 years.
The government has flatly denied engaging in favoritism. However, several internal documents created by the education ministry, leaked to the media in May, quoted Cabinet Office officials as saying it was Abe's intent to favor Kake Gakuen.
The Cabinet initially refused to launch an investigation into these papers, insisting they were not "administrative documents" because it could not find copies of any of them in a shared online folder used by ministry officials.
But later it was revealed that ministry officials shared digital copies of some of the leaked documents by email. Copies of others were found on the computers of bureaucrats in multiple sections of the ministry.
Still, the Cabinet has insisted they are not "administrative documents" but "private memos" kept by ministry officials.
Many experts argue that all of the leaked Kake Gakuen papers, including those shared by email, are "administrative documents" as defined by the law.
Article 2 of the act simply defines all government papers that are prepared or obtained by government workers and shared for "organizational use" as "administrative documents." No other conditions are given.
"Now officials seem to be trying to regard some documents as 'nonadministrative' because they want to hide papers that are inconvenient for them. Such an interpretation of the law is wrong," Sebata said.
How about the data cover-up scandal that forced Defense Minister Tomomi Inada to resign on Friday?
Inada stepped down to take responsibility for "failing to oversee" Defense Ministry and Ground Self-Defense Force officials who tried to cover up daily activity logs of the GSDF's peacekeeping operation in South Sudan in February.
The GSDF found digital copies of the data owned by a GSDF member in December and was obliged to disclose them under the information disclosure law in response to a request from a freelance journalist.
But officials reportedly decided to conceal the data files by regarding them as documents privately owned by the GSDF member, instead of as "administrative documents" held by the GSDF.
This decision was "inappropriate" and violated both the information disclosure law and the Self-Defense Forces Law, according to a report released Friday by a special government inspection team looking into the scandal.
Under the information disclosure law, any administrative document is to be released to the public if requested unless it violates privacy or causes problems in diplomacy, defense or other sensitive government matters.
Article 56 of the SDF law meanwhile stipulates that SDF personnel must comply with laws and ordinances in performing their duties.
scandals, Defense Ministry, Moritomo Gakuen, Kake Gakuen


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text:
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Dirty Machine (2009)
Alternative rock, blended with Jah dropping reggae, ass shaking funk, and just a touch of hip-hop. Their unique blend of college rock coupled with their consistently superb songwriting makes them a force to be reckoned with in the underground music scene.
Their recently released debut album, Dirty Machine, at a whopping 15 tracks, has received rave reviews. Corky Laing of 70's super group, Mountain, says the songwriting on the album, "speaks for itself." When asked about their wide range of musical influences, Blueshift responded, "Any music we feel passionate about naturally becomes an element of our own unique style." Blueshift formed in the summer of 2004 when childhood friends Jared O'Connell and Waylon Nicholson wanted to start a band together. After recruiting Tim Qualls for drums and Alex Izzarelli for bass Blueshift set out collaborating on a batch of songs, and fine-tuning originals already written by Jared O'Connell, Tim Qualls, and Waylon Nicholson. In the summer of 2005 Blueshift added Nick Tudor to the band on saxophone, and keys to give Blueshift the full sound that is has today.
http://www.blueshiftrocks.com
Blueshift has over 25 original songs (and counting). In each set you will hear approximately 1-3 covers, depending on the length of the set.
A typical Blueshift setlist would look something like:
In My Own Way
E.C.L.
Dirty Machine
Sir Duke (Stevie Wonder cover)
Wounded Man
We All Belong
Happy Later
That Something
Watchin' the detectives (Elvis Costello cover)
These Daze
Be Now
Four-Leaf Clover
The Seed 2.0 (The Roots cover)
These are Times
Messin'


