text:
\chapter{INTRODUCTION}
\pagenumbering{arabic}

\section{Observational Evidences for Dark Matter}
\vspace{-7.5mm}
\noindent Dark Matter is a very strange form of matter. It does not interact
with known objects because of the lack of electromagnetic interaction. However, it
has a mass and we know that it exists.The main reason for this view
is from gravitational interactions on the visible matter which holds
galaxies and galaxies of clusters together. The idea of the existence
of a new form of matter escaping electromagnetic detections, traces
back at least to 1915. The name ``dark matter'' was firstly used
by the Jacobus Kapteyn in 1922 in his studies of the motions of stars
in our galaxy \cite{1}. He found that there is no need of Dark Matter
within and around the Solar System. In 1923, Jan Oort arrived to an
opposite conclusion that there should be twice as much dark matter
as visible matter in the Solar vicinity. This is the first claim of
evidence for dark matter. However, since later observations have disproved
this early claim, in 1933 the discovery of dark matter is usually
credited to Fritz Zwicky who made the first correct claim about the
existence of dark matter.He concluded that the velocities of the galaxies
in the Coma cluster \cite{2} are much larger than the expected one.
Zwicky found that orbital velocities are almost a factor of ten larger
than expected from the total mass of the cluster \cite{29}. Zwicky
concluded that, in order to hold galaxies together in the cluster,
the cluster should contain huge amounts of some Dark (invisible) matter.
The galaxy rotation curve v, where r marks the distance from the
galaxy's center.

\begin{equation}
\frac{v^{2}}{r}=G\frac{M(r)}{r^{2}}\,,
\end{equation}

\noindent where M(r) is the mass inside radius r and $G_{N}=6.7\times10^{8}cm^{3}g^{-1}sec^{-2}$.
After rearranged the above equation reads

\begin{equation}
v=\sqrt{\frac{GM(r)}{r}}\end{equation}

If the mass is only inside the radius, the velocity should decrease
when there is large value of radius as
\begin{equation}
v\propto1/\sqrt{r}\end{equation} , where $G=1$.

However, for values of r bigger than the size of the galactic bulge,
the velocity of stars remains approximately constant\cite{22}. It means that there is a some unknown energy there such that
\begin{equation}
M(r)\propto r \end{equation}

\begin{figure}
\centering \includegraphics{1} \caption[Distribution of dark matter in NGC 6503] \label{Distribution of dark matter in NGC 6503. Rotation curve of NGC 6503. The curves labeled ìgas,î ìdisk,î and ìhaloî represent the
contributions from the mass in gas, stars, and a dark halo. This plot of the rotation curve
is from Bertone et al. (2005b) using data from Begeman et al. (1991) \cite{22}}
\end{figure}

\noindent For an orbit around a compact central mass, such as planets in the
Solar system, we get Kepler's third law which is given at Eqn.(1.3).

\noindent As an example if the star is placed in the center of a galaxy, that is
the mass density of a galaxy decreases as a power law i.e
\begin{equation}
\rho\propto r^{-n}
\end{equation}
 The mass inside radius r is
\begin{equation}
M(r)\propto\int r^{2}r^{-n}dr\propto r^{3-n}
\end{equation}

\noindent Thus the rotation velocity is
\begin{equation}
v(r)=r^{1-n/2}
\end{equation}

\noindent Near the center of the galaxy, observed rotation curves of a galaxy
v(r) increase with r from Eqn.(1.3), however then suddenly becomes $v(r)\propto$
constant. From the Eqn.(1.5), the density profile is
\begin{equation}
\rho\propto r^{-2}
\end{equation}

\noindent On the other side, the density of stars falls faster when goes to
the edges of the galaxy. The total mass from stars, gas and dust clouds, is
very very small so that they are not able to provide the rotational speed
at large distances. This means that there is another invisible, massive
matter. This matter would be only dominant in the outer parts. The
dark component forms a dark halo which holds galaxies and galaxies
of clusters together.

\begin{figure}
\centering \includegraphics{8} \caption[WMAP data] \label{WMAP data. Credit: NASA / WMAP Science Team \cite{25}}
\end{figure}

\noindent At galactic scales, there is also additional evidence for dark matter
which is based on the mass modeling of the detailed rotation curves
\cite{3}. An evidence of Dark Matter from cluster of galaxies was
first noticed, as mentioned already, by \cite{2} in 1933. On the cluster scales, the $\Omega_{M}$
is today`s mass density including baryonic mass and dark matter \cite{4,5}

\begin{equation}
\Omega_{M}\approx 0.2-0.3
\end{equation}

\begin{figure}
\centering \includegraphics{5} \caption[CMB Temperature fluctuations]\label{ CMB Temperature fluctuations. Image from NASA / WMAP Science Team \cite{25}}.
\end{figure}

\noindent As known that  matter relic density component is bounded by the observation
of the large scale structure.As reported by Sloan Digital Sky Survey
(SDSS) $\Omega_{M}h^{2}=0.135 $ for $\Omega_{b}h^{2}=0.025$
\cite{6}. The mass density of baryons and the mass density of matter in the universe
by using WMAP data are found to be \cite{18,7}  \\

\begin{equation}
\Omega_{b}h^{2}=0.0223
\end{equation}
\begin{equation}
\Omega_{M}h^{2}=0.127
\end{equation}

\begin{figure}
\centering \includegraphics[scale=0.75]{2} \caption[WMAP observes the first light of the universe]\label{WMAP observes the first light of the universe. Credit: NASA / WMAP Science Team \cite{25}}
\end{figure}

\noindent From WMAP`s data and large scale structe observations`s data for relic abundance are consistent. In physical cosmology,
Big Bang nucleosynthesis provides us also a constraint\cite{13}

\noindent The difference between $\Omega_{M}h^{2}$ and $\Omega_{b}h^{2}$ is
the clue of the existence of the non-baryonic dark matter.

\noindent There are many experiments which support the existence of Dark Matter
such as CMB anisotropy, galaxy surveys, etc. so we think that there
is Dark Matter. Unfortunately, the nature of dark matter is now an open problem.
So this is a very hot topic in physics.

\noindent Furthermore, there are some additional constraints on the amount of
dark matter in the Universe. We know very well from the concordance
cosmology measurements(it's basically a combination of looking at
the microwave background fluctuations, the baryon acoustic oscillations,
and the supernova brightness versus redshift relation)what are the
relative fractions of dark energy and mass in the Universe. We also
have pretty good constraints from primordial abundances of the elements
on what the relative fractions are for baryonic and non-baryonic dark
matter because if there were too high a density of protons in the
early universe, then there would have been more fusion in the early
universe\cite{30}.
\vspace{-7.5mm}

\section{Baryonic Dark Matter(BDM)}
\vspace{-7.5mm}
\noindent MACHO(massive compact halo object); planet-like objects, plasma and other compact objects are the candidates
for BDM. Other examples of this class of dark matter candidates include
primordial black holes created during the big bang, neutron stars,
white dwarf stars and various exotic stable configurations of quantum
fields, such as non-topological solitons. Gravitational Microlensing
is one of the ways to detect these objects. However, this method
only gives us the information about the mass, distance and velocity
of them and nothing more.
\\
\noindent Heavier, relatively faint objects such as old white dwarfs and mini
black holes,are the most important candidates for this BDM. If there
are primordial mini black holes produced in the big bang before BBN(Big Bang Nucleosynthesis),
they would not contribute to $\Omega_{b}$.
\\
\noindent $0.07M_{\odot}$ is required by a star to start to shine as a star
by igniting thermonuclear fusion. Brown dwarfs are not completely
dark because they radiate faint thermal radiation. However, the typical
mass of these MACHOs should be $\approx0.5M_{\odot}$, which is much
larger than the brown dwarf mass. In addition, white dwarf has a mass
which is suitable for dark matter but there is not enough number of
observed white dwarfs. Hence, BDM is not as good candidates for dark
matter as nonbaryonic dark matter.

\vspace{-7.5mm}
\section{Nonbaryonic Dark Matter}
\vspace{-7.5mm}
\noindent Hot Dark Matter (HDM) and Cold Dark
Matter (CDM) is considered as a nonbaryonic dark matter. Other more special options have been considered, such
as for example warm dark matter (WDM).\\

\noindent Dark matter particles that are called HDM, are relativistic at the time
of matter-radiation equality time. This requirement implies that their
mass has to be lower than about 100 eV. Their thermal velocities,
when structure formation begins are large because of the small mass.
In contrast, CDM has large mass so its velocities are negligible.
Candidates between hot and cold are called warm dark matter.\\

\noindent Effect of the pull of gravity causes to form galaxies and galaxy clusters
from early homogeneously distributed. This is called structure formation.
Today the best way to differentiate between HDM, WDM and CDM is through
the observed large-scale structure, i.e. CMB which shows the seeds
of structure. We show in Fig. (1.3) the results of a simulation of
the halo of dark matter around the Milky Way and two other galaxies.
For CDM, there is more substructure and satellites around the galaxy,
while their formation is suppressed for WDM. According to observations,
there is an order of magnitude less satellites observed around the
Milky Way than predicted by CDM models. However, the observations
are not complete, and the discrepancy may also be due to other causes
than WDM.

\begin{figure}
\centering \includegraphics[scale=0.5]{3} \caption[Comparison of the expected halo of the MilkyWay and the galaxies M31 and M33 in CDM and WDM models]\label{ Comparison of the expected halo of the MilkyWay and the galaxies M31 and M33 in CDM and WDM models. From http://www.clues-project.org/images/darkmatter.html.}
\end{figure}

\noindent The most common candidates for non-baryonic dark matter are Weakly
Interacting Massive Particles, or WIMPs \cite{17}. Cold dark matter has a most important candidate which is WIMPs. Because
they have neutral charge and they are long lived particles. Only weak
force and gravitational force effect them. Large amount of WIMPs are
produced and then the interaction rate of WIMPs was decreasing so
decoupling increasing between them in the thermal bath of the early universe when cools
down, like neutrinos, but are much heavier, so that they are a form
of CDM. After the decoupling, their relic density remains constant
as consistent with experiments. This is called WIMPs miracle. Furthermore
the interactions of some dark matter candidates are stronger or weaker.
For example, gravitinos have only gravitational interactions, while
TIMPs (Technicolour Interacting Massive Particles) have much stronger
interactions.
 \noindent Neutralino (bino+wino+2higgsino) lightest supersymmetric
particle is the best candidate for WIMP in Minimal Supersymmetric Standard Model (MSSM)\cite{14,15}.
\noindent The other candidate for WIMP is the lightest Kaluza Klein (LKP) which
is coming from Universal extra-dimensions (UED) model .

