text:
\section{Introduction}

Since the discovery of quasi-periodic-oscillations (QPOs) in the tail of the giant X/$\gamma$-ray flares of SGR 1806-204 (Israel et al 2005)  and SGR 1900+14 (e.g., Strohmayer \& Watts 2005, 2006, Watts \& Strohmayer 2006),
oscillations of strongly magnetized neutron stars, i.e., magnetars (e.g., Woods \& Thompson 2006; Mereghetti 2008) have gained much attention in the astrophysics community.
Because of the suggestion by Duncan (1998), before the discovery of the magnetar QPOs,
that crustal torsional oscillations of neutron stars are most easily excited by seismic events, theoretical studies for the QPOs were first focused on torsional oscillations of the solid crust of neutron stars possessing strong magnetic fields and, later on, on global toroidal oscillations
of magnetized neutron stars, whose frequencies
are proportional to the strength of the magnetic fields.
We may call global modes of strongly magnetized stars Alfv\'en modes or magnetic modes when the oscillation
frequency is proportional to the field strength.
The frequency ranges of the crustal modes and the Alfv\'en modes are found consistent to
the observed QPO frequencies (e.g., Watts 2011).

Using a toy model for global oscillations of magnetized neutron stars,
Levin (2006, 2007) suggested that torsional modes in the solid crust will be strongly damped by frequency resonance with Alfv\'en continuum in the fluid core.
Motivated by Levin's suggestions, many authors carried out MHD calculations that simulate time evolution of small amplitude axisymmetric toroidal perturbations to investigate the modal properties of magnetars
(e.g., Sotani et al. 2008; Cerd\'a-Dur\'an et al. 2009; Colaiuda \& Kokkotas 2011; Gabler et al. 2011, 2012).
For example, Gabler et al (2011, 2012) showed that because of resonant damping
with Alfv\'en continuum in the core the damping timescales of crustal torsional modes are too short to
be consistent with the observed QPOs, and suggested that Alfv\'en modes, instead of crustal modes, could be responsible for the QPOs if the magnetic fields are stronger than $\sim 10^{15}$G at the surface
since the damping timescales of Alfv\'en modes
are much longer than that of the crustal torsional modes that suffer resonant damping with Alfv\'en continuum.
Sotani \& Kokkotas (2009), on the other hand, computed axisymmetric $spheroidal$ oscillations of stars magnetized with a poloidal field, and they obtained Alfv\'en modes of low frequency as well as acoustic oscillations of high frequency.
They also suggested that Alfv\'en continuum in the core is irrelevant to the modal properties.

These early studies of oscillations of magnetars are mainly concerned with axisymmetric toroidal modes
of the stars, and pure toroidal modes do not produce any pressure and density perturbations.
For axisymmetric oscillations of magnetized stars, spheroidal and toroidal components of
the perturbed velocity fields are decoupled
and can be treated separately for a purely poloidal or toroidal magnetic field configuration if the effects of rotation are neglected.
This property remains true even for general relativistic treatment.
In other words, for non-axisymmetric oscillations of magnetized stars the spheroidal and toroidal
velocity components are coupled even if we assume a pure poloidal or toroidal magnetic field and ignore the effects of rotation.

Lander et al. (2010), Passamonti \& Lander (2013) discussed, using MHD simulations,
such non-axisymmetric oscillation modes of magnetized stars assuming a purely toroidal magnetic field.
For rotating magnetized stars, the modal property will be more complicated because spheroidal (polar) and toroidal (axial) components of the perturbed velocity fields are coupled and rotational modes such as
inertial modes and $r$-modes come in.
Lander \& Jones (2011) calculated non-axisymmetric oscillations of magnetized rotating stars for
a purely poloidal magnetic field.
They obtained polar-led Alfv\'en modes which reduce to inertial modes in the limit of ${\cal M}/{\cal T}\to 0$, where $\cal M$ and $\cal T$ are magnetic and rotation energies of the star.
Lander \& Jones (2011) also suggested that the axial-led Alfv\'en modes could be unstable.

For mixed poloidal and toroidal magnetic field configurations, coupled
spheroidal and toroidal velocity fields have to be considered to describe global oscillations of magnetized stars
even for axisymmetric oscillations.
Colaiuda \& Kokkotas (2012) calculated axisymmetric toroidal oscillations of
neutron stars adding a toroidal magnetic field to a poloidal one.
They found that the oscillation spectra of toroidal modes
are significantly modified, losing their continuum character, by introducing a toroidal field component and
that the crustal torsional modes now become long-living oscillations.
This finding may be similar to the finding by van Hoven \& Levin (2011, 2012) who suggested the existence of
discrete modes in the gaps between frequency continua, using a spectral method.
Using MHD simulations, Gabler et al. (2013) discussed axisymmetric toroidal modes of magnetized stars
assuming various magnetic field configurations.
It is interesting to note that Gabler et al. (2013) found no long-lived discrete crustal modes in the gap
between Alfv\'en continua in the core, that is, their numerical results do not fully confirm
those by Colaiuda \& Kokkotas (2012) and by van Hoven \& Levin (2011, 2012).

Normal mode analysis is another method employed to study small amplitude oscillations of magnetized stars,
where the time dependence of
oscillation is given by the factor $e^{{\rm i} \omega t}$
and we determine the oscillation frequency $\omega$ as an eigenfrequency of a system of linear differential equations
that govern the oscillations.
Assuming a force-free dipole magnetic field, Lee (2007) computed axisymmetric normal modes of a neutron star.
Lee (2008) and Asai \& Lee (2014)
calculated $axisymmetric$ toroidal modes of magnetized neutron stars for poloidal magnetic fields,
employing Newtonian gravity in the former and general relativity in the latter, while
Asai, Lee, \& Yoshida (2016) calculated $non$-$axisymmetric$ magnetic modes for a poloidal magnetic field
and obtained both stable and unstable magnetic modes.
Assuming a toroidal magnetic field, on the other hand, Asai, Lee, \& Yoshida (2015) computed
non-axisymmetric oscillation modes of rotating stars, taking account of the equilibrium deformation
caused by the toroidal magnetic field.
They obtained $g$-, $f$-, $p$-modes for non-rotating stars and $r$-modes and inertial modes for rotating stars.
It is important to note that the numerical results obtained by the normal mode analyses are not necessarily consistent with those obtained by numerical MHD simulations.
The frequency ranges of magnetic modes obtained by normal mode calculations and MHD simulations are similar
between the two methods of analysis.
However, although Lee (2008) and Asai \& Lee (2014) obtained discrete toroidal magnetic normal modes of neutron stars for a poloidal magnetic field, MHD simulations for axisymmetric toroidal oscillations do not necessarily support the existence of such discrete magnetic normal modes.
The reason for the discrepancy, however, is not necessarily well understood.

We may employ normal mode analysis to investigate the stability of magnetized stars, but its application to
general field configurations is extremely difficult to formulate.
In this respect the stability analysis based on variational principle will be more flexible and tractable.
See Herbric \& Kokkotas (2017) and Akg\"un et al (2013) for recent studies, and see also Tayler (1973), Markey \& Tayler (1973, 1974) for classical works.

In this paper, we revisit the problem of axisymmetric spheroidal normal modes of magnetized stars for a poloidal
magnetic field.
Although we employ Newtonian gravity, this paper may be regarded as a normal mode analysis version of Sotani \& Kokkotas (2009), who carried out
numerical MHD simulations for small amplitude perturbations in general relativistic framework.
\S 2 is for method of solution and \S 3 is for numerical results.
We conclude in \S 4.

\section{Method of solution}

\subsection{Equilibrium State}

For a static magnetic field, we assume an axisymmetric poloidal field given in spherical polar coordinates $(r,\theta,\phi)$ by
\begin{equation}
B_r=2f(r)\cos\theta, \quad B_\theta=-{1\over r}{dr^2f(r)\over dr}\sin\theta, \quad B_\phi=0,
\end{equation}
for which $\nabla\cdot\pmb{B}=0$.
If we assume that the electric current is toroidal and is given by $\pmb{J}_\phi=cj_\phi r\sin\theta\pmb{e}_\phi$
with $c$ being the velocity of light, the Ampere law given by
$
\nabla\times\pmb{B}=4\pi \pmb{J}_\phi/c
$
leads to
\begin{equation}
{d^2f\over dr^2}+{4\over r}{df\over dr}=-4\pi j_\phi,
\end{equation}
where we assume that in the vicinity of $r=0$ the function $f$ behaves as
\begin{equation}
f(r)=\alpha_0+O(r^2)
\end{equation}
with $\alpha_0$ being a constant.
The Lorenz force is then given by
\begin{equation}
(\nabla\times\pmb{B})\times\pmb{B}
=4\pi j_\phi\nabla\left(r^2f\sin^2\theta\right),
\end{equation}
and the hydrostatic equation reduces to
\begin{equation}
{1\over\rho}\nabla p+\nabla\Phi-{j_\phi\over\rho}\nabla\left(r^2f\sin^2\theta\right)=0,
\end{equation}
where $p$ is the pressure, $\rho$ is the mass density, and $\Phi$ is the gravitational potential.
This may suggest that a possible choice of the function $j_\phi$ is
\begin{equation}
j_\phi=c_0\rho,
\end{equation}
where $c_0$ is a constant.
For this choice of $j_\phi$ the hydrostatic equation simplifies to
\begin{equation}
{1\over\rho}\nabla p+\nabla\left(\Phi-c_0r^2f\sin^2\theta\right)=0,
\end{equation}
where the term $c_0r^2f\sin^2\theta$ is responsible for deviation of the equilibrium from spherical symmetry.
For simplicity, however, we ignore the term $c_0r^2f\sin^2\theta$ to construct equilibrium structures
so that $p$, $\rho$, and $\Phi$ depend only on the radial distance $r$ from the centre.
See Asai et al (2016),
who took account of the equilibrium deformation caused by toroidal magnetic fields to calculate
various oscillation modes.

The constants $c_0$ and $\alpha_0$ are determined by using surface boundary conditions for
the function $f$.
We assume that $j_\phi=0$ outside the star, and hence the exterior solution $f^{\rm ex}$
is given by $f^{\rm ex}=\mu_b/r^3$, where $\mu_b$ is the magnetic dipole moment of the star.
The constants $c_0$ and $\alpha_0$ are determined so that the interior solution $f$ and $df/dr$
are matched with the exterior solution $f^{\rm ex}$ and $df^{\rm ex}/dr$ at the surface $r=R$
with $R$ being the radius of the star.