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I have a new to me 71 0r 72 Speedway Blue Angel. It has an HS40-55395C Serial Number1295B.
I was checking the point gap and I see there is no condenser. All of the wires seem to have a home and I have spark at the plug.
Is there suppose to be a condenser in this ignition circuit?
I probably should have posted this on the Tecumseh thread. I'm a newbee.
Yes, it should have a condenser. There wont be any extra wires, since the condenser contains a wire with a terminal lug. It is connected to your points. Part number 30548B.
Something else you should know is that the engine will run without a condenser. The purpose of the condenser is to decrease voltage across the points as they open. The condenser is there to protect the points.
The other thing you should know is that these engines need to be timed to where the points open at a specific distance before top dead center of the piston. That is an adjustment found in the appropriate section of the Tecumseh manual. You can find the manual on line as a sticky here.
You basically use a depth gauge to measure your piston "in the hole" and an ohm meter (or continuity tester) to ensure the points open at exactly what "in the hole" depth it is supposed to be for a particular engine. In your case, it is .035" before top dead center. The place at which the points open at is set via the "stator plate" which is that aluminum piece your magneto sits on. Loosen the two bolts and rotate it.
Sorry to sound like a broke record. If you are missing the damn condenser, someone has been in there screwing around. I'd clean the points with emery cloth, get a condenser, and time it.
Thanks for the informative reply. I've watched the factory tech youtube video on timing I just got stuck on the condenser issue. Thanks for the BTC setting. Back to the garage.
The points were opening at .044 reset to .035 and ordered a condenser Thanks again.
I think your points set at .020 , timing might be at .035 BTDC. Good Luck and you do need a condenser for sure !
You're welcome. Good job of timing it. Note the position of that condenser. You'll need that long screw that holds it as well.
Got my condenser buttoned everything up. It fired right up and ran great for about 30 seconds and then gas started shooting out of a breather hole on the side of my shiny new chinese carb. That ones going back to the ebay seller tomorrow.
You need to adjust the float level. Too much fuel is in the bowl, causing the engine to flood. They don't come in the mail with the proper float level set. I go for level on the Tecumseh's.
You are right about that. I took the bowl off to check the float, the needle was there but the seat was missing. The poor guy is going to have more in postage than you can make on a ten dollar carburetor. On the positive side it fired right up.
The seat is a tiny O ring that sits so far up the tiny bore there that it borders on impossible to see. That seat doesn't fall out, in fact some people even think it is not there and insert another seat on top of it. The float adjusts like all of them, with the tang which strikes the base of the needle.
Like others said, just do an adjustment before you go through the trouble of sending the carb back. they often need some adjustment right out of the box.
There was no seat up in that bore...just a hole at the end. It's now in a box on it's way back to new york. Amazon is sending me one, should be here tomorrow.
if your dealing with a china clone carb you need to take another look at your carb.
they are just little different then a factory carb. they have a brass seat and a rubber tip on the needle.
I think you are right about the rubber tipped needle , I don't know if I could have adjusted the problem away. I didn't expect a factory adjusted carb to shoot gas 6" out the side. With only 9.00 at stake I tend to give up quickly.
Make sure your float is adjusted to it shuts off fuel when it's level. There is an actual measurement for this, but this is what I do for a stock engine. I do this and then check it with fuel flow, and lift the floats and ensure it shuts off. Makes a mess.
Backfiring sounds like an air leak or timing. Sorry. If it doesn't go away with the float setting, that is where you have to look.
Adjusting Chinese carbs, set both needles one turn out. Chain removed, or bike supported.
Screw in throttle stop screw so it will idle high. Start the bike. If it over revs, reduce the idle a bit. You need it to be at a high idle, not running into the high speed circuit.
Turn the idle mixture screw in slowly. RPM should increase as it gets leaner. Turn throttle stop screw out to lower RPM. Keep doing this back and forth until turning it one way and then the other makes it want to quit. The sweet spot.
High speed setting can now be adjusted. Get it to where it will accelerate without a load, and run smoothly at half throttle. After that, I ride them, and keep adjusting until the bike will both accelerate crisply, and maintain high RPM with a load. You cant do much adjusting of the high side with the bike sitting there with no load.
I appreciate you taking the time to respond. It's running pretty good now but I haven't tried it under a load.
The main thing I had wrong was the throttle plate was too open to get the idle circuit to draw. I found this it was pretty helpful.
Start the engine and allow it to warm up to normal operating temperature (3 - 5 minutes).
Set the speed control to the HIGH position. From the recommended preset position, turn the main mixture adjustment screw in (clockwise) slowly until the engine begins to run erratic (lean). Note the position of the screw. Now, turn the screw out (counterclockwise) until the engine begins to run erratic (rich). Turn the screw in (clockwise) midway between these two positions. This will be the best setting.
(counterclockwise) 1/8 turn at a time.
If the engine smokes excessively (rich), turn the main adjusting screw in (clockwise) 1/8 turn at a time.
After the main mixture screw is set, move the speed control to the IDLE or SLOW position. If the engine does not idle smoothly, turn the idle mixture screw 1/8 turn either in (clockwise) or out (counterclockwise) until engine idles smoothly.
Yes, but that assumes you are loading it up with a lawn mower blade at the full throttle setting. You wont have that luxury with a bike, so all you can do is set idle.
Also, with the Chinese carbs we've found that sometimes they like to be barely cracked open to hold a good idle. The key is keeping the RPM down low enough to adjust the pilot side without drawing from the main.
Lastly, your going to want better throttle response than you would from a garden implement. Generally that involves a trade off between leaning it to get response, but having it rich enough to hold the load.
Good job getting it this far. It sounds like you just about have it. Take a screwdriver with you on your first ride, so you can stop and start several times and adjust that main jet.