\vspace{-7.5mm}
\subsection{Hot Dark Matter (HDM)}
\vspace{-7.5mm}
\noindent For the HDM neutrinos are candidates. Energy density today is dominated
by their rest masses so to make a significant contribution to the
density parameter, neutrinos should have a rest mass about 1 eV.
\noindent The present upper limit to HDM in the form of massive neutrinos leads
to the conservative mass limit from WMAP data.

\begin{equation}
\sum m_{\nu}\leq0.62eV
\end{equation}

\noindent Therefore the maximum contribution of neutrinos is $\Omega_{\nu}h^{2}\leq0.02$,
at most the same order of magnitude as baryonic matter. If neutrinos
were the dominant form of matter, there would be a lower limit on
their mass from constraints on the phase space density, called the
Tremaine-Gunn limit. Essentially, in order to achieve a certain rotation
velocity for galaxies, you need a certain amount of mass inside a
given volume, and the Pauli exclusion principle constrains the number of particles you can pack inside a given volume. Even though
we know that neutrinos are a subdominant component of dark matter,
the Tremaine-Gunn limit applies to any fermionic dark matter candidate,
even if its distribution is not thermal. (There is no similar lower
limit on the mass of a bosonic dark matter particle.)

\vspace{-7.5mm}
\subsection{Cold Dark Matter (CDM)}
\vspace{-7.5mm}
\noindent Most of the matter in the universe has to be CDM because of data on
large scale structure combined with structure formation theory. WIMPs
(Weakly Interacting Massive Particles) are the main candidates of
CDM.
\noindent Dark matter candidates are with masses in the 100 GeV to TeV range.
Particles with GeV to TeV masses and weak-scale interaction cross
sections are known as Weakly Interacting Massive Particles (WIMPs).
There are also another candidates for DM. However, WIMP dark matter
is compelling for two main reasons:
\begin{enumerate}
\item In the early universe, when WIMPs were in thermal equilibrium annihilated
with each other with a weak scale cross section. As the universe expanded
and has frozen out, WIMPs cooled to obtain a relic density today which
is equal to the measured dark matter density.

As mentioned before that this is known as the WIMP Miracle.

\item The other reason is that WIMP dark matter are present in many of the
favored extensions of the Standard Model.For example, the Minimal
Supersymmetric Standard Model (MSSM) has a favourite WIMP candidate.
\end{enumerate}

\chapter{EXTENDED GRAVITY: $f(R)$ GRAVITY}

\section{Introduction to $f(R)$ Gravity}
\vspace{-7.5mm}
\noindent By changing the law of gravity, it could be possible that the observations
are explained. Until the dark matter particle is detected, there is
some room for uncertainty. The problem for modified gravity is that
there are so many different observations for dark matter, in different
physical systems: motions of stars in galaxies, motions of galaxies
in clusters, gravitational lensing, large-scale structure, CMB anisotropies
and so on. Gravity has to be adjusted in a different manner for these
different observations, and the resulting models are somewhat contrived.
Expressed another way, the dark matter scenario is very predictive:
the simple hypothesis of a massive particle with weak couplings to
itself and to the Standard Model particles explains a number of disparate
observations and has made successful predictions.\\
\noindent In 1919 and 1922 respectively by Weyl and Eddington \cite{51,52}
gravitational action firstly studied. However, until 1960s, there
was not any indications of complicating the gravitational action.
Because of cosmological problems such as the dark energy problem,
dark matter problem, this type of modification is needed to fix the
problems. At $f(R)$ theory, the main idea is to take action as a function
instead of a constant curvature such as:

\begin{equation}
S=\frac{1}{16 \pi G}\int d^{4}x\sqrt{-g}[f(R)]
\end{equation}

\noindent By using the $f(R)$ function , it provides usage of many different properties,
which are very important for explaining unknown matters
such as dark matter and dark energy. For instance, considering f as
a series expansion i.e \cite{54,55,56,57,58,59}

\begin{equation}
f(R)=...+\frac{\alpha_{2}}{R^{2}}+\frac{\alpha_{1}}{R}-2\Lambda+R+\frac{R^{2}}{\beta_{2}}+\frac{R^{3}}{\beta_{3}}
\end{equation}
\noindent where $\alpha_{i}$ and $\beta_{j}$ coefficients have the appropriate
dimensions. So it can be seen that a number of interesting terms appear. \cite{53}

\noindent Without matter action is given above, now after adding matter on the
action, our $f(R)$ action is

\begin{equation}
S=\frac{1}{16\pi G}\int d^{4}x\sqrt{-g}[f(R)+S_{M}(g_{\mu\nu},\psi)].
\end{equation}

\noindent Varying the action with respect to $g_{\mu\nu}$ provides

\begin{equation}
f_{R}R_{\mu\nu}-\frac{1}{2}fg_{\mu\nu}-\nabla_{\mu}\nabla_{\nu}f_{R}+g_{\mu
\nu}\square f_{R}=\kappa T_{\mu\nu}%
\end{equation}

\noindent where $f_{R}=\frac{df}{dR}$ \ , $\square f_{R}=\frac{1}{\sqrt{-g}}%
\partial_{\mu}\left(  \sqrt{-g}\partial^{\mu}\left(  \frac{df}{dR}\right)
\right)  $ \ \ and \ $\nabla^{\nu}\nabla_{\mu}f_{R}=g^{\alpha\nu}\left[
\left(  f_{R}\right)  _{,\mu,\alpha}-\Gamma_{\mu\alpha}^{m}\left(
f_{R}\right)  _{,m}\right]  $

So

\begin{equation}
\square f_{R}=\square\frac{df}{dR}=\frac{1}{\sqrt{-g}}\partial_{1}\left(
\sqrt{-g}g^{11}\partial_{1}\left(  \frac{df}{dR}\right)  \right)  =\frac
{1}{\sqrt{-g}}\partial_{1}\left(  \sqrt{-g}g^{11}\left(  \frac{df}{dR}\right)
^{^{\prime}}\right)
\end{equation}

\begin{equation}
\nabla^{0}\nabla_{0}f_{R}=\nabla^{0}\nabla_{0}\frac{df}{dR}=-\frac{1}{2}%
g^{00}\Gamma_{00}^{1}\left(  \frac{df}{dR}\right)  ^{^{\prime}}=-\frac{1}%
{2}g^{00}g^{11}g_{00,1}\left(  \frac{df}{dR}\right)  ^{^{\prime}}%
\end{equation}

\begin{equation}
\nabla^{1}\nabla_{1}f_{R}=\nabla^{1}\nabla_{1}\frac{df}{dR}=g^{11}\nabla
_{1}\nabla_{1}\frac{df}{dR}=g^{11}\left(  \frac{df}{dR}\right)  ^{^{^{\prime
\prime}}}-g^{11}\Gamma_{11}^{1}\left(  \frac{df}{dR}\right)  ^{^{\prime}}%
\end{equation}

\begin{equation}
\nabla^{2}\nabla_{2}f_{R}=-g^{22}\Gamma_{22}^{1}\left(  \frac{df}{dR}\right)
^{^{\prime}}=\frac{1}{2}g^{22}g^{11}g_{22,1}\left(  \frac{df}{dR}\right)
^{^{\prime}}%
\end{equation}

\noindent in which a prime means d/dr and its variation with respect to $g_{\mu\nu}$ yields, after some
manipulations and modulo surface terms, the field equation

\begin{equation}f_{R}R_{\mu\nu}-\frac{f(R)}{2}g_{\mu\nu}=\nabla_{\mu}\nabla_{\nu}f_{R}-g_{\mu\nu}\Box f_{R}+\kappa T_{\mu\nu}\end{equation}

\noindent where $\nabla_{\mu}$ is the covariant derivative associated with
Levi-Civita connection of the metric, and $\Box=\nabla^{\mu}\nabla_{\mu}$.

\noindent These equations above are fourth order partial differential equations
in the metric. The alternative name ``fourth order gravity'' used
for this theories because in the first two terms on the right hand
side fourth order derivatives appear.

\noindent Furthermore, the contraction of the  above equation  yield the
trace equation
\begin{equation}
f_{R}R-2f+3\square f_{R}=\kappa T
\end{equation}

\noindent where $T=T_{\mu}^{\mu}=0$

\noindent the trace equation can be used to simplify the field
equations and then keep it as a constraint equation.

\noindent Therefore
\begin{equation}
f_{R}R_{\nu}^{\mu}-\frac{1}{4}\delta_{\nu}^{\mu}\left(  f_{R}R-\square
f_{R}-\kappa T\right)  -\nabla^{\nu}\nabla_{\nu}f_{R}=\kappa T_{\nu}^{\mu}%
\end{equation}

\noindent The trace of this equation is

\begin{equation}
f_{R}R-2f(R)+3\Box f_{R}=8\pi GT
\end{equation}
where $T=g^{\mu\nu}T_{\mu\nu}$

\noindent Here we can see that when $T=0$ , not anymore says that $R=0$ or constant.

\noindent Another important thing is that when $R=constant$ and $T_{\mu\nu}=0$,
it reduces to

\begin{equation}f_{R}R-2f(R)=0\end{equation}

\noindent Maximally symmetric solutions is affected by f function, and they
will be Minkowski, de Sitter or anti-de Sitter.
Hence, We can now write the field equations in the form of Einstein
equations as

\begin{equation} G_{\mu\nu}=R_{\mu\nu}-\frac{1}{2}g_{\mu\nu}R=\frac{\kappa T_{\mu\nu}}{f_{R}}+g_{\mu\nu}\frac{[f(R)-Rf_{R}]}{2f_{R}}+\frac{[\nabla_{\mu}\nabla^{\nu}f_{R}-g_{\mu\nu}\Box f_{R}]}{f_{R}}   \end{equation}

\noindent After some algebra the above equation, takes the form

\begin{equation} F(R)R_{\mu\nu}-\nabla_{\mu}\nabla^{\nu}F(R)-kT_{\mu\nu}=-g_{\mu\nu}(\frac{1}{2}f(R)-\nabla_{\alpha}\nabla^{\alpha}F(R))\end{equation}  where $F(R)=df/dR=f_{R}$.

