The fascinating front page story in Wednesday's Star Tribune brought forth an admission by Rep. Matt Entenza that he hired a private firm to investigate the visitor's log, contractual relations, and purchasing patterns of the Attorney General's office under Mike Hatch. Given that both are from the same party, and that Entenza is now running to replace Hatch while Hatch moves on to run against Governor Tim Pawlenty, Entenza's motivation for the surreptitious investigation seems on the surface to be a real head-scratcher.
Entenza's explanation--that he wanted to "get a better understanding of how some aspects of the office worked"--was a real howler. Instead of spending hundreds, possibly thousands, of dollars to get a third party to file a Data Practices request, Entenza could have gained first-hand "understanding" of the job simply by asking Hatch directly. When it came to conveying an impression of full disclosure about what he was up to, Entenza may as well have told the Strib that the dog ate his homework.
According to minnesotademocratsexposed (or MDE), the website that back in August of last year first published rumors of Entenza investigating Hatch, Entenza's motivation was to get dirt on Hatch so that he would step aside and let Entenza run for Governor. (Yesterday, the site also pointed out that Entenza previously worked in the AG's office, making his explanation to the Strib all the more specious.) Or, as a Wednesday afternoon story in the online version of the St. Paul Pioneer Press infers, citing another aspect of the original MDE post, it could have been to strong-arm Hatch into anointing Entenza as his successor rather than Minnesota Solicitor General and close Hatch associate Lori Swanson.
But to my knowledge, nobody has yet speculated that what Entenza was really after was a way to get Hatch to stop involving himself in the operation of Medica; specifically pushing to get Medica to sever its management contract with United Health (UHC), the corporation that has made Entenza's wife fabulously wealthy; wealth that in turn has enabled Entenza to exercise enormous political leverage via campaign contributions.
For a more thorough explanation of how Entenza's connection to United Health has benefited him politically, antagonized his relationship with Hatch, and created significant potential conflicts of interst should he be elected AG, see the story I wrote for City Pages back in January. But here's a thumbnail chronology.
In 2001, Attorney General Hatch conducted an audit of Allina/Medica that uncovered exorbitant management contracts that the company had been paying to United, including processing fees that were at least 26 percent higher than the next highest industry standard on a per-claim basis, helping to produce a whopping 35 percent profit margin for United. Hatch's investigation also uncovered notes from Medica's consulting firm from the 1990s saying that, in spite of these high payments, United's "substandard" service cost Medica about $10 million in losses. These revelations, along with juicy details about corporate perqs such as golf club memberships and lavish trips, enabled Hatch to gain the authority to break up Allina and Medica into two separate companies and to hand-pick Medica's board of directors.
Two years later, Medica's board of directors asked the court to remove Hatch's oversight function. Hatch fought the request, claiming that the board was allowing the company to slip back into some old bad habits, and contending that the board needed to recruit more of its membership from the premium-paying members of the nonprofit HMO. Hatch doggedly pursued his claim until a judge resoundingly ruled against him and legally freed the operation of Medica out of his control in August 2005. It was right around the time of the judge's verdict that the MDE website first leaked rumors of Entenza investigating Hatch.
We now know that Entenza hired the investigators in February 2004, almost exactly halfway between the time Medica asked for its independence in early 2003 and the judge granting it in August 2005. The nature of Entenza's search--delving into purchases of artwork and furniture for Hatch's office, and how much Hatch was paying outside contractors--seems very consonant with the kind of investigation Hatch conducted of Medica.
"I have said, and I still believe, that Medica is a front for UHG"--United Health Group--Hatch told me last December. "United literally runs it--they are the guts of the company." The guts of a company that incurred over $45 million more in administrative expenses than any other HMO in the state, according to the last report from the Minnesota Department of Health. Meanwhile, Entenza's wife, Lois Quam, is a United executive who has exercised more than $4 million worth of United stock options over the past three years, and, like her boss, William McGuire, has many millions more in stock and other compensation stemming from her employment at United.
I have no proof that Matt Entenza hired a private firm to dig up dirt on Mike Hatch so that Hatch would back off on his oversight of Medica, enabling Medica to continue a business relationship that has been very lucrative for the corporation that employs Entenza's wife. But it sounds a lot more plausible than the explanation Entenza gave the Star Tribune.


text:
\section{Introduction}

The probably presence of an unknown form of energy in the universe, called dark energy, and confirmed by a large number of observations, starting by the data of Supernovae IA in 1998 \cite{riess}, have leaded to explore the possible theoretical origin for this fluid. Since it is the direct responsible of the present accelerating expansion of the universe, a negative pressure is required which leads to a negative equation of state parameter. The most popular candidate, the cosmological constant, which posses a constant equation of state (EoS), $p_{\Lambda}=-\rho_{\Lambda}$, can explain quite well the cosmological evolution. However,  the open possibility that the EoS is not completely constant but evolutes dynamically (even crossing the phantom barrier more), and the quite large difference between the observed dark energy density and the vacuum energy density predicted by quantum field theories, have leaded to explore other possibilities, as the existence of scalar fields, vector fields or modifications of General Relativity (GR), among others (for a review on dark energy candidates, see \cite{copeland}).
\par
In the context of modified gravities, a wide range of possibilities have been explored, being $f(R)$ gravity probably the most popular one due to its simplicity since it generalizes the Hilbert-Einstein action to a more complex function of the Ricci scalar (for a review on $f(R)$ gravity, see \cite{reviews,Bamba:2012cp}). Nevertheless, other kind of theories have been suggested, where other curvature invariants are included as the Gauss-Bonnet gravity. In this paper, we study the so-called $f(T)$ gravity, which in analogy to f(R) gravity, consists in a generalization of the action of Teleparallel gravity, a theory that assumes Weitzenbock connection instead of the Levi-Civita connection, which yields to a null curvature but a non-vanishing torsion (for a review see \cite{pereira1}). In this gravitational theory, the main field is represented by the so-called tetrads instead of the metric as in GR. This kind of theories has become very popular recently as can also explain the accelerated expansion of the universe with no need of dark energy, and even the inflationary epoch (see \cite{ferraro1}-\cite{ratbay}). Then, a wide number of aspects have been studied in the context of $f(T)$ gravity, as  its local Lorentz invariance \cite{barrow}, static solutions \cite{daouda1}, non-diagonal tetrads \cite{daouda3}, or the presence of wormholes \cite{boehmer}, as well as other aspects \cite{x,cemsinan}. Also a large effort has been done to study cosmological solutions for this class of theories, as well as possible cosmological predictions (see Refs.~\cite{houndjo}-\cite{li}).
\par
At the present work, we are interested to study some particular cosmological solutions in $f(T)$ gravity, where the appropriate action is reconstructed for each case. Specifically, the Bianchi type-I, Kantowski-Sachs (KS) and Bianchi type-III models are considered, and particularly some important solutions, such as power law and de Sitter (dS) expansion, or more complex ones as exponential functions for the scale factor in each direction of the space. Since power law and dS solutions can provide a good description for some specific phases of the universe evolution, their reconstruction in $f(T)$ gravity becomes a crucial point in order to consider this class of theories as serious candidates for explaining the whole cosmological history. In addition, here we assume more general cosmological metrics than Friedmann-Lema\^itre-Robertson-Walker (FLRW) metrics,  in particular anisotropic universes described by the Bianchi type-I, Kantowski-Sachs (KS) and Bianchi type-III metrics, in order to provide the most general description of the cosmological evolution in the context of $f(T)$ gravity.  Moreover, exponential solutions are also considered, this kind of expansions has become very popular recently as they may conduct the universe to a non-singular state, where some bounded systems may be broken. Such state suggested in Ref.~\cite{LittleRip}, and called {\it Little Rip},  has already been studied in $f(R)$ gravity (see Ref.~\cite{Nojiri:2011kd}), as well as in $f(T)$ theories \cite{bambamyr}. Even more,  the possible occurrence of a   {\it Little Rip} has been also explored in the context of the so-called viable modified gravities (see Ref.~\cite{SaezGomez:2012ek}). Note that anisotropic
cosmological metrics have been already studied in the context of GR with the presence of isotropic and anisotropic fluids, as well as the stability of the solutions \cite{barrow3,stability}.
\par
Furthermore, the use of an auxiliary scalar field, in analogy to the equivalence of Brans-Dicke theories for $f(R)$ gravity (see for instance Ref.~\cite{STFR}), is also implemented, from which may result a useful tool to reconstruct the appropriate action as well as for studying the properties of $f(T)$ gravity.
\par
The main motivations of assuming  the assumption of a model with anisotropic geometry are based on several physical aspects as: the famous problem of the CMB quadrupole can be solved by considering a universe with planar symmetry \cite{campanelli1} where eccentricity in decoupling, generated by a uniform cosmic magnetic field whose current strength,  $ B(t_0) \sim 10^{-9}$ Gauss, should be close to $e_{dec}\sim 10^{-2}$; the Bianchi type models in Loop Quantum Cosmology \cite{lqc}, $^4He$ abundance \cite{campanelli2}, cosmic parallax \cite{campanelli3,fontanini}, small anisotropic pressures \cite{barrow2}, cosmological solutions of the low energy string effective action \cite{massimo}, anisotropic inflationary universe \cite{inflation} and some other \cite{x-1}. In the $f(R)$ theory, we already have some good results \cite{can,sharif2}, therefore, we propose to establish the equations here and get the first results in $f(T)$ gravity, for the Bianchi type-I, type-III and KS models.
\par
Then, the paper is organized as follows: in section \ref{sec2}, the basic concepts of $f(T)$ gravity are introduced. In section \ref{BK} , the equations for general  Bianchi type-I, type-III and Kantowski-Sachs (KS) models are deduced in a particular coordinate system and diagonal tetrads. Section \ref{sec2a} deals with the reconstruction of the $f(T)$ action for some relevant solutions, and where several techniques are considered, including a kind of scalar-tensor theory for torsion gravity. Finally, section \ref{conclusions} is devoted to the conclusions and discussions on the results found in the paper.
\section{\large Preliminary definitions and equations of motion}\label{sec2}

As previously mentioned, the $f(T)$ theory of gravity is defined in the Weitzenbock's space time in which the line element is described by
\begin{equation}\label{el}
dS^{2}=g_{\mu\nu}dx^{\mu}dx^{\nu}\; ,
\end{equation}
where $g_{\mu\nu}$ are the components of the metric which is symmetric and possesses $10$ degrees of freedom. One can describe the theory in the spacetime or in the tangent space, which allows us to rewrite the line element (\ref{el}) as follows
\begin{eqnarray}
dS^{2} &=&g_{\mu\nu}dx^{\mu}dx^{\nu}=\eta_{ij}\theta^{i}\theta^{j}\label{1}\; ,\\
dx^{\mu}& =&e_{i}^{\;\;\mu}\theta^{i}\; , \; \theta^{i}=e^{i}_{\;\;\mu}dx^{\mu}\label{2}\; ,
\end{eqnarray}
where $\eta_{ij}=diag[1,-1,-1,-1]$ and $e_{i}^{\;\;\mu}e^{i}_{\;\;\nu}=\delta^{\mu}_{\nu}$ or  $e_{i}^{\;\;\mu}e^{j}_{\;\;\mu}=\delta^{j}_{i}$. The square root of the metric determinant is given by  $\sqrt{-g}=\det{\left[e^{i}_{\;\;\mu}\right]}=e$ and the matrix $e^{a}_{\;\;\mu}$ are called tetrads and represent the dynamic fields of the theory.
\par
By using theses fields, one can define the Weitzenbock's connection as
\begin{eqnarray}
\Gamma^{\alpha}_{\mu\nu}=e_{i}^{\;\;\alpha}\partial_{\nu}e^{i}_{\;\;\mu}=-e^{i}_{\;\;\mu}\partial_{\nu}e_{i}^{\;\;\alpha}\label{co}\; .
\end{eqnarray}
The main geometrical objects of the spacetime are constructed from this connection. The components of the tensor torsion are defined by the antisymmetric part of this connection
\begin{eqnarray}
T^{\alpha}_{\;\;\mu\nu}&=&\Gamma^{\alpha}_{\nu\mu}-\Gamma^{\alpha}_{\mu\nu}=e_{i}^{\;\;\alpha}\left(\partial_{\mu} e^{i}_{\;\;\nu}-\partial_{\nu} e^{i}_{\;\;\mu}\right)\label{tor}\;.
\end{eqnarray}
The components of the contorsion are defined as
\begin{eqnarray}
K^{\mu\nu}_{\;\;\;\;\alpha}&=&-\frac{1}{2}\left(T^{\mu\nu}_{\;\;\;\;\alpha}-T^{\nu\mu}_{\;\;\;\;\alpha}-T_{\alpha}^{\;\;\mu\nu}\right)\label{contor}\; .
\end{eqnarray}
In order to make more clear the definition of the scalar equivalent to the curvature scalar of RG, we first define a new tensor $S_{\alpha}^{\;\;\mu\nu}$, constructed from the components of the tensors torsion and contorsion as
\begin{eqnarray}
S_{\alpha}^{\;\;\mu\nu}&=&\frac{1}{2}\left( K_{\;\;\;\;\alpha}^{\mu\nu}+\delta^{\mu}_{\alpha}T^{\beta\nu}_{\;\;\;\;\beta}-\delta^{\nu}_{\alpha}T^{\beta\mu}_{\;\;\;\;\beta}\right)\label{s}\;.
\end{eqnarray}
We can now define the torsion scalar by the following contraction
\begin{eqnarray}
T=T^{\alpha}_{\;\;\mu\nu}S^{\;\;\mu\nu}_{\alpha}\label{te}\; .
\end{eqnarray}