We use polytropes of the indices $n=0.5$, 1, and 1.5 as background models for modal analysis in this paper,
where no deformation of the polytropes is considered, and the mass $M=1.4M_\odot$ and the radius $R=10^6$cm are assumed.
As the index $n$ increases, the concentration of the mass density into the central region becomes stronger.
Figures \ref{fig:fdfdr} and \ref{fig:bfldlines} show the functions $f$ and $df/dr$ versus $x=r/R$ and
the internal magnetic field lines on the $x$-$z$ plane for the polytropes, where $f$ and $df/dr$ normalized respectively by $B_S\equiv\mu_b/R^3$ and $B_S/R$ are shown, and
the $x$ axis is in the equatorial plane and the $z$ axis is along the magnetic axis of the star.
With increasing $n$ the centre of the closed magnetic field region moves inward and the volume of the region increases.

\begin{figure}
\begin{center}
\resizebox{0.33\columnwidth}{!}{
\includegraphics{f1a.eps}}
\resizebox{0.33\columnwidth}{!}{
\includegraphics{f1b.eps}}
\resizebox{0.33\columnwidth}{!}{
\includegraphics{f1c.eps}}
\end{center}
\caption{Functions $f$ (solid line) and $df/dr$ (dashed line) versus $x=r/R$ for polytropes of the indices $n=0.5$, 1, and 1.5, from the left to right panels, where $f$ and $df/dr$ normalized respectively by $B_S\equiv \mu_b/R^3$ and $B_S/R$ are shown.
}
\label{fig:fdfdr}
\end{figure}

\begin{figure}
\begin{center}
\resizebox{0.33\columnwidth}{!}{
\includegraphics{f2a.eps}}
\resizebox{0.33\columnwidth}{!}{
\includegraphics{f2b.eps}}
\resizebox{0.33\columnwidth}{!}{
\includegraphics{f2c.eps}}
\end{center}
\caption{Internal magnetic field lines in the x-z plane for polytropes of the indices $n=0.5$, 1, and 1.5.
}
\label{fig:bfldlines}
\end{figure}

\subsection{Perturbation Equations}

Neglecting equilibrium deformation caused by the poloidal magnetic field and
assuming spherical symmetry of the star,
we linearize ideal MHD equations to derive the oscillation equations of magnetized stars,
which are
\begin{equation}
\rho'+\nabla\cdot\left(\rho\pmb{\xi}\right)=0,
\label{eq:conteq}
\end{equation}
\begin{equation}
-\omega^2\pmb{\xi}
+{1\over\rho}\nabla p'-{\rho'\over\rho^2}{dp\over dr}\pmb{e}_r
-{1\over 4\pi \rho}\left[\left(\nabla\times\pmb{B}'\right)\times\pmb{B}+\left(\nabla\times\pmb{B}\right)\times
\pmb{B}'\right]=0,
\label{eq:eqmot}
\end{equation}
\begin{equation}
\pmb{B}'=\nabla\times\left(\pmb{\xi}\times\pmb{B}\right),
\label{eq:inductioneq}
\end{equation}
\begin{equation}
{\rho'\over\rho}={V\over\Gamma_1}{p'\over\rho g r}-rA{\xi_r\over r},
\label{eq:rhoprime}
\end{equation}
where $\pmb{\xi}$ is the displacement vector and
the prime $(')$ indicates Euler perturbations, and we have assumed that the time dependence of the
perturbations is given by the factor $e^{{\rm i} \omega t}$ with $\omega$ being the oscillation frequency.
The Schwarzschild discriminant $rA$ may be defined as
\begin{equation}
rA={d\ln\rho\over d\ln r}-{1\over\Gamma_1}{d\ln p\over d\ln r},
\end{equation}
where $\Gamma_1=(\partial\ln p/\partial\ln \rho)_{\rm ad}$.
Note that we have applied the Cowling approximation neglecting $\Phi'$, the Eulerian perturbation of
the gravitational potential, and that the linearized induction equation (\ref{eq:inductioneq}) guarantees
$
\nabla\cdot\pmb{B}'=0.
$
For polytropes of the index $n$, the adiabatic exponent for the perturbations are assumed
to be given by
\begin{equation}
{1\over\Gamma_1}={n\over n+1}+\gamma,
\end{equation}
where $\gamma$ is a constant, and
we have $rA=-\gamma(d\ln p/d\ln r)\equiv\gamma V$.
The equilibrium configuration may be called radiative for $\gamma<0$, isentropic for $\gamma=0$, and convective for $\gamma>0$.

Because of the Lorentz terms in equation (\ref{eq:eqmot}), separation of variables is not possible
to represent the perturbations of magnetized stars.
We therefore employ a series expansion for the perturbations.
For the displacement vector $\pmb{\xi}$, we write for axisymmetric perturbations of $m=0$
\begin{equation}
{\xi_r\over r}=\sum_j^{j_{\rm max}}S_{l_j}(r)Y_{l_j}^m(\theta,\phi)e^{{\rm i}\omega t},
\end{equation}
\begin{equation}
{\xi_\theta\over r}=\sum_j^{j_{\rm max}}
H_{l_j}(r){\partial\over\partial\theta}Y_{l_j}^m(\theta,\phi)
e^{{\rm i}\omega t},
\end{equation}
\begin{equation}
{\xi_\phi\over r}=-\sum_j^{j_{\rm max}}
T_{l'_j}(r){\partial\over\partial \theta}Y_{l'_j}^m(\theta,\phi)
e^{{\rm i}\omega t},
\end{equation}
and for the perturbed magnetic fields $\pmb{B}'$
\begin{equation}
{B'_r\over f}=\sum_j^{j_{\rm max}}b^S_{l'_j}(r)Y_{l'_j}^m(\theta,\phi)e^{{\rm i}\omega t},
\end{equation}
\begin{equation}
{B'_\theta\over f}=\sum_j^{j_{\rm max}}
b^H_{l'_j}(r){\partial\over\partial\theta}Y_{l'_j}^m(\theta,\phi)
e^{{\rm i}\omega t},
\end{equation}
\begin{equation}
{B'_\phi\over f}=-\sum_j^{j_{\rm max}}b^T_{l_j}(r){\partial\over\partial \theta}Y_{l_j}^m(\theta,\phi)
e^{{\rm i}\omega t},
\end{equation}
where $l_j=2(j-1)$ and $l'_j=2j-1$ for even modes and
$l_j=2j-1$ and $l'_j=2(j-1)$ for odd modes for $j=1,~ 2,~3,\cdots$.
The pressure perturbation $p'_{l_j}$ is given by
\begin{equation}
p'=\sum_j^{j_{\rm max}}p'_{l_j}(r)Y_{l_j}^m(\theta,\phi)e^{{\rm i}\omega t}.
\end{equation}

Substituting the series expansion into the perturbed basic equations (\ref{eq:conteq}) to (\ref{eq:rhoprime}),
we obtain sets of linear ordinary differential equations for the expansion coefficients.
For the dependent variables defined as
\begin{equation}
\pmb{y}_1=\left({S_{l_j}}\right), \quad \pmb{y}_2=\left({p'_{l_j}\over \rho g r}\right), \quad
\pmb{y}_3=\left(H_{l_j}\right), \quad \pmb{y}_4=\left(b^H_{l'_j}\right),\quad \pmb{b}^S=\left(b^S_{l'_j}\right),
\quad \pmb{t}=\left(T_{l'_j}\right), \quad \pmb{b}^T=\left(b^T_{l_j}\right),
\end{equation}
we obtain for the spheroidal components $\pmb{y}_i$ with $i=1,~2,~3,~4$
\begin{equation}
r{d\pmb{y}_1\over dr}=\left({V\over \Gamma_1}-3\right)\pmb{y}_1-{V\over\Gamma_1}\pmb{y}_2+\pmbmt{\Lambda}_0\pmb{y}_3,
\label{eq:y1}
\end{equation}
\begin{eqnarray}
r{d\pmb{y}_2\over dr}&=&\left[\left(c_1\bar\omega^2+rA\right)\pmbmt{1}-{1\over 8\pi V}{f^2\over p}\left({{\cal Q}\over f}\right)^2
{{\cal R} \over f}\pmbmt{C}_0\pmbmt{B}_0^{-1}\pmbmt{W}_0\pmbmt{W}_1\right]\pmb{y}_1
-\left[\left(rA+U-1\right)\pmbmt{1}+{1\over 2}{{\cal Q}\over f}\pmbmt{C}_0\pmbmt{B}_1^{-1}\pmbmt{\Lambda}_0\right]\pmb{y}_2\nonumber\\
&&+{{\cal Q}\over f}\left({1\over 2}c_1\bar\omega^2\pmbmt{C}_0\pmbmt{B}_1^{-1}\pmbmt{\Lambda}_0
-{1\over4\pi V}{f^2\over p}{{\cal R}\over f}\pmbmt{C}_0\pmbmt{B}_1^{-1}\pmbmt{W}_0\pmbmt{B}_0\right)\pmb{y}_3-{1\over 4\pi V}{f^2\over p}{{\cal R}\over f}\pmbmt{C}_0\pmb{y}_4,
\label{eq:y2}
\end{eqnarray}
\begin{eqnarray}
r{d\pmb{y}_3\over dr}={1\over 2}{{\cal Q}\over f}\left(3-{V\over\Gamma_1}+{{\cal Q}\over f}-{d\ln {\cal Q}/f\over d\ln r}\right)
\pmbmt{B}_0^{-1}\pmbmt{W}_1\pmb{y}_1+{1\over 2}{V\over\Gamma_1}{{\cal Q}\over f}\pmbmt{B}_0^{-1}\pmbmt{W}_1\pmb{y}_2
+{{\cal Q}\over f}\left(\pmbmt{1}-{1\over 2}\pmbmt{B}_0^{-1}\pmbmt{W}_1\pmbmt{\Lambda}_0\right)\pmb{y}_3
+{1\over 2}\pmbmt{B}_0^{-1}\pmbmt{\Lambda}_1\pmb{y}_4,
\label{eq:y3}
\end{eqnarray}
\begin{eqnarray}
r{d\pmb{y}_4\over dr}
&=&{{\cal Q}\over f}\left(\pmbmt{1}+{1\over 2}{{\cal R}\over f}\pmbmt{B}_1^{-1}\pmbmt{W}_0\right)\pmbmt{W}_1\pmb{y}_1
+2\pi V{p\over f^2}\pmbmt{B}_1^{-1}\pmbmt{\Lambda}_0\pmb{y}_2
+\left[2\left(\pmbmt{1}+{1\over 2}{{\cal R}\over f}\pmbmt{B}_1^{-1}\pmbmt{W}_0\right)\pmbmt{B}_0-2\pi V{p\over f^2}c_1\bar\omega^2\pmbmt{B}_1^{-1}\pmbmt{\Lambda}_0\right]\pmb{y}_3\nonumber\\
&&-{d\ln rf\over d\ln r}\pmb{y}_4,
\label{eq:y4}
\end{eqnarray}
and for the toroidal components ${\rm i}\pmb{t}$ and ${\rm i}\pmb{b}^T$
\begin{equation}
r{d{\rm i}\pmb{t}\over dr}=
-{{\cal Q}\over f}\left({1\over 2}\pmbmt{B}_1^{-1}\pmbmt{\Lambda}_0\pmbmt{C}_0-\pmbmt{1}\right){\rm i}\pmb{t}
+{1\over 2}\pmbmt{B}_1^{-1}\pmbmt{\Lambda}_0{\rm i}\pmb{b}^T,
\end{equation}
\begin{equation}
r{d{\rm i} \pmb{b}^T\over dr}=-2\pi V{p\over f^2}c_1\bar\omega^2\pmbmt{B}_0^{-1}\pmbmt{\Lambda}_1{\rm i}\pmb{t}
-\left({1\over 2}{{\cal Q}\over f}\pmbmt{B}_0^{-1}\pmbmt{W}_1\pmbmt{\Lambda}_0
+{d\ln fr\over d\ln r}\pmbmt{1}\right){\rm i}\pmb{b}^T,
\label{eq:bt}
\end{equation}
where
\begin{equation}
\bar\omega={\omega\over\sigma_0}, \quad \sigma_0=\sqrt{GM\over R^3}, \quad
V=-{d\ln p\over d\ln r}, \quad U={d\ln M_r\over d\ln r}, \quad c_1={(r/R)^3\over M_r/M},
\end{equation}
\begin{equation}
{\cal Q}=-{1\over r}{d(r^2f)\over dr},
\quad {\cal R}
=-r^2\left({d^2f\over dr^2}+{4\over r}{df\over dr}\right),
\end{equation}
and $\pmbmt{1}$ denotes the identity matrix, and
the matrices $\pmbmt{B}_0$, $\pmbmt{B}_1$, $\pmbmt{W}_0$, and $\pmbmt{W}_1$ are defined as
\begin{equation}
\pmbmt{B}_0=\pmbmt{Q}_1\pmbmt{\Lambda}_0+\pmbmt{C}_1, \quad \pmbmt{B}_1=\pmbmt{Q}_0\pmbmt{\Lambda}_1+\pmbmt{C}_0, \quad \pmbmt{W}_0=2\pmbmt{Q}_0+\pmbmt{C}_0, \quad \pmbmt{W}_1=2\pmbmt{Q}_1+\pmbmt{C}_1,
\end{equation}
and the definition of the matrices $\pmbmt{Q}_0$, $\pmbmt{Q}_1$, $\pmbmt{C}_0$, $\pmbmt{C}_1$, $\pmbmt{\Lambda}_0$, and $\pmbmt{\Lambda}_1$ is given in Yoshida \& Lee (2000).
It is important to note that since the expansion coefficient $H_{l_1}=H_0$, for example, vanishes identically for even modes,
we take $H_{l_2}$ to $H_{l_{j_{{\rm max}}+1}}$ as dependent variables and hence we have to redefine the matrices given above accordingly (see, e.g., Lee 2008).
To simplify the set of differential equations for the spheroidal components we have used
\begin{equation}
\pmb{b}^S={Q\over f}\pmbmt{W}_1\pmb{y}_1+2\pmbmt{B}_0\pmb{y}_3,
\label{eq:induction_r}
\end{equation}
which comes from the radial component of the induction equation (\ref{eq:inductioneq}), and
\begin{equation}
r{d\pmb{b}^S\over dr}={Q\over f}\pmb{b}^S+\pmbmt{\Lambda}_1\pmb{y}_4,
\label{eq:nablab}
\end{equation}
which comes from $\nabla\cdot\pmb{B}'=0$.
As shown by equations (\ref{eq:y1}) to (\ref{eq:bt}), for axisymmetric modes of $m=0$
the sets of differential equations for the spheroidal and toroidal components are decoupled from each other
(see, e.g., Lee 2007).