\noindent For solving above equation we need a metric and its components\cite{53}
. Here we are using spherically symmetric metric with radial components B(r) and X(r) :

\begin{equation} ds^2=-B(r)dt^2 + \frac{X(r)}{B(r)}dr^2 + r^2d\Omega^2 \end{equation}

\noindent  Ricci scalar of this metric can be written as

\begin{equation} R(r)=\frac{2}{r^2}+\frac{X'} {X^2}(\frac{B'}{2}+\frac{2B}{r})-\frac{1}{X}(B''+\frac{4B'}{r}+\frac{2B}{r^2}) \end{equation}

\noindent For empty space if we solve the Einstein Equation with the form of $f(R)$ gravity, two independent field equations are found :

\begin{equation} \frac{X'}{X} = \frac{2rF''}{2F+rF'}  \end{equation}

\begin{equation} B''+(\frac{F'}{F}-\frac{X'}{2X})B'-\frac{2}{r}(\frac{F'}{F}-\frac{X'}{2X})B-\frac{2}{r^2}X=0 \end{equation}

\noindent where the prime means d/dr. After that are choose our ansatz with constants $ F_{0}$, $X_{0}$ and $B_{0} $ as

\begin{equation} F(r)=F_{0}r^{n}, X(r)=X_{0}r^{\alpha}, B(r)=B_{0}r^{\alpha} \end{equation}

\noindent Constans are bounded by two constraints as:

\begin{equation} \alpha=\frac{2n(n-1)}{n+2}, X_{0}=[1+\frac{n(2-\alpha)}{2}-\frac{\alpha^2}{4}]B_{0}.\end{equation}

\noindent After that \begin{equation} R(r)=\frac{2R_{0}(n,\alpha)}{r^2} \end{equation} is obtained.

\noindent where

\begin{equation} R_{0}(n,\alpha)=1-\frac{1+\frac{\alpha}{2} +\frac{\alpha^2}{8}}{1+n(1-\frac{\alpha}{2})-\frac{\alpha^2}{4}} \end{equation}

\noindent This will be the well known solution of Schwarzschild  when $\alpha$ or n goes to zero. After using those constraints and definitions, an asymptotic form of $f(R)$ where
$\Lambda_{0}$= constant of integration is found as

\begin{equation} f(R)= \frac{f_{0}(2R_{0})^{(\frac{n}{2})}}{1-(\frac{n}{2})}R^{(1-\frac{n}{2})} + \Lambda_{0} \end{equation}

\noindent In the paper of A Model of $f(R)$ Gravity as an Alternative for Dark Matter in Spiral Galaxies they took $F_{0}=1 $ when n is going to zero and action goes to $F_{0}R+\Lambda_{0}$.

\noindent For the application  of this in the rotation curve, geodesic equation is used in the weak field approximation. The test particle is rotating around the central mass and obtains as
\begin{equation} \ddot{r}+\Gamma^{r}_{tt}=0 \end{equation}  where the dot means d/dt. After using the affine connection which we found by using metric :

\begin{equation}
\Gamma_{t t}^r = \frac{B}{2XB'} , \Gamma_{t r}^t = \frac{B'}{2B} , \Gamma_{r r}^r = \frac{X'B-XB'}{2BX} ,  \Gamma_{r \theta}^{\theta} = \Gamma_{r \phi}^{\phi}=\frac{1}{r} ,
\Gamma_{\theta \theta}^r = \frac{Br}{X} \end{equation}

\begin{equation}
 \Gamma_{\theta \theta}^r = \frac{Br}{X} , \Gamma_{\theta \phi}^{\phi} = tan(\theta) , \Gamma_{\phi \phi}^{r} =  \frac{Br sin(\theta)^2}{X} , \Gamma_{\phi \phi}^{\theta} = -\frac{sin(\theta)}{2}
\end{equation}

\noindent velocity for a test particle is obtained as

\begin{equation} v^{2}=\frac{rc^{2}B'B}{X}= \frac{c^{2} \alpha B_{0}r^{\alpha}}{2} \end{equation}

\noindent After considering some assumption for the large distances from center of galaxy, such as using  $r^{\alpha}=1+\alpha\ln(r)$  where $\alpha$ is  smaller than 1, one finds that

\begin{equation}v^{2}_{\infty}=\frac{c^{2}\alpha B_{0}}{2}  \end{equation}

\noindent For taking \(B_{0}=2\sqrt{\mu M_{galaxy}}\) where $\mu$ is the proportional coefficient with mass inverse dimension and M is mass of galaxy, hence asymptotic velocity is found

\begin{equation} v^{2}_{\infty}=c^{2}\alpha\sqrt{\mu M_{galaxy}}  \end{equation}

\noindent where $\alpha$ and $\mu$ depend on experimental datas. For instance, if this values taken as  \( \alpha^{2} \mu=(v_{\infty}/c)^{4} /M_{galaxy}=10^{-54}kg^{-1}\), the velocity is found exactly $200 kms^{-1}$ and this value is consistent with Tully-Fisher`s relation. \cite{53}

\noindent Furthermore,  another good testing is made by using the Modified Newtonian dynamics (MOND).

\begin{equation} \alpha^{2}\mu=0.98\times10^{-54}kg^{-1} \end{equation} for the velocity of typical galaxy.

 \noindent There are many difficulties of this theory. One example which gained a lot of publicity a few years ago is the
Bullet cluster. A solution of the Dark matter conundrum in terms of a new elemantary particle is quite successful to explain the Bullet cluster, while explanations in terms of modified gravity models encounter serious difficulties. Another problem in this way of solution is that ansatz is choosen by hand and not naturally comes out.

\chapter{DARK MATTER PRODUCTION}

\section{Thermal Production}
\vspace{-7.5mm}
\noindent WIMPs and many other dark matter candidates are in thermal equilibrium
in the early universe and decouple once their interactions become
too weak to keep them in equilibrium. Those particles are called thermal
relics, as their density today is determined by the thermal equilibrium
of the early universe. When the annihilation processes of WIMPs into
SM particles and vice versa happend at equal rates, there is a equilibrium
abundance. When the Universe cooled down and the rate of expansion
of the universe H exceeds the annihilation rate, the WIMPs effectively
decouple from the remaining SM particles. So the equilibrium abundance
drops exponentially until the freeze-out point.The abundance of cosmological
relics remained almost constant until today \cite{35}.

\noindent If the candidate is stable or has a long lifetime, the number of particles
is conserved after it decouples, so the number density falls like
$a^{-3}$. Specifically, we use the Lee-Weinberg Equation \cite{61}. It describes
annihilation and creation of $\chi$ particles \cite{60,62}.

\begin{equation}
\frac{dn_{\chi}}{dt}+3Hn_{\chi}=-<\sigma v>(n_{\chi}^{2}-n_{\chi,eqn}^{2})
\end{equation}

\noindent with $n_{\chi,eqn}^{2}$ ,the  number density of the
relic particles in equilibrium. Furthermore Hubble constant make expanding universe effect. The thermal average of the
annihilation cross section $\sigma$ multiplied with the relative
velocity v of the two annihilating $\chi$ particles. The first (second)
term on the right-hand side (RHS) of the equation describes the decrease
(increase) of the number density due to annihilation into (production
from) lighter particles. Kinetic equilibrium  is satisfied by the Lee-Weinberg equation for $\chi$

\noindent Now we use Hubble constant effect which provide  universe expansion by considering
the evolution of the number of particles in a portion of comoving
volume given by

\begin{equation}
N=n_{\chi}R^{3}
\end{equation}
We can then introduce the convenient quantity
\begin{equation}
\bar{N}=\frac{n_{\chi}R^{3}}{N(0)}
\end{equation}

\noindent such that $\bar{N(0)}=1$.

\noindent In addition, since the interaction term usually depend explicitly
upon temperature rather than time, we introduce the $x=\frac{m}{T}$, the
scaled inverse temperature.

\noindent During the radiation dominated period of the universe, thermal production
of WIMPs takes also place . For this time, one can find the expansion rate

\begin{equation}
H=\sqrt{\frac{8\Pi^{3}gg_{\chi}T^{2}}{90}}
\end{equation}
and then
\begin{equation}
\Longrightarrow H(x=1)=m^{2}\sqrt{\frac{8\pi^{3}gg_{\chi}}{90}}
\end{equation}
where $H(x)=\frac{H(x=1)}{x^{2}}$ and where $_{\chi}$ refer the
number of intrinsic degrees of freedom such a like that spin or color for $\chi$ particle.

\noindent Hence we can write the last format of our equation a

\begin{equation}
\frac{d\bar{N}}{dt}=-\frac{<\sigma v>N(0)}{R^{3}Hx}(\bar{N}^{2}-\bar{N}_{eqn}^{2})
\end{equation}
where
\begin{equation}
\frac{N(0)}{R^{3}}=\frac{3\zeta[3]m^{3}}{4 \Pi^{2} x^{3}}
\end{equation}

\noindent After all little tricks , our Lee-Weinberg equation can be recast
as

\begin{equation}
\frac{d\bar{N}}{dt}=-\frac{\Psi(\chi)}{x^{2}}(\bar{N}^{2}-\bar{N}_{eqn}^{2})
\end{equation}

\noindent where we defined
\begin{equation}
\Psi(\chi)=\frac{3\zeta[3]}{4\Pi^{2}}\sqrt{\frac{45}{4\Pi^{3}}}\frac{g_{\chi}}{\sqrt{g_{\chi}}}mM_{Pl}<\sigma v>=0.055\frac{g_{\chi}}{\sqrt{g_{\chi}}}mM_{Pl}\sigma_{0}
\end{equation}

where $\zeta$ is EulerñRiemann zeta function
\noindent To integrate the Lee-Weinberg equation, we need to have an expression
for the equilibrium number density in comoving volume.Once the particle
is non-relativistic, the difference in statics is not important.

\noindent The general equation of equilibrium number density in comoving volume
is

\begin{equation}
\bar{N(x)}_{eqn}=\frac{2}{3\zeta[3]}\int_{0}^{\infty}\frac{y^{2}}{1+\exp^{\sqrt{x^{2}+y^{2}}}}dy
\end{equation}

\noindent For the nonrelativistic case at low temperatures $T\gg m_{\chi}$ one
obtains,
\begin{equation}
\bar{N(x)}_{eqn,NR}=\frac{2}{3\zeta[3]}\frac{\Pi}{2}x^{3/2}\exp^{-x}
\end{equation}

\noindent At great value of temperatures, dark matter quickly is destroyed by its own antiparticle. Shortly after that, until $\Gamma_{\chi}=\bar{N(x)}<\sigma v> \ll  H $, T has dropped too much which is under the value of  $m_{\chi}(T<<m_{\chi})$, also the number density of dark matter drops exponentially. The temperature at which the particle decouples (The time when the number of particles reaches this constant value) is called freeze-out temperature $T_{F}$. Hence the number density per comoving volume becomes almost constant because dark matter particles are no longer able to annihilate efficiently.