The action of the theory is defined by generalizing  the Teleparallel theory, as
\begin{eqnarray}\label{action}
S=\int e\left[f(T)+\mathcal{L}_{Matter}\right]d^4x\;,
\end{eqnarray}
where $f(T)$ is an algebraic function of the torsion scalar $T$. Making the functional variation of the action  (\ref{action}) with respect to the tetrads, we get the following equations of motion \cite{barrow,daouda1,daouda2}
\begin{eqnarray}
S^{\;\;\nu\rho}_{\mu}\partial_{\rho}Tf_{TT}+\left[e^{-1}e^{i}_{\mu}\partial_{\rho}\left(ee^{\;\;\alpha}_{i}S^{\;\;\nu\rho}_{\alpha}\right)+T^{\alpha}_{\;\;\lambda\mu}S^{\;\;\nu\lambda}_{\alpha}\right]f_{T}+\frac{1}{4}\delta^{\nu}_{\mu}f=4\pi\mathcal{T}^{\nu}_{\mu}\label{em}\; ,
\end{eqnarray}
where $\mathcal{T}^{\nu}_{\mu}$ is the energy momentum tensor, $f_{T}=d f(T)/d T$ and $f_{TT}=d^{2} f(T)/dT^{2}$. By setting $f(T)=a_1T+a_0$,  the equations of motion (\ref{em}) are the same as that of the Teleparallel theory with a cosmological constant, and this is dynamically equivalent to the GR.  These equations clearly depend on the choice made for the set of tetrads \cite{cemsinan}.
\par
The contribution of the interaction with the matter fields is given by the energy momentum tensor which, is this case, is defined as
\begin{eqnarray}
\mathcal{T}^{\,\nu}_{\mu}=  diag\left(1,-\omega_x,-\omega_y,-\omega_z\right)\rho                         \label{tem}\; ,
\end{eqnarray}
where the $\omega_i$ ($i=x,y,z$) are the parameters of equations of state related to the pressures $p_x$, $p_y$ and $p_z$.

\section{Field equations for Bianchi type-I, type-III and Kantowski-Sachs models} \label{BK}

Let us first establish the equations of motion of a set of diagonal tetrads using the Cartesian coordinate metric, for  describing models of Bianchi type-I, type-III and Kantowski-Sachs (KS). We propose to start with the Bianchi type-III case, from which Bianchi type-I and KS can be recovered. For the Bianchi type-III case, the metric reads
\begin{equation}
dS^2=dt^2-A^2(t)dx^2-e^{-2\alpha x}B^2(t)dy^2-C^2(t)dz^2\,\,\,,\label{metrictype3}
\end{equation}
where $\alpha$ is a constant parameter. Note that the Bianchi type-I is recovered by setting $\alpha=0$ from the Bianchi type-III, while KS is recovered when one takes $\alpha=0$ and $B(t)=C(t)$. Let us choose the following set of diagonal tetrads related to the metric (\ref{metrictype3})
\begin{eqnarray}
\left[e^{a}_{\;\;\mu}\right]=diag\left[1,A,e^{-\alpha x}B,C\right]\;. \label{matrixtype3}
\end{eqnarray}
The determinant of the matrix (\ref{matrixtype3}) is $e=e^{-\alpha x}ABC$. The components of the tensor torsion (\ref{tor}) for the tetrads (\ref{matrixtype3}) are given by
\begin{eqnarray}
T^{1}_{\;\;01}=\frac{\dot{A}}{A}\,,\,T^{2}_{\;\;02}=\frac{\dot{B}}{B}\,,\, T^{2}_{\;\;21}=\alpha\,,\,T^{3}_{\;\;03}=\frac{\dot{C}}{C}\;,\label{torsiontype3}
\end{eqnarray}
and the components of the corresponding tensor contorsion are
\begin{eqnarray}
K^{01}_{\;\;\;\;1}=\frac{\dot{A}}{A}\,,\,K^{02}_{\;\;\;\;2}=\frac{\dot{B}}{B}\,,\,K^{12}_{\;\;\;\;2}=\frac{\alpha}{A^2}\,,\,K^{03}_{\;\;\;\;3}=\frac{\dot{C}}{C}\;.\label{contorsiontype3}
\end{eqnarray}
The components of the tensor $S_{\alpha}^{\;\;\mu\nu}$, in (\ref{s}),  are given by
\begin{eqnarray}
S_{0}^{\;\;01}=S_{3}^{\;\;31}=\frac{\alpha}{2A^2}\,,\,S_{1}^{\;\;10}=\frac{1}{2}\left(\frac{\dot{B}}{B}+\frac{\dot{C}}{C}\right)\,,\,S_{2}^{\;\;20}=\frac{1}{2}\left(\frac{\dot{A}}{A}+\frac{\dot{C}}{C}\right)\,,\,S_{3}^{\;\;30}=\frac{1}{2}\left(\frac{\dot{A}}{A}+\frac{\dot{B}}{B}\right)\;.\label{tensortype3}
\end{eqnarray}
By using the components (\ref{torsiontype3}) and (\ref{tensortype3}),  the torsion scalar (\ref{te}) is given by
\begin{eqnarray}
T=-2\left(\frac{\dot{A}\dot{B}}{AB}+\frac{\dot{A}\dot{C}}{AC}+\frac{\dot{B}\dot{C}}{BC}\right)\; \label{torsionScalar1}.
\end{eqnarray}
The equations of motion are given by
\begin{eqnarray}
16\pi \rho &=& f+4f_T\Big[\frac{\dot{A}\dot{B}}{AB}+\frac{\dot{A}\dot{C}}{AC}+\frac{\dot{B}\dot{C}}{BC}-\frac{\alpha^2}{2A^2}\Big]\,\,,\label{densitytype3}\\
-16\pi p_x &=& f+2f_T\left[\frac{\ddot{B}}{B}+\frac{\ddot{C}}{C}+\frac{\dot{A}\dot{B}}{AB}+\frac{\dot{A}\dot{C}}{AC}+2\frac{\dot{B}\dot{C}}{BC}\right]\nonumber\\&+&2\left(\frac{\dot{B}}{B}+\frac{\dot{C}}{C}\right)\dot{T}f_{TT}\;,\label{radialpressuretype3}\\
-16\pi p_y&=&f+2f_T\left[\frac{\ddot{A}}{A}+\frac{\ddot{C}}{C}+\frac{\dot{A}\dot{B}}{AB}+2\frac{\dot{A}\dot{C}}{AC}+\frac{\dot{B}\dot{C}}{BC}\right]\nonumber\\&+&2\left(\frac{\dot{A}}{A}+\frac{\dot{C}}{C}\right)\dot{T}f_{TT}\;,\label{tangentialpressure1type3}\\
-16\pi p_z=f&+&2f_T\left[\frac{\ddot{A}}{A}+\frac{\ddot{B}}{B}+2\frac{\dot{A}\dot{B}}{AB}+\frac{\dot{A}\dot{C}}{AC}+\frac{\dot{B}\dot{C}}{BC}-\frac{\alpha^2}{A^2}\right]\nonumber\\&+&2\left(\frac{\dot{A}}{A}+\frac{\dot{B}}{B}\right)\dot{T}f_{TT}\;,\label{tangentialpressure2type3}\\
\frac{\alpha}{2A^2}\left[\left(\frac{\dot{A}}{A}-\frac{\dot{B}}{B}\right)f_T-\dot{T}f_{TT}\right]&=&0 \,\,\,, \label{constraint1} \\
\alpha\left(\frac{\dot{A}}{A}-\frac{\dot{B}}{B}\right)f_T&=&0\;.\label{constraint2}
\end{eqnarray}
In the particular case where $f(T)=T-2\Lambda$, the equations (\ref{densitytype3})-(\ref{constraint2}) are identical to that of the GR \cite{akarsu}. The equation of constraint (\ref{constraint2}) appears in both the GR as in $f(R)$ gravity \cite{sharif2}. But here we have a second equation of constraint (\ref{constraint1}), which appears as a generalization of the previous one, because here we have a contribution of a term of second derivative of the function $f(T)$ with respect to $T$.
\par

By setting $\alpha=0$, the Bianchi type-I case is recovered and the equations of motions read
\begin{eqnarray}
16\pi \rho &=& f+4f_T\Big[\frac{\dot{A}\dot{B}}{AB}+\frac{\dot{A}\dot{C}}{AC}+\frac{\dot{B}\dot{C}}{BC}\Big]\,\,\,,\label{densitytype1}\\
-16\pi p_x &=& f+2f_T\left[\frac{\ddot{B}}{B}+\frac{\ddot{C}}{C}+\frac{\dot{A}\dot{B}}{AB}+\frac{\dot{A}\dot{C}}{AC}+2\frac{\dot{B}\dot{C}}{BC}\right]+2\left(\frac{\dot{B}}{B}+\frac{\dot{C}}{C}\right)\dot{T}f_{TT}\;,\label{radialpressuretype1}\\
-16\pi p_y&=&f+2f_T\left[\frac{\ddot{A}}{A}+\frac{\ddot{C}}{C}+\frac{\dot{A}\dot{B}}{AB}+2\frac{\dot{A}\dot{C}}{AC}+\frac{\dot{B}\dot{C}}{BC}\right]+2\left(\frac{\dot{A}}{A}+\frac{\dot{C}}{C}\right)\dot{T}f_{TT}\;,\label{tangentialpressure1type1}\\
-16\pi p_z&=&f+2f_T\left[\frac{\ddot{A}}{A}+\frac{\ddot{B}}{B}+2\frac{\dot{A}\dot{B}}{AB}+\frac{\dot{A}\dot{C}}{AC}+\frac{\dot{B}\dot{C}}{BC}\right]+2\left(\frac{\dot{A}}{A}+\frac{\dot{B}}{B}\right)\dot{T}f_{TT}\;\label{tangentialpressure2type1}\;.
\end{eqnarray}
The equations of motion corresponding to KS model are obtained by setting $\alpha=0$ and $B=C$, yielding
\begin{eqnarray}
16\pi\rho&=&f+4f_T\left[\left(\frac{\dot{B}}{B}\right)^2+2\frac{\dot{A}\dot{B}}{AB}\right]\;,\label{densityks}\\
-16\pi p_x&=&f+4f_T\left[\frac{\ddot{B}}{B}+\left(\frac{\dot{B}}{B}\right)^2+\frac{\dot{A}\dot{B}}{AB}\right]+4\frac{\dot{B}}{B}\dot{T}f_{TT}\;,\label{radialpressureks}
\end{eqnarray}
\begin{eqnarray}
-16\pi p_y&=&f+2f_T\left[\frac{\ddot{A}}{A}+\frac{\ddot{B}}{B}+\left(\frac{\dot{B}}{B}\right)^2+3\frac{\dot{A}\dot{B}}{AB}\right]+2\left(\frac{\dot{A}}{A}+\frac{\dot{B}}{B}\right)\dot{T}f_{TT}\;,\label{tangentialpressureks}\\
p_y&=&p_z\nonumber\,\,\,.
\end{eqnarray}
In the next section we will perform the reconstruction scheme of the action of the system for some particular cases.

