text:
\section{Introduction}
One of the most fascinating mysteries in modern Cosmology is the phenomenology of primordial Universe.
The inflationary paradigm provides the most effective way to describe the dynamics of primordial era of our Universe, solving many discrepancies of standard Big Bang cosmological model such as the horizon and flatness problem, the initial entropy problem and the explanation for the non-existence of magnetic monopoles.
According to inflationary mechanism the early Universe expanded with an accelerating rate. In the simplest case, a scalar field, corresponding to the quasi de-Sitter expansion, slowly rolls down the potential \cite{Guth:1980zm}.

An alternative approach of this theory is the kinetically driven inflation(k-inflation),
which was first introduced by Mukhanov, Damour and Armendariz-Picon \cite{Armendariz-Picon:1999hyi}. According to this pioneer work, the inflaton may involve higher-order kinetic terms, for instance non-quadratic. Furthermore, accelerating expansion can be achieved with or without the existence of scalar potential. Even though the observational constraints of inflation become more accurate the recent years, the effective Lagrangian of inflation has not been specified by the data until today. Based on the effective field theory of inflation \cite{Cheung:2007st}, the Primordial era of our Universe can be described in the context of a generalized way in classical Einstein's gravity with the presence of quantum fluctuations around a quasi de Sitter background.
According to this reasoning, inflationary era dates in between the classical era and the
quantum era where all fundamental forces were unified and the Universe was governed by a quantum theory of gravity. It is reasonable to consider that the effective Lagrangian may involves higher gravitational terms like $f(R)$ gravitational terms \cite{Nojiri:2017ncd,Capozziello:2011et,Capozziello:2010zz,Nojiri:2006ri,Nojiri:2010wj,Olmo:2011uz,Venikoudis:2021irr} and also Chern-Simons terms \cite{Venikoudis:2021oee,Nojiri:2020pqr,Nojiri:2019nar,Odintsov:2019evb,Odintsov:2019mlf,Alexander:2009tp,Qiao:2019hkz,Nishizawa:2018srh,Wagle:2018tyk,Yagi:2012vf,Yagi:2012ya,Molina:2010fb,Izaurieta:2009hz,Smith:2007jm,Konno:2009kg,Sopuerta:2009iy,Matschull:1999he,Haghani:2017yjk}. In this work we focused on the impact of Chern-Simons corrections on the inflationary phenomenology and the primordial gravitational waves which can be produced. Specifically, the existence of Chern-Simons term in Lagrangian does not affect the background equations and the scalar spectral index of primordial curvature perturbations, but it has strong impact on tensor perturbations of a given theory.
We shall also investigate whether is possible the tensor spectral index to be shifted to the blue \cite{Camerini:2008mj}. Primordial gravitational waves with blue tensor spectral index have not been detected yet, but if this happen, then the existence of Chern-Simons term in the effective Lagrangian of inflation might be involved. In addition, based on Huang and Noh paper \cite{Hwang:2005hb} the Chern-Simons parity violating term leads to asymmetric generation and evolution of two circular polarization states of gravitational waves.

K-essence models provide  an attractive class of inflationary  models to be examined, as they generate results compatible with observational constraints
see, Ref.\cite{Nojiri:2019dqc,Oikonomou:2019muq,Mohammadi:2019qeu,Myrzakul:2016ets,Sebastiani:2016ojm,Rahmati:2014cwa,Saitou:2011hv,Nojiri:2010aj,Arroja:2010wy,Bose:2008ew}.
In this project it is assumed that the k-essence scalar field is minimally coupled with the scalar curvature and involves a higher order and a linear kinetic term. Firstly, the theoretical framework of k-essence overall phenomenology is presented for the purpose of examining the impact of Chern-Simons term in dynamics of inflation. Furthermore, the observational indices are presented in order to ascertain the viability of models. The first proposed model involves a power-law scalar potential and an exponential scalar Chern-Simons coupling function while the second involves a trigonometric potential and a power-law scalar Chern-Simons coupling function. Both models admit a quadratic noncanonical kinetic term.