\noindent An approximate solution for the relic abundance is given by
\begin{equation}
\bar{N}(t)\equiv\bar{N}(\infty)\cong\frac{x_{f}}{\Psi}
\end{equation}
. where $x_{f}=\frac{m}{T_{f}}$ and $T_{f}$ is the so called `freeze-out`
temperature and approximately, for the typical case $x_{f}\succ\succ1$,one
has that $x_{f}$ is a solution of

\begin{equation}
\sqrt{x_{f}}e^{x_{f}}=\Psi
\end{equation}

\noindent We can then finally calculate the contribution of $\chi$ to the energy
density parameter finding a well know result

\begin{equation}
\Omega_{\chi}h^{2}\cong4\times10^{-10}\frac{GeV^{-2}}{\sigma_{0}}
\end{equation}

\noindent It is intriguing that so called ``WIMPS''(e.g. the lightest supersymmetric
particle) dark matter particles seem to reproduce naturally the right
abundance since they have a weak cross section

\begin{equation}
\sigma_{0}\cong\frac{\alpha^{2}}{m^{2}}\cong10^{-9}(\frac{100GeV}{m^{2}})
\end{equation}
and masses $m_{x}~m_{ew}~100GeV$. This observations is called the
``WIMP miracle'' and typically considered as an encouraging point
supporting WIMPS as Dark Matter candidates.
\begin{figure}
\centering \includegraphics{133} \caption[ Evolution of $\bar{N}$  and $\bar{N}_{eqn} $  as function of x ] \label{ Evolution of $\bar{N}$  and $\bar{N}_{eqn} $  as function of x for m =100 GeV, $g_{\chi} =2 $, g =90 (constant), $\sigma_{0}=10^{-14} , 10^{-15} and  10^{-16} $  , $M_{Pl} =1.9 \times10^{19}  GeV^2 $   }
\end{figure}

\noindent The LW eqn. can be solved by approximately analytic
calculation or numerical plotting by using Mathematica.We have plotted
those equation by using both of the ways. As you can see Fig. 2.1.

\noindent LW Eqn., the termal production, is the most traditional
mechanism but that many other mechanisms have been considered in the
literature such as non thermal production of very massive particles(so
called WIMPZILLAS) at preheating or even right-handed neutrino oscillations.

\chapter{CONCLUSION}

\noindent The observational evidence for dark matter is overwhelming and now
we are entering one of the perhaps most exciting periods in physics
history where a wide array of experiments may have the potential to
unveil its nature.In this thesis I review some important concepts
about dark matter. One of the best motivated candidates for dark matter
so far is the WIMPS which I mentioned before. In this thesis the focus
was on dwarf spheroidal galaxies, promising targets that are assumed
to be strongly dark matter dominated systems due to their high mass-tolight
ratios up to few hundred solar units. Dwarf galaxies of the Milky
Way have the advantage of relative proximity and low astrophysical
background as they do not lie within the galactic plane. Great importance
was given to studying the properties of these systems and how their
dark matter profiles can be derived from kinematical studies. However
a precise estimation of the density distribution is a challenging
task and due to too little data available in particular the shape
of the dark matter halo inner regions remains poorly known. Cusped
profiles suggested from simulations like the Navarro-Frenk-White profile
are not ruled out in general although observations seem to favor profiles
with a flat inner core.

\noindent The two investigated dwarf spheroidal galaxies Sagittarius and Canis
Major are particularly attractive targets as they are the closest
dwarf galaxies discovered so far. The uncertainty concerning their
inner region is reflected in the plots of sensitivity limits for both
investigated dwarf galaxies, where the distances between the two lines
of a cored and a cusped profile are about one order of magnitude.

\noindent Better opportunities for a significant dark matter detection could
be obtained for instance by the next generation ground-based CTA (Cherenkov
Telescope Array) experiment with bigger effective areas due to many
Cherenkov telescopes in the order of 50 and also IceCube experiment
. Here, stereoscopy will be possible for small energies. Moreover
the space based ray telescope FERMI will yield interesting results
in the future.Apart from Sagittarius and Canis Major, there could
be promising faint dwarf galaxies that are not discovered yet. However,
there should be as many undiscovered dwarf galaxies in the other direction,
too, which, when discovered, will provide interesting targets for
the search of dark matter.

\noindent In chapter 2 we gave a simple example of $f(R)$ extended gravity in which the effect of DM is not due to exotic sources but due to the wrong choice of Lagrangian. Einstein`s model, which extends that of Newton is characterized by the specific choice $f(R)=R$. In the $f(R)$ model this has been modified to different polynomial powers of R. As an example the choice $f(R) \approx R^{1-\frac{n}{2}}$ where $ n\ll 1 $, describes asymptotic behaviours of flat rotation curves and experimental results of Tully-Fisher (i.e. $v^{4}\approx$ Mass). For n=0 the model reduces to the Einstein`s general relativity model which fails to explain flat rotation curves unless supplemented by exotic sources.

redpajama_set_name: RedPajamaArXiv


What are you listening to, Thomas?
One of 2010 best albums, came from this man. Thomas Jonsson, AKA I'm Kingfisher. The album, "Arctic" was released by Playground Music, the harbour of great swedish music. I'm Kingfisher is one of the greatest in that crowd.
The man has toured with artists like Ed Harcourt, and has recorded stuff with artists such as Rosie Thomas (one of my all time favorites) Damien Jurado, Ned Oldham and other great acts.
He is currently on tour with Damien Jurado, and will be playing @ Pustervik (Woody West, again with the majestic bookings) and later in Malmö and Stockholm.
Thomas is a man with a plan, Arctic is just a part of a trilogy plan, and one can only imagine the great stuff that is coming our way. We'll be waiting. Impatiently, but still.
– A lot of instrumental drone stuff. I just fell in love with Earth's newest album 'Angels of darkness, demons of light I'. This year I think Earth, Mogwai, Tennis, Thomas Hine and James Blake have done really good stuff.
I've also recently listened a lot again to last year's best album "St Bartlett" of Damien Jurado, since I just got it on vinyl after our show in Copenhagen a couple of days ago. And oh, it has also been a lot of Efterklang's newest.
That I will tour as much as I want while finishing the recordings of my next album, as well as an album with a new Swede-Swede-French collaboration project I'm a part of. That mink farming will be banned once and forever. That sound engineers on my shows from now on and forever will set my guitar sound as loud as I want without questioning me.
Three artists who inspire you?
Recently: Victoria Legrand, singer of Beach House.
For the Arctic album: Six Organs of Admittance. Forever: M Ward.
Who deserves a breakthru in 2011?
– Dear Euphoria, my favorite Swedish band, whose 2010 EP "This Night will Flee" contains "Rescue", one of last year's two best pop singles (together with Sleigh Bells' "Rill Rill"). It's on Spotify!
I for one, is going to see I'm Kingfisher on sunday, and I know for a fact that you can still pick up some tix.
This entry was posted on fredag, april 15th, 2011 at 23:30and is filed under . You can follow any responses to this entry through the RSS 2.0 feed. You can leave a response, or trackback from your own site.


Birthday wishes have been pouring in all over the Internet for Paul Stanley today (Jan. 20), on what is the Kiss frontman's 60th birthday. His bandmates took to KissOnline.com to help celebrate the big day with posts for their fellow Kiss member and friend, who was born in New York on Jan. 20, 1962.
Meanwhile, Kiss recently finished recording their forthcoming new album, 'Monster,' and in a Twitter note posted yesterday Thayer reveals that the band is working on cover art for the disc. "Heading into town to meet @genesimmons, Paul Stanley, and Eric Singer for album cover photo shoot," he wrote.
We're not quite sure what town he was headed into, but we should find out soon enough. No release date for 'Monster' has been announced, but in the meantime you can get a taste of what's in store for Kiss fans by checking out our 'Monster' album preview.


Ideal for, casseroles, cobblers and more, the All-Clad, E901946, 8 in. Covered square baker makes a useful addition to any kitchen. The pan provides upright handles for a secure hold from oven to table, along with gently rounded edges and corners for easily removing baked food with a spatula. Even more, the baker's fitted BPA-free plastic lid makes transport to potlucks and holiday parties hassle-free-plus allows for refrigerating leftovers right in the pan. Forged from heavy-gauge stainless steel, the All-Clad square baker distributes heat quickly and evenly and promotes pure-tasting results thanks to its non-reactive, highly polished surface. Experience All-Clad renowned quality and craftsmanship with the All-Clad 8 in. Covered square baker.