Today, though, Thomas was occupied with other thoughts. A religious teacher was rumored to be coming to town. His arrival was expected sometime in the coming week. This theologian had been fabulously well-received and he was gaining quite a following. He was known for his inspired teaching and his ability to touch the hearts of his listeners. Thomas hoped that he would be honored to host the man in his home. Perhaps a banquet would be appropriate, with invitations going out to all the learned people in this and nearby towns. Thomas instructed his servant to plan for an event that could be held on short notice.
The next day Thomas was working in his study when a servant rushed in to tell him that the teacher was just outside of town and a crowd had gathered in a field to hear him speak. Thomas threw down his pen, wiped his ink-stained fingers and rushed outside. The teacher had arrived earlier than anyone had expected. Thomas was grateful he had planned ahead for a banquet.
When Thomas arrived, a crowd had already surrounded the teacher and Thomas was forced to stand a long way off from him. The crowd continued to grow and press around him. In spite of his distance, though, Thomas had no trouble hearing the strangely familiar voice of the teacher. His words filled him with a glorious vision of the holiness of God, His love for His children, and His willingness to forgive. Thomas was filled with wonder at thoughts of this awesome God, yet, at the same time, he was filled with shame for his own life of hypocrisy.
The man finished teaching and the crowd began to break up. Thomas pressed forward to issue his invitation. He hoped that the teacher had heard of Thomas' fine reputaion in the town. He rehearsed his invitation in his mind. Finally he burst through the crowd and found himself face-to-face with the teacher.
"Sir, my name is Thomas," he blurted out. Then he stopped. He knew this man. This teacher, this man who had been teaching the crowd was a son of the king! Why had he not identified himself as the crown prince? Why was he here wearing the clothes of an ordinary man? Thomas was about the same age as the prince. They had grown up together in the palace, but of course Thomas was a mere servant--and not a very good one. This prince knew all about Thomas' transgressions and Thomas was filled with horror.
This was it. This was the moment Thomas had always feared. Now his shame would be revealed.
Thomas was stunned. He stared into the eyes of the prince. No words came. Suddenly he burst forth, "Forgive me, please!" Nearby townspeople stared in curiosity.
"May I sojourn at your home for a few days, Thomas?" The teacher took him by the arm and walked with him toward the town, away from staring eyes.
Thomas whispered, not wanting to reveal the prince's secret identity. "But I know who you are! Don't you recognize me?"
"Then why are you willing to speak with me?"
"I forgive you, Thomas. That is behind us. Now we have work to do."
"We will teach this town about the wonders of God's grace."
"I have been a teacher all my adult life, but I do not think that…"
"I will do the teaching for now," the prince smiled, "but I will need a host in this town."
"Oh, yes, of course. Well I had made some plans. You see I had hoped that you--well that was before I knew you were you--I had hoped you would be a guest in my home and we could invite the learned townspeople to a banquet."
"Yes. I want anyone who wants to come to be able to come."
"But, where shall I seat them all, and the food--"
"Yes, Sir, if you say so, but what about—"
The prince clapped his hand about Thomas' shoulder."I am most pleased to see you today, my brother Thomas. We have been apart too long."
Tears filled Thomas' eyes. He calls me his brother.