Apart from k-essence models, there is another class of scalar fields which produce viable kinetically driven inflation namely Dirac-Born-Infeld scalar field. These fields arise from quantum theories of gravity such as string theory. Based on string theory the relativistic motion of a D3 brane in a higher dimensional warped spacetime generates D-brane inflation with Dirac-Born-Infleld scalar kinetic term, see Ref.\cite{ Nguyen:2021emx,Yang:2021enz,Motaharfar:2021egj,Chakraborty:2020kjy,Chen:2020uhe,Rashidi:2020wwg,Nozari:2019esz,Seo:2018abc,Mohammadi:2018zkf,Lahiri:2018erp,Nazavari:2016yaa,Bielleman:2016grv,Nozari:2013wua,Zhang:2013asa,Koehn:2012np,Miranda:2012rm,Weller:2011ey,Chimento:2010un,Franche:2010yj,Bessada:2009pe,Arroja:2009pd,Langlois:2008wt,Bean:2007eh,Lidsey:2007gq,Spalinski:2007dv,Spalinski:2007qy,Spalinski:2007un,Kecskemeti:2006cg,Chen:2005fe}. In this paper we shall examine the phenomenology considering that during inflationary era the scalar potential remains constant for simplicity.

\section{INFLATIONARY PHENOMENOLOGY OF K-ESSENCE MODELS IN EINSTEIN-CHERN-SIMONS GRAVITY}
The k-essence inflationary models can be described in the context of $f(R,\phi,X)$ class of theories where, R denotes the Ricci scalar, $\phi$ stands for the scalar field with X being $X=\frac{1}{2}\nabla^{\mu} \phi \nabla_{\mu}\phi$. The proposed gravitational action during the inflationary era includes the k-essence scalar field in the presence of Chern-Simons term and can be defined as,
\begin{equation}
\centering
\label{action}
S=\int {d^4x\sqrt{-g}\left[\frac{f(R,\phi,X)}{2}+ \frac{1}{8}\nu(\phi)R\Tilde{R}\right]},
\end{equation}
where $g$ is the determinant of the metric tensor and $\nu(\phi)$ is the Chern-Simons scalar coupling function. The Chern-Simons term represents parity violation in gravity and it is given by the expression  $R\Tilde{R}=\epsilon^{a bcd}R^{\ \ e f}_{a b}R_{cdef}$ where, $\epsilon^{abcd}$ is the totally antisymmetric Levi-Civita tensor in 4-dimensions. The line-element is assumed to have the
Friedmann-Robertson-Walker form,
\begin{equation}
\centering
\label{metric}
ds^2=-dt^2+a(t)^2\delta_{ij}dx^idx^j,\,
\end{equation}
where $a(t)$ is the scale factor of the Universe and the metric tensor has the form of $g_{\mu\nu}=diag(-1, a(t)^2, a(t)^2, a(t)^2)$. It is both sensible and convenient to assume that the scalar field participating in the aforementioned gravitational action is homogeneous, or in other words only time dependent. In consequence the kinetic term, which is of paramount importance in the k-essence model can be simplified as $X=-\frac{1}{2}\dot\phi^2$, where the dot as usual implies differentiation with respect to cosmic time $t$.
Additionally, the general form of the $f(R,\phi,X)$ function can be considered as,
\begin{equation}
\centering
\label{f}
f(R,\phi,X)=\frac{R}{\kappa^2}-2\alpha X^m-2\alpha_0 X-2V(\phi),
\end{equation}
where $\kappa=\frac{1}{M_P}$ is the gravitational constant while, $M_P$ denotes the reduced Planck mass, and $V(\phi)$ is the scalar potential. Note that in the present form, the auxiliary parameters introduced, in particular $\alpha_0$ and $\alpha$ must have proper dimensions. In particular, while the first is to be considered as dimensionless with possible values of $0,\pm1$, with $-1$ specifying phantom scalar field, the latter must have mass dimensions of eV$^{4-4m}$ for consistency. Hereafter, parameter $\alpha_0$ shall be assumed to be equal to unity, unless stated otherwise however it is presented in subsequent equations as free parameters for the sake of generality. In addition, parameter $m$ is to be replaced with $m=2$ in the following k-essence toy models however in order to be inclusive the general case for an arbitrary exponent $m$ is showcased. Finally, as long as the metric is flat, the Ricci scalar term is topological invariant and can be written as $R=12H^2+6\dot H$ where $H$ is Hubble's parameter and in addition, the ``dot'' denotes differentiation with respect to the cosmic time. Let us now proceed to the proper phenomenology of the inflationary era.