Privacy by Design is a concept that businesses should adopt as they modernize their operations, especially in this data-driven world.
The GDPR is fast approaching and it is important to identify the weak links in your enterprise. Where can security be improved? Past experience has shown that third party suppliers are particularly susceptible to attacks.
DDoS attackers have gaming enterprises in their sights, but there are effective security strategies and solutions available to mitigate these attacks.
An enterprise guide on network segmentation; how it works to secure large enterprise networks, why it's needed, and examples of some of the most widely used network models for different industries.
Proper network segmentation is the most critical proactive step in protecting networks against targeted attacks. See why it's important for organizations to properly identify and categorize their own users and the networks they access.


text:
Hannibal, MO (63401)
Cloudy skies. Low 28F. Winds WNW at 10 to 15 mph..
Cloudy skies. Low 28F. Winds WNW at 10 to 15 mph.
Lame duck actions can haunt a nation
To The Courier-Post:
As the end of 2020 approaches, a year like no other, Americans are pondering Donald Trump's lame-duck period (between the election and successor's inauguration). March 4 was the date "for commencing proceedings," until the 20th Amendment (aka Lame Duck Amendment), ratified in 1935, shifted inaugurations to January.
History confirms lame ducks leave positive or negative imprints. Bound by few constraints, they construct their legacy by actions or inactions, such as executive orders and pardons.
The sympathetic portrayal of Herbert Hoover in "An Extraordinary Life in Extraordinary Times" (2017) offered this character assessment of Hoover who thwarted his successor's, Franklin Roosevelt's, tendency towards statism, promises of hope, and assistance for the needy: "He was determined to succeed by any means necessary, subordinating questions of right or wrong to the good of his career." Hoover's 146-day lame-duck period left scars — high unemployment and widespread poverty (e.g., Hoovervilles).
President Trump's legacy will be determined by the totality of his presidency. However, he will be remembered, primarily, for his handling of a cataclysmic event (COVID-19) and his lame-duck period. What will the actions, or inactions, of the 45th president be as a lame duck? We will see.
John C. Schafer
Lame Duck
Totality
David M. Walterscheid
Larry W. Tischer Sr.
Mary E. Abright
Arrest made in Hannibal Inn burglary
Robert L. "Bob" Moser
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redpajama_set_name: RedPajamaCommonCrawl


Nepal, a small and beautiful mountainous country in the lap of Himalayas.
Characterized by its extreme topography, a sharp rise in altitude, diverse biodiversity and agriculture-based-economy, Nepal is highly vulnerable to climate change induced hazards.
Due to climate change, our serene environment is at risk, our biodiversity is at jeopardy, our agricultural system is becoming vulnerable and overall; our livelihood has been challenged. With all the challenges looming around, there's much to wonder about; how can we mitigate the changing climate using limited available resources?
Developing countries like Nepal need locally adaptable strategies and resource efficient innovations to cope with climate change which are affordable, adaptable and accessible to the most targeted population. Having realized this need, YPARD Nepal attempted to bring youths together for a discussion, aiming to generate innovative ideas on agricultural practices for adapting with changing climate through the program YPARD Café on climate-smart agriculture at the premises of Agriculture and Forestry University.
On August, 26th, 2018, YPARD café was organized with twenty-five young agriculture students in the presence of YPARD Nepal representative, Mr. Abhishek Khadka, also the focal person of the program.
It started with an introduction to YPARD and about the concept of YPARD café. Which was then followed by the presentation on YPARD; its network, objectives, visions and opportunities within YPARD, presented by Mr. Bishal Mahatara (YPARD Nepal AFU coordinator). Some points were also added by Mr. Abhishek Khadka (YPARD Nepal representative) which justified the curiosities expressed by the participants. This presentation efficiently fulfilled the underlying aim of introducing YPARD Nepal among the students of the university through the program.
Moving on to the topic of discussion "climate-smart agriculture", Mr. Bikram Nepali (Local Representative, YPARD Nepal) illustrated the present scenario of climate change and some of the accepted ways of mitigation through few well-organized video clips, which also encouraged the participants to build up their ideas.
The idea pitching and discussion was further facilitated with the presentation from the focal person, Mr. Khadka. He highlighted that climate change in Nepal is more severe than the overall global condition and focused on how Good Agricultural Practice (GAP) could be one of the solutions.
He also emphasized some of the physiological effects being observed in the plants and impacts on livestock due to climate change. All in all, he appealed to adapt climate-smart agricultural practices in order to march towards sustainability.
The participants were randomly divided to form five groups and were given few minutes to discuss how we can form a "climate-smart village" in Nepalese context. All of the groups consecutively presented their ideas regarding the establishment of climate-smart village.
From the group discussions, the members identified the cooperative focused integrated farming system as one of the solutions to tackle climate-induced hazards. The inclusion of the components like rainwater harvest, plastic pond, solar-powered water pump, climate-smart varieties and the implementation of scientifically proven indigenous knowledge were also among the raised concerns. Similarly, recognition of the barriers, a realization of the needs for change and then acting accordingly were perceived as the key process for adapting climate-smart agriculture.
Replacement of chemical pesticides with bio-pesticides, an increment in the use of organic manure, vermiponics, and reduction in methane production through waste management, soil conservation, varietal development, agroforestry ideologies and grass-root level empowerment were also some of the common voices among the participants.
Climate change is happening and its impacts are imminent in agriculture sector, which is highly vulnerable of its hazards. With increasing evidence of climate change hazards in Nepalese agriculture system, the mitigating measures suggested by the young participants in this forum really need a strong implementation from concerned stakeholders.
Only then, we can achieve an agricultural system that is really farmers' friendly, climate adaptive and can lead us towards sustainable agriculture.
Lastly I would like to thank Anil Banstola (Programme Coordinator of YPARD Nepal) for guiding and Abhishek Khadka for his valuable presence.


text:
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You saw the beautiful vegetables we were given yesterday. Here's what I did with them this evening.
How beautiful! Loved the tomatoes in my little Gail Pittman dish. Cucumbers and onions in vinegar - good!
Little wax beans and shallots sauteed together.
To top it all off - country cornbread - a big hoecake hot from the oven with butter melting on it!
Glad you visited my blog; it's lovely to "meet" you!


Hong Kong: Microsoft's Internet search engine war with Google will revitalise the ailing media industry by helping it profit more from online news, the head of US news agency the Associated Press said Tuesday.
Microsoft's move in July to team up with Yahoo! and challenge Google's dominance of the online search market is a turning point in the traditional media's efforts to adapt to the Internet, AP president and CEO Tom Curley said.
Newspaper executives have complained that Google reaps the benefits from its popular news aggregation site Google News, while the industry gains little revenue from the service which readers access for free.
"We stand at an enviable moment where Microsoft and Google have decided to go to war," Curley said in an address to the Foreign Correspondents' Club in Hong Kong.
"And we who produce content can begin to figure out whether there's an opportunity for us to help that sharing in a way that reverses the outflow of money from media and takes it back."
Curley said that increased competition from the turf war, and Microsoft's plans to improve the reliability of news sources, would all benefit the media industry.
While he declined to criticise Google, the AP boss told reporters that Microsoft has proved keener to collaborate on how to improve the profitability of online news.
Curley said AP was in talks with the software giant about its new Internet search technology, which includes a feature allowing Web surfers to search using image galleries instead of text links.
He expected new strategies to improve readers' experience of online news to bear fruit in the next three to fifteen months.
"I think you'll see a lot more effort and a lot more announcements that are a lot more bullish from media companies than you have in the last decade," he said.
The AP is owned by 1,400 US newspapers but declining circulation, a drop in advertising revenue and Internet competition has decimated the industry with seven major companies in bankruptcy and 30,000 jobs lost since 2007.
Earlier this year the AP launched an industry initiative to protect news content from unauthorized use online, including a "news registry" to track the use of its stories on the Web.


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The Center's Research Services allow healthcare organizations, the design industry and product manufacturers access to vast research resources and a top-notch research team. Covering a wide spectrum of needs from complete, customized research studies to simpler research needs, or on-call expertise, consultation and advice on how to implement research into facility design, CHD's Research Advisory Services can be utilized for any healthcare facility planning, design and construction initiatives.
The Center's team of experienced researchers can provide accessible and affordable research expertise and support when you need it most. From literature scans to research guidance and custom tool development, our research team will help you add crediblity to any project.
Ellen Taylor, PhD, AIA, MBA, EDAC, Vice President for Research
Ellen Taylor brings more than 30 years of experience in architecture, research, and business to leading The Center's research team. She is a registered architect and member of the AIA who was recognized by Healthcare Design as the HCD10 Researcher in 2017, an award recognizing significant contributions to the industry. A nationally and internationally recognized writer and speaker, she has led numerous grant-funded research programs and published numerous peer-reviewed papers. Ellen has a bachelor's degree in architecture from Cornell University's College of Architecture, Art and Planning, Global Executive MBA degrees from Columbia University and London Business School, and a PhD in design, patient safety and human factors from Loughborough University in England. She serves as the Vice Chair for the FGI Health Guidelines Revisions Committee, on the Editorial Advisory Boards of the Health Environments Research & Design (HERD) Journal and American Journal of Infection Control (AJIC), and she was the 2022 President of the AIA Academy of Architecture for Health.
Melissa Piatkowski, MS, EDAC, Research Associate
For the past 20 years, Melissa has dedicated her career to exploring the connection between design and health. As a Research Associate with The Center for Health Design, she is a proud to work with her fellow "geeks" on developing tools and resources intended to support evidence-based design. She leads The Center's Just Health Design group, a task force committed to moving the healthcare design field forward towards a more just, diverse, equitable, and inclusive future.
Prior to joining The Center for Health Design, Melissa led Evidence-Based Design efforts at Davis Partnership Architects and Huelat Davis Healing Design. Melissa has a bachelor's degree in environmental design from the University of Colorado and a master's degree in environmental psychology from Cornell University.
Addie Abushousheh, PhD, Assoc. AIA, EDAC, Research Associate
Addie Abushousheh is a gerontologist, researcher, and consultant for organizational and environmental development in long-term care. She explores cultural and bio-psycho-social perspectives, organizational structures and processes, physical environments, workforce models, and regulatory and financial frameworks in relation to decision making, resource management, and quality improvement. With combined expertise in architecture, organizational development, aging and applied research, Addie is uniquely positioned to advance comprehensive and translational agendas related to quality assessment and performance improvement within the continuum of care. In addition to consultation and research, Addie publishes and presents regularly and serves in a review and advisory capacity to industry organizations.
Yolanda Keys, PhD, DHA, RN, NEA-BC, EDAC, Research Associate
Yolanda Keys is a registered nurse and brings over 25 years of nursing experience that has included roles as a clinician, leader and academician. With doctorates in healthcare administration and nursing, her research focuses on nurse leaders and healthy work environments – especially the built environment. She is an active member of the Nursing Institute for Health Design (NIHD), serving as president in 2017 and acting as an NIHD liaison for The Center's Knowledge Repository for many years. She brings a clinical perspective to the research team, as well as a deep understanding of the important contribution nurses can have during planning and design.
Alan J. Card, PhD, MPH, Research Associate
As a Research Associate with The Center for Health Design, Dr. Card has been invaluable in several special projects including the development of the CHD online Safety Risk Assessment and a systematic review investigating the impact of single-patient rooms. He also serves as an Assistant Professor at the University of California, San Diego School of Medicine, and is the former Editor of the Journal of Healthcare Risk Management. His research tackles questions related to quality, safety, risk, and well-being in healthcare, with a particular focus on improving how healthcare organizations improve. He holds a PhD from the University of Cambridge in England, an MPH from the University of South Florida, and professional certifications in healthcare quality and healthcare risk management