\section{ Reconstructing $f(T)$ gravity in inhomogeneous universes}\label{sec2a}

Let us now consider the reconstruction of the $f(T)$ action for some particular solutions of the class of metrics explored in the previous section. Specifically, we consider solutions of the type of de Sitter, power law evolutions and exponential solutions. Note that de Sitter and power law solutions have been widely explored in other contexts of modified gravity, as $f(R)$ and Gauss-Bonnet gravities (see Ref.~\cite{Nojiri:2009kx}), since they can provide a well description of  the cosmological evolution along its particular phases.\\
Let's start by considering for simplicity Bianchi type-I and Kantowski-Sachs $(\alpha=0)$ metrics. Then, the conservation equation for the energy momentum tensor (\ref{tem}) can be easily obtained,
\begin{equation}
\dot{\rho}+\left(H_x+H_y+H_z\right)\rho+H_x p_x+H_y p_y +H_z p_z=0\ ,
\label{D1}
\end{equation}
where we have defined $H_x=\frac{\dot{A}}{A}\ \ H_y=\frac{\dot{B}}{B}\ \ H_z=\frac{\dot{C}}{C}$. We can now analyse de Sitter, power law solutions and exponential expansion in  Bianchi type-I metric by one side, and Kantowski-Sachs metric by the other, where $B=C$ that implies $p_y=p_z$.

\subsection{De Sitter solutions}

De Sitter solutions are well known in the context of cosmology since the current epoch, where the universe expansion is being accelerated, can be described approximately with a de Sitter solution. This kind of solutions consists on an exponential expansion of the scale factor, which yields a constant Hubble parameter. In the case of Bianchi type-I and Kantowski-Sachs metrics $(\alpha=0)$ in (\ref{metrictype3}), we may assume an exponential expansion for each spatial direction,
\begin{equation}
A=A_0 {\rm e}^{a t}\ \ B=B_0 {\rm e}^{b t}\ \ C=C_0 {\rm e}^{c t}\ ,
\label{D2}
\end{equation}
and the rates of the expansion for each direction can be defined as,
\begin{equation}
H_x=\frac{\dot{A}}{A}=H_{x0}\ \ H_{y}=\frac{\dot{B}}{B}=H_{y0}\ \ H_c=\frac{\dot{C}}{C}=H_{z0}\ ,
\label{D3}
\end{equation}
where $\{H_{x0}=a,H_{y0}=b,H_{z0}=c\}$ are constants. The torsion scalar defined in (\ref{torsionScalar1}) is given by,
\begin{equation}
T_0=-2\left(H_{x0}H_{y0}+H_{x0}H_{z0}+H_{y0}H_{z0}\right)\ .
\label{D4}
\end{equation}
Then, by assuming $p_x=p_y=p_z=p$ and an equation of state $p=w\rho$, the conservation equation (\ref{D1}) can be easily solved for the ansatz  (\ref{D2}),
\begin{equation}
\rho=\rho_0{\rm e}^{-(H_{x0}+H_{y0}+H_{z0})(1+w)t}\ .
\label{D5}
\end{equation}
Hence, the field equations (\ref{densitytype1})-(\ref{tangentialpressure2type1}) become,
\begin{eqnarray}
16\pi \rho_0{\rm e}^{-(H_{x0}+H_{y0}+H_{z0})(1+w)t}=f(T_0)+4\left[H_{x0}H_{y0}+H_{z0}(H_{x0}+H_{y0})\right]f_T(T_0)\ , \label{D6} \\
-16\pi w\rho_0{\rm e}^{-(H_{x0}+H_{y0}+H_{z0})(1+w)t}=f(T_0)+2(H_{y0}+H_{z0})(H_{x0}+H_{y0}+H_{z0})f_T(T_0)\ , \label{D7}\\
-16\pi w\rho_0{\rm e}^{-(H_{x0}+H_{y0}+H_{z0})(1+w)t}=f(T_0)+2(H_{x0}+H_{z0})(H_{x0}+H_{y0}+H_{z0})f_T(T_0)\ , \label{D8}\\
-16\pi w\rho_0{\rm e}^{-(H_{x0}+H_{y0}+H_{z0})(1+w)t}=f(T_0)+2(H_{x0}+H_{y0})(H_{x0}+H_{y0}+H_{z0})f_T(T_0)\ . \label{D9}
\end{eqnarray}
Note that the only possible solution in the presence of a perfect fluid is one with $w=-1$ as the r.h.s. of equations (\ref{D6})-(\ref{D9}) is independent of time, according to the expression of the scalar torsion for a pure de Sitter solution (\ref{D4}), unless $H_{x0}+H_{y0}+H_{z0}=0$, which would imply a decelerating expansion in a particular direction, being $H_{i0}<0$. Moreover, for a particular $f(T)$ action, the system of equations (\ref{D4})-(\ref{D9}) reduces to an algebraic system of equations for the variables $\{H_{x0},H_{y0},H_{z0}\}$. Since  the system of equations (\ref{D4})-(\ref{D9}) are composed by four equations, while there are only three variables,
the above 4-equations system has to be reduced. However, even in the case of  Kantowski-Sachs metric, where $B(t)=C(t)\rightarrow H_{y0}=H_{z0}$, the system (\ref{D4})-(\ref{D9}) still posses three independent equations with two variables. Hence, the only possible solution imposes,
\begin{equation}
 A(t)=B(t)=C(t)\rightarrow H_{x0}=H_{y0}=H_{z0}=H_0\ ,
 \label{D10}
\end{equation}
And the metric (\ref{metrictype3}) reduces to the well known Friedmann-Lema\^itre-Robertson-Walker metric with an exponential expansion, $A(t)=A_0{\rm e}^{H_0\ t}$. Hence, the only solution for a pure de Sitter expansion in  Bianchi type-I and Kantowski-Sachs metrics gives a FLRW universe\footnote{Recall that we have assumed here that the pressures are equal, $p_x=p_y=p_z$.}, and the system of equations (\ref{D4})-(\ref{D9}) reduces now to a unique independent equation,
 \begin{equation}
 16 \pi \rho_0=f(T_0)+12H_{0}^2f_T(T_0)\ .
 \label{D11}
 \end{equation}
 Then, the roots of the algebraic equation (\ref{D11}) give the de Sitter points of a particular $f(T)$ action. In order to illustrate such possibility, let us consider the action,
 \begin{equation}
 f(T)=\left(-T\right)^n\ ,
 \label{D12}
 \end{equation}
 where $n$ is a real constant. Then, the equation (\ref{D11}) is rewritten as,
 \begin{equation}
 16\pi \rho_0=(1-2n)(6H_{0}^2)^n\ ,
 \label{D13}
 \end{equation}
 whose solution is given by,
 \begin{equation}
 H_{0}^2=\frac{1}{6}\left(\frac{16\pi\rho_0}{1-2n}\right)^{1/n}\ .
 \label{D14}
\end{equation}
 Hence, the only physical solution ($\rho_0,H_0^2\geq0$) imposes $n\leq1/2$. Then, the de Sitter solution is a direct consequence of the energy density $\rho_0$, which can be interpreted as a cosmological constant according to the condition imposed above for its equation of state, $w=-1$. Nevertheless, in vacuum the equation (\ref{D13}) reduces to $0=(1-2n)(6H_{x0}^2)^n$, whose only solution is given by $n=1/2$, rising to $f(T)=\sqrt{-T}$ that posses an infinite number of de Sitter points. Moreover, we may consider in vacuum the action,
 \begin{equation}
 f(T)=C_1 T+C_2 \left(-T\right)^n\ ,
 \label{D15}
 \end{equation}
where $\{C_1,C_2\}$ are the coupling constants and $n$ is a real constant. The field equation (\ref{D11}) in vacuum yields,
 \begin{equation}
0= C_1 6H_{0}^2+C_2(1-2n)(6H_{0}^2)^n\ .
\label{D16}
\end{equation}
So the roots of this equation give the dS points allowed by the class of theories expressed in (\ref{D15}). Note that now, the exponential expansion is a direct consequence of the action instead of the contribution of a kind of cosmological constant as in the case shown above. For instance, $n=2$, it yields the solution,
\begin{equation}
H_{0}=\sqrt{\frac{C_1}{18C_2}}\ .
\label{D17}
\end{equation}
While for higher powers of $n$, more de Sitter points can be obtained for the action (\ref{D15}). Note that in $f(R)$ theories, dS points constitutes the critical points of the dynamical system, which may be (un)stable, and could explain both the inflationary and dark energy epochs (see \cite{Cognola:2008zp}), which may be the case also in $f(T)$ gravity.

\subsection{Power law solutions}

Let us now explore a cosmological evolution described by a power law in each direction of the space expansion. In such case, the scale parameters for the Bianchi type-I and Kantowski-Sachs  metric (\ref{metrictype3}), where we set $(\alpha=0)$, can be expressed as,
\begin{equation}
A(t)=A_0t^a\ , \ B(t)=B_0t^b\ , \ C(t)=C_0t^c\ ,
\label{D18}
\end{equation}
where $\{a,b,c\}$ and $\{A_0,B_0,C_0\}$ are constants to be determined by the field equations, and initial conditions respectively. The expansion rates are given by,
\begin{equation}
H_x=\frac{a}{t}\ , \ H_y=\frac{b}{t}\ , \ H_z=\frac{c}{t}\ .
\label{D19}
\end{equation}
While the expression for the torsion scalar (\ref{torsionScalar1}) yields,
\begin{equation}
T=-2\left(\frac{ab}{t^2}+\frac{ac}{t^2}+\frac{bc}{t^2}\right)\ .
\label{D20}
\end{equation}
Then, introducing the above quantities in the field equations (\ref{densitytype1})-(\ref{tangentialpressure2type1}), we get the following system of differential equations in $f(T)$,
\begin{eqnarray}
16\pi \rho(T)=f(T)-2Tf_T(T)\ , \label{D21} \\
-16\pi w\rho(T)=f(T)+\frac{(b+c)(1-a-b-c)}{bc+a(b+c)}Tf_T(T)+2\frac{(b+c)}{bc+a(b+c)}T^2f_{TT}(T)\ , \label{D22}\\
-16\pi w\rho(T)=f(T)+\frac{(a+c)(1-a-b-c)}{bc+a(b+c)}Tf_T(T)+2\frac{(a+c)}{bc+a(b+c)}T^2f_{TT}(T)\ ,\label{D23} \\
-16\pi w\rho(T)=f(T)+\frac{(a+b)(1-a-b-c)}{bc+a(b+c)}Tf_T(T)+2\frac{(a+b)}{bc+a(b+c)}T^2f_{TT}(T)\ , \label{D24}
\end{eqnarray}
where we have assumed for simplicity that $p_x=p_y=p_z=p$ and an EoS $p=w\rho$. Hence, the system (\ref{D21})-(\ref{D24}) is a set of differential equations in f(T) with the torsion scalar $T$ as the independent variable. \\

Firstly let us consider the vacuum case, or in other words, the homogeneous part of the first equation (\ref{D21}), which becomes $f(T)-2Tf_T(T)=0$ and whose solution is given by,
\begin{equation}
f(T)=C_1 \sqrt{-T}\ ,
\label{D26}
\end{equation}
where $C_1$ is an integration constant. In order to satisfy the rest of the equations (\ref{D22})-(\ref{D24}), the condition $a=b=c$ must be imposed, so that the Hubble parameters (\ref{D19}) reduce to the usual FLRW cosmology reproducing  power law solution. \\