In this paper, we discuss axisymmetric ($m=0$) spheroidal modes of neutron stars magnetized by a poloidal magnetic field.
We solve the set of linear ordinary differential equations from (\ref{eq:y1}) to (\ref{eq:y4}), using
a relaxation method, as an eigenvalue problem of the frequency $\omega$, applying
boundary conditions at the center and the surface of the star.
The inner boundary conditions we use are the regularity conditions for the perturbations
$\pmb{\xi}$, $\pmb{B}'$, and $p'$ at the stellar centre.
The outer boundary conditions are $\delta p=0$ and $\pmb{b}^S+\pmbmt{L}^+\pmb{b}^H=0$ at the surface of the star where $\delta$ indicates
the Lagrangian perturbation and $(\pmbmt{L}^+)_{ij}=(l'_j+1)\delta_{ij}$.
See Asai, Lee, \& Yoshida (2016) for the details of the surface boundary conditions.

\begin{table*}
\begin{center}
\caption{Normalized eigenfrequency $\bar{\omega}$ of the magnetic modes of polytropes of the indices $n=0.5$, 1, and 1.5 for $\gamma=0$.}
\begin{tabular}{cccccc}
\hline
 & even  &  & & odd &\\
\hline
$n=0.5$ & $n=1$ & $n=1.5$ & $n=0.5$ & $n=1$ & $n=1.5$ \\
\hline
\multicolumn{6}{c}{$B_S=10^{14}$G} \\
\hline
0.001154 & 0.001425  & 0.001833  & 0.0005510 & 0.0007268  & 0.001006\\
0.001134 & 0.001401  & $\cdots$  & 0.0005001 & 0.0006937  & 0.0009860\\
$\cdots$ & $\cdots$ & $\cdots$  & 0.0004848 & 0.0006794 & $\cdots$\\
\hline
\multicolumn{6}{c}{$B_S=10^{15}$G} \\
\hline
0.01154 & 0.01425  & 0.01835  & 0.005510 & 0.007268  & 0.01001\\
0.01134 & 0.01400  & 0.01816  & 0.005001 & 0.006939  & 0.009878\\
$\cdots$ & $\cdots$ & $\cdots$ & 0.004851 & 0.006831 & 0.009756\\
\hline
\multicolumn{6}{c}{$B_S=10^{16}$G} \\
\hline
0.1153 & 0.1422  & 0.1828  & 0.05502 & 0.07253  & 0.1003\\
0.1134 & 0.1405  & 0.1809  & 0.04993 & 0.06924  & 0.09864\\
0.1122 & $\cdots$ & $\cdots$ & 0.04845 & 0.06841 & 0.09744\\
\hline
\hline
\end{tabular}
\medskip
\end{center}
\end{table*}

\section{Numerical Results}

We use polytropes of the indices $n=0.5$, 1, and 1.5 as equilibrium models for modal analyses,
where the mass $M=1.4M_\odot$ and the radius $R=10^6$cm are assumed.
For a given field strength $B_S\equiv \mu_b/R^3$ and a given expansion length $j_{\rm max}$,
we find numerous solutions to the set of equations (\ref{eq:y1}) to (\ref{eq:y4}),
and we pick up those solutions whose eigenfrequency $\omega$ and eigenfunctions converge
with increasing $j_{\rm max}$.
For a given field strength $B_S$, we usually find only a few solutions that reach a good convergence.

\subsection{Magnetic Modes}

Numerical results for axisymmetric spheroidal magnetic modes
are summarized in Table 1 where the normalized eigenfrequency $\bar\omega=\omega/\sigma_0$
with $\sigma_0=\sqrt{GM/R^3}$
is tabulated for both even and odd modes for the field strength $B_S=10^{14}$G, $10^{15}$G, and $10^{16}$G
and for $\gamma=0$.
We may convert the normalized frequency $\bar\omega$ to $\nu$(Hz) using $\nu\approx 2170\times\bar\omega$ for
$M=1.4M_\odot$ and $R=10^6$cm.
The magnetic modes in the table may correspond to polar Alfv\'en modes discussed by Sotani \& Kokkotas (2009).
Note that only magnetic modes that attain a good convergence with increasing $j_{\rm max}$ are tabulated.
As in the case of non-axisymmetric ($m\not=0$) spheroidal magnetic modes of polytropes,
the frequency $\bar\omega$ of the magnetic modes decreases as the number of nodes of the dominating eigenfunctions increases (see Asai et al 2016).
From the table we find that the frequency of the magnetic modes is in a good approximation
proportional to the field strength $B_S$, which may suggest that compressibility as the restoring force for acoustic modes plays only a minor role for low frequency magnetic modes.
We find it difficult to compute magnetic modes for field strength $B_S<\kern-1.2em\lower1.1ex\hbox{$\sim$} 10^{13}$G even for
$\gamma=0$.
This situation is different from that for axisymmetric toroidal magnetic modes of polytropes for
poloidal magnetic fields, for which we can find toroidal magnetic modes for any values of $B_S$ (e.g., Lee 2008).

Figures 3 shows the wave patterns
$\xi_r(x,z)$ and $\xi_\theta(x,z)$ of axisymmetric magnetic modes of even parity for
polytropes of the indices $n=0.5$, 1, and 1.5 for $B_S=10^{15}$G, where $x=r\sin\theta$ and $z=r\cos\theta$,
and the amplitudes in each panel are normalized by their maximum value.
The normalized frequency of the modes in the figure is
$\bar\omega=0.01154$, 0.01425, and 0.01835 for $n=0.5$, 1, and 1.5, respectively.
The magnetic modes in the figure are those of highest frequency $\bar\omega$ for given $n$ and $B_S$ and
show simplest wave patterns.
For even modes, the patterns of $\xi_r$ is symmetric about the equator and those of $\xi_\theta$ antisymmetric.
The amplitudes of $\xi_r$ is confined to the region around the magnetic axis, and this amplitude
confinement becomes stronger as $n$ increases.
The same is true for $\xi_\theta$, which show some complex structures in the region of closed magnetic field lines (see Figure \ref{fig:bfldlines}).
This complex patterns of $\xi_\theta(x,z)$ in the region of closed field lines become
more conspicuous as $n$ increases.

Figure 4 shows the wave patterns $\xi_r(x,z)$ and $\xi_\theta(x,z)$ of the magnetic mode of even parity
having the frequency $\bar\omega=0.01400$ for $n=1$ and $B_S=10^{15}$G.
Comparing to the middle panels of Figure 3, we note that the numbers of nodal lines parallel to the magnetic axis
in the patterns of $\xi_r(x,z)$ has increased by one.
As the number of nodal lines increases with decreasing frequency $\bar\omega$,
the patterns tend to show complex structures around and within the region of closed field lines,
which may make it difficult to compute correctly convergent magnetic modes.

Figure 5 shows the wave patterns of $\xi_r(x,z)$ and $\xi_\theta(x,z)$ for the odd parity magnetic modes of highest frequency for $B_S=10^{15}$G
and their frequencies are $\bar\omega=0.00551$, 0.007268, and 0.01001 for
$n=0.5$, 1, and 1.5, respectively.
For odd modes, the patterns of $\xi_r$ and $\xi_\theta$ are respectively antisymmetric and symmetric about the
equator.
The amplitudes are also confined to the region along the magnetic axis and the region of closed field lines
does not necessarily manifest itself conspicuously.
Comparing Figures 3 and 5, we find that the wave patterns $\xi_r$ and $\xi_\theta$ of the odd magnetic modes of highest frequency are much less complicated than those of the even magnetic modes of highest frequency.

\begin{figure}
\begin{center}
\resizebox{0.33\columnwidth}{!}{
\includegraphics{f3aa.eps}}
\hspace*{-1.41cm}
\resizebox{0.33\columnwidth}{!}{
\includegraphics{f3ab.eps}}
\hspace*{-1.41cm}
\resizebox{0.33\columnwidth}{!}{
\includegraphics{f3ac.eps}}
\end{center}
\vspace*{-1.5cm}
\begin{center}
\resizebox{0.33\columnwidth}{!}{
\includegraphics{f3ba.eps}}
\hspace*{-1.41cm}
\resizebox{0.33\columnwidth}{!}{
\includegraphics{f3bb.eps}}
\hspace*{-1.41cm}
\resizebox{0.33\columnwidth}{!}{
\includegraphics{f3bc.eps}}
\end{center}
\vspace*{-1.3cm}
\caption{Wave patterns $\xi_r(x,z)$ (top panels) and $\xi_\theta(x,z)$ (bottom panels)
of the axisymmetric even magnetic modes of polytropes of the indices
$n=0.5$, 1, and 1.5, from the left to right panels, where $B_S=10^{15}$G and $\gamma=0$ are assumed.
The normalized frequency $\bar\omega$ is $0.01154$, 0.01425, and 0.01835 for $n=0.5$, 1, and 1.5, respectively.
Note that the amplitudes of $\xi_r(x,z)$ and $\xi_\theta(x,z)$ are normalized by their maximum values.
}
\end{figure}

\begin{figure}
\begin{center}
\resizebox{0.33\columnwidth}{!}{
\includegraphics{f4a.eps}}
\hspace*{-1.41cm}
\resizebox{0.33\columnwidth}{!}{
\includegraphics{f4b.eps}}
\vspace*{-1.3cm}
\end{center}
\caption{
Wave patterns $\xi_r(x,z)$ (left panel) and $\xi_\theta(x,z)$ (right panel)
of the axisymmetric even magnetic modes $\bar\omega=0.01400$ of the $n=1$ polytropes for $B_S=10^{15}$G and $\gamma=0$.
The amplitudes are normalized by their maximum values.}
\end{figure}

\begin{figure}
\begin{center}
\resizebox{0.33\columnwidth}{!}{
\includegraphics{f5aa.eps}}
\hspace*{-1.41cm}
\resizebox{0.33\columnwidth}{!}{
\includegraphics{f5ab.eps}}
\hspace*{-1.41cm}
\resizebox{0.33\columnwidth}{!}{
\includegraphics{f5ac.eps}}
\end{center}
\vspace*{-1.5cm}
\begin{center}
\resizebox{0.33\columnwidth}{!}{
\includegraphics{f5ba.eps}}
\hspace*{-1.41cm}
\resizebox{0.33\columnwidth}{!}{
\includegraphics{f5bb.eps}}
\hspace*{-1.41cm}
\resizebox{0.33\columnwidth}{!}{
\includegraphics{f5bc.eps}}
\end{center}
\vspace*{-1.3cm}
\caption{Same as Figure 3 but for the magnetic modes of odd parity.
The eigenfrequency $\bar\omega$ is 0.005510, 0.007268, and 0.01001 for
$n=0.5$, 1, and 1.5, respectively.
}
\end{figure}

We have examined the response of the frequency $\bar\omega$ of the magnetic modes to buoyancy by increasing $|\gamma|$ from $\gamma=0$
for $\gamma<0$ and we find the behavior of the frequency with increasing $|\gamma|$ is the same as
that found by Asai et al (2016) for non-axisymmetric spheroidal magnetic modes.
Note that we find no unstable magnetic modes for axisymmetric spheroidal oscillations.