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Alaska Trout Unlimited
Advocacy Featured
United by Hope: Bristol Bay dialogues
A month from winter solstice, Dillingham, Alaska – where the Nushagak River dumps into Bristol Bay – was dark, quiet, and chilly last November. Snow and wind blew across the surrounding tundra not far from her windows when texts started flooding into Alannah Hurley's phone. The news: A major permit for the proposed Pebble mine…
Nelli Williams
Conservation Featured
Mat-Su Basin Salmon Habitat Partnership hosts tour of Little Susitna River
A headwater stream of the Little Susitna River. Photo by Ted Eischeid. On a rainy day in late August a group of diverse individuals gathered together on the banks of the Little Susitna River. Attendees included staff from state and federal wildlife agencies, tribal representatives, members of local government, political staffers from the governor and…
Marian Giannulis
Alaskan lake trout: All you need to know
Alaskan lake trout (Salvelinus namaycush) Species summary and status: Lake trout have a body shape similar to that of trout and salmon. They generally have small cream or yellow, irregular shaped spots on a silvery-to-dark background. Males and females are similar, with males having a slightly longer, more pointed snout. Lake trout can be distinguished from…
Trout Unlimited Staff
Mistakes you don't get to make twice
An Alaskan rainbow trout prepares to swim away after being caught on a tributary to the Susitna River in Alaska. Daniel A. Ritz photo. Western Native Trout Challenge: Alaskan rainbow trout Daniel Ritz is fishing across the Western United States this summer in an attempt to reach the Master Caster class of the Western Native Trout Challenge,…
Daniel A. Ritz
The Alaskan rainbow trout: All you need to know
Alaska's rainbow trout populations are still largely intact and robust, largely because of remote locations with limited accessibility, abundant and pristine habitat, and conservative management.
Alaskan Rainbow Trout (Oncorhynchus mykiss) Species Summary and Status: The rainbow trout native to Alaska is also known as coastal rainbow trout (Behnke 2002). There are two forms of coastal rainbow trout native to Alaska: the freshwater resident form and the searun form more commonly called steelhead. For the purposes here, only the resident form is…
Utah approves TU's first in-stream flow lease
Fly tying: Rusher's Steelhead Nymph
Trout Tips: Can you see your thumb?
Fly tying: Holy Grail Caddis Emerger


Levi Jacobs headed to World Junior Ultimate Championships! In Italy!
After attending tryouts in Seattle, Washington this March, Levi Jacobs was selected among the top 25 players in the USA to represent our country at the World Junior Ultimate Championships in Lecco, Italy this July. Below you can read about the awesome opportunity this is for him and Indiana Ultimate. All costs for his attendance fall on the players and their families, including travel to the mandatory training camp in Boston and the trip to Italy, so we are making a concerted effort to help him attend. (goal has been reached). Please feel free to read below to learn about this player.
Levi Jacobs is a third year player, senior, and captain on Holy Mackerel. From the beginning, Ultimate seemed to be so much more than a hobby for this young player, as it quickly developed into a life style and priority for him.
Competing fiercely, with a constantly dedicated work ethic, he has always worked to push himself to his limits. Rising quickly from his first year on Mackerel he now captains the A team. He also plays in unsanctioned college tournaments with his future university, plays with Indiana's elite club team Brickyard, and with the states youth YCC team INferno. He has even been selected for the 2014 AlleyCats' roster, all at the age of only 17.
Beyond the many teams he plays with, Levi captains summer league and winter league teams at all levels of play, showing a clear knack for leadership and a great interest in giving back to the ultimate community. After graduating at the end of this year, he already has plans to come back and coach with Holy Mackerel year round.
Beyond skill and leadership, he also pays active attention to spirit of the game, doing his best to be an ambassador for the sport with his attitude as well.
This past March, Levi was chosen to attend a tryout in Seattle, Washington against the best youth players in the country for a spot on the U19 division of Team USA. To our great joy, we were notified he had been selected as one of the most talented 25 players in the country and that he is to be sent to Italy with Team USA to compete at the World Junior Ultimate Championships against the best players from countries all over the world.
At WJUC twenty or more countries will compete with the best Ultimate athletes they have to offer in hopes of bringing home a gold medal, representing their country, and making international connections through the sport of Ultimate.
This is the first time any Indiana youth athlete has been selected for Team USA, of any division, and is an event attesting to his hard work and good attitude, as well as the general growth of Ultimate in the Indianapolis area.
We have reached our fundraising goal! We'd like to give an enormous thank you to the incredible Indiana ultimate community that showed so much support!


There should be no difference to learning from success and failure.
Kipling wrote, in "If" - "if you can meet with triumph and disaster, and treat those two impostors just the same..".
As knowledge managers we try to collect lessons from projects which have been triumphs and projects which have been disasters, but these are seldom treated the same way by the project teams.
OK, the statements above are generalisations and your particular company may differ, but there is a reality behind them representing two different biases; in the first case, the bias against "showing off to your peers"; in the second case, the bias against "appearing to have failed in front of your manager". These two biases affect the way in which teams approach the collection of lessons.
In reality, of course, we need to learn from both success and failure, particularly when these are unexpected. We need to seize on, and repeat, the breakthroughs, and map out and eliminate the pitfalls. As someone from NASA told me a couple of years ago - there are no successes and failures, there are just events. NASA learns from events. In other words, NASA treats those two impostors - triumph and disaster - just the same when it comes to learning.
So when you meet with triumph and disaster, success and failure, treat them just the same in terms of learning.


We stock and can supply a wide range of charts for barographs and similar recording instruments. Ungummed charts are for use with clocks with a chart clamp and gummed charts are for use with clocks without a chart clamp.
Charts for 7-day rotation are supplied in 100 chart pack. They are available for different barometric ranges and start dates. Our monthly rotation chart is supplied in a pack of 13 charts. All prices include VAT and postage and packing for delivery to addresses with UK postcodes (including the Channel Islands). For delivery to other addresses, please contact us for a quotation for delivery costs.
As well as charts for our own instruments, we can supply charts to for instruments manufactured by Negretti & Zambra, Short & Mason, Gradko, Sewills, Darton, Lizars, Metcheck, Rapport, Barigo, Fischer, Carl Zeiss, VFB, Chadburn, Lufft, Naudet, Maxant and the Met Office.
Full details of all our charts can be found in the following table. When you have found the reference number for the chart you want to order - in the red column - scroll down to the bottom of the page where all the products are listed and click on the relevant product. You can then complete your purchase.


1. Following Jesus requires giving Him our lives.
"Then Jesus said to His disciples, 'If anyone desires to come after Me, let him deny himself, and take up his cross, and follow Me. For whoever desires to save his life will lose it, but whoever loses his life for My sake will find it'" (Matthew 16:24-25).
2. We should study and follow His example (asking ourselves, what would Jesus do?).
"For to this you were called, because Christ also suffered for us, leaving us an example, that you should follow His steps: 'Who committed no sin, nor was deceit found in His mouth'" (1 Peter 2:21-22).
3. Following takes diligence, hope, faith and patience, but the promises are worth it!
"And we desire that each one of you show the same diligence to the full assurance of hope until the end, that you do not become sluggish, but imitate those who through faith and patience inherit the promises" (Hebrews 6:11-12).
For more on this subject, see "What Is a Disciple of Jesus Christ?"


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Tag: hawaii radio djs
HEAR KORN – NEW SEPTEMBER CLASSIC INTERVIEW PLAYER ISSUE
In late July I had the pleasure of speaking with Korn's front man and vocalist, Jonathan Davis. He was soft-spoken, very cool, easy to talk with, and I think you'll really dig this interview. What a laid back, very nice cat.
You may recall checking out some of this interview via HPR, and the extended interview with Jonathan on-demand in my DL New Releases Blog. What's cool about this month's Classic Interview Player is it more than doubles the length of what you've heard so far, with a whole bunch more conversation. Nearly twenty minutes now, it's a meaty feature that also includes lots of the Korn Live The Encounter videos from their historic crop-circle gig. It has a special live in-concert cover that's relevant considering some of our… shall we say… Floyd-based discussion, too : ). Also check out some cool pics, links, background and more…
Hope you dig it!
It's a brand new full-length interview you can hear on-demand all month with Korn's Jonathan Davis, in the Classic Interview Player's new September issue.
By Dave Lawrence September 1, 2010 September 1, 2010 173 WordsLeave a comment
NEW INTERVIEW PODCAST FOR DECEMBER WITH BRUCE SPRINGSTEEN E STREET BAND GUITARIST NILS LOFGREN
Just days after the arrival of Bruce Springsteen's new Working On A Dream song, which is streaming on-demand a couple posts below, we have a well-timed new interview podcast coming to the Dave Report for December: the return of Bruce Springsteen & The E Street Band guitarist Nils Lofgren. At NILSLOFGREN.COM, download his new nostalgic Yankee Stadium and other mp3s, get instructional lessons from a pro in one of the biggest bands on earth, go through a complete historical overview of his career in a multimedia history, and learn about the personal side of one of rock's most down-to-earth, easy going cats. I'm proud to welcome him back for a brand new interview. Nils, one of rock's true nice guys, has been a fixture with BRUCE SPRINGSTEEN since 1984 in a rock n roll journey that continues into the future. He performs with Bruce this February at the Superbowl, one of pop culture's largest audiences. The moment will be even sweeter for Nils as he celebrates his next album with The Boss, the new Bruce Springsteen album Working On A Dream out January 27; the first song from it stormed radio in the past several days. At this amazing crossroads in his career, certainly timing is everything: we speak with Nils just before the upcoming gig at the Superbowl, and new Bruce Springsteen release, with it's inspirational title Working On A Dream, premiering just as Bruce-favorite Barack Obama formally arrives. join me for a very special conversation you don't want to miss. Coming next week as a new December interview podcast feature in the DAVE REPORT.
By Dave Lawrence November 26, 2008 November 26, 2008 266 Words


A now quiet and peaceful area of rolling hills and farmland is what remains to preserve the memory of the fight that took place here during the American Civil War. Federal and Confederate troops battled to decide here, on October 8, 1862, who would control Kentucky. 7600 men fell that day to answer the question. Cannons such as these remain to remind the casual visitor of the blood, faith, sweat, and tears that were and are required to make America what she is today. This one was shot before sunset in silhouette against the sky and clouds.
Photo © copyright by Jeremy Brasher.


From the most successful wrestling game series of all-time comes the ultimate achievement in sports entertainment - WWE SmackDown! vs RAW 2006. Enter the ring for the fight of your life against top WWE Superstars and, if you're good enough, the championship. Lace up your boots for the definitive wrestling experience that is WWE SmackDown! vs RAW 2006.