text:
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Provinces of Sweden
Historical and cultural geographical region
Population of Swedish provinces in 2016[1]
The provinces of Sweden (Swedish: Sveriges landskap) are historical, geographical and cultural regions. Sweden has 25 provinces and they have no administrative function, but remain historical legacies and the means of cultural identification. Dialects and folklore rather follows the provincial borders than the borders of the counties.
Several of them were subdivisions of Sweden until 1634, when they were replaced by the counties of Sweden (län). Some were conquered later on from Denmark–Norway. Others, like the provinces of Finland, were lost. Lapland is the only province acquired through colonization.
In some cases, the administrative counties correspond almost exactly to the provinces, as is Blekinge to Blekinge County and Gotland, which is a province, county and a municipality. While not exactly corresponding with the province, Härjedalen Municipality is beside Gotland the only municipality named after a province. In other cases, they do not, which then enhances the cultural importance of the provinces. In addition, the administrative units are subject to continuous changes–several new counties were for instance created in the 1990s–while the provinces have had their historical borders outlined for centuries. Since 1884 all the provinces are also ceremonial duchies, but as such have no administrative or political functions.
The provinces of Sweden are still used in colloquial speech and cultural references, and can therefore not be regarded as an archaic concept. The main exception is Lapland where the population see themselves as a part of Västerbotten or Norrbotten, based on the counties. Two other exceptions are Stockholm and Gothenburg, where the population see themselves as living in the city, not in a province, since both cities have province borders through them.[citation needed]
2.1 The lands of Sweden
3.1 Götaland
3.2 Svealand
3.3 Norrland
Provinces[edit]
Ångermanland Angermannia
Blekinge Blechingia
Bohuslän Bahusia
Dalarna Dalecarlia
Dalsland Dalia
Gotland Gotlandia
Gästrikland Gestricia
Halland Hallandia
Hälsingland Helsingia
Härjedalen Herdalia
Jämtland Jemtia
Lappland Lapponia Suecana
Medelpad Medelpadia
Norrbotten Norbothnia
Närke Nericia
Öland Olandia
Östergötland Ostrogothia
Skåne Scania
Småland Smolandia
Södermanland Sudermannia
Uppland Uplandia
Värmland Wermlandia
Västmanland Westmannia
Västerbotten Westrobothnia
Västergötland Westrogothia
English and other languages occasionally use Latin names as alternatives to the Swedish names. The name Scania for Skåne predominates in English. Some purely English exonyms, such as the Dales for Dalarna, East Gothland for Östergötland, Swedish Lapland for Lappland and West Bothnia for Västerbotten (and corresponding forms) are common in English literature.[2][3][4] Swedes writing in English have long used Swedish-language name forms only.[5][6]
Sweden's provinces from 1658 to 1809
The origins of the provincial divisions lay in the petty kingdoms that gradually became more and more subjected to the rule of the Kings of Sweden during the consolidation of Sweden. Until the country law of Magnus Ericson in 1350, each of these lands still had its own laws with its own assembly (the thing), and in effect governed themselves. The historical provinces were considered duchies, but newly conquered provinces added to the kingdom either received the status of a duchy or a county, depending on their individual importance.
After the separation from the Kalmar Union in 1523 the Kingdom incorporated only some of its new conquests as provinces. The most permanent acquisitions stemmed from the Treaty of Roskilde in 1658, in which the former Danish Scanian lands – the provinces of Skåne, Blekinge, Halland and Gotland – along with the Norwegian Bohuslän, Jämtland and Härjedalen, became Swedish and gradually integrated. Other foreign territories were ruled as Swedish Dominions under the Swedish monarch, in some cases for two or three centuries. Norway, in personal union with Sweden from 1814 to 1905, never became an integral part of Sweden.
The division of Västerbotten that took place with the cession of Finland caused Norrbotten to emerge as a county, and eventually to be recognized as a province in its own right. It was granted a coat of arms as late as in 1995.
Some scholars suggest that Sweden revived the province concept in the 19th century.[7]
The lands of Sweden[edit]
Historically, Sweden was seen as containing four "lands" (larger regions):
Götaland (southern Sweden)
Svealand (central Sweden)
Österland (Finland)
Norrland (northern parts of present-day Sweden and north-western Finland)
In the Viking age and earlier, Götaland and Svealand consisted of a number of petty kingdoms that were more or less independent; Götaland in the Iron Age and Middle Ages did not include Scania and other provinces in the far south which were part of Denmark. The leading tribe of Götaland in the Iron Age was the Geats; the main tribe of Svealand, according to Tacitus ca 100 AD, was the Suiones (or the "historical Swedes"). "Norrland" was the overall denomination for all of the unexplored northern parts, the outward boundaries of which and control by the Swedish king were weakly defined into the early modern age. Österland ("Eastern land"; the name had early gone out of use) in southern and central Finland formed an integral part of Sweden. In 1809 Finland was annexed by Russia, reunited with some frontier counties annexed several decades earlier to form the Grand Duchy of Finland, and becoming in 1917 the independent country of Finland.