\subsection{Modes Corresponding to Radial Acoustic Modes}

Using the Alfv\'en velocity given by $v_A=B_S/\sqrt{4\pi\rho_c}$ with $\rho_c$ being
the mass density at the stellar centre, we may define the lower limit to the frequency of Alfv\'en modes
as $\omega_{\rm LL}\equiv\pi v_A/R$ with $R$ being the radius of the star.
For $B_S=10^{15}$G, we have $\bar\omega_{\rm LL}=1.86\times10^{-3}$, $1.39\times10^{-3}$,
and $1.03\times10^{-3}$ for the polytropes of $n=0.5$, 1, and 1.5, respectively.
These small values of $\bar\omega_{\rm LL}$ suggest that Alfv\'en waves have very short wavelengths in the frequency region
$\bar\omega>\kern-1.2em\lower1.1ex\hbox{$\sim$} 1$ of acoustic modes, which makes it difficult to numerically correctly calculate
acoustic modes that are coupled with very short Alfv\'en waves.
Interestingly, however, we find a few acoustic modes corresponding to the radial ($l=0$) fundamental and first harmonic modes of $\bar\omega>\kern-1.2em\lower1.1ex\hbox{$\sim$} 1$ for magnetized stars, although we find it very difficult to obtain acoustic modes corresponding to non-radial ($l\not=0$) $p$-modes.
The results are given in Table 2 where $\bar\omega$ is tabulated for two lowest radial order modes corresponding to
the radial fundamental and first harmonic modes of polytropes of the indices $n=0.5$, 1, and 1.5 for
$B_S=10^{14}$G, $10^{15}$G, and $10^{16}$G.
As the table indicates the effect of the magnetic field of strength $B_S<\kern-1.2em\lower1.1ex\hbox{$\sim$} 10^{16}$G on the high frequency modes
is quite minor.
For the field strength $B_S=10^{14}$G the frequencies $\bar\omega$ we obtain are practically those of radial pulsations obtained by ignoring the magnetic fields.
As $B_S$ increases, the frequency deviation from the radial pulsation modes increases
but it is still quite small even for $B_S\sim 10^{16}$G.
This deviation is found larger for larger $n$ polytropes and for the radial first harmonic modes compared to
the radial fundamental modes.
For a magnetic field as strong as $B_S>\kern-1.2em\lower1.1ex\hbox{$\sim$} 10^{17}$G, however,
it becomes difficult to find well converged modes that correspond to the
radial modes of non-magnetized stars.
This is probably because the frequencies of magnetic modes of lowest radial order become comparable to
those of the radial fundamental and first harmonic modes.
The expansion coefficients $S_{l_1}$ and $x^2p'_{l_1}/\rho g r$ are plotted versus $x=r/R$ for the $n=1$ polytrope for $B_S=10^{14}$G.
The functions $S_{l_1}$ and $x^2p'_{l_1}/\rho g r$ are almost indistinguishable from those of
radial pulsation modes.

\begin{figure}
\begin{center}
\resizebox{0.45\columnwidth}{!}{
\includegraphics{f6a.eps}}
\resizebox{0.45\columnwidth}{!}{
\includegraphics{f6b.eps}}
\end{center}
\caption{Expansion coefficients $S_{l_1}$ (solid line) and $x^2p'_{l_1}/\rho gr$ (dashed line) versus $x=r/R$ for
the modes corresponding to the radial fundamental (left panel) and first harmonic (right panel) modes
of the $n=1$ polytrope for $B_S=10^{14}$G where $M=1.4M_\odot$ and $R=10^6$cm.
The amplitude normalization is given by $b^H_{l'_1}=1$ at the surface.
}
\end{figure}

\begin{table*}
\begin{center}
\caption{Eigenfrequency $\bar{\omega}$ of acoustic modes corresponding to the radial fundamental and first harmonic modes
of polytropes for the indices $n=0.5$, 1, and 1.5 for $\gamma=0$.}
\begin{tabular}{ccccccccc}
\hline
\multicolumn{3}{c}{$B_S=10^{14}$G}&\multicolumn{3}{c}{$B_S=10^{15}$G}&\multicolumn{3}{c}{$B_S=10^{16}$G} \\
\hline
$n=0.5$ & $n=1$ & $n=1.5$ & $n=0.5$ & $n=1$ & $n=1.5$ & $n=0.5$ & $n=1$ & $n=1.5$\\
\hline
3.0982 & 2.5930  & 2.4451  & 3.0982 & 2.5930  & 2.4451 & 3.0983 & 2.5933 & 2.4456\\
5.4026 & 4.3937  & 4.0237  & 5.4026 & 4.3937  & 4.0238 & 5.4036 & 4.3967 & 4.0310\\
\hline
\hline
\end{tabular}
\medskip
\end{center}
\end{table*}

\section{Conclusions}

We have computed axisymmetric spheroidal normal modes of polytropes magnetized with a poloidal magnetic field.
This paper may be regarded as an addition to a series of papers that discuss normal modes of magnetized stars (Lee 2005, 2007, 2008; Asai \& Lee 2014, Asai, Lee, \& Yoshida 2015, 2016).
Spheroidal and toroidal modes of stars magnetized with a poloidal field
are decoupled for axisymmetric oscillations of $m=0$, while they are coupled
for non-axisymmetric oscillations of $m\not=0$ even for a purely poloidal magnetic field (e.g., Lee 2008).
In this paper, assuming axisymmetric spheroidal oscillations
we obtained magnetic modes of low frequency $\bar\omega\sim\bar\omega_{\rm LL}$
and modes of high frequency $\bar\omega>\kern-1.2em\lower1.1ex\hbox{$\sim$} ~1$ that correspond to acoustic radial $l=0$ modes, where
the frequency of the former is approximately proportional to the field strength $B_S$ and that of the latter
is almost insensitive to $B_S$.
This result may be consistent with that obtained by Sotani \& Kokkotas (2009), who employed MHD numerical simulations for small amplitude oscillations.
As in the case of non-axisymmetric magnetic normal modes (Asai, Lee, \& Yoshida 2016),
as the frequency of the magnetic modes decreases
the wave patterns become complex having more nodal lines in the patterns and it becomes
more and more difficult to obtain well converged modes.
It is also to be noted that we could not obtain $g$-modes of magnetized stars for $\gamma<0$, the result of which
is the same as that by Asai et al (2016) for non-axisymmetric spheroidal oscillations.
Note also that we found no unstable magnetic modes with $\omega^2<0$ for axisymmetric modes
although Asai et al (2016) found unstable magnetic modes for non-axisymmetric ones (see also Lander \& Jones 2011).

As suggested by Table 1, the frequencies of axisymmetric spheroidal magnetic modes computed for $B_S\sim 10^{15}$G
are consistent with low frequency ($\sim 30$Hz) QPOs detected for SGR 1806-20 and SGR 1900+14.
However, it is obvious that all the identified QPOs for the SGRs cannot be explained in terms of
spheroidal magnetic normal modes alone.

Using MHD simulations for mixed poloidal and toroidal magnetic fields, for example,
Colaiuda \& Kokkotas (2012) indicated that the frequency spectra of
toroidal modes will be significantly modified and lose continuum character.
Since we do not have any reliable knowledges concerning magnetic field configuration
in the interior of neutron stars,
it is useful to study normal modes of magnetized stars for more general magnetic field configurations that consist of
both poloidal and toroidal fields.
As a first step toward such normal mode analyses we may add a weak toroidal field component to the dominant poloidal one
in order to examine how the normal modes respond to such a weak toroidal component.

redpajama_set_name: RedPajamaArXiv


text:
Joe Biden is in hot water from some circles for once making nice with the segregationists. But it would be helpful for the aggrieved parties to read the entire quote and context.
Mr. Biden, speaking at a fund-raiser at the Carlyle Hotel in New York City on Tuesday night, stressed the need to "be able to reach consensus under our system," and cast his decades in the Senate as a time of relative comity. His remarks come as some in his party say that Mr. Biden, the former vice president, is too focused on overtures to the right as he seeks the Democratic presidential nomination.
At the event, Mr. Biden noted that he served with the late Senators James O. Eastland of Mississippi and Herman Talmadge of Georgia, both Democrats who were staunch opponents of desegregation. Mr. Eastland was the powerful chair of the Senate Judiciary Committee when Mr. Biden entered the chamber in 1973.
"I was in a caucus with James O. Eastland," said Mr. Biden, 76, slipping briefly into a Southern accent, according to a pool report from the fund-raiser. "He never called me 'boy,' he always called me 'son.'"
He called Mr. Talmadge "one of the meanest guys I ever knew, you go down the list of all these guys."
"Well guess what?" Mr. Biden continued. "At least there was some civility. We got things done. We didn't agree on much of anything. We got things done. We got it finished. But today you look at the other side and you're the enemy. Not the opposition, the enemy. We don't talk to each other anymore."
Many of those staking a claim on the far left hand side of the Democratic party like Cory Booker have an issue with Biden here. I don't.
Because he is absolutely right. You have to talk with the people who don't agree with you. You don't make deals with your friends, you make deals with your enemies. I am so sick of the current shortsightedness and self righteousness from both Republicans and Democrats. And nothing is getting done in our country. And it looks like it won't for the foreseeable future.
There is absolutely nothing wrong with working with political opponents that you disagree with and we have a long history of doing so in this country. Look at Hatch and Ted Kennedy. We need to stop looking for perfect people who would never compromise. Because we are basically split right down the middle.
I was at a gathering the other day and was heavily outnumbered by conservatives. Tried to have some meaningful exchanges and was mostly successful.
But one stood out.
A man complained that dems were doing everything they could to obstruct the President. And I pointed out that Obama was treated the very same way by a Republican congress, pointing out McConnell's famous one term in office quote and the failure of them to back him on anything.
"That was different," he said. "That was about policy."
And I had to sillily point out that we on my side had a problem with the Republican's policy too. But I had heard the same argument from Mitch McConnell himself last week. He is not going to take up any House votes because the left is full of creeping socialists, etc. Mitch, that left you so greatly despise represents a majority of Americans right now. And you are abdicating your position and responsibility to your office and the citizens of the United States by not respecting that majority.
For the first time in my memory, I'm going to agree with Nancy Pelosi. I am indeed the grim reaper when it comes to the socialist agenda that they've been ginning up over in the House with overwhelming Democratic support and sending it over to America, things that would turn us into a country we've never been. Sen. Mitch McConnell
We discussed this situation at K's house today. Kip thought the Biden bashing was unfair, D preferred a more progressive candidate. I personally don't think a Bernie Sanders is what our country needs right now, free this and free that and we'll worry about paying for it later. Prefer a Biden or Buttigieg type that is more centrist or moderate in their views, that might track with the great undecided block that floats down the middle.
D said something interesting, that Obama tried to take a middle position and got screwed by the right, no matter how accommodating he tried to be it was never enough for the conservatives and strategically a failure.
An interesting and horrible conundrum but not one that looks like it will get fixed anytime soon. A Democratic President and House with a Senate that refuses to take up any legislation is still a big zero.
Kerr A. Lott said...
Left a comment on the wrong article.
I'll try and remember my brilliant comment.
If democratic socialism can work in just about every other rest advanced nation, why not here?
Democratic socialism is not about free this and fee that and who's going to pay for it.
It's about taking power away from the fat cats, the industrialist, the war profiteers.
If Bernie Sanders is elected, the only losers are the oligarchs, Jeff Bezos the trillionaire, various billionaires and millionaires, the military industrial complex, for profit prisons and hospitals, big pharma, etc., etc..
I always welcome your opinion.
Ain't No Fun When The Rabbit's Got The Gun
Sausage making time
Warner Williams and Eddie Pennington
Flying Leslie
No Expectations
Kadir Nelson
Nowadays Clancy Can't Even Sing
Yerba Buena Whitewash
Stupidos
Wrong way ticket
John Baldry - Flying
Wednesday Mail Call
Kicks keep getting harder to find
Wall around your heart
Supreme Leaders
Ron Wood & Bo Diddley - Crackin' Up
Female Harrier glide at SJWA
Rick and Levon
Defend the rooster
Blue Heron Anthology
Lesley Duncan - Love Song
Self portrait with caution tape
David Lee Roth - Soul Kitchen
Crosses and Supremes
Carpet Crawlers
Scam the scammers
Walk in beauty
Arthur Lee and Love
Babies and bodhisattvas
Purple one
Hey, at least he wasn't naked.
Cortez the Killer
Leitz 10 x 40 trinovid binoculars
Sam Cooke - Little Red Rooster
biff boff
puppy braid
The raptor's perch
Funky Revelation
The Straw Hat
Sour Milk Sea (Esher Demo)
Felinous assault
Little Sun Glover
Dear Prudence (Esher Demo)
Smite the Palm Haters!
I Walk On Guilded Splinters
Sick of Mick
Save the country
Honest appraisal
Please don't talk about me when I'm gone
Western Kingbird pondering the meaning of existence.
Transformative change is needed
First Snoop, now this...
Sunday antics
The Byrds - Triad
Gadzooks, it's a godwit!