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Home > Tech
Amazon Echo Show 10 review: 5 things to know
The new Echo Show is a smart display that works for you.
By Marc Chacksfield
The Amazon Echo Show 10 is Amazon's smartest smart display yet. It combines the audio power of its wide-ranging Echo line-up, with a 10-inch screen that follows you around the room, meaning that you no longer have to stay in one place while having a video conversation.
Having the moving screen means it has many guises: a security system, a kitchen companion, entertainment device and video conference hub.
We've been playing with the Amazon Echo Show 10 for a little while now - here are 5 things you need to know.
1. Make sure you have space for setup
The big Amazon Echo Show 10 USP is its motorised screen, which rotates and follows you around the room. Because of this, a chunk of the setup process is making sure that the device has enough room to swivel around. If there isn't enough room, then you will soon know about it as a warning appears. The calibration process for this is fun, though, and it will ask where you have put the thing, whether it's in the corner of a room on a breakfast bar etc.
All of this will determine how much tracking it needs to do. The rest of the setup is the same as any other Echo device, linking it to your Alexa account so it is compatible with any other smart things you might have in your house.
2. Design-wise, it's an Amazon mash-up
Amazon hasn't strayed far from its current device line-up when making the new Amazon Echo Show 10. It looks a bit like an Amazon Fire tablet connected to an Amazon Echo, although the design is a lot better than that sounds. As you can tell from the name, the screen is 10.1 inches, while the cylinder base is a decent size at 6.7 inches. Other design flourishes include the sizeable camera lens on the front and some physical buttons on the top of the device, as well as slider to cover the camera for privacy.
3. The screen is key
The 10.1-inch screen has a chunky bezel but it's brilliantly clear at 1280 x 800 pixels (incidentally, the camera is 13MP so you will be shown off in good quality to whoever you are speaking to). It can move 45 degrees on its axis, so you can have it flush to its base or raised a bit. You can't shift the screen to horizontal to vertical positions, though, which would have been a nice bonus. But the main thing here is that the device follows you, swivelling on the motorised base - it's silent when it moves and is a touch disconcerting at first but you soon get used to it. The moving screen makes the device a lot more desirable to use.
4. It likes to move it, move it
Depending on where you have situated the Amazon Echo Show 10, the device can rotate some 175 degrees in either direction. So even if you are rushing around getting all the ingredients you need for your dinner, the screen will be where you want it. Like the jokers we are, we tried to catch the motion sensor out a few times but it really does work and works well.
Amazon isn't the first to offer this type of feature (Facebook Portal also uses a similar technique, albeit digitally) but it is the slickest version of it we have seen. The only time it did stutter was when we were close to the screen and especially the lens - moving your hand near it, which you would do as it is a touchscreen, does confuse it and it may try and turn away from you like it's in a sulk but this didn't happen often.
5. It's a smarter smart hub
We found ourselves using the Amazon Echo Show 10 for myriad things, once we got used to it. The 10-inch screen means it's decent for watching Prime Movies and Netflix (no YouTube, unfortunately) and it worked well with our Ring devices, so you can see clearly who is at your door and ignore them. It's compatible with Zigbee devices, which means you don't need a separate hub for those. The audio on this thing was far better than we thought it would be, too. Load up Spotify or Amazon Music and there's a decent amount of bass thanks to the 5.3-inch woofer.
Final Verdict: Best in Show
The Amazon Echo Show 10 is a fantastic smart hub for the home. The motion tracking works well, is silent and really does make a difference if you are moving around a room a lot. While we tried it out in a few places, because of the tracking it worked best in the kitchen.
It does come at a price, though, at £239.99/$249.99 - which is double what the Echo Show 8 costs. It's a far superior bit of kit tech wise, though, and the rotating screen is a real game changer.
You can pre-order the Amazon Echo Show 10 now.
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Tom Martinsen (4. srpna 1943 – 31. března 2007) byl norský fotograf.

Životopis
Narodil se v Tønsbergu.

V letech 1968–1971 studoval fotografii a dokumentární film u Christera Strömholma ve Stockholmu. Sám popsal setkání se školou a Strömholmem jako "dostat pánví do hlavy". Roky ve Fotoskolanu byly pro Martinsenův pohled na fotografie rozhodující. Od roku 1973 byl jmenován zpravodajským fotografem pro noviny Dagbladet. V roce 1972 získal cenu za Fotografii roku. Byl spoluzakladatelem galerie Fotogalleriet v Oslu v roce 1977.

Martinsenovy fotografie byly zakoupeny Norskou kulturní radou, Norským muzeem fotografie – Preus museum v Hortenu, Lillehammer Art Museum a Moderna Museet ve Stockholmu.

Nová generace norských fotožurnalistů
Patřila k ní generace fotografů Toma Martinsena a s jeho fotografickým vzděláním představoval generační změnu v norské novinářské fotografii. Nejen proto, že měl fotografické vzdělání (fotožurnalisté do té doby málokdy měli významné odborné vzdělání), ale také díky svému přístupu k fotografii. Jednou řekl: "ohnisková vzdálenost je věcí morálky. Teleobjektiv je nemorální věc, pokud jde o lidi. Se širokým objektivem se musíte ukázat. Postavíte se na pozici, která je otevřená a čestná."

Některé z nejslavnějších fotografií v norských médiích z posledních let pocházejí z ruky a fotoaparátu Toma Martinsena. Příkladem tohoto jsou jeho známé fotografie: osvícený Bob Dylan (Scandinavium, Göteborg) fotografovaný v zákulisí nebo barevný portrét spisovatele Daga Solstada na noční zasněžené ulici.

Martinsen byl také vášnivým fotografem přírody a byl také známý svými přírodovědnými studiemi v černobílém provedení, zejména z Tjøme Vestfold a krajiny USA.

Martinsen mnoho let editoval pravidelný sloupec Moment v sobotní příloze Magasinet novin Dagbladet. Každý týden popisoval klíčová díla z historie fotografie. Název sloupce vzal z výrazu Henri Cartier-Bressona "rozhodující okamžik", který Bresson definoval jako "současné zachycení významného okamžiku ve zlomku vteřiny, jakož i přesné uspořádání prvků, které dají události správný výraz."

Výstavy
 Bilder fra Verdens Ende, Fotogalleriet, Oslo (1979)
 Separatutstilling, Preus Fotomuseum, Horten
 Min egen road movie, Filmfestivalen, Haugesund (1994)
 Vest – en veifortelling, Fotogalleriet, Oslo (1994)
 Lillehammer kunstmuseum, Lillehammer (2003) (med Rolf M. Aagard), samostatná výstava
 Kunstforeningen Verdens Ende, Tjøme (2005), samostatná výstava
 Nord for havets ende, Preus Fotomuseum, Horten (2006)

Knihy
Mezi jeho nejznámější publikace patří kniha 118 øyeblikk (118 momentů) z roku 2003.

 118 Øyeblikk. Norske reportasjefotografier utvalgt og presentert av Tom Martinsen Dinamo Forlag (2003) ISBN 82-8071-052-3
 Tom Martinsen. Rolf M. Aagard Labyrinth Press (2003)

Odkazy

Reference

Související články
 Fotografie v Norsku
 Seznam norských fotografů

Externí odkazy
 Tom Martinsen na fotografi.no
 Tom Martinsen v muzeu Preus

Norští fotografové
Narození v Tønsbergu
Narození v roce 1943
Narození 4. srpna
Úmrtí v roce 2007
Úmrtí 31. března
Muži

redpajama_set_name: RedPajamaWikipedia


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Q: how can docker containers have a different flavor than the host My understanding of linux containers is that each container uses the same host kernel, and any installations on the container are just an isolated filesystem layer over the host.
I was going through coreos getting started guide. In that it shows how an ubuntu container can be started on a host containing coreos.
How is this possible ? How can the host and the container have different flavours ?
Thanks,
Murtaza

A: The kernel and the userland are two different things. The kernel will be almost the same across all distributions. Of course, each distributions will have slightly different settings. For instance, one distribution might decide to exclude some drivers because they aren't completely free. Another might decide to include extra features (like Debian and Ubuntu have AUFS support, which is usually not found in other distro's kernels). Red Hat has their own "battle tested" kernel, which is essentially 2.6.32 with tons of stability fixes (it sounds old, but it's insanely reliable).
99% of the time, you can boot distro X with the kernel of distro Y without a problem. And that's why it's OK to run a Ubuntu container on a CoreOS host: the container is exclusively userland. It's just a bunch of processes running on the machine, and as long as the kernel supports namespaces and control groups (the low level features needed to run Linux Containers), it doesn't matter where the kernel comes from.

redpajama_set_name: RedPajamaStackExchange


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Produced by Maureen Holloway |Directed by Paula Worley
In 2016 the world is commemorating 400 years since the death of William Shakespeare. April 23, 2016, marks the 400th anniversary of William Shakespeare's death at age 52. His plays and sonnets have been performed in nearly every major language on every continent. To mark the event, festivals, performances, and exhibitions will take place all around the world by major theater companies and small community theaters. Some will be produced in the traditional Elizabethan style, while others will present more modern-day interpretations of his work. All to celebrate the legacy of arguably the greatest playwright in the English language.
Northumberland Players are pleased to announce that their 2016 production of a Shakespearean play will be Twelfth Night by William Shakespeare. Twelfth Night is Shakespeare's most hilarious romantic comedy:
The shipwrecked Viola is determined to survive when she finds herself unexpectedly washed up on the shores of Illyria, believing her family to be lost at sea. With outrageous characters, mistaken identity and disguise, intertwined subplots of seduction and revenge, and the music and songs of Feste the Clown.
The director, Paula Worley, directed Macbeth last year and A Midsummer's Night Dream in 2014. Paula has extensive experience as a Shakespearean director and has directed for her own company, Shakespeare Street Theatre, for many years before joining Northumberland Players.
Northumberland Players strives to include youth in all aspects of theare production. There are several younger – but seasoned – actors in Twelfth Night: Aurielle Diotte, Ireland Farrell, Shane McGovan, and Oliver Graf making his acting debut after working on the technical side of several productions.
Twelfth Night will be performed with Elizabethan costumes, thanks to designer Ann Hancock and the resources of the Costume House, and staging on a traditional thrust stage: enjoy an authentic slice of Shakespeare close to home!
Suitable for 14+.
The Firehall Theatre, Cobourg, November 4 to 12, 2016. Also student matinées.
The simple thrust stage set is inspired by the original Globe Theatre:
Read Cecelia Naismith's preview in Northumberland Today at Northumberland Players to present Shakespeare at Firehall Theatre
Read Selena Forsyth's review in Northumberland Today at Twelfth Night another strong production by Players
For details about this production, see Twelfth Night Program