The borders of these regions have changed several times throughout history, adapting to changes in national borders, and Norrland, Svealand and Götaland are only parts of Sweden and have never superseded the concept of the provinces.
Heraldry[edit]
At the funeral of King Gustav Vasa (Gustav I) in 1560 some early versions of coats of arms for 23 of the provinces listed below were displayed together for the first time, most of them having been created for that particular occasion. Erik XIV of Sweden modeled the funeral processions for Gustav Vasa on the continental renaissance funerals of influential German dukes, who in turn may have styled their display of power on Charles V's funeral procession, where flags were used to represent each entry in the long list of titles of the dead. Having only three flags as a representation of the entities Svealand, Götaland and Wends mentioned in Vasa's title, "King of Sweden, the Goths and the Wends", would have been diminutive in comparison with the pompous displays of ducal power on the continent, so flags were promptly created to represent each of the provinces. At the funeral of Charles X Gustav more flags were added to the procession, namely the coats of arms for Estonia, Livonia, Ingria, Narva, Pomerania, Bremen and Verden, as well as coat of arms for the German territories Kleve, Sponheim, Jülich, Ravensberg and Bayern.
Since most of the historical Swedish provinces did not have set coats of arms at the time of Gustav Vasa's death, they were promptly created and granted. However, some of the coats of arms designed for the occasion were short-lived, such as the beaver picked to represent Medelpad, the wolverine in the coat of arms for Värmland and the rose-adorned coat of arms for Småland. Östergötland was for the occasion represented by two coats of arms, one with a Västanstång dragon and one with a Östanstång lion. The current coat of arms for Östergötland, listed below, was created in 1884. The savage representing Lappland was not used in King Gustav's procession, but was adopted as a coat of arms at the funeral procession of Charles IX in 1612, where the savage was initially black. The current coat of arms for Lappland, with a red, club-carrying man, was created in 1949. The list of coats of arms appearing below is thus different from the funeral procession flags, and consists of more recent inventions, many created during a period of romantic nationalism in the 19th century.
After the separation of Sweden and Finland the traditions for respective provincial arms diverged, most noticeably following an order by the King in Council on January 18, 1884. This established that all Swedish provinces carry ducal coronets, while the Finnish provincial arms still discriminated between ducal and county status. A complication was that the representation of Finnish ducal and county coronets resembled Swedish coronets of a lower order, namely county and baronial. The division of Lapland necessitated a distinction between the Swedish and the Finnish arms.
For more information, see Lands of Sweden or articles on the individual lands or provinces.
Götaland[edit]
Götaland (Gothia, Gothenland) consists of ten historical provinces located in the southern part of Sweden. Until 1645 Gotland and Halland were parts of Denmark. Furthermore, until 1658 Blekinge and Scania were parts of Denmark and Bohuslän part of Norway.
Scania (Skåne)
Svealand[edit]
Svealand (Swealand) consists of the following six provinces in middle Sweden. Until 1812 Värmland was a part of Götaland.
Norrland[edit]
Norrland (Northland) consists today of nine provinces in northern and central Sweden. Until 1645 the provinces of Jämtland and Härjedalen were parts of Norway. Swedish Lapland was united with Finnish Lapland as Lapland until 1809. Norrbotten was separated from Västerbotten and developed as a province of its own during the 19th century.
Lands of Sweden
Dominions of Sweden
Historical provinces of Finland
Counties of Sweden
^ "Folkmängd i landskapen den 31 december 2016" (in Swedish). Statistics Sweden. 21 March 2017. Retrieved 17 April 2018.
^ Eric Linklater in The Life of Charles XII
^ Robert Nisbet Bain in Gustavus III and His Contemporaries
^ Bernard Quaritch in The stories of the Kings of Norway Called the Round World (Heimskringla)
^ R. Svanström & C.F. Palmstierna in A History of Sweden (1934)
^ Nils Ahnlund in Gustav Adolf the Great (1940)
^ Jacobsson, Benny (2000). "Konstruktion av landskap. Exemplet Uppland" Archived 2009-02-02 at the Wayback Machine. Idéhistoriska perspektiv. Ed. Ingemar Nilsson, Arachne 16, Göteborg 2000, p. 109-119. Retrieved 20 October 2006. (In Swedish).
Lands and Provinces of Sweden
Sweden articles
Kalmar Union
Rise to become Great Power
Swedish Empire
Great Northern War
Age of Liberty
Gustavian era
Sweden–Norway union
Famine of 1867-1869
Extreme points
Krona (currency)
Rehn–Meidner model
source: https://en.wikipedia.org/wiki/Provinces_of_Sweden
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text:
Q: Функция recv с сокетом в неблокирующем режиме работы Сокет, полученный функцией accept был переведен в неблокирующий режим работы функцией set_non_block_mode(socket[i]).Когда писал клиент,посылал 4 байта, переведенные в сетевой порядок , а потом и в строку
number_of_message2_to_send=htonl(number_of_message2);
memcpy(nmsg,&number_of_message2_to_send,4);
send(s,nmsg,4,MSG_NOSIGNAL);