redpajama_set_name: RedPajamaCommonCrawl


Provide your canine companion with a fun food challenge! The Bento Ball is a half ball which can be filled with kibble, treats and capped with an Everlasting Treat! Everlasting Treats can be placed upside down or into the centre of the Bento Ball for a greater challenge! Providing dogs with a treat dispensing toy helps to promote natural behaviour, keeping them stimulated for hours! Featuring gentle rubber dimples, the Bento Ball promotes dental and oral hygiene by helping to keep teeth clean whilst chewing. The Bento Ball is dishwasher safe, making it simple and convenient to maintain!
Provides hours of chewing fun and raised dimples help to clean teeth too!


The world of eSports will be headed to the big screen. The production company Gary Sanchez, along with Media Group Mosaic, has announced that they are currently working on an untitled project that centers around the ever expanding part of gamer culture that is home to some of the best players in the world. And better yet, it will include Will Ferrell.
The film will star Will Ferrell as a member of a professional eSports team. His character will be an odd addition to the cast considering he will be a key player in a sport that usually sees its players retire at a very young age. The hand-eye coordination and reaction times required for eSports start to deteriorate in a person's mid to late 20s.
There are currently negotiations taking place between producers and top eSport teams Evil Geniuses and Fnatic to appear in the film, as an attempt to add to its authenticity.
The film will be distributed by the American media company, Legendary Pictures who has produced such films as Warcraft, Pacific Rim, and Jurassic World. According to the company, the film will be similar to another film that Ferrell starred in, Talladega Nights, a comedy that centered around the sport of NASCAR. This new project aims to give viewers a look into the competitive world that is eSports.


I just got a chest and I did some research on this chest from the guide. Seems to be an O42 with lid restraints, which would put it between 43 and 59.
What I can't see is a decal or name plate on the bottom drawer that would narrow down the dates. It doesn't look like any name plate has ever been "nailed" into the drawer, so maybe it's a foil oval that has fallen off.
Some of the hardware is missing and I don't have a key.
The "nameplates" of this generation were decals and were not "nailed on". The ovals were either decals or glued on labels. The later art deco style rectangular decals were glued on.
Further, the chest had self-restraining hinges, not lid restraints, which were chains.
There is a code on the side of the lock that may help you obtain a key.
You have a great chest. I think the reason why there is no decal and no faded place where the decal used to be is that your chest has been refinished at some point in it's life.


Now that Bella is a vampire and Renesmee is born, the Twilight Saga is going to be even more fascinating!
The release date of The Twilight Saga Breaking Dawn 2 is set for November 16, 2012.
By the way, are you wondering about the release date of the first official trailer of Breaking Dawn Part 2? Well, it's set for March 23, 2012: a first trailer of Twilight Breaking Dawn Part 2 will indeed be shown in front of the Hunger Games.


text:
Sector(s): Regulation, consumers and competition
National Audit Office report: NAO Business perceptions survey 2010
NAO Business perceptions survey 2010
Over half of all businesses believe there is too much regulation, according to a survey of businesses commissioned by the National Audit Office and the Local Better Regulation Office. Although most businesses believe that the purpose of regulation is clear, over 60 per cent of businesses think that the level of regulation is an obstacle to their success.
"Our survey highlights areas that are still of concern for business, many of which have remained the same over the last four years. Businesses still find regulation burdensome and they are particularly concernedabout the introduction of new regulations or continuing changes to existing regulations. It therefore remains a priority for departments to manage the creation and removal of regulation properly in order to minimize the impact on business."
Chris Shapcott, National Audit Office director of regulatory reform
This is the NAO's fourth annual survey of businesses' perceptions of regulation. The survey found that 29 per cent of businesses believe that complying with regulation has become more burdensome over the previous 12 months. At the same time, only 1 per cent of businesses feel that regulation has become less difficult or less time consuming than previously.
A number of positive findings have emerged from the survey:
three in five businesses feel well-informed about the laws and regulations that affect them, with businesses feeling most informed about Health and Safety law;
58 per cent of businesses find it easy to comply with regulation specific to their business sector.
Despite this, a number of issues still remain:
fewer than 30 per cent of businesses believe that the government understands business well enough to regulate, or consults well before any change to regulation;
having to keep up to date with the introduction of new regulations is seen as the most burdensome and time consuming activity, particularly regarding employment law.
Full report (pdf - 844KB) Opens in new window
Technical Report (pdf - 1188KB) Opens in new window
Office of Fair Trading: regulating consumer credit
(Dec 2012)
The NAO's work on regulatory reform
Regulatory reform in the UK – NAO briefing for Regulatory Reform Select Committee


Here we consider the influencing factors that increase the probability of sustaining a stress fracture to the metatarsals. The topic is addressed with regards to the movement management system that is The Performance Matrix, powering the TPM Active, TPM Elite and TPM Active philosophies.
The metatarsals provide a broad surface for load sharing on the foot's plantar surface, forming the connection for both phalangeal and mid-foot articulations. Stress fractures to these structures are common, certainly within particular groups who endure large volumes of weight bearing (Cakir et al., 2014). Milgrom et al, (1992) showed that out of a total of 184 stress fractures, 7.6% of were of the metatarsals within a group of 205 military personnel.
A number of risk factor have been identified for this injury. The perspective taken here is that of an interactive and accumulative effect brought about by a number of issues including those relating to training, fatigue status, hormonal state, contact surface and whole body movement quality and others. Firstly, we consider volume of training.
Stress fractures can be considered as either as a normal system failing to meet the demands on that system (fatigue stress fracture) such as when exposed to high volumes of repetitive loading (>15 hours a week) or a compromised system failing to meet a constant demand (Insufficiency stress fracture). An increase in volume of ground contacts associated with running leads to a disruption of the usual cycle of bone remodelling. Osteoclast activity increases ('breaking down bone') whilst there is a lag in the activity of osteoblasts ('building bone'). This change to the system can increase the chance of a stress fracture. This is suggested to a risk if volume increases more than 10% in a week and is compounded if volume of running already exceeds >15 hours a week.
To profile an individual at higher risk for this injury we would identify a female with low body fat percentage, involved in high volume of running. They may have recently increased their volume or be at a peak volume of running in preparation for an upcoming event. The knowledge of this important event may itself be a stressor to the system, increasing fatigue, which in turn may also increase risk. One way in which this may operate is the following example. The runner may begin to experience discomfort in the foot, indicative of a problem. Rather than resting the runner sticks to their programme as the race 'really matters'. There is now an interaction between the stress of the upcoming race, the worry of the foot and the concern over the need to maintain the running volume.
One very simple reason is the size of bone in female compared to male feet. On average, the female foot will be smaller. Additionally, when body fat is very low (<12% for females) there is a risk of disruption to the monthly cycle, indicative of a change in hormonal status. The hormones involved are closely related to bone density, therefore heightening fracture risk. If the female runner is also deficient in vitamin D, iron and/or calcium bone health is further compromised.
The accumulative effect of fatigue is seen to problematic. It reduces the body's natural self-monitoring system or CCTV typically called proprioception, which tells us about our movement. Also, fatigue is seen to reduce the ability to absorb shock efficiently as an event progresses, increasing pressure below the mid-foot (where the metatarsals lie) (Weist et al., 2004).
It appears it is the change in surface that can be an issue. Those accommodated to a softer surface may experience issues when switching to harder running environments and vice versa. This is probably related to gaining familiarity with efficiently 'hitting' a novel surface and problems may arise before this solution is found. The same can be considered for shoe type and running style (how you hit the floor- heel-toe or mid-fore foot) – it appears to the transition to the new that carries risk; although old shoes (worn out) are also associated to increased risk.
OK- what about stress fractures, movement quality & The Performance Matrix?
In distance events, people typically aim to run in a straight line. During movement analysis we might discover somebody really struggles not to allow their pelvis and low back swing/rotate from side to side- they just can't stop it happening. During running this could be trouble for the feet. If the hips consistently rotate in this way the runner's feet, which are aiming to keep the runner in a straight line and are loaded with a multiple of body weight in each step, are consistently twisted. Combined with some of the factors already mentioned this might just be a stress, placed a direction in which the metatarsals are not their most robust, to start the process of injury.
This is just one combination of a movement issue in one region producing a potential issue in another. Finally, on the topic stress fractures, previous injuries are still the biggest predictor for re-injury. We believe these injuries leave a movement fault 'signature' that linger once the original injury has gone which then leads to more problems. The Performance Matrix goes looking for these signs, and helps you fix them before find re-injury is becoming a regular part of your training year.
The topic is complicated as many factors increase risk. One thing we can find and fix is your movement. Addressing the other concerns mentioned above and working on your movement quality is a course of action to keep you doing the things you like, love or to keep allowing you to have the things that doing this gives you.
Cakir H, Van Vlit-Koppert ST, Van Lieshout EM, De Vries MR, Van Der Elst M, Schepers T, Demographics and outcome of metatarsal fractures. Archives of Orthopaedic and Trauma Surgery (2011); 131: 241-245.
Comerford, M. & Mottram, S. (2012). Kinetic Control: The Management of Uncontrolled Movement. Australia: Elsevier.
Weist R, Eils E, Rosenbaum D. The influence of muscle fatigue on electromyogram and plantar pressure patterns as an explanation for the incidence of metatarsal stress fractures. Am J Sports Med 2004;32(8):1893–8.