In the presence of a kind of isotropic perfect fluid $p=w\rho$, we can first solve the continuity equation (\ref{D1}) in order to obtain $\rho=\rho(T)$, which yields,
\begin{equation}
\rho=\rho_0 t^{-(a+b+c)(1+w)}=\rho_0 \left(-\frac{T}{2(ab+ac+bc)}\right)^{\frac{(a+b+c)(1+w)}{2}}\ .
\label{D25}
\end{equation}
Hence, the solution for the set of equations (\ref{D21})-(\ref{D24}) is given by $f(T)=f_h(T)+f_p(T)$, where $f_h(T)$ is the solution of the homogeneous equation, which coincides with the vacuum solution (\ref{D26}), and $f_p(T)$ is the particular solution. Then, by using (\ref{D25}) in the equation (\ref{D21}), the particular solution can be easily found,
\begin{equation}
f_{p}(T)=\chi\ T^{\frac{(1+w)(a+b+c)}{2}}\ ,
\label{D27}
\end{equation}
 where $\chi$ is a constant given by
\begin{equation}
 \chi=\frac{2^{4-(1+w)(a+b+c)/2}\pi \rho_0}{\left[-1+(1+w)(a+b+c)\right] \left[-bc-a(b+c)\right]^{\frac{(1+w)(a+b+c)}{2}}}\ .
 \label{D28}
\end{equation}
Note that the condition $(1+w)(a+b+c)=2\ n$ with $n$ being any natural number,  has to be imposed in order to avoid a complex gravitational action that would lacks any physical sense, recall  that $T<0$ for an expanding universe according to (\ref{D20}).   In order to satisfy the complete set of equations (\ref{D21})-(\ref{D24}), we introduce the solution (\ref{D27}) into the field equations (\ref{D22})-(\ref{D24}), and the following solutions for the parameters  $\{a,b,c\}$ are found,
\begin{enumerate}[ i.]
\item $\ c=\frac{1-w(a+b)}{w}\ $, where $w\neq 0$. This provides an anisotropic solution in $f(T)$ gravity with $A(t)$, $B(t)$ and $C(t)$ being different functions in (\ref{D18}), and recalling that the perfect fluid assumed is an isotropic fluid. This does not hold in GR or Teleparallel Theory (TT) but is possible here due to the presence of second derivatives of the function $f(T)$ with respect to the torsion scalar $T$ in (\ref{D21})-(\ref{D24}). Note that field equations may be rewritten as the usual equations in TT,
\[
H_xH_y+H_xH_z+H_yH_z=16\pi(\rho +\rho_{f(T)})\ ,\; \;
-\dot{H}_y-H_{y}^2-\dot{H}_z-H_{z}^2-H_y\ H_z=8\pi (w\rho +p_{f(T)}^x)\ ,
\]
\begin{equation}
-\dot{H}_x-H_{x}^2-\dot{H}_z-H_{z}^2-H_x\ H_z=8\pi (w\rho +p_{f(T)}^y)\ ,\; \;
-\dot{H}_x-H_{x}^2-\dot{H}_y-H_{y}^2-H_x\ H_y=8\pi (w\rho +p_{f(T)}^z)\ .
\end{equation}
Here, the extra terms coming from $f(T)$ are defined as an energy density $\rho_{f(T)}$ and pressures $\{p_{f(T)}^x, \ p_{f(T)}^y, \ p_{f(T)}^z\}$, which are the origin of the anisotropic evolution. In this case, we have to fix $C_1=0$  in (\ref{D26}) in order to satisfy the whole system.
\item $a=b=c$. The cosmological evolution expressed by \ref{D18} reduces to a FLRW metric as in the homogeneous part of the equations, so that $C_1\neq0$.
\item $c=-ab/(a+b)$. In spite of this satisfies equations (\ref{D21})-(\ref{D24}) once (\ref{D27}) is substituted in the equations, it gives $T=0$, and the r.h.s of equations (\ref{D21})-(\ref{D24}) become null while the l.h.s. are not, since $\rho=\rho(t)$ as given in (\ref{D25}), so this is not a real solution.

\end{enumerate}�
\par
Therefore,  we have obtained a complete set of power law solutions for Bianchi type-I  universe and Kantowski-Sachs metrics in the context of $f(T)$ gravity. Nevertheless, the action is clearly dependent on the EoS parameter $w$. Note also that in vacuum, the only possible solution reduces to a FLRW metric.

\subsection{General exponential solutions}

In this subsection we consider a more general exponential expansion for each spatial direction by
\begin{eqnarray}
A=A_0e^{g_x(t)}\,\,\,, \quad B=B_0e^{g_y(t)}\,\,\,,\quad C=C_0e^{g_z(t)}\,\,\,,
\end{eqnarray}
where the function $g_i(t)$ is assumed as
\begin{eqnarray}
g_i(t)=h_i(t)\ln{\left(t\right)}\,\,,\quad i=x,y,z\;\;,
\end{eqnarray}
 and $A_0$, $B_0$ and $C_0$ are positive constants. Note that the previous cases, the de Sitter solutions and power law solutions can be recovered from this one by setting $h_i(t)=a_it/(\ln{(t)})$ and $h_i(t)=a_i$, respectively, where $\{a_i\}=\{a,b,c\}$. In what follows, we will use an adiabatic approximation for the expansion in each spatial direction and neglect the derivatives of $h_i(t)$, i.e., setting $(\dot{h}_i\sim \ddot{h}_i\sim 0)$. The expansion rates in this case are given by
\begin{eqnarray}
H_x=\frac{h_x(t)}{t}\,\,,\quad H_y=\frac{h_y(t)}{t}\,\,,\quad H_z=\frac{h_z(t)}{t}\,\,.
\label{steph62}
\end{eqnarray}
Thus, the torsion scalar (\ref{torsionScalar1}) becomes
\begin{eqnarray}
T=-2\left[\frac{h_x(t)h_y(t)}{t^2}+\frac{h_x(t)h_z(t)}{t^2}+\frac{h_y(t)h_z(t)}{t^2}\right]\,\,.\label{steph63}
\end{eqnarray}
The acceleration in each direction is given by
\begin{eqnarray}
\ddot{A}=\frac{h_x(h_x-1)}{t^2}A\,\,,\quad \ddot{B}=\frac{h_y(h_y-1)}{t^2}B\,\,,\quad \ddot{C}=\frac{h_z(h_z-1)}{t^2}C\,\,.\label{steph64}
\end{eqnarray}
Since $A$, $B$ and $C$ are positives, the acceleration is guaranteed in each direction when $h_i>1$, while for $0<h_i<1$, the universe  is in deceleration.\par
The simplest example of $h_i(t)$ is
\begin{eqnarray}
h_i(t)=\frac{h_{i\,in}+h_{i\,out}\,qt^2}{1+qt^2}\,\,\,,\label{steph65}
\end{eqnarray}
where $h_{i\,in}$, $h_{i,out}$ and $q$ are positive constants, and the $q$ is assumed to be enough small in order to make $h_i(t)$ varying slowly. Thus, the torsion scalar is always negative. From (\ref{steph65}), we see that at early time $t=0$, $h_i\rightarrow h_{i\,in}$ and for late universe, $h_i\rightarrow h_{i\,out}$. By using
(\ref{steph65}) and (\ref{steph63}), one gets the following equation
\begin{eqnarray}
q^2Tt^6+\left(2qT+2q^2X\right)t^4+\left(T+2qY\right)t^2+2Z=0\,\,\,,\\
X=h_{x\,out}h_{y\,out}+h_{x\,out}h_{z\,out}+h_{y\,out}h_{z\,out}\,\,,\quad
Y=h_{x\,in}h_{y\,out}+h_{x\,out}h_{y\,in}+h_{x\,in}h_{z\,out}+\nonumber\\
h_{x\,out}h_{z\,in}+h_{y\,in}h_{z\,out}+h_{y\,out}h_{z\,in}\,\,,\quad
Z=h_{x\,in}h_{y\,in}+h_{x\,in}h_{z\,in}+h_{y\,in}h_{z\,in}\,\,,\nonumber
\end{eqnarray}
whose solutions read
\begin{eqnarray}
t^2&=&\left\{\Psi_0(T),\;\;\Psi_{\pm}(T)\right\}\,,\label{steph67}\\
\Psi_0(T)&\equiv& \alpha^{1/3}+\beta_0\alpha^{-1/3}+\beta_1\,\;\;\Psi_{\pm}(T)\equiv e^{\mp 2i\pi/3}\alpha^{1/3}+e^{\pm 2i\pi/3}\alpha^{-1/3}+\beta_1\,\,,\;\;\,\nonumber\\ \alpha&=&\frac{\sqrt{\alpha_1}}{q^2T^2}-\alpha_2\,\,,\;
\beta_0=\frac{qT(8X-6Y)+4q^2X^2+T^2}{9q^2T^2}\,\,,\quad \beta_1=-\frac{2qX+2T}{3qT}\,\,,\nonumber\\
\alpha_1&=&\frac{1}{27qT}\Big[27qT^2Z^2+[(-36q^2TX-36qT^2)Y+16q^3X^3+48q^2TX^2+30qT^2X-2T^3]Z\nonumber
\\&+&8q^2TY^3+(-4q^3X^2-8q^2TX+8qT^2)Y^2+(-4q^2TX^2-8qT^2X+2T^3)Y-qT^2X^2-2T^3X\Big]\,\,,\nonumber\\
\alpha_2&=&\frac{qT^2(27Z-18Y+15X)+q^2T(24X^2-18XY)+8q^3X^3-T^3}{27q^3T^3}\,\,.\nonumber
\end{eqnarray}
We see from (\ref{steph67}) that there are one real positive solution, $\Psi_0(T)$, and two complex solutions $\Psi_{\pm}(T)$. By using (\ref{steph62})-(\ref{steph64}) the system of equations of motion (\ref{densitytype1})-(\ref{tangentialpressure2type1}) becomes
\begin{eqnarray}
16\pi\rho&=&f-2Tf_T\,\,\,,\label{steph68}\\
-16\pi p_x&=&f+2f_T\left[\frac{(h_y+h_z)^2-(h_y+h_z)-h_yh_z}{\Psi_0(T)}-\frac{T}{2}\right]+4\left(\frac{h_y+h_z}{\Psi_0(T)}\right){T}f_{TT}\,\,,\label{steph69}\\
-16\pi p_y&=&f+2f_T\left[\frac{(h_x+h_z)^2-(h_x+h_z)-h_xh_z}{\Psi_0(T)}-\frac{T}{2}\right]+4\left(\frac{h_x+h_z}{\Psi_0(T)}\right){T}f_{TT}\,\,,\label{steph70}\\
-16\pi p_z&=&f+2f_T\left[\frac{(h_x+h_y)^2-(h_x+h_y)-h_xh_y}{\Psi_0(T)}-\frac{T}{2}\right]+4\left(\frac{h_x+h_y}{\Psi_0(T)}\right){T}f_{TT}\,\,,\label{steph71}\\
h_i&=&\frac{h_{i in}+h_{i out}q\Psi_0(T)}{1+q\Psi_0(T)}\,\,\,.\label{steph72}
\end{eqnarray}
\subsubsection{A special case}\label{numero1}