The equations of motion for the theory can be derived by implementing the variational principle in the gravitational action (\ref{action}) with respect to the metric tensor and the scalar field separately which read,
\begin{equation}
\centering
\label{motion1}
3H^2F=f_{,X}X+\frac{FR-f}{2}-3H\dot F,\,
\end{equation}
\begin{equation}
\centering
\label{motion2}
-2\dot H F=f_{,X}X+\Ddot{F}-H\dot F,\,
\end{equation}
\begin{equation}
\centering
\label{motion3}
\frac{1}{\alpha^3}\frac{d}{dt}(\alpha^3 \dot \phi f_{,X})+f_{,\phi}=0 \
\end{equation}
where $F=\frac{\partial f}{\partial R}$ represents the partial derivative with respect to the Ricci scalar while, $f_{,X}=\frac{\partial f}{\partial X}$, $f_{,XX}=\frac{\partial f_{,X}}{\partial X}$ and finally $f_{,\phi}=\frac{\partial f}{\partial\phi}$. The first describes the Friedmann equation or the temporal component of the field equations, the second being the Raychadhuri equation and the third stands for the continuity equation of the scalar field or in other words the Klein-Gordon equation for an expanding background. In essence, the Klein-Gordon equation for the aforementioned model is quite nontrivial due to the additional noncanonical kinetic term. Substituting Eq.$(\ref{f})$ into the equations of motion the resulting equations are,
\begin{equation}
\centering
\label{motion11}
\frac{3H^2}{\kappa^2}=-\alpha_0 X-\alpha X^m(2m-1)+V(\phi),\,
\end{equation}
\begin{equation}
\centering
\label{motion22}
\frac{\dot H }{\kappa^2}=\alpha_0X+\alpha m X^m,\,
\end{equation}
\begin{equation}
\centering
\label{motion33}
\Ddot{\phi}[\alpha_0+\alpha m(2m-1)X^{m-1}]+3H\dot \phi(\alpha_0+\alpha m X^{m-1})+V'=0\
\end{equation}
where the prime denotes differentiation with respect to the scalar field $\phi$. Obviously, the resulting system of equations is perplexed to be solved with an analytic way. On account of this, the slow-roll approximations are imposed as long as inflation last. Specifically, the following approximations are considered to hold true,
\begin{align}
\label{approx}
\centering
\dot H&\ll H^2,& \mid \alpha_0 X+\alpha m X^m \mid&\ll V,& \ddot\phi\ll3 H\dot\phi,\
\end{align}
therefore, the equations of motion can be simplified greatly. In the following sections it is proved numerically that indeed these conditions are in effect for the presented models. The simplified equations are,
\begin{equation}
\centering
\label{motion11}
H^2\simeq\frac{\kappa^2V}{3},\,
\end{equation}
\begin{equation}
\centering
\label{motion33}
3H\dot \phi(\alpha_0+\alpha m X^{m-1})+V'\simeq 0,\
\end{equation}
while Eq.(\ref{motion22}) remains the same and carries the impact of the k-essence term. Considering $m=2$ for simplicity as expressed previously and substituting the kinetic term X into the continuity equation for the k-essence field, Eq.(\ref{motion33}) reduced to the simple form,
\begin{equation}
\centering
\label{scalar}
3H \dot \phi(\alpha_0-\alpha \dot \phi^2)+V' \simeq 0,
\end{equation}
where the quadratic term of the derivative of the scalar field with respect to cosmic time is negligible compared to $\dot \phi$. One can easily obtain the expression of the time derivative of the scalar field as,
\begin{equation}
\centering
\label{fdot}
\dot \phi \simeq -\frac{V'}{3H\alpha_0}.