Lord Drakkon is Tommy Oliver from a world where he never strayed from the path of evil. Get a look at the character in action in the latest trailer for the upcoming game. Power Rangers: Battle for the Grid is slated for release in spring 2019 for PlayStation 4, Xbox One, Nintendo Switch, and Steam.


text:
Theater capstone projects display students' college journey
April 25, 2016 Rachel Librach
Rachel Librach
rlibrach@uccs.edu
Just as an architect completes the construction of an arch with a capstone, seniors are tasked to complete a project that symbolizes the pinnacle of their undergraduate college career.
Senior theater majors must prepare a ten minute performance that communicates the major events in their life as part of their senior capstone project.
Some performances are humorous while others are more tragic.
VAPA instructor Leah Chandler-Mills said she has seen many senior capstones over the years and believes each one to be different.
Projects are not limited to one medium; students have expressed their message through dance, song, instrument and acting, said Chandler-Mills.
"Some of them showcase multiple characters that they've learned to physically and vocally be. People play instruments, sing and dance, whatever they know they can do to tell their story of where they've come from," she said.
Chandler-Mills said the process students go through to create their project is vulnerable.
"These capstones tend to be very revealing about what students in the class go through or have gone through or what talents they possessed that maybe none of us have ever been aware of or come to realize," she said.
Senior theater major Alex Williams is preparing a play for his capstone. The play is about a friend who committed suicide over the holiday break.
After coming to terms with the event, Williams wanted his capstone project to be not only a tribute to his friend, but also an exploration into the physiological aspects of death and gun violence.
Williams said he will explore the fear of death and other philosophical concepts.
"I go on to use a toy gun as a prop saying that it's not real, and it can't hurt me, and I'm in control of this," he said.
Williams composed scenes in his performance where he is using physical theater and displaying emotion through the body's movements rather than relying on text.
The VAPA department has helped to develop these skills, according to Williams, who added that a big misconception is that VAPA students have it easy and they don't have to work as much.
"We spend hours just like anybody else would for their capstone, but whereas other people go out and do research or field work, our way of doing that is trial and error," he said.
"Every class we come up with something new to present and everyone helps give constructive criticism on your work."
← Political arguments are out of hand, debates need to turn into discussions
Biology professor wins professor of the year for second time →
'Downtown 20' event offers deals with more bang for your buck
A Transgender Journey with Jessica Lynn seeks to normalize stigma surrounding gender identity
March 12, 2017 Daryn Vlad
Committee to vote on next All Campus Read book


text:
The Woods Takes Down Carlow University; Jarrett's 3-Pt Basket Seals the Victory
Saint Mary-of-the-Woods College (2-0, 1-0) 22 19 27 16 84
Carlow University (0-2, 0-1) 23 19 23 18 83
Pts: Delaney Kendall - 17
Reb: Maggie Reimer - 8
Ast: Avalee Jeffers - 1
Pts: Emily Grandy - 17
Reb: Emma Stille - 19
MONACA, Pa. - Saint Mary-of-the-Woods College women's basketball team battled NAIA's Carlow University tonight. The contest was held at the Penn State Beaver gymnasium. The Pomeroys defeated the Celtics 84-83 to win their second game in-a-row.
SMWC and the Celtics challenged each other all game long. At the end of the first quarter, SMWC trailed 23-22. Delaney Kendall had nine first-quarter points to lead both teams. At halftime, the Pomeroys remained down one-point 42-41. In the third quarter, The Woods took the lead 68-65 after they scored 27 points. In the fourth, the lead changed multiple times. The Celtics grabbed the lead with just over a minute to play until Delaney Jarrett knocked down a huge 3-PT shot with 50 seconds left in the game. This gave SMWC an 84-83 lead and the Pomeroy defense was able to hold on despite Carlow having the last shot of the game.
From Head Coach Robert Belf
On what the biggest success of the night was..
"The biggest thing overall was how hard we played after a seven-hour bus ride. For us to come with that type of intensity after sitting a long ride was huge. We worked hard and got good very shots which put us in the place to be in the lead down the stretch."
On winning two games in-a-row...
"This is just another step in the direction where we want to be. It is nice to win while we improve because it keeps the team positive."
On who stood out in tonight's contest...
"We had a ton of contribution from multiple players tonight. Delaney Jarett stepped up and hit a big 3-PT basket for us in the final minute."
From Callan Taylor
On getting the team clicking so well tonight...
"Our team is really starting to play together. This was a team win and everyone had their role to play. We are all excited and know that this weekend is big since we are playing other USCAA schools. It was a fun game to play in and even better than we could get the win."
From Delaney Kendall
On her 17-point night and the team victory...
"To me, it's not about how many points I score- it's about coming together as one. This was a huge win for us. From the bench to the starting five everyone contributed. We are not done, and this is just the foundation of what this team is capable of."
From Maggie Reimer
"Overall, it was a very good team win. We all worked hard and contributed when it was needed. There was also great energy through the whole game which helped us keep a positive mindset and play to a higher potential."
Delaney Kendall finished with 17 points for the secon game in-a-row, she was the leading scorer tonight for SMWC while she grabbed five rebounds and came up with five steals
Maggie Reimer tallied 16 points tonight, she added eight rebounds and one steal
Callan Taylor notched 14 points and grabbed one rebound
Delaney Jarrett was extremely clutch as she drilled a 3-PT basket with 57 second left in the game to give the Pomeroys an 84-83 lead
Paetyn Hayes and Avalee Jeffers both had nine points a piece
By The Numbers...
19 | The Woods offense only committed 19 turnovers
37.5 | SMWC shot 37.5 % from the field as they knocked down 27-of-72
3 | The Pomeroys had 3 players score in double-digits
11 | Overall, 11 of the 14 active members of the team tallied points on the box score, this is the second game in-a-row the Pomeroys have had 11 player's score
Next Match-Up...
SMWC will be back on the court on Saturday, November 17th against Penn State-Beaver and on Sunday, November 18th versus Washington Adventist.
Follow Us | Facebook, Instagram, Twitter, YouTube
Download Our Mobile Apps | iOS (iPhone & iPad), Android
Download Team Schedules | Download Center
Tag Us | @SMWCAthletics
#PomeroyPr1de


text:
The Gala Performance at the Paris Opéra | Eugène Louis Lami | Royal Collection Trust/© Her Majesty Queen Elizabeth II 2018 | Licence: All Rights Reserved
Victoria and Albert's precious watercolour albums
'My valuable albums … containing most beautiful water color[sic] paintings by the first Artists, and some by Amateurs, collected by my beloved Husband & myself, and representing the different places we visited & scenes of our life etc; arranged by my dearly beloved Husband.'
- Queen Victoria, after 1861
Watercolours today are experienced by gallery visitors as individual works of art, frequently mounted and framed up on a wall or perhaps displayed in a case. So it is in Royal Collection Trust's current touring exhibition celebrating the bicentenary of the births of Queen Victoria and Prince Albert: 'Victoria & Albert: Our Lives in Watercolour'. Queen Victoria herself reminds us, though, that the original context of these watercolours was quite different, and the exhibition includes a reconstruction of one of her watercolour albums which gives visitors a sense of how the Queen and her husband would have enjoyed some of their collection.
The wedding of the Princess Royal and Prince Frederick William of Prussia, 1858, Egron Sellif Lundgren. Royal Collection Trust / © Her Majesty Queen Elizabeth II 2019
Enthusiasts and amateur practitioners themselves of watercolour painting, together Victoria and Albert created albums of watercolours that they had commissioned, purchased at exhibitions or received as gifts. Probably the most important of these was the series of nine volumes which Victoria called her 'View Albums'. The royal couple chose which watercolours should be included and in what order they were mounted, as well as deciding on the text for the captions inscribed on the page underneath each work. Victoria and Albert organised the series chronologically, meaning that it formed a visual record of their marriage and the first two decades or so of the Queen's reign.
Prince Albert's closing address at the Great Exhibition, 15 October 1851, dated 1852, Joseph Nash. Royal Collection Trust / © Her Majesty Queen Elizabeth II 2019
Initially somewhat introspective (the first album contained several views of the royal family's homes), the scope of the albums broadened considerably over the years. When husband and wife turned the pages together, or engaged in the common social after-dinner activity of looking at albums with others, they reminisced over scenes of family life, such as their eldest daughter's wedding day, placed alongside views of modern Britain from their travels around the kingdom, watercolours illustrating the pomp and pageantry of State Visits abroad and those capturing events of national significance, including the Crimean War and Great Exhibition.
The Gala Performance at the Paris Opéra, 1855, Eugene-Louis Lami. Royal Collection Trust / © Her Majesty Queen Elizabeth II 2019
The shared act of creating the albums was clearly as important to Queen Victoria as the watercolours they contained. Testament to this is the fact that she ended the series after Prince Albert's untimely death in 1861. The albums themselves no longer survive (they were dismantled c.1930), probably a reflection of their frequent consultation by the widowed queen. That the watercolours they contained were preserved demonstrates the recognition in the 20th century of their intrinsic documentary and artistic value.
The Britannia tubular bridge over the Menai Straits, dated 1852, Frank Dillon. Royal Collection Trust / © Her Majesty Queen Elizabeth II 2019
As part of 'Victoria & Albert: Our Lives in Watercolour', apprentices in the Royal Bindery have produced a facsimile of one of the View Albums. It is a little smaller (for ease of handling) than the originals were, but is bound in blue leather and bears Queen Victoria's cypher on the cover in accordance with the surviving evidence detailing the appearance of the albums the queen and prince made. The reproductions of the original watercolours inside appear in the order given in a listing of their contents made c.1910, before the albums were disassembled. As well as enjoying the detailed, vibrant original watercolours on the walls of the gallery, visitors to the exhibition can also look through the facsimile album at their leisure as Victoria and Albert did themselves nearly 200 years ago.
Browse one of Queen Victoria's View Albums online
'Victoria & Albert: Our Lives in Watercolour' was previously at the Laing Art Gallery, Newcastle, and travels to Poole Museum and Art Gallery (26 October–5 January 2020) and Wolverhampton Art Gallery (7 March–31 May 2020). Carly Collier is the exhibition curator and Assistant Curator of Prints and Drawings, Royal Collection Trust.
The Watercolour World | Registered in England & Wales with the Charity Commission in England & Wales (CCEW) with charity number 1167968 | Company no. 10179857 | Registered address: Poplar Hall Cottage, Burns Green, Benington, Stevenage, SG2 7DB
Website by 3B Digital


Many sourcing products are releasing "diversity features" and then selling you the same product from 2 years ago except with the additional false promise of also improving diversity and inclusion at your company.
If you want to have a strong impact on diversity and inclusion on your team, beware of buying software based on just these diversity features if that's not the core mission of the company selling it. If the company's mission is to do something else but they're selling you diversity, it probably means their core value isn't strong enough, or they're only selling you diversity because it's trendy, not because it's a value they provide.
Here are a couple of features that I'm starting to see across sourcing products that bill themselves as a silver bullet to improving your organization's diversity. Don't fall for these. Save your money and spend it on throwing a happy hour for a URM (Underrepresented Minority) Affinity Group, allocate higher budgets for professional development in your ERGs (Employee Resource Group) or announce a referral bonus for URM hires, as Freada Klein would tell you.
Filter by Gender, Ethnicity, Race, Orientation, etc.
Sales people will tell you that this is something you can use to effectively fill diversity quotas, which may not be a good idea in the first place.
The technology behind these filters is hard to get right, since this is not generally based on candidate-reported data, it's more often guessed by a machine learning algorithm based on name / age / facial rec on profile images, etc. This means that if there is any bias in the technology behind this it's going to mess up your sourcing.
If the teams you are hiring on know about your use of this feature, they may perceive this as lowering the bar, even though it may not be. This will hurt your culture more than actually lowering the bar.
Harder to control one-time outreach. For example, how do you know if you already reached out to that person on LinkedIn Recruiter, or if they're already in your interview process?
Harder to gain competitive advantage through network based sourcing. E.g if you find a candidate that looks great and they are the same school and year as someone on your team, you'd want to ask that person if they can reach out to the candidate in order to maximize your chances of getting a response.
Is there any tech that can actually help with D&I?
Of course there is! It's only fair that I mention some tech and features that are actually being built with equal opportunity as an objective.
Demographic Analytics — features and software that gives you insight into what your candidate pipeline looks like at various stages of the hiring process. What is not measured will not be improved.
At the end of the day, you can use exactly the same tools that you use today and still make a big dent in your team's diversity and inclusion challenges.
It's not always about getting better tools, it's about improving the way you use them.
Did I miss any? Tweet me @pseudovirtual and I'll add them.