Here, we assume that the expansion rates are equal in the three spatial directions ($h_x=h_y=h_z$), and the system (\ref{steph68})-(\ref{steph71}) reduces to
\begin{eqnarray}
16\pi\rho&=&f-2Tf_{T}\,\,,\label{steph73}\\
-16\pi p_x&=&f-2f_T\left(T+\sqrt{\frac{-2T}{3\Psi_0(T)}}\right)+4T\sqrt{\frac{-2T}{3\Psi_0(T)}}f_{TT}\,\,,\label{steph74}\\
p_x&=&p_y=p_z\,\,\,,\nonumber
\end{eqnarray}
which means that the assumption of having the same rate in the three spatial direction leads to an isotropic matter content. By combining (\ref{steph73}) and (\ref{steph74}), one gets
\begin{eqnarray}
4T\sqrt{\frac{-2T}{3\Psi_0(T)}}f_{TT}-2f_T\left[(1+\omega)T+\sqrt{\frac{-2T}{3\Psi_0(T)}}\,\right]+(1+\omega)f=0\,\,\,,\label{steph75}
\end{eqnarray}
where we used the barotropic equation $p_x=\omega\rho$. Let us consider an asymptotic analysis, looking for the early universe (small time) and the late time one (large time), for which the function $h_i(t)$ yields $h_{i\,in}$ and $h_{i\,out}$, respectively. Thus, for the early universe Eq. (\ref{steph75}) reduces to
\begin{eqnarray}
4T^2f_{TT}+6Tf_{T}\left[3h_{i\,in}(\omega+1)-1\right]-3h_{i\,in}(\omega+1)f=0\,\,\,,\\
h_{i\,in}=h_{x\,in}=h_{y\,in}=h_{z\,in}\,\,\,,\nonumber
\label{steph76}
\end{eqnarray}
whose general solution reads
\begin{eqnarray}
f(T)=C_3T^{\gamma_+}+C_4T^{\gamma_-}\,\,,\quad \gamma_{\pm}=\frac{5-9h_{x\,in}(1+\omega)\pm\sqrt{25-78h_{x\,in}(1+\omega)+81h^2_{x\,in}(1+\omega)^2}}{4}\,\,,\label{steph77}
\end{eqnarray}
where $C_3$ and $C_4$ are integration constants. From (\ref{steph77}), by writing the radicand as $\left[5-9h_{x\,in}(1+\omega)\right]^2+12h_{x\,in}(1+\omega)$, one observes that, for any $\omega>-1$, $\gamma_{+}>0$ and $\gamma_{-}<0$. Moreover, in this context of asymptotic analysis, we observe from (\ref{steph63}) that for small $t$, the torsion scalar $T$ is large, while for large $t$, the torsion is small. Thus, for small $t$ with $h_{x\,in}>1$, corresponding to the inflation, the algebraic expression of $f(T)$ is given by
\begin{eqnarray}
f(T)=C_3T^{\gamma_{+}}\,\,\,.
\end{eqnarray}
Since $h_x(t)$ reduces to $h_{x\,out}$ in the late universe, the model corresponding to the late accelerated universe can be obtained by replacing $h_{x\,in}$ by $h_{x\,out}$. Precisely, for large $t$, the torsion scalar is small, and for $h_{x\,out}>1$, the dominate term in (\ref{steph77}), corresponding to the model of late time universe, is
\begin{eqnarray}
f(T)=C_4T^{\gamma_{-}'}\,\,\,,\;\;\gamma_{\pm}'=\frac{5-9h_{x\,out}(1+\omega)\pm\sqrt{25-78h_{x\,out}(1+\omega)+81h^2_{x\,out}(1+\omega)^2}}{4}\,\,.
\end{eqnarray}
This model is equivalent to the teleparallel gravity for $C_4=1$ and $h_{x\,out}=2/(5+5\omega)$. It is easy to see from this that, for any ordinary matter, i.e., $\omega>0$, one gets $h_{x\,out}<1$, meaning that the teleparallel gravity without cosmological constant cannot provide the late acceleration of the universe (remembering that the acceleration is guaranteed for $h_{x\,out}>1$, and $0<h_{x\,out}<1$ characterising a decelerated expanding universe). Thus, the contribution of the $f(T)$ terms plays the role of the dark energy.\par
Looking for the expression of $f(T)$ for large cosmic time $t$, i.e., the expression (\ref{steph77}) (replacing $h_{x\,in}$ by $h_{x\,out}$), a similarity can be observed with a result of Bamba et al in \cite{bambamyr}. In this work, they undertook $f(T)$ theory in the FLRW metric, first assuming a power-law expression for $f(T)$ in the Eq.~(4.6) for investigating what type of finite future time singularities may appear. Later, they introduced a correction term, still in the form of power-law, their Eq.~(4.22), in order to analyse the possible avoidance of the singularities. Then, they obtained the global expression (4.23) of \cite{bambamyr}. Note that this expression is equivalent to our Eq.~(\ref{steph77}). Moreover, they shown in their ``TABLE II" that the Big Rip and the Big Freeze can be removed if the product of the exponents is negative. This is exactly our result, since $\gamma_{+}'$ and $\gamma_{-}'$ are always positive and negative, respectively ($\gamma_{\pm}'$ are obtained from $\gamma_{\pm}$ by replacing $h_{x\,in}$ by $h_{x\,out}$). This means that for both Bianchi type-I and KS, if the expansion of the universe occurs with the same rate in all direction, models that can realize the late time accelerated expansion of the universe, and able to prevent the Big Rip and the Big Freeze can be reconstructed.

\subsubsection{Using an auxiliary scalar field}\label{numero2}
In this subsection, we would like to use the reconstruction scheme, for which an auxiliary scalar field is introduced in the action of the theory. By this way, the functional form of $f(T)$ can be found through two other scalar functions $P$ and $Q$
(for more clarification on the method, see the case of $f(R)$ gravity \cite{odintsov-asf} and other of $f(T)$ gravity \cite{daouda3}).
Here, we return to the general system (\ref{steph68})-(\ref{steph72}), where we introduce the auxiliary scalar field $\phi$, by defining the algebraic function $f(T)$ by
\begin{eqnarray}
f(T)=P(\phi)T+Q(\phi)\,\,\,. \label{steph78}
\end{eqnarray}
By using (\ref{steph78}) and varying the action (\ref{action}) with respect to the scalar field $\phi$, one gets
\begin{eqnarray}
P'(\phi)T+Q'(\phi)=0\,\,\,,
\end{eqnarray}
which may be solved with respect to $\phi$, yielding  $\phi=\phi(T)$. Here, the prime (') denotes the derivative with respect to $\phi$. By using (\ref{steph78}), one obtains
\begin{eqnarray}
f_T(T)=P(\phi(T)) \,\,\,,\quad f_{TT}(T)=P_T(\phi(T))\,\,\,. \label{steph80}
\end{eqnarray}
Making use of (\ref{steph80}), one can rewrite the system (\ref{steph68})-(\ref{steph71}) as
\begin{eqnarray}
16\pi\rho&=&P(\phi)T+Q(\phi)-2TP(\phi)\,\,\,,\label{steph81}\\
-16\pi p_x&=&P(\phi)T+Q(\phi)+2P(\phi)\left[\frac{(h_y+h_z)^2-(h_y+h_z)-h_yh_z}{\Psi_0(T)}-\frac{T}{2}\right]\nonumber\\&+&4\left(\frac{h_y+h_z}{\Psi_0(T)}\right){T}P_T(\phi)\,\,,\label{steph82}
\end{eqnarray}
\begin{eqnarray}
-16\pi p_y&=&P(\phi)T+Q(\phi)+2P(\phi)\left[\frac{(h_x+h_z)^2-(h_x+h_z)-h_xh_z}{\Psi_0(T)}-\frac{T}{2}\right]\nonumber\\
&+&4\left(\frac{h_x+h_z}{\Psi_0(T)}\right){T}P_T(\phi)\,\,,\label{steph83}\\
-16\pi p_z&=&P(\phi)T+Q(\phi)+2P(\phi)\left[\frac{(h_x+h_y)^2-(h_x+h_y)-h_xh_y}{\Psi_0(T)}-\frac{T}{2}\right]\nonumber\\
&+&4\left(\frac{h_x+h_y}{\Psi_0(T)}\right){T}P_T(\phi)\,\,\label{steph84} \,\,.
\end{eqnarray}
Let us consider that $p_y=p_z$. Then, by equating (\ref{steph83}) with (\ref{steph84}), one gets
\begin{eqnarray}
TP_T(\phi)=-\frac{1}{2}P(\phi)\left(h_x+h_y+h_z-1\right)\,\,\,.\label{steph85}
\end{eqnarray}
Using (\ref{steph85}), the system (\ref{steph81})-(\ref{steph84}) reduces to
\begin{eqnarray}
16\pi\rho&=&Q(\phi)-TP(\phi)\,\,\,,\label{steph86}\\
-16\pi p_x&=&Q(\phi)+TP(\phi)\,\,\,,\label{steph87}\\
p_x&=& p_y=p_z \,,\,\omega_x=\omega_y=\omega_z\label{steph88}\,.
\end{eqnarray}
By using (\ref{steph86}), one can determine $Q(\phi)$ as
\begin{eqnarray}
Q(\phi)=16\pi~\rho+TP(\phi)\,\,\,,\label{steph90}
\end{eqnarray}
which, substituted in (\ref{steph87}) and (\ref{steph88}), yields
\begin{eqnarray}
-16\pi(\omega_x+1)\rho=2TP(\phi)\label{steph91}\,.
\end{eqnarray}
As one can redefine the scalar field properly, we may choose $\phi=t$, then $P(\phi)=P(t)=\bar{P}(T)$. Note that in the case where $\omega_x=-1$, one gets $\bar{P}(T)=0$, and the algebraic function $f(T)=Q(t)=16\pi\rho=\bar{Q}(T)$. But this requires to have the complete expression of $\rho$ depending on $T$, i.e., solving the equation of continuity. Let us consider in general the case where $\omega_x\neq-1$ and try to solve the equation of continuity, which will help us to determine  $\bar{P}(T)$ and $\bar{Q}(T)$, leading to the reconstruction of the algebraic function $f(T)$. We choose the case of KS geometry ($h_y=h_z$), where the equation of continuity is written as
\begin{eqnarray}
\dot{\rho}+\rho(1+\omega_x)(H_x+2H_y)=0\,\,\,,
\end{eqnarray}
which can be solved, giving
\begin{eqnarray}
\rho(t)&=&C_5\exp{\left[G_1(t)+G_2(t)\right]}\label{steph93}\,\,\,,\\
G_1(t)&=&\frac{(1+\omega_x)(h_{x\,in}+2h_{y\,in})}{t}\,\,\,,\\
G_2(t)&=&\sqrt{q}\left[(1+\omega_x)(h_{x\,in}-h_{x\,out}+2h_{y\,in}-2h_{y\,out})\right]
\arctan{\left(\sqrt{q}t\right)}\,\,\,,
\end{eqnarray}
where $C_5$ is an integration constant.
Making use of (\ref{steph67}), one can cast $\rho(t)$ in terms of $T$. Also, from Eq.~(\ref{steph91}), one obtains $P(t)$ in functions of $T$, and from (\ref{steph90}), one gets $Q(t)$ in terms of $T$. Therefore, we can reconstruct the algebraic function  $f(T)$, given in  (\ref{steph78}), as
\begin{eqnarray}
f(T)&=&-16\pi C_3 \omega_x \exp\left[\frac{g_1}{\sqrt{\Psi_0 (T)}}+g_2 \arctan\left(\sqrt{q\Psi_0 (T)}\right)\right]\label{steph103}\,,
\end{eqnarray}
where $g_1=(1+\omega_x)(h_{x\,in}+2h_{y\,in})$ and $g_2=\sqrt{q}(1+\omega_x)(h_{x\,in}-h_{x\,out}+2h_{y\,in}-2h_{y\,out})$.
\par
In principle, with (\ref{steph103}), some cosmological models can now be reproduced. Let us focus our attention to the  early universe (which may be characterized by the inflation), and the late time universe (characterized by its accelerated expansion) in the three spatial direction. \par
At early time, i.e., for small $t$  (or  large $T$), $\Psi_0(T)$ is very small, and the corresponding algebraic function is
\begin{eqnarray}
f(T)=-16\pi C_3\omega_x\exp{\left[\frac{g_1}{\sqrt{\Psi_0 (T)}}\right]}\,\,\,.
\end{eqnarray}
At late time, the time $t$ is large (corresponding to small torsion scalar and large $\Psi_0(T)$), and the algebraic function reads
\begin{eqnarray}
f(T)=-16\pi C_3\omega_x\exp{\left[g_2 \arctan\left(\sqrt{q\Psi_0 (T)}\right)\right]}\,\,\,.
\end{eqnarray}
Thus, we see that models corresponding to the inflation and the late time accelerated universe can be reconstructed within KS metrics where the matter content is partially isotropic ($p_y=p_z$). Since in this work we fall in the situation where $\omega_x=\omega_y=\omega_y$ one could use the WMAP data and try to check if they fit with this anisotropic model. Because of having ultimately $p_x=p_y=p_z$ and $h_y=h_z$, one can just use the first two equations of motion of KS case, i.e., (\ref{densityks})-(\ref{radialpressureks}). In order to put out the contribution of the modified part of the algebraic function $f(T)$, we cast it into the form $f(T)=T+j(T)$, as the teleraparallel term plus the modified additive algebraic function $j(T)$. Thus, the equations (\ref{densityks}) and (\ref{tangentialpressureks}) become
\begin{eqnarray}
8\pi \rho_{eff}&=& \left(\frac{\dot{B}}{B}\right)^2+2\frac{\dot{A}\dot{B}}{AB}\,\,,\label{effectivedensity}\\
-8\pi p_{x\,eff}&=& 2 \frac{\ddot{B}}{B}+\left(\frac{\dot{B}}{B}\right)^2\,\,,\label{effectivepressure}
\end{eqnarray}
where $\rho_{eff}$ and $p_{x\,eff}$ are the effective energy density and effective pressure, respectively, and defined by
\begin{eqnarray}
\rho_{eff}&=&\rho-\frac{1}{16\pi}\left\{j+4j_T\left[ \left(\frac{\dot{B}}{B}\right)^2+2\frac{\dot{A}\dot{B}}{AB}\right]\right\}\,\,\,,\\
p_{x\,eff}&=&p_{x}+\frac{1}{16\pi}\left\{j+4j_T\left[\frac{\ddot{B}}{B}+\left(\frac{\dot{B}}{B}\right)^2+\frac{\dot{A}\dot{B}}{AB}\right]+4\frac{\dot{B}}{B}\dot{T}j_{TT}\right\}\,\,\,.
\end{eqnarray}
By dividing (\ref{effectivepressure}) by (\ref{effectivedensity}), using $\omega_{eff}=p_{x\,eff}/\rho_{eff}$, one gets
\begin{eqnarray}
\omega_{eff}=\frac{2-3h_y}{h_y+2h_x}\label{steph104}\,.
\end{eqnarray}
Since the observational data from the WMAP project do not depend on the spatial direction, i.e., are not based on an anisotropic geometry, we have to impose $h_x=h_y$ in (\ref{steph104}), for getting a suitable cosmological feature. Thus, assuming that the accelerated expansion of the universe is realized with the same rate in all directions, $h_x=h_y=h_z>1$, and that the universe is essentially filled  by the dark energy, where we can neglect the usual matter content such that $\omega_{eff}\sim \omega_{DE}$. Therefore, using (\ref{steph104}), we have the possibility to regain the well known range of values  allowed by the current 7-year WMAP data for the parameter of the equation of state of the  dark energy, $\omega_{DE}= -1.1 \pm 0.14$  WMAP \cite{wmap}.