Сейчас сервером пытаюсь получить это сообщение:
char some_msg[5] = "\0";
rcv =  recv(sockets[i], some_msg, sizeof(some_msg), 0);

Но в отладчике не вижу ничего записанного в строку some_msg.
int set_non_block_mode(int s)
{
#ifdef _WIN32
unsigned long mode = 1;
return ioctlsocket(s, FIONBIO, &mode);
#else
int fl = fcntl(s, F_GETFL, 0);
return fcntl(s, F_SETFL, fl | O_NONBLOCK);
#endif
}

Это функция для перевода в неблокирующий режим
И ещё один вопрос: как убедиться, что сокет действительно переведен в неблокирующий режим работы?

A: Для проверки перевода в неблокирующий режим достаточно проверить результат ioctlsocket. Также индикатором неблокирующего режима сокета будет являть ошибка функции send, которую нельзя просто так использовать с неблокирующим сокетом, результат который вы игнорируете.

redpajama_set_name: RedPajamaStackExchange


text:
Брізі Джонсон  — американська гірськолижниця, учасниця зимових Олімпійських ігор 2018 року, призерка етапів Кубка світу. Спеціалізується на швидкісних дисциплінах.

Спортивна кар'єра

Брізі Джонсон народилася в Джексоні (штат Вайомінг), виховувалась у сусідньому містечку Вікторі. На лижі стала в три роки, а перші уроки їй давав батько. Ще вихованкою дитячого садка почала брати участь у дитячих змаганнях. У 13 років, потренувавшись у лижному клубі Джексон-Гоул, вона перейшла до лижної академії Роумарк у Солт-Лейк-Сіті.