This Lowden S-35 is a lively concert-bodied acoustic that packs a serious punch despite its small size. It is quite touch-sensitive, and you can coax a ridiculously wide variety of timbres out of its alpine spruce top simply by altering your technique. Because it presents the player with such a smorgasbord of tones, it provides a supremely expressive playing experience, so let's take a closer look at the sounds it has on tap!
The spectacular rosewood back and sides help give it uncommonly deep, rich bass response—in fact, Lowden may have violated some sort of law to imbue such a small guitar with such powerful resonance, because it is borderline unnatural! Facetiousness aside, the low-end of this guitar is quite special. It's deep and powerful, but quite clear. Imagine a classically trained, operatically-inclined baritone singer with a mellifluous, warm vocal tone, and you'll get an excellent idea of how clear yet rich the rock-solid low end of this lovely Lowden sounds.
Meanwhile, the Alpine Spruce top helps this guitar produce a strong fundamental, and while it has plenty of headroom, it also captures an uncommon amount of subtlety and nuance at low volumes. It allows the player's brasher, louder moments to come through with force and power while also faithfully reproducing every detail of the player's input during more introspective, mellow moments.
The midrange is also quite inspiring! It's quite smooth, warm, and woody when you ease off with your right hand, but when you pick hard it "hulks out" and all sorts of delightful even-order harmonics start to pop out of the top.
The top end showcases a similar level of touch-sensitivity. The trebles have a glassy, golden quality when you pick softly, and they shimmer and jangle more and more as you play forcefully.
In an odd way, the way this guitar responds when the top is maxed-out reminds me of an old Vox Amplifier (though, frankly, the Lowden has deeper bass response, so its not an apples-to-apples comparison). Every acoustic guitar can only get louder to a point, and once they reach that level they become more and more compressed—just like an electric amp when you crank the master volume! Harmonics start to pop out all over the place, and everything sounds fuller and richer. The sweet, bell-like overtones that bloom out of this S-35 remind me of that classic Vox jangle, but acoustic-ified!
Speaking of headroom, this Alpine spruce top starts to compress in just the right spot. It's easy for fingerpickers and flatpickers alike to coax this beautiful note-bloom out of the wood, but it still has enough headroom to sound open when you play at a solid mezzo forte.
In other words, this Lowden S-35 doesn't just hit the sweet spot: it lives there! Anyone seeking a concert-bodied acoustic with a tremendously wide range of dynamics and incredible touch-sensitivity will love this serial, and we are proud to offer such an inspiring guitar to our exceptional customers.


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Erik Skjoldbjærg (born December 14, 1964) is a Norwegian director and writer best known for co-writing and directing the film Insomnia and the long awaited Narvik. His film Pioneer was selected to be screened in the Special Presentation section at the 2013 Toronto International Film Festival.

Filmography

As director
 Vinterveien (Near Winter, short film, 1993, also wrote)
 Close to Home (short film, 1994, also wrote)
 Spor (1996, also wrote)
 Insomnia (1997, also wrote)
 Prozac Nation (2001)
 Skolen (TV series, unknown episodes, 2004)
 En folkefiende (An Enemy of the People, 2005, also wrote)
 Størst av alt (TV series, 3 episodes, 2006)
 Nokas (2010)
 Pionér (Pioneer, 2013, also wrote)
 Pyromaniac (2016)
 Forsvinningen - Lørenskog 31. oktober 2018 (The Lørenskog Disappearance, miniseries, 3 episodes, 2022)
 Narvik (2022)

As writer
 Insomnia (1997 screenplay, 2002)
 Occupied (2015–20)

References

External links

Living people
1964 births
Norwegian film directors
People from Tromsø


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Anti-Angiogenic miR-222, miR-195, and miR-21a Plasma Levels in T1DM Are Improved by Metformin Therapy, Thus Elucidating Its Cardioprotective Effect: The MERIT Study
Lookup NU author(s): Dr Fahad Ahmed, Dr Sherin Bakhashab, INDA Bastaman, Dr Rachel Crossland, Dr Michael Glanville, Dr Jolanta Weaver
Published version [.pdf]
This work is licensed under a Creative Commons Attribution 4.0 International License (CC BY 4.0).
Type 1 diabetes (T1DM) is associated with increased cardiovascular disease (CVD) and reduced life expectancy. We thus hypothesized that anti-angiogenic miRs are increased in T1DM, and the cardioprotective effect of metformin is mediated via reducing those miRs. In an open label, case-controlled study, 23 T1DM patients without CVD were treated with metformin for eight weeks (TG), matched with nine T1DM patients on standard treatment (SG) and 23 controls (CG). Plasma miR-222, miR-195, miR-21a and miR-126 were assayed by real-time RT-qPCR. The results were correlated with: endothelial function (RHI), circulating endothelial progenitor cells (cEPCs) (vascular repair marker, CD45dimCD34+VEGFR2+ cells) and circulating endothelial cells (cECs) (vascular injury marker, CD45dimCD34+CD133-CD144+ cells). miR-222, miR-195 and miR-21a were higher in T1DM than CG; p = 0.009, p < 0.0001, p = 0.0001, respectively. There was an inverse correlation between logmiR-222 and logRHI (p < 0.05) and a direct correlation between logmiR-222 and logCD34+ (p < 0.05) in TG. Metformin reduced miR-222, miR-195 and miR-21a levels in TG; p = 0.007, p = 0.002 p = 0.0012, respectively. miRs remained unchanged in SG. miR-126 was similar in all groups. There was a positive association between changes in logmiR-222 and logcECs after metformin in TG (p < 0.05). Anti-angiogenic miRs are increased in T1DM. Metformin has cardioprotective effects through downregulating miR-222, miR-195 and miR-21a, beyond improving glycemic control.
Publication metadata
Author(s): Ahmed FW, Bakhashab S, Bastaman IT, Crossland RE, Glanville M, Weaver JU
Journal: International Journal of Molecular Sciences
Online publication date: 19/10/2018
Date deposited: 19/10/2018
ISSN (electronic): 1422-0067
URL: https://doi.org/10.3390/ijms19103242
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Private Hire Driver dies from horrific crash injuries two weeks after his passenger was killed
The driver of a private hire vehicle which was involved in a crash which claimed the life of a passenger has died, police confirmed on Thursday 14. Passenger Michelle Jennings, who was 35-years-old, was killed in the crash while travelling in the Ford Mondeo which was involved in a collision with a BMW during the early morning hours of Wednesday, February 27.
The police have now confirmed the tragic news that the driver, 51-year-old Dave Sherwin, has also died from his injuries. He passed away in hospital on Wednesday, March 13. Police made a fresh plea for witnesses to the crash to come forward.
A police spokesman told the Liverpool Echo: "The 51-year-old male taxi driver, died on Wednesday in hospital." The BMW driver - a 26 year-old man - has been arrested on suspicion of causing death by dangerous driving. Michelle Jennings has been described as 'the most lovely person ever' by her devastated family.
She leaves behind a devastated family , including husband Ged and children, five year-old daughter Sophia and son Harry, who is due to turn seven tomorrow. Paying tribute to his 'beautiful' wife in an emotional post on Facebook, Ged said: "She was the most lovely person ever. Her kids were her world. Family was her everything. I am beyond distraught. I didn't deserve her."
Officers would continue to urge anyone with information, who witnessed this collision or who has dash-cam footage, to contact @MerPolCC, call 0151 777 5747 or 101, quoting reference 19100077634 or @CrimestoppersUK on 0800 555 111.
Image credit: Police signage;
Source: Geograph
Author: Lewis Clarke


PRODUCT DESCRIPTION: Clipper ship Aluminum Fibre Coating meets ASTM-D-2824-85 Type III specifications and is 100% ASBESTOS-FREE. This material is an asphalt cutback blended with fibres and aluminum paste. BASIC USES: Clipper ship Aluminum Fibre Coating is a protective coating used to produce an ultra-bright aluminum reflective for all types of surfaces. LIMITATIONS: DO NOT HEAT container. DO NOT thin or exceed 900 rpm when mixing or applying or use a roller for application. DO NOT apply over soft asphalt or coal tar surfaces or areas that hold ponded water. DO NOT back-brush or disturb product after leafing process has begun or surface may brown. APPLICATION: Clipper ship Aluminum Fibre Coating must be applied to a surface that is dry and clean from all foreign matter. This material should be applied when the temperature is 50° F and rising. This material can be applied by brush or spray equipment (recommend airless or piston pump). The coverage rate should be 50-75 square feet per gallon. STORAGE: Clipper ship Aluminum Fibre Coating can be used year round and the only protection would be from weathering on the container. COMPOSITION: Asphalt Mineral Spirits Aluminum Paste Desiccant Fibre Diatomite CAS 8052-42-4 CAS 64741-41-9 CAS 7429-90-5 CAS 63231-67-4 CAS 9004-34-6 CAS 61790-53-2 This information is to assist customers in determining if this product is suitable for the proposed application, and to satisfy themselves as to suitability of the contents. Nothing herein shall constitute a warranty, expressed or implied, including any warranty of merchantability or fitness, nor is protection from law or patent implied.


text:
//
//  QMUserProfileProtocol.h
//  QMServices
//
//  Created by Andrey Ivanov on 28.04.15.
//  Copyright (c) 2015 Quickblox Team. All rights reserved.
//

#import <Foundation/Foundation.h>
#import <Quickblox/Quickblox.h>

/**
 *  Main QMServices protocol.
 */

NS_ASSUME_NONNULL_BEGIN

@protocol QMServiceManagerProtocol <NSObject>
@required

/**
 *  Get user from current session
 *
 *  @return QBUUser instance
 */
- (nullable QBUUser *)currentUser;

/**
 *  Check is current session is authorized
 *
 *  @return YES if authorized
 */
- (BOOL)isAuthorized;

/**
 *  This method called when some QBReqest falling. Use this method for handling errors, like show alert with error.
 *
 *  @param QBResponse instance. See response.error for falling inforamtion.
 */
- (void)handleErrorResponse:(QBResponse *)response;

@optional

- (NSString *)appGroupIdentifier;

@end

NS_ASSUME_NONNULL_END

redpajama_set_name: RedPajamaGithub