\subsection{On Bianchi type-III solutions}

In this section, we propose to present some comments on Bianchi type-III solutions. This case is quite exceptional since we do not have the freedom of making cosmological reconstruction as in the case of Bianchi type-I and KS, due to the constraints equations
(\ref{constraint1}) and (\ref{constraint2}). \par
From (\ref{constraint2}), since the parameter is different from zero and the algebraic function cannot be a constant, one gets
\begin{eqnarray}
\frac{\dot{A}}{A}=\frac{\dot{B}}{B}\,\,\,,
\end{eqnarray}
which, injected in (\ref{constraint1}) leads to
\begin{eqnarray}
\dot{T}f_{TT}=0\,\,\,,\label{constraint3}
\end{eqnarray}
meaning that one has $\dot{T}=0$ or $f_{TT}=0$. The first case, $\dot{T}=0$ implies that one has a constant torsion scalar, i.e.,
\begin{eqnarray}
\frac{\dot{A}^2}{A^2}+2\frac{\dot{A}\dot{C}}{AC}=K\,\,,\label{steph111}
\end{eqnarray}
where $K$ is positive constant. Let us consider $A=C^n$, with $n$ bigger than zero or less  than $-2$. Thus, Eq.~(\ref{steph111}) can be solved yielding
\begin{eqnarray}
C(t)=C_0'\exp{\left(\pm\sqrt{\frac{K}{n(n+2)}}\;t\;\right)}\,\,\,,\label{soluC}
\end{eqnarray}
leading to
\begin{eqnarray}
A(t)=B(t)=(C_0')^n\exp{\left(\pm n\sqrt{\frac{K}{n(n+2)}}\;t\;\right)}\,\,\,,
\end{eqnarray}
where $C_0'$ is a positive constant. It is important to note that in order to guarantee the expansion of the universe, one need to have
\begin{eqnarray}\label{vincent18}
A(t)=B(t)=\left\{\begin{array}{ll}
(C_0')^n\exp{\left(- n\sqrt{\frac{K}{n(n+2)}}\;t\;\right)}\,\,\,,\quad \mbox{for}\,\,\, n<-2 \\
(C_0')^n\exp{\left( n\sqrt{\frac{K}{n(n+2)}}\;t\;\right)}\,\,\,, \;\;\;\quad \mbox{for}\,\,\, n>0\,\,\,.\end{array}\right.
\end{eqnarray}

In this case, we see that the rate of expansion is constant for the three spatial direction: this is the de Sitter universe.\par
Now we can perform the reconstruction of the algebraic function $f(T)$.  One can cast Eqs.~(\ref{densitytype3})-(\ref{tangentialpressure2type3}) in the following system
\begin{eqnarray}
16\pi\rho&=&f+4f_T\left(K-\frac{\alpha^2}{2A^2}\right)\,\,\,,\label{jesuis}\\
-16\pi\omega_x\rho&=&f+2Kf_T\left[\frac{2n^2+3n+1}{n(n+2)}\right]\,\,\,,\label{tues}\\
-16\pi\omega_z\rho&=&f+4Kf_T\left(\frac{2n+1}{n+2}\right)-2\frac{\alpha^2}{A^2}f_T\;\;,\label{ilest}\\
p_x&=&p_y\,\,\,.
\end{eqnarray}
By combining (\ref{jesuis}) with (\ref{ilest}), one can eliminate the term containing $\alpha$, obtaining
\begin{eqnarray}
-16\pi(\omega_z+1)\rho=\frac{4K(n-1)}{n+2}f_T \,\,.\label{noussommes}
\end{eqnarray}
The energy density $\rho$ can be eliminated by combining (\ref{tues}) with (\ref{noussommes}) yielding the following differential equation
\begin{eqnarray}
2K\left[2n(n-1)\omega_x-(\omega_z+1)(2n^2+3n+1)\right]f_T-n(n+2)(\omega_z+1)f=0\,\,\,,
\end{eqnarray}
whose general solution is
\begin{eqnarray}
f(T)&=&C_6\exp{\left[R(n)T\right]}\,\,\,,\\
R(n)&=&\frac{n(n+2)(\omega_z+1)}{2K\left[2n(n-1)\omega_x-(\omega_z+1)(2n^2+3n+1)\right]}\,\,,\nonumber
\end{eqnarray}
where $C_6$ is an integration constant. Note that for $n=1$ and $\omega_x=\omega_z$, Eq.~(\ref{D10}) is recovered.
\par
The second case from (\ref{constraint3}), $f_{TT}=0$, implies that $f_{T}$ is constant, that we choose to be minus two times the cosmological constant $\Lambda$, then, $f(T)$ is written as
\begin{eqnarray}
f(T)=T-2\Lambda\,\,\,,
\end{eqnarray}
which is the teleparallel gravity with cosmological constant.

\section{Conclusion} \label{conclusions}

Along the paper, the Bianchi type-I, Kantowski-Sachs, and Bianchi type-III metrics have been studied in the context of $f(T)$ gravities. Particularly, we have shown the reconstruction of some important cosmological solutions, obtaining the corresponding $f(T)$ action. We have assumed initially a particular choice of coordinates and tetrads, specifically cartesian coordinates and a diagonal set of tetrads have been imposed in order to avoid the well known constraint $f_{TT}=0$, which reduces trivially to the action of teleparallel gravity (see Ref.~\cite{Tamanini:2012hg}).\par
Then, several important cosmological solutions have been considered. In particular, dS solutions, where the scale factor is an exponential function of the cosmic time, has been considered for Bianchi type-I and Kantowski-Sachs metrics by imposing a particular exponential expansion in each direction of the space.  We have shown that the only possible solution turns out to the FLRW metric, such that no possible dS anisotropic evolution can be found in $f(T)$, unless one considers an anisotropic fluid. Nevertheless, in the case of power law solutions, we have found that in the presence of a perfect isotropic fluid, an anisotropic cosmological evolution can be found for a particular choice of the action $f(T)$, while in vacuum the action reduces to FLRW metric.\par
Moreover, we have extended the cosmological reconstruction scheme to a general exponential solutions, from which the above de Sitter law and power law solutions are particular cases. We have assumed an adiabatic approximation for the expansion in each spatial direction. We undertook two cases, a special case and a second where an auxiliary field is used. In the both cases, we shown that the models can realize the early accelerated universe, characterized by the inflation, and the late time acceleration of our current universe. In the special case, the model presents an interesting aspect because it ensures the avoidance of the Big Rip and the Big Freeze. In the case where the auxiliary field is used, the model corresponding to the late time accelerated universe fits with the 7-year WMAP data, confirming the consistency of the result.
\par
The Bianchi type-III case  presents some constraints from which only two forms of the algebraic function $f(T)$ can be obtained. The first is the well known teleparallel gravity with cosmological constant, and the second is a de Sitter type solution.

\vspace{0,25cm}
{\bf Acknowlegments} The authors thank Prof. J. D. Barrow for useful discussions. MER thanks  UFES for the hospitality during the development of this work. MJSH thanks CNPq/FAPES for financial support. DSG acknowledges support from a postdoctoral contract from the University of the Basque Country (UPV/EHU) under the program ``Specialization of research staff'', and support from the research project FIS2010-15640, and also by the Basque Government through the special research action KATEA and UPV/EHU under program UFI 11/55.

redpajama_set_name: RedPajamaArXiv


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text:
Books › A Very Stable Genius: @realDonaldTrump
A Very Stable Genius: @realDonaldTrump
Luckovich, Mike
How do you poke fun at a man who's so absurd he practically satirizes himself? Even two-time Pulitzer Prize–winning cartoonist Mike Luckovich admits it's been a challenge covering the Cheeto-in-Chief in his internationally syndicated political cartoons. But Mike rose to the challenge, pulling no punches and stripping down Trump and his cronies with his signature wit and style.
Covering Trump's antics from the 2016 election through to the Mueller investigation, the cartoons in A Very Stable Genius tackle key moments in Trump's political career, offering scathing insights on everything from his disastrous track record with women to his revolving-door cabinet to his suspiciously intimate relationship with a certain Russian leader. Woven through with searing commentary and personal anecdotes, Mike's cartoons will shock and delight you, making you think as much as they make you laugh — when you're not too busy being terrified.
Mike Luckovich is a Seattle native and has worked for the Atlanta Journal-Constitution since 1989. His cartoons are reprinted in newspapers across the country. He won Pulitzer Prizes in 1995 and 2006 for his editorial cartoons and the 2006 Reuben Award, presented by the National Cartoonist Society, for best cartoonist. His previous books include Lotsa Luckovich and Four More Wars!
Dimensions: 8 x 5.75 in.
Paperback - $21.95 CAD ePub - $18.99 CAD Full-Color Ebook Edition - $20.99 CAD PDF - $18.99 CAD Mobi - $18.99 CAD
"The selection of Luckovich's profound cartoons drawn since early 2016 provides a pulse of our current climate . . . Many are funny, plenty are laced with a heavy dose of eeriness, and all convey Luckovich's knack for exaggerating important moments into unforgettable images." — Atlanta Journal-Constitution

redpajama_set_name: RedPajamaCommonCrawl


text:
Appling County High School (formerly known as Appling County Comprehensive High School) is a high school in Baxley, Appling County, Georgia, United States. It is part of the Appling County School District.

It has approximately 1,000 students and 70 teachers in grades 9-12. The students are 66% white, 30% African-American, and 4% Hispanic.  62% of the school's students are eligible for free lunch, above the state average of 50%.

Academics
The average ACT score at Appling County was 18, lower than the Georgia state average of 20 and the national average of 21.