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May 17, 2016 May 19, 2016 yodamoLeave a comment
Stagecraft: Book: Performance
You've gotta love Annie, one of the most perfectly paced & melody packed musicals of the modern era. Created for Broadway in the 70s by Charles Strouse (music), Martin Charnin (lyrics) & Thomas Meehan (book), it was based on the adventures of 'Little Orphan Annie,' a 20th daily comic strip set in New York. So is Annie, but Guys & Dolls it definitely isn't. There's not much of the city at all – only one sing 'NYC' giving us any geographical pointers. But the story is timeless, & could be set in any major city of the modern world. Annie is an eleven year old foundling, but one of some spunk. Taken in one christmas by the billionaire Oliver Warbucks, the story revolves around Annies search for her parents & Oliver's attempts to adopt her, which are challenged by the Miss Hannigan – the orphanage boss – & her scoundrel of a brother, Rooster, hell-bent on the $50,000 offered by Warbucks to the real parents of Annie. Around this fun & cutely fantastic plot are a number of classic tunes, such as 'Its a Hard Knock Life', & the eternal ear-worming, still singing it as I write this, 'Tomorrow.' This last number is of course the musicals leibmotif, & one particular reprise encompasses the essence of Annie – its when she finds herself with President Rooseveldt & manages – through the media of song & dance – to lift America out of the Depression and inspire Roosevelt's New Deal (The Sun Will Come Out Tomorrow…)
This particular revival has been brought to us by Nikolai Foster, artistic director of Curve in Leicester, & you can feel the love of the Annie musical he must have, for his version is truly a joy to watch. Five years after its first appearance at the West Yorkshire Playhouse, of its birth Foster told the Mumble, "like a lot of people, I'd vaguely been aware of Annie & had the view that it was saccharine-soaked with all these moppets dancing around doing jazz-handy stuff. I hadn't given it the attention or respect that it deserved. Then about five years ago, I was rehearsing a production of Kes at the Liverpool Playhouse & there was a touring production of Annie playing at the Liverpool Empire. I though it'd be a bit of a laugh, however it was very clear that this was an incredibly well-structured, intelligent, socially relevant piece of writing. I felt so stupid that this brilliant Broadway musical had passed me by."
Jonny Fines
As for last night's performance, I was like a massive big kid loving every minute of it. Elaine C Smith was superb, pure comedy timing from a quality comic.Her battle with Annie – one of personality versus power – was highly entertaining. Annie was irrepressible, a multi-talented lassie who, despite being dwarfed on stage by the old uns, dwarfed them all with her sheer ability. She will be a massive star, this one, if she avoids the many teenage pitfalls of our modern age. Saying that, Jonny Fines, as Rooster, was class – oozing cool & dancing like Hermes on the winds he was an addictive spectacle indeed. There was also Sandy the dog who darted across the stage with accurate & startling regularity, & the six little lady orphans, despite their scruffy attire, gave vivacious performances &, my god, the whole was just bloody brilliant. A cross-generational, cross-status, multi-faceted crystal of a musical, Annie, & in particular this Annie, are a must watch for us all.
Reviewer : Damo Bullen
The Day I Found The Blues


text:
Neelwafurat.com, arabiska نيل و فرات.كوم, är ett e-handelsföretag på internet, snarlikt det amerikanska företaget amazon.com. Det riktar sig främst till köpare i Mellanöstern och Arabvärlden. Företaget säljer böcker, tidskrifter, filmer och programvaror. Det grundades 1998 och var del i den då stora uppgången för arabisk e-handel.

Företagsnamnet Neelwafurat anspelar på floderna Nilen och Eufrat. Neel betyder "Nilen", "wa" är den fonetiska stavningen av den sjätte bokstaven waw i den arabiska konsonantskriften och furat betyder "Eufrat". Namnet ska leda tanken till den koppling Amazon.com har  till Amazonfloden.

Huvudkontoret ligger i Beirut i Libanon.

Referenser

Noter

Företag bildade 1998
E-handelsföretag

redpajama_set_name: RedPajamaWikipedia


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text:
Save $100 on This Android Phone with Integrated Alexa
By Louis Ramirez 19 July 2017
Built-in Alexa, blazing performance, and a new lower price make this a deal you can't miss.
If you're in the market for a big-screen phone that offers blazing performance, exceptional battery life, and a boatload of features, look no further than the Huawei Mate 9.
Normally priced at $599, the Android smartphone is currently on sale for $499.99 via Amazon. That's an extra $41 off its Prime Day price of $540.
The Mate 9 has a giant, 5.9-inch, full-HD screen that offers bright, gorgeous colors. Although it uses an LCD screen instead of OLED, it offers a peak brightness of 630 nits, which in our hands-on review proved to be brighter than the Google Pixel XL, iPhone 7 Plus, and LG V20.
Huawei Mate 9 UnlockedView Deal
The phone packs Huawei's Kirin 960 chip, 4GB of RAM, and 64GB of storage. Its Geekbench 4 score topped mainstream competitors like the iPhone 7 Plus and Google Pixel XL. For everyday use, that means you'll notice no lag or slowdowns whatsoever. Its battery also lasted 12 hours and 6 minutes, which again blew away the competition.
The Mate 9 is also one of a few smartphones with Alexa integration. The one caveat is that you must push an icon on the screen in order to speak with Alexa.
All things said, the Mate 9 is a solid pick if you want an Android smartphone with the top-tier performance and unique features.
Best Tech Deals of Today
Back-to-School Checklist: Great Gear on the Cheap


This past weekend, Tina Fey acted as both host and resident "cool mom" on Saturday Night Live while delivering an excellent performance of System Of A Down's top songs.
Check the performance from here SNL episode, below!
During the episode, the iconic mother and daughter duo of Roberta and Susan (Fey and Melissa Villaseñor) performed a few classics during Susan's high school talent show.
The first time the pair walks onstage, Roberta wants to do a cover of Cyndi Lauper's "Girls Just Wanna Have Fun," a song choice that isn't something her daughter Susan is completely down with, which inevitably forces the duo to change things up.
System Of A Down recently announced three shows in October with support from At The Drive In and Skeleton Witch.


text:
A380 Suite
A380Suite Lavatory
A380 Business Class
A380 Economy
Aviation / Travel
Singapore Air's Unveils New First-class Fleet
Singapore Airlines has just unveiled its new first-class suites, soon to be fitted onto its A380 fleet. Literally the height of luxury, these upmarket boltholes come complete with fully flat beds, personal wardrobes, mood lighting and 32-inch screens.
The new Singapore Airlines A380 fleet cost $850 million to upgrade and will have 471 seats altogether across four classes: six Suites, 78 Business Class seats, 44 Premium Economy Class seats and 343 Economy seats — each with individual AC and USB sockets for keeping devices charges, as well as 18-inch HD screens for entertainment.
Round-trip flights from London to Sydney will set passengers back at least £9,500.
Daily Digest>
Devialet's All-New Audio Systems
Machined from a single block of aluminum, the Devialet 240, Devialet 170 and Devialet 110 were created to effortlessly connect impeccable audio engineering to....
Jackson Pollock's Number 5 to Auction at Christie's
At the Post-War and Contemporary Art Evening Sale at Christie's on May 13, one of Jackson Pollock's most well-known masterpieces, Number 5 "Elegant Lady"....
Picasso's La Colombe d'Or in Provence
Though it would be unfair to dub the exclusive Provençale La Colombe d'Or a "hotel", it's become impossible to name the property that once housed....
Some of New York's Best Restaurants
In an exhaustive study penned for the New York Times, renowned food critic Pete Wells narrates the ever-changing landscape of New York dining in all its....
The Monocle Cafe
The Top Of The Standard
Pier A Harbor House
Claude Bosi At Bibendum
Chiltern Firehouse
Scene Network's Exclusive Club Offers Members-Only Events and Entertainment
Les Visonnaires by Grey Goose
Monocle Launches Travel Guide Series


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text:
import {Directive, Input, OnChanges, SimpleChanges} from '@angular/core';

import {NavigationMode} from '../navigation/navigation-mode.interface';
import {ConfigurableNavigationMode} from '../navigation/configurable-navigation-mode';
import {WizardComponent} from '../components/wizard.component';

/**
 * The [[awNavigationMode]] directive can be used to customize wizard'd navigation mode.
 *
 * There are several usage options:
 *
 * ### Option 1. Customize the default navigation mode with [[navigateBackward]] and/or [[navigateForward]] inputs.
 *
 * ```html
 * <aw-wizard [awNavigationMode] navigateBackward="deny" navigateForward="allow">...</aw-wizard>
 * ```
 *
 * ### Option 2. Pass in a custom navigation mode
 *
 * ```typescript
 * import { BaseNavigationMode } from 'angular-archwizard'
 *
 * class CustomNavigationMode extends BaseNavigationMode {
 *
 *   // ...
 * }
 * ```
 *
 * ```typescript
 * @Component({
 *   // ...
 * })
 * class MyComponent {
 *
 *   navigationMode = new CustomNavigationMode();
 * }
 * ```
 *
 * ```html
 * <aw-wizard [awNavigationMode]="navigationMode">...</aw-wizard>
 * ```
 *
 * ### Additional Notes
 *
 * - Specifying a custom navigation mode takes priority over [[navigateBackward]] and [[navigateForward]] inputs
 *
 * - Omitting the [[awNavigationMode]] directive or, equally, specifying just [[awNavigationMode]] without
 *   any inputs or parameters causes the wizard to use the default "strict" navigation mode equivalent to
 *
 * ```html
 * <aw-wizard [awNavigationMode] navigateBackward="deny" navigateForward="allow">...</aw-wizard>
 * ````
 */
@Directive({
  selector: '[awNavigationMode]',
})
export class NavigationModeDirective implements OnChanges {

  /**
   * Custom navigation mode instance (optional).
   */
  @Input()
  public awNavigationMode: NavigationMode|null;

  /**
   * A parameter for the default navigation mode.  Controls whether wizard steps before the current step are navigable:
   *
   * - `navigateBackward="deny"` -- the steps are not navigable
   * - `navigateBackward="allow"` -- the steps are navigable
   */
  @Input()
  public navigateBackward: 'allow'|'deny'|null;

  /**
   * A parameter for the default navigation mode.  Controls whether wizard steps after the current step are navigable:
   *
   * - `navigateForward="deny"` -- the steps are not navigable
   * - `navigateForward="allow"` -- the steps are navigable
   * - `navigateForward="visited"` -- a step is navigable iff it was already visited before
   */
  @Input()
  public navigateForward: 'allow'|'deny'|'visited'|null;

  constructor(private wizard: WizardComponent) { }

  public ngOnChanges(changes: SimpleChanges): void {
    this.wizard.navigation = this.getNavigationMode();
  }

  private getNavigationMode(): NavigationMode {
    if (this.awNavigationMode) {
      return this.awNavigationMode;
    }
    return new ConfigurableNavigationMode(this.navigateBackward, this.navigateForward);
  }

}

redpajama_set_name: RedPajamaGithub


text:
Maria Stevens
Tue, 06/03/2014 - 10:07 admin
Maria Lana Stevens, age 72, of Boone and formerly of Jefferson, died May 30, at the Israel Family Hospice House in Ames. Her wishes were to be cremated. A Memorial Service will be June 4, at 11:00 a.m. at the Open Bible Church in Boone with Rev. Phil Waldo officiating. Burial of her cremains will be in the Grand Junction Cemetery at a later date. Friends may call at the Church on June 4 from 10:00 a.m. until service time.
Maria Lana Stevens was born in Grand Junction, Iowa, on November 9, 1941, the daughter of John and Edith (Wright) Reineman. She grew up in Grand Junction and graduated from Grand Junction High School. On February 25, 1961, Maria married Earl Stevens in Scranton in the Church of Christ parsonage. The couple lived in Scranton and the Scranton area until they moved to Boone. She was employed as a clerk at the Scranton Grocery Store and at Casey's. Then Maria worked as a housekeeper at the Jefferson Manor and worked in the laundry department at Jefferson Hospital. She retired in 2008. Maria loved her pet cats, dogs and goats, especially Poochie, her beloved Shih Tzu. Maria also loved to cook for her family, especially during the holidays. Her family favorites were fried chicken, cream puffs, and angel food cake. She was always one step ahead of everyone taking care of people.
Maria is preceded in death by her parents, an infant sister Pauline, and a sister Gertrude Morgan. She is survived by her husband Earl of Boone; four daughters, Tina (Lou) Abundis of Winston-Salem, North Carolina, Cindy (Gary) Russell of Boone, Annette (Nick) Foster of Jefferson, and Kristy (Mike) Rohde of Boone; her twin brother John (Carol) Reineman of Jefferson; three sisters Vivian Betts and Wilma Willett, both of Jefferson and Mary Thorpe of Grand Junction; 11 grandchildren; 11 great grandchildren; and nieces and nephews.
In memory of Maria, memorials may be directed to the family.
Schroeder Memorial Chapel at Sixth and Marshall in Boone is in charge of arrangements. Online condolences may be made to www.schroedermemorialchapel.com.