У 15 років вона дебютувала на міжнародних змаганнях серед юніорів. У Кубку світу дебютувала в сезоні 2015—2016, 4 грудня у Лейк-Луїзі на трасі швидкісного спуску. Рік по тому на цій же трасі вона набрала перші бали до заліку Кубка світу.

На Чемпіонаті світу дебютувала на 2017 року в Санкт-Моріці, де посіла 15-те місце у швидкісному спуску та 28-ме — в супергіганті.

На зимових Олімпійських іграх 2018 у Пхьончхані змагалась у двох дисциплінах. Фінішувала 7-ю у швидкісному спуску та 14-ю в супергіганті.

У вересні 2018 року Брізі зазнала значної травми, розриву хрестоподібних зв'язок, через яку пропустила весь сезон 2018—2019 років і не взяла участі в чемпіонаті світу 2019 року в Оре.

У грудні 2020 року Джонсон вперше у кар'єрі зійшла на п'єдестал пошани на етапі Кубка світу. Це сталося на трасі швидкісного спуску у французькому Валь-д'Ізері. Тут їй вдалося одразу два спуски завершити на третьому місці.

Результати в Кубку світу
Усі результати наведено за даними Міжнародної федерації лижного спорту.

Підсумкові місця в Кубку світу за роками

П'єдестали в окремих заїздах

 7 п'єдесталів (7 ШС); 18 топ-десять

Результати на чемпіонатах світу
Усі результати наведено за даними Міжнародної федерації лижного спорту.

Результати на Олімпійських іграх
Усі результати наведено за даними Міжнародної федерації лижного спорту.

Примітки

Гірськолижники на зимових Олімпійських іграх 2018
Гірськолижниці США
Спортсмени з Айдахо

redpajama_set_name: RedPajamaWikipedia


This was an intricate patio, flowerbed & driveway build which involved careful planning to ensure that the design matched the style of the property. The look of the sandstone patio really compliments the house, and has transformed a garden into a space which both compliments the house and is a pleasure to relax in.
The contrast between the sandstone patio and the black brick driveway creates a stunning look which has transformed the image of this property whilst at the same time creating a functional space for all the family through driveway and garden.


text:
Driver Arrested on Suspicion of DUI After 8 Injured in Crash Involving Celebrity Tour Bus
By Eric Leonard
Published Jun 24, 2019 at 4:23 PM | Updated at 6:49 PM PDT on Jun 24, 2019
Tour Bus Driver Arrested After Crash
//www.nbclosangeles.com/news/local/Tour-Bus-Driver-Arrested-After-Crash_Los-Angeles-511759852.html
The driver of a celebrity tour van was arrested after he crashed on Coldwater Canyon and injured multiple people and left wrecked vehicles just outside a Beverly Hills Fire Department station. Eric Leonard has more on NBC4 News at 6 p.m. on Monday, June 24, 2019. (Published Monday, June 24, 2019)
The driver of a celebrity tour van was arrested on suspicion of driving under the influence after a crash on Coldwater Canyon that injured nearly a dozen people and left wrecked vehicles just outside a Beverly Hills Fire Department station.
Beverly Hills police said the collision happened around 9:45 Sunday night when the tour van, with 11 people on board, was struck from behind by another vehicle and pushed into another car. When officers arrived at the scene they began to suspect the tour van driver was impaired, said Sgt. Sean Smollen.
"They observed signs of impairment, and at that point they put him through a field sobriety test," and took the driver into custody, Smollen said.
The driver, Howard Ferguson, 57, was released after he was issued a citation and was ordered to appear in court Wednesday, booking records show.
2019 Southern California Images in the News
The van was operated by Los Angeles USA Tours. The person answering the phone at its office Monday hung up when asked about the crash. CHP records show the company was last inspected in March and its facility and vehicle were given a, "satisfactory," rating.


For those of you that own you own board, whether it is a surfboard, paddleboard or longboard, you bought it because it suited you. Well why not have your own custom IrishCarver surfboard pendant made to mimic your favorite ride.
Just shoot me a picture of your board. I'll transfer the shape to a piece of bone or wood, your choice, and get carving it.