Notable alumni

 Byron Buxton ('12), MLB outfielder for the Minnesota Twins
 Dexter Carter, former professional football player
 Frankie King, NBA guard for Los Angeles Lakers (1995); born in Baxley
 Jamie Nails, NFL guard for Buffalo Bills (1997-2000) and Miami Dolphins (2002-2003); born in Baxley
 Carl Simpson, defensive tackle for Chicago Bears (1993-1997), Arizona Cardinals (1998-1999), and Las Vegas Outlaws (2001)
 Harry Skipper, defensive back in the CFL for seven years; played for the Montreal Concordes and Saskatchewan Roughriders 1983–1989

References

External links

Schools in Appling County, Georgia
Public high schools in Georgia (U.S. state)

redpajama_set_name: RedPajamaWikipedia


Does failure to attend an insurer's examination forbid an accident victim to apply for accident benefits?
The decision of the Licence Appeal Tribunal (LAT) in the case called S.L. v Certas Home and Auto Insurance Company answers the question on whether or not the failure to attend an insurer's examination (IE) forbid an accident victim to apply for accident benefits.
The applicant in this case, S. L., was injured in an accident on July 17, 2011. On September 20, 2011, the applicant submitted three treatments plans to her insurer Certas Home and Auto Insurance Company. On the same date, the applicant also filed for accident benefits with the insurance company.
Between September 29, 2011 to November 29, 2011, Certas notified the applicant to attend four scheduled insurer's examinations (IEs). The applicant refused to attend the scheduled IEs, arguing that the Cantonese interpreter provided by the insurance company was not accredited by the Ministry of the Attorney General. As a result of the applicant's failure to attend the scheduled IEs, the insurance company did not pay the applicant's accident benefits.
Due to the insurance company's failure to pay her accident benefits, the applicant applied for arbitration before the Financial Services Commission of Ontario (FSCO) on November 20, 2013. The applicant later on withdrew her arbitration application. On November 19, 2015, FSCO ordered that the applicant be permitted to withdraw her arbitration application.
On December 14, 2015, the applicant submitted a new treatment plan worth $9,236.48 to Certas – an amount exceeding the Minor Injury Guideline (MIG) limit which was $3,500. For this 2015 treatment plan, the insurance company did not require the applicant to attend an IE. On January 16, 2016 the insurance company denied the applicant's 2015 treatment plan.
As a result of the insurance company's denial, the applicant asked the assistance of the LAT, arguing that that she is entitled to have her dispute be heard before the LAT as the 2015 treatment plan "creates a new and independent obligation on the Insurance Company". The applicant added that she is entitled to have her dispute be heard before the LAT since the insurance company has not requested that she attend an IE for the 2015 treatment plan.
The insurance company, for its part, asked the LAT to prohibit the applicant from claiming accident benefits as she failed to attend the insurer's examinations.
The insurance company must prove that it provided the applicant a notice of an examination in accordance with SABS.
The applicant failed to attend the insurer's examination.
The Tribunal ruled that the dispute regarding the interpreter's qualification was "resolved when the Appellant withdrew her arbitration application to FSCO." The Tribunal added that no decision was made on the merits of the FSCO arbitration application. "Since receiving the December 14, 2015 treatment plan, it remains open to the Insurance Company to serve the appropriate notice for her to attend one or more IEs," the Tribunal added.
The Tribunal ordered that the applicant's accident benefit claim against Certas proceed to hearing.


text:
NavigationLifestyleHealthTravelSocial MediaReligionPress
Sudan: 11 killed in clashes between protesters and security
Uniformed Sudanese soldiers flash the victory sign as they stand among protesters at a demonstration near the military headquarters, Tuesday, April 9, 2019, in the capital Khartoum, Sudan. Activists behind anti-government protests in Sudan say security forces have killed at least seven people, including a military officer, in another attempt to break up the sit-in outside the military headquarters in Khartoum. A spokeswoman for the Sudanese Professionals Association, said clashes erupted again early Tuesday between security forces and protesters who have been camping out in front of the complex in Khartoum since Saturday. (AP Photo)
CAIRO — Clashes between Sudanese security forces and protesters holding a large anti-government sit-in outside the military's headquarters in the capital Khartoum killed at least 11 people including six security forces, the government's spokesman said Wednesday.
Information Minister Hassan Ismail, who also serves as the Sudanese government spokesman, did not give further details on the violence a day earlier.
Sudanese security forces tried again to break up the sit-in, which began over the weekend, killing at least 14 people on Tuesday, activists behind the demonstration said, disputing the government's figure.
Attempts by security forces to break up the sit-in have killed at least 22 since Saturday, including five soldiers who protest organizers said were defending the sit-in.
The demonstration is the latest in nearly four months of anti-government protests that have plunged Sudan into its worst crisis in years. The protests initially erupted last December with demonstrations against a spiraling economy, but quickly escalated into calls for an end to embattled President Omar al-Bashir's 30-year rule.
Sudan's state news agency, meanwhile, said the country's ruling party would hold a rally Thursday in support of al-Bashir in Khartoum. But the party said later that it had canceled the rally for security reasons.
A photo of a woman protester in a traditional white Sudanese dress and golden, moon-shaped earrings went viral on social media, instantly becoming a symbol for the role of women in the uprising against the autocratic leader.
The image drew a comparison to America's Statue of Liberty and the ancient Nubian Sudanese queens known as kandaka who live on in Sudanese folklore as women who accomplished and sacrificed for their country.
Her white dress is traditionally worn by professional Sudanese women in the workforce, said Hammour Ziada, a Sudanese novelist. "The outfit is symbolic of the identity of a working Sudanese woman that's able to do anything and at the same time keep her culture and traditions," he said.
Video circulating online showed the woman, Alaa Salah, singing traditional songs to protesters in the sit-in outside the military's headquarters.
She chanted: "They burned us in the name of religion, killed us in the name of religion, jailed us in the name of religion," while a crowd around her shouted "revolution."
The image was taken by activist Lana Haroun on Monday during the third day of the sit-in outside the military's headquarters. It has since received 55,000 likes and was picked up by Twitter Moments.
The protests against al-Bashir gained momentum last week after Algeria's President Abdelaziz Bouteflika, in power for 20 years, resigned in response to weeks of similar protests.
Saturday's marches marked the 34th anniversary of the overthrow of former President al-Nimeiri in a bloodless coup. It was one of the largest turnouts in the current wave of unrest.
The military removed Nimeiri after a popular uprising in 1985. It quickly handed over power to an elected government. The dysfunctional administration lasted only a few years until al-Bashir — a career army officer — allied with Islamist hard-liners and toppled it in a coup in 1989.
Al-Bashir has banned unauthorized public gatherings and granted sweeping powers to the police since imposing a state of emergency last month, and security forces have used tear gas, rubber bullets, live ammunition and batons against demonstrators.
Security forces have responded to the protest movement with a fierce crackdown, killing dozens of people.
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East Africa's transmittion of information in the region reached an ample improvement when Kenya Data Network (KDN) which was acquired by Liquid Telecom, the region's Fiber Optic Provider announced that it has extended it's fibre network into Tanzania.
KDN will be the first Network Operator to connect a single fibre network in the East African capitals of Kampala, Kigali, Nairobi and Tanzania's Dar es Salaam.
The new cable of 120km will link Nairobi and Namanga on the Tanzania Kenya border and is one of the cables that is going to impact capacity for KDN's clients including government, homes, carriers, Internet Services Providers (ISPs) and businesses of all sizes.
CEO of Liquid Telecom Nic Rudnick said "We believe that technology should be for everyone and completion of the Namanga fiber will be another major milestone in consolidating Liquid's fiber coverage as the widest in Africa and confirming our position as the leading pan-African communications connectivity provider".
The key impact of the network is integration and connecting customers across southern, central and eastern Africa.
Liquid Telecom is involved in several milestone projects to connect the African continent and lower the latency rate by retaining communication traffic in Africa instead of it being routed from South Africa to the rest of Africa via Europe, this will no longer be the case.
Rudnick also said "With the completion of the KDN's Namanga fiber we will provide even more secure and reliable solutions to businesses in Kenya , Tanzania , Uganda , Rwanda and Burundi ," Rudnick said.
"This fiber will improve business opportunities providing more capacity, more routes and higher speeds to fixed and mobile operators, as well as Africa 's leading companies" Rudnick concluded.
As Tanzania approaches a new era in it's economic development, efficient network services will enhance the country's growth and productivity and ensure the transition from low to middle-income status is backed by advanced communications.


Really enjoying the stark simplicity of this work by Matthew Craven. It could be that he's touching on some of our current obsessions, but it's also just badass.
Matthew Craven's dizzying mix of ink patterns, cut-outs and ancient culture is as powerful as it is studied.


A cast of characters from Disney, Marvel and Star Wars is joining forces with the Army & Air Force Exchange Service to bring a special, dedicated section to approximately 60 Exchange locations. The standalone section, called "Disney at the Exchange," includes dolls, action figures, role play items and clothing, as well as toys and other merchandise tied to current Walt Disney Company theatrical releases and television content. Military shoppers will find a wide selection of their favorite Disney characters at both the Exchange and at ShopMyExchange.com at www.shopmyexchange.com.


text:
Twitter reportedly in talks to merge with TikTok
by Peter Heck · Aug 11th, 2020 10:12 am
Following President Trump's recent announcement that social media platform TikTok will have to close down U.S. operations by September 15 due to its affiliation with the Chinese communist government, Twitter has reportedly expressed interest in merging with the company.
The president had previously blasted TikTok, forbidding any American company from doing business with them.
"TikTok automatically captures vast swaths of information from its users, including Internet and other network activity information such as location data and browsing and search histories," Trump wrote in the executive order banning the app. "This data collection threatens to allow the Chinese Communist Party access to Americans' personal and proprietary information — potentially allowing China to track the locations of Federal employees and contractors, build dossiers of personal information for blackmail, and conduct corporate espionage."
It was not immediately clear how a merger with Twitter would affect the efficacy of the TikTok ban.
? Microsoft has also been in talks with the video-sharing platform.
Virginia couple, married 70 years, dies within minutes of one another: "I'm not gonna let him go alone"
Chief resigns after Seattle City Council approves $3 million cut to police budget, elimination of 100 officers


text:
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Each year, part of his free time is dedicated to his personal self education and journey, family, and friends. He also believes in helping the community and participating in various charity fund raising events.
To read more about any of his services on offer click the appropriate link: Life Coaching, Business Coaching or Executive Coaching, and Healing.
TO GET IN TOUCH
E-mail: tony@thevelvetjourney.com
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2013 © The Velvet Journey


Our luxurious cow hide bag FRAN has it all: Style and Room. Made entirely from brown & white hide this tote bag will serve you in all situations.
Click the button below to add the FRAN Luxurious Bag in Brown & White Cowhide to your wish list.


RFL Respect Barriers : Touchline Logos | FA, RFL, FAI Approved Respect Zone Touchline Barriers, We are the only approved supplier to the FA, RFL and FAI for Touchline Respect Zone Barriers.
Thanks to their passively safe, light weight and reliable design the new RFL Respect Barriers based on our original Logopost design first pioneered in 2006 have now replaced the old style "Tape" RFL Respect Barriers of the past and as such are now the preferred and only barriers to be approved and endorsed by the RFL for its ongoing Respect programme.
The new barriers come in easy to use and easy to carry sets and have been specifically designed to suit all pitch sizes and age groups.
Ideally suited for both soft and firm ground, the barriers can also cope with all weather conditions including the strongest of match day winds.


Are you a fan of hospital drama shows? Children's Hospital isn't your traditional hospital drama show. It's a comedic parody. Most of the doctors (particularly Owen and Ritchie) act like children. Just because they act like children, I don't really think this is quite a child friendly show. The complete third season of Children's Hospital is now available on DVD. If you're interested in the DVD, you can find it in the WBShop. Season Four is also about to begin!
Have ever acted like a child in an embarrassing activity or just for fun? Maybe you were trying to make up for a missed opportunity as a child or maybe you were doing it just for fun (there's nothing wrong with that.) With three kids, I always do random weird things and it's usually just to keep them entertained. The other day, I jumped on the ride outside of the grocery store just to make my two year old laugh. We went to Funderland Park in Sacramento, CA last week and I rode a water log all by myself because I was so close to the weight limit. I totally did that to fulfill some child-like need.
Is there something embarrassing or very child-like that you did to make up for a missed opportunity or just for the fun of it?
Filed Under: Promotions Tagged With: Comedy, Television, Warner Bros.


Shunned from London society for being the daughter of England's most notorious spy, Alyce Hythe desires only to clear her father's name. For years, she has been hidden away from all prying eyes, given a new identity and told to forget who she was. But strange things have been happening causing old rumors to once more be whispered.
Long has Lord Julian Casvelyn lived with guilt brought on when his brother was murdered by England's most infamous traitor. But one eventful night has changed everything Lord Julian believed about his brother's death. Never did he suspect the woman he has just saved from certain harm is the daughter of that man. Now Julian is caught in midst of a conspiracy and desire for that woman. Thrown together by fate, the two search for answers long denied them and along the way discover a love that can free them both.
This entry was posted in Amazon, Best Selling Author, Bestselling Series, Books, Free ebook, Romance Books, Romantic Picks, Romantic Suspense, Western Romance and tagged Colleen Connally, Indie Author, Indie Book, Seductive Secrets. Bookmark the permalink.