text:
Sustainability isn't new – ask Nan
Written by Rebecca Jones on 30th Apr 2019
There are some that would be forgiven for thinking sustainability is a new idea. An obsession, perhaps, of a sensitive generation of millennials keen to virtue signal their way to 1 million Instagram followers all applauding their use of shampoo-soap and biodegradable wet-wipes.
However, while the latter may have more than a painful twinge of truth about it, the former assertion is, unequivocally, balderdash.
Indeed, while we 30-somethings are busily inventing plant-based plastic bags and compostable take-away coffee cups, another generation is quietly parking their decades old shoppers in caf's across the land as they sit to a (ceramic) mug of tea, perhaps accompanied by a digestive – or two.
That's right kiddo: Nan and Grandad are more eco-friendly than you'll ever be: and don't you forget it.
While our generation has been raised on shrink-wrapped convenience, many of Britain's octogenarians remember a time before Pret a Manger, before microwaves – before refrigerators, even. A time when groceries were bought on the day, put in a pot and made the best of. And if you didn't like it? Well, you went hungry.
According to a recent survey by the Company Shop Group, the over 55's continue to be significantly more sustainable in the supermarket than youngsters. Less than one in ten surveyed by the surplus food distributor claimed to have an issue with wonky veg, compared to a staggering 39 per cent of 16 to 34 year olds who said they would not buy imperfect produce.
And when questioned as to whether they would mind buying food in unbranded packing, just 11 per cent of over 55's said they would think twice, while a third of young people said they would be unnerved by a no-logo product.
The only point of agreement was on buying chilled food, with 50 per cent in both categories claiming they would avoid products approaching their use-by dates – demonstrating, perhaps, the corrupting influence of said fridge-freezers.
Commenting on the findings, group managing director of Company Shop Group Jane Marren said: "This fascinating research shows that while there is a shift happening in the consumer habits of older generations, the admirable environmentalism of young adults today isn't yet translating into what they are buying at the supermarket."
If it's yellow….
Arguably, the survey findings underline an attitude to waste that has – until now – been largely forgotten; or rather relegated to an impoverished past that we have all been glad to say our economy has developed beyond.
Today, anything less than a shower a day – two if you hit the gym – is considered unhygienic. However, our grandparents can recall a time when bathing was a weekly event: an occasion requiring several buckets of water boiled over an open fire that were then poured into a tin bath shared by the entire family, dirtiest going last (if you were lucky).
And while we can now couple our toilet time with quilted, scented, ultra soft loo-roll in a centrally heated bathroom, five year old granny Jones fondly remembers trotting out to her outdoor toilet in the dark armed only with lovingly cut squares of The Daily Mirror.
On lunch breaks across the land we now sit hunched over our computers munching mindlessly at mass produced sandwiches pulled from plastic cartons, however somewhere in the 1950's colleagues are sitting down to meals in a company canteen enjoying a hot meal and, perhaps, a conversation.
Make and mend
And as summer approaches, our grandmothers might regale us with tales of once sewing their own floral dress – recounting the joy of a new fabric their mothers showed them how to turn into something that would become her picnic outfit until it quite literally unravelled.
Meanwhile, we make our third ASOS purchase this month from our smartphone, perhaps as Netflix plays on a laptop in the background, adding next day delivery to a carbon footprint already bursting at the seams of an item made in two minutes by an impoverished mother in Bangladesh.
Sustainability is not, then, a new thing at all. It is a very old thing – a centuries old thing in-fact. The difference today of course is that eco and sustainable living is a choice (at the moment at least, until the penny really drops), rather than an unavoidable by-product of poverty or lack of other options.
In the modern world we are faced with a dilemma our grandparents' generation never imagined: give up the hard won comforts of 'progress', or perish. Today, we find ourselves looking backwards to look forwards, recognising that there was a time not too long ago when plastic water bottles were not a feature of everyday life, but dysentery and cholera were – and trying to find a solution.
The challenges we face as we attempt to lead healthier, longer and better lives while not sacrificing the living world around us are vast and not perhaps as easy as turning back the clock. Nonetheless, we could likely all benefit from taking a a square or two from Nanny Jones's pile of newspaper cuttings.
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The remoteness of the Trans-Labrador Highway challenges drivers from around the world. To survive this epic roadtrip into unparalleled wilderness, one must be as capable of dealing with mechanical faults as with persistent bloodsucking insects, bone-soaking rain, and moose hell-bent on auto-suicide.
For much of the 1185km you can feel like the Last Great Driver on Earth.
Length of Trip : About a 5-8 days return. It all depends on weather, road conditions, construction, and your pace. The guide suggests 8 hours from Baie Comeau to Labrador City, 6 hours then to Goose Bay and 8 hours to Blanc Sablon. Factor in an additional 1-2 hours per day for rest stops, wildlife viewing, construction delays, and bad weather.
Cost : Gas, accommodation and meals. Being this remote, things can be a little pricier.
Best time to go : July and August, although things get going May to September.
Where to eat : Although rest stops are few and far between, most of the small towns and villages you pass through have a restaurant, usually attached to the local hotel. Here's a list of the places I visited: Port Hope Simpson: Alexis Hotel - wonderful service from this family-run hotel/restaurant. Port Hope Simpson: Campbell's Place. Freshly baked bread with partidgeberry jam = great breakfast! Forteau: Seaview Cottage and Restaurant. Staple diner fair. Just ask for "da restaurant!" Happy Valley-Goose Bay: Bentley's Beer Market (97 Hamilton River Rd). Good views, cheap pool tables, a friendly server who looked like Samwell Tarly from Game of Thrones, and a good place to try cod tongues for the first time. There's a Jungle Jim's in the Hotel North II. Load up on the traditional jigs dinner buffet at Mariner's Galley just outside the airport. Red Bay: Whaler's Restaurant & Cabins: Traditional diner fare, good soup for upset tummies! Labrador City: I drove around for a while looking for something different before settling on the Pizza Delight chain next door to the Northern Inn motel. It was actually pretty good! They let you grill your own bread, and you can go heavy on the garlic butter. Big portions for the price too. Also tried the Jungle Jim's in the mall for lunch. Go for the burgers over the healthy looking stuff (which isn't nearly as good). Churchill Falls: Midway Restaurant is your only option, located in the community centre/hotel/supermarket. Top up on poutine before or after your underground tour.
Where to Stay : There are hotels and B&B's at various communities along the route. Consult the driving guide for more info. Here's a list of some of the places I stayed at: Forteau: Grenfell Louis A Hall B&B (also known as "Peggy's"). A former Grenfell hospital with a warm, homely and historical feel. Wonderful clean rooms, outstanding breakfasts, and a host aka Peggy who goes the extra mile (always important on an epic road trip!) Port Hope Simpson: Alexis Hotel - Clean, comfortable, and wonderful service in this family owned hotel/restaurant. Labrador City: Northern Inn and Suites - clean, comfortable centrally located motel next door to the Pizza Delight. Red Bay: Whaler's Restaurant & Cabins: Located in Red Bay and include a restaurant, gift shop and several cottages located throughout the Community of Red Bay; all of which overlook the ocean.
Getting There : You can visit Central Labrador via route 389/500 starting at Baie Comeau Quebec (Via 389), traveling north east to Route 500 to Labrador City and then east past Churchill Falls towards Goose Bay.
Note from Robin : Although conditions would be ideal for a rental car, most rental agreements in Newfoundland specifically prohibit taking the car on the Trans-Labrador Highway. So there goes that idea. The bugs are ferocious. You will want to camp wherever there is a breeze, and have a good supply of Deet. There is no cell phone service, but you can borrow a free satellite phone for use between Labrador City, Goose Bay and Port Hope Simpson, with drop-offs at hotels along the way.
Does the Trans-Labrador Highway belong on the Great Canadian Bucket List?


Children begin identifying colours around the 18-month mark, and start learning the names of different colours between two to three years of age. Teaching your child about colour isn't as simple as saying, "This apple is red" or "The sky is blue". For a young mind to understand a concept as abstract as colour, requires them to be exposed to plenty of information that'll help them distinguish colour from other variables like shape, size and texture. It is a lengthy process that requires much emphasis on a daily basis.
Ready to introduce your little one to the gorgeous colours of the rainbow but not sure where to begin? Here are some everyday tips and tricks to help your kiddo learn the names of every shade.
Use food and snacks to encourage bubba to learn about colours. Set a plate of assorted fruits, veggies, crackers or even candy and ask your little one to sort 'em out according to its colours. It's a fun game with a delicious reward at the end!
Because toddlers are still adding new words to their vocabulary, keep the learning process as simple as possible by using identical objects in different colours and shades. It'll be easier for them to observe colour differences when there aren't any other variables to confuse or distract.
Don't get overexcited when introducing your child to different colours. A fun way to encourage your little one's understanding of individual colours would be to set up a colour week, where that entire span of time would be to dedicated to a specific colour. For example, during Yellow week, your child will pick out outfits only in yellow, or munch on banana-hued snacks, and play with minion-coloured toys. As experiential learners, the little ones will benefit greatly from being able to explore colours through their senses.


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The future of France
French evangelicals hope Macron's "calmed laicité" will protect right to share one's faith publicly
"Any restriction of freedom of worship, conscience, or expression would impoverish the nation spiritually and intellectually, and affect evangelical Christians who publicly testify to their faith", says CNEF representative Thierry Le Gall.
AUTHOR Evangelical Focus PARIS 27 JUNE 2017 17:07 h GMT+1
A boy holds a French flag in Paris. / Laurie Schall (Flickr, CC)
The political scenario has changed much in France in the last three months.
After winning the Presidential and the parliamentary election, President Emmanuel Macron and his "En Marche!" party aim to re-establish the priorities for the country's future.
During the campaign prior to the election, the new President said "religious expression must not be repressed in the private sphere".
French evangelical Christians now hope the ongoing fight against radical Islamism will not "tempt" the new government to reduce the religious freedom in the country.
Thierry Le Gall is Director of Pastoral Services to Members of Parliament of the National Council of Evangelicals in France (CNEF). He answered to Evangelical Focus questions in the following interview.
Question. Which should be some of the top priorities of the new French government for the coming years?
Thierry Le Gall.
Answer. The priority is economic recovery, but not at any price. Mass unemployment is a scourge that affects all categories of the population, especially the youngest, and those who are over 50 years old.
Nevertheless, the needed reforms should not be the cause of a greater impoverishment or an increase in the number of "poor workers" in France.
The French government must also take special care of the families in the aspects that concern them directly: housing, education, social protection, and health.
Question. What are your expectations when it comes to religious freedom and freedom of speech in France?
The President, the Prime Minister and his government have given reassuring signals to religions in France regularly evoking the will to maintain a "calmed laicité".
The struggle against radical and armed Islam must not be to the detriment of the fundamental religious freedoms enjoyed by believers in France. It will, however, be tempting for the legislator to tighten laws in the hope of better protecting the nation and citizens.
Any restriction of freedom of worship, conscience, or speech would impoverish the nation spiritually and intellectually and directly implicate evangelical Christians who publicly testify to their faith. This is an important point of vigilance on which we are working with the Presidency of the Republic and the Parliament.
Question. How will evangelical Christians pray for the new government? Will you have a role in holding the government accountable?
Answer. The CNEF and our partner organisation Protestant Committee for Human Dignity (CPDH, in French) frequently encourage Christians and the churches in France to pray for the authorities.
During our last General Assembly, Pastor Etienne L'Hermenault, the President of the CNEF, said that our struggle as a body of Christ is not to conquer political power, but to keep our hands free to assume our prophetic role in society.
Read more news stories about France.
What does Macron believe about laicité?
Macron's moderate and pro-European message wins in France
European evangelicals urged to pray for the French election
CNEF
Thierry Le Gall
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