The ACUVUE disposable contact lens from Johnson & Johnson is thin and comfortable. Because it is made of a highly oxygen permeable material and is replaced frequently, ACUVUE is healthier for your eyes than many other contact lenses. It is approved for monovision fitting, and, like all ACUVUE lenses, it contains UV blocker. Acuvue recommends these lenses to people who want to wear contact lenses night and day. Original Acuvue contact lenses are a flexible wear lens and can be worn up to two weeks when removed at night. Eye care practitioners provide a schedule when they issue a prescription. This lens offers UV Blocking, visibility tint, and an inside out mark. This is a very reasonably priced two week contact lens. Acuvue manufacturer rebates are usually available for 12 boxes, which should cover 3 months use depending on eye practitioner wear schedules. Online coupons are available for further Oasys savings.
AClens reviewers point out that even though this is an Acuvue original contact lens, they don't see the need to change to later model lenses. They are quite happy with current comfort and vision performance. Lens.com reviewers report similar sentiments and say they have been using these lenses for quite a long time and are very happy with them.


text:
package com.sartor.javaee.daos;

import java.util.List;
import javax.persistence.EntityManager;
import javax.persistence.PersistenceContext;
import javax.persistence.TypedQuery;
import javax.persistence.criteria.CriteriaBuilder;
import javax.persistence.criteria.CriteriaQuery;
import javax.persistence.criteria.Root;

/**
 *
 * @author Rodrigo de Bona Sartor
 * @param <T> DB Entity class
 * @param <P> Primary key type
 */
public abstract class BaseDao<T, P> {

  @PersistenceContext( unitName = "SAMPLE_PU" ) // Unit name from persistence.xml
  private EntityManager em;

  private final Class<T> entityClass;

  public BaseDao( Class<T> entityClass ) {
    this.entityClass = entityClass;
  }

  public void create( T entity ) {
    this.em.persist( entity );
  }

  public void edit( T entity ) {
    this.em.merge( entity );
  }

  public void remove( T entity ) {
    this.em.remove( this.em.merge( entity ) );
  }

  /**
   *
   * @param id
   * @return If id exists return an instance of T, else return null
   */
  public T find( P id ) {
    return this.em.find( this.entityClass, id );
  }

  /**
   *
   * @return List with all the results, if there is no result returns an empty list
   */
  public List<T> findAll() {
    return findAll( 0, 0 );
  }

  /**
   *
   * @param qtyByPage How many rows it will fetch, if qtyByPage is equals or less than zero it will fetch all rows
   * @param page Page number of the fetch starting from one, if page is equals or less than zero it will fetch all rows
   * @return List with all the results, if there is no result returns an empty list
   */
  public List<T> findAll( int qtyByPage, int page ) {
    CriteriaBuilder cb = this.em.getCriteriaBuilder();
    CriteriaQuery cq = cb.createQuery();
    Root rootSelect = cq.from( this.entityClass );
    cq.select( rootSelect );
    return findAll( cq, qtyByPage, page );
  }

  /**
   *
   * @param cq CriteriaQuery
   * @param qtyByPage How many rows it will fetch, if qtyByPage is equals or less than zero it will fetch all rows
   * @param page Page number of the fetch starting from one, if page is equals or less than zero it will fetch all rows
   * @return List with all the results, if there is no result returns an empty list
   */
  protected List<T> findAll( CriteriaQuery cq, int qtyByPage, int page ) {
    TypedQuery query = this.em.createQuery( cq );
    if ( qtyByPage > 0 && page > 0 ) {
      int first = (qtyByPage * page) - qtyByPage;
      query.setFirstResult( first );
      query.setMaxResults( qtyByPage );
    }
    return query.getResultList();
  }

  /**
   *
   * @return Row count
   */
  public int count() {
    CriteriaBuilder cb = this.em.getCriteriaBuilder();
    CriteriaQuery cq = cb.createQuery();
    Root rootSelect = cq.from( this.entityClass );
    cq.select( cb.count( rootSelect ) );
    javax.persistence.Query q = this.em.createQuery( cq );
    return ((Long) q.getSingleResult()).intValue();
  }

}

redpajama_set_name: RedPajamaGithub


text:
CBS Sunday Morning on July 6, 2014
Charles Osgood introduced the stories for July 6, 2014. The headlines began with the US State Department protesting the beating of an American boy [Tariq Khdeir ]. There was online video of the head of ISIS [Abu Bakr al-Baghdadi; aka Caliph Ibrahim ]. The Ukrainian flag raised in Slovyansk, Ukraine [ The Ukrainian flag was raised Saturday over Slovyansk and Kramatorsk, ] Weather: sunny and warm in northeast.
The piece on Louis Zamperini was a recycle of previous presentations. CBS Sunday Morning on May 27, 2012 and CBS Sunday Morning on August 12, 2012 . Zamperini died at age 97. There was a mention of a 1998 story by Bob Simon.
Almanac was on the arrest of Captain Kidd on July 6, 1699 in Boston. He would be executed May 23, 1701.
The piece by Faith Salie on kitchen magnets was a recycle from CBS Sunday Morning on June 9, 2013
Anthony Mason interviews Robin Thicke on "Blurred Lines." Thicke's album Paula is a 14 song apology, in which he begs his former wife [Paula Patton] to come back. Robin put out his first solo album in 2002. "Lost Without You." The video "Paula" includes text messages between Robin and Paula. Vultures tweet.
16 million American viewers for World Cup. Alexandra Pride opinion piece on the World Cup. Soccer is something you can teach a three year old to do badly. We are supposed to get involve in conflicts we can win.
Wynton Marsalis. Barbeque in Lockhart, Texas. Smokestack Lightning. "Texas Monthly." Black's Barbeque.
Low and slow cooking. Index: Charcoal grill preferred by 58%.
Steve Hartman on Presidio, Texas. Sheila Condido, teacher, who ran the rocket club. Previous story by Hartman in 2012. "Aerospace teacher of the year." Goat auctions. Last fall, letter telling her to depart. Texas Congressman, Pete Gallego looked into it. Letter was supposed to be a green card.
Zach Braff profiled by Tracy Smith. Bullets over Broadway. Garden State. Zach's dad was an attorney.
Manhattan Murder Mystery. Scrubs. "Wish I was Here." kickstarter.com.
Mo Rocca talks to George Will about the Chicago Cubs. The Cubs have not won the World Series since 1908, two years before Mark Twain died. Wrigley Field. Will saw Cubs play the Dodgers in 1950. Will played Little League: Mittendorf Funeral Home Panthers. Wrigley Field opened in 1914. Friendly Confines. Ladies Day: come in free. Attendance correlates with beer price. If you're not sober when you come in, you will be when you leave.
Next week: July 7: running of the bulls in Pamplona. July 8: Elvis Presley, That's all right. July 9: Raul Wallenburg. July 10: Emmy naming July 11: 100th anniversary of Babe Ruth's debut, as a pitcher.
Boyhood. David Edelstein. Time is the story. 7 year old. Before Sunrise. Before Sunset.
Snowpiercer endorsed by Edelstein.
Next week: Sunday at the shore.
Moment of nature. Caprock Canyon State Park in Texas, home of state bison heard.
850 Caprock Canyon Park Road, Quitaque, TX 79255
Communication among robots, and bacteria
Mapping biofuel potential, incompletely?
First copyrighted map of the US?
Fifty years of "James Bond" legal fighting ended i...
Koh says noh to saying "troll"
Challenge to AIA fails in Madstad
Abbvie loses on "written description" grounds
Kinetic Concepts [KCI] and Wake Forest settle vacu...
Attribution of CNN news stories: take it and make...
SnoWizard loses in snoball case


text:
Psychic 'hole' crying out to be filled | Inquirer Entertainment
entertainment / Columns
Psychic 'hole' crying out to be filled
By: Nestor U. Torre
Philippine Daily Inquirer / 12:46 AM July 24, 2016
Our continuing quest for TV shows that inspire and edify (as opposed to the "dumbing down" variety) has produced a fine, new find in "Last Hope with Troy Dunn."
The program host has made it his lifelong advocacy to reunite adopted children with their birth mothers—an often difficult, complicated and frustrating task, given the secrecy surrounding the adoption process.
But, Troy Dunn knows that the search for one's real roots and identity is an all-important and self-defining priority for the "searchers" and "questors" involved.
So, he and his team doggedly pursue even the faintest and murkiest tip to effect and complete the reunification cycle.
The telecast we viewed of "Last Hope" focused on a young man who was given up for adoption in early childhood, and ended up with a loving adoptive family.
He was grateful for his good fortune, but when he became a teenager, he realized that despite his adoptive parents' love and care, he still had this "hole" in his psyche that cried out to be filled.
On his own, he did what he could to find his birth mother, but kept getting frustrated as lead after lead fizzled out.
Finally, he reached out to Dunn's show for help, and the program host saw how much it meant to the questor, so he decided to make it a personal mission to provide the answer he so desperately needed to get.
Dunn worked really hard on "Jacob's" case—and was overjoyed when he was finally able to get the long-missing birth mother's most recent address and phone number.
However, the long-yearned-for reunion was not to be—because Jacob's mother had passed away six years ago.
Now, Dunn's problem was having to give him the sad news—and Jacob took it really badly, as expected.
But, after he mourned the death of the woman who had given birth to him (whom he'd even more sadly never even met), Dunn revealed that all was not lost, because his birth mother had had other children after him.
So, he "suddenly" had a brother and sister—and they were just waiting for him to meet them!
The change in Jacob's feelings was instantaneous: From being "all alone" in the world, he now had an "instant" family to possibly share his sorrows and joys with!
So, the longed-for reunion did take place, in a different but also psychically consoling form!
More realistically, however, Jacob's perception of his long-absent mother ended up being altered, because his newfound siblings revealed to him that she was not the "angel" that he had imagined and idealized her to be for so many years.
Yes, she loved them—but she also had a mental problem that caused her to be viciously cruel to them from time to time.
Well, that's life—you have to take the bad with the good, "win some, lose some."
But, Jacob was still grateful to "Last Hope with Troy Dunn" for helping fill the "hole" in his psyche.
For our part, we appreciate the show's selfless determination to help bring families together again, years or even decades after they were torn apart.
We've seen some local TV shows or portions of programs do the same, so we honor and celebrate them, as well.
Carlo Obispo's '1-2-3- opens 12th Cinemalaya
TAGS: Last Hope with Troy Dunn, psychic, TV


text:
Telangana unemployed rally to demand jobs
A rally of unemployed youth and students here on Monday demanded the Telangana government to immediately fill the vacancies even as two students ended their lives since Sunday reportedly after failing to get jobs.
Speakers at the "Koluvula Kotlaata" (Fight for jobs) rally, organised by Telangana Joint Action Committee (TJAC), appealed to students and unemployed youth not to resort to suicide but unite for a struggle to force the government to honour its promise.
TJAC chairman M. Kodandaram alleged that police tried to foil the meet by arresting several leaders and workers coming to Hyderabad from different parts of the state, though the court had give permission for the meet.
While one student of Osmania University hanged himself in the hostel, another unemployed youth killed himself in Nirmal district on Sunday.
E. Murali, 21, a first-year student of MSc Physics at Osmania University here ended his life in bathroom on Sunday. The incident, the first after formation of Telangana state, triggered protest by students.
According to police, a suicide note was found in the pocket of Murali in which he stated that he was taking the extreme step due to depression and the fear of failing in exams. However, student groups alleged that the letter was forged and claimed that he was depressed due to government not releasing the job notification.
Tension prevailed on the campus as students refused to hand over the body to police, demanding the government to first announces a job and Rs 50 lakh compensation for Murali's family. Police broke open the doors of a hostel room in the early hours of Monday to forcibly shift the body for autopsy and later to his native place.
However, the campus remained tense through the day as students staged protest and boycotted the classes.
When the TJAC meeting was on, report came in from Nirmal district that an unemployed youth committed suicide. B. Ramesh, who had done MSc, was reportedly depressed on not getting a job.
At the meeting, TJAC presented before people family members of four youth who committed suicide recently.
Kodandaram, who had played a key role in the movement for separate Telangana state, alleged that the government had failed to fulfill the promise to provide jobs and this had led to frustration among youth.
He demanded that the government take steps on war-footing to fill 3 lakh vacancies. He said instead of addressing the issue, ruling Telangana Rashtra Samithi (TRS) was branding them politically unemployed. "This is not Telangana which we had fought and the martyrs laid down their lives for," he said.
Revolutionary balladeer Gaddar urged students to come together and become a political force.
Eminent academician Chukka Ramaiah found fault with the government for creating hurdles for organizations fighting for the rights of students and unemployed.
Telugu Desam Party's state president L. Ramna called for a united struggle to pressurize the government to fulfill its promises. - IANS


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Blunt continues to work with Matrix on advertising campaigns and brand-extension initiatives.