\end{equation}
The dynamics of inflation in the context of $f(R, \phi, X)$ gravity is described in terms of the slow-roll parameters based on Huang and Noh paper \cite{Hwang:2005hb} as,
\begin{align}
\centering \epsilon_1&=-\frac{\dot
H}{H^2},&\epsilon_2&=\frac{\ddot\phi}{H\dot\phi},&\epsilon_3&=\frac{\dot E}{2HE},&\epsilon_4&=\sum_{L,R}\frac{\dot Q_t}{2HQ_t},
\end{align}
where summation over $L$ and $R$ implies summation over left and right handed polarization of gravitational waves.
During the first horizon crossing, the
parameter $Q_{tCS}$ is defined as,
\begin{equation}
 Q_{t_{CS}}=F+2\lambda_l\dot \nu H.\
\end{equation}
 Such auxiliary functions are important for studying the behavior of the gravitational wave modes. The analysis has already been performed in \cite{Hwang:2005hb}.
Finally, the parameter E which is given by the following expression,
\begin{equation}
E=-\frac{F}{2 X}\left(X f,_X+2X^2 f,_{XX}\right),
\end{equation}
is reduced to the form,
\begin{equation}
\centering
E=\frac{1}{\kappa^2}\left(\alpha_0+\alpha m(2m-1)X^{m-1}\right).
\end{equation}
The slow-roll indices for unspecified scalar potential and Chern-Simons scalar coupling function are given by the following expressions,
\begin{equation}
\label{e1k}
\centering
\epsilon_1 \simeq  \frac{V'^{2}}{ \alpha_0 \kappa^2 V^2}(\frac{1}{2}-\frac{\alpha V'^{2} }{7\kappa^2 \alpha_0^3 V}) ,
\end{equation}
\begin{equation}
\label{e2k}
\centering
\epsilon_2\simeq \epsilon_1-\frac{V''}{\kappa^2 V},
\end{equation}
\begin{equation}
\label{e3k}
\centering
\epsilon_3\simeq \frac{\alpha V'^{2}(2VV''-V'^{2})}{2\kappa^2 V^2(\alpha_0^4 \kappa^2 V-\alpha_0 \alpha V'^{2})},
\end{equation}
\begin{equation}
\label{e4k}
\centering
\epsilon_4\simeq \frac{4\kappa^2 \nu' V'^{2}(V'\nu''+\nu'V'')}{\alpha_0 V(9\alpha_0^2-4\kappa^4 \nu'^{2}V'^{2})} .
\end{equation}
The involvement of Chern-Simons quantum corrections affects only the index $\epsilon_4$ and in consequence only the tensor observed indices presented in the following section.

\section{Compatibility of INFLATIONARY MODELS WITH THE LATEST PLACK DATA}
At this point it is worth to be mentioned that Cosmology is at a phase where the observational constraints needs to be explained theoretically. Thus, our goal is to speculate and fit the parameters of the aforementioned theory in order to produce results compatible with the latest Planck data \cite{Planck:2018jri} and consequently viable. In this section we propose models which are consistent with the observations. Firstly, in Einstein-Chern-Simons gravitational theory according to Ref. \cite{Hwang:2005hb} we shall evaluate the following observational quantities, namely the scalar spectral index of primordial curvature perturbations $n_\mathcal{S}$, the tensor-to-scalar-ratio $r$ and finally, the tensor spectral
index $n_\mathcal{T}$. The observational indices are strongly related with the slow-roll indices which described by the Eq.(\ref{e1k}-\ref{e4k}),
\begin{align}
\label{observed}
\centering
n_s&=1-2\frac{2\epsilon_1+\epsilon_2+\epsilon_3}{1-\epsilon_1},&n_T&=-2\frac{\epsilon_1+\epsilon_4}{1-\epsilon_1},&r&=8|\epsilon_1|\sum_{\lambda=L,R}\left|\frac{1}{\kappa^2Q_t}\right|c_A,
\end{align}
where $c_A$ stands for the field propagation velocity defined as,
\begin{equation}
\centering
\label{soundwave}
c_A^2=\frac{f_{,X}}{f_{,X}+2Xf_{,XX}}.\,
\end{equation}
The sound wave velocity for k-essence models is reduced to the following form,
\begin{equation}
\centering
c_A^2=\frac{a_0X+\alpha mX^m}{a_0X+(2m-1)\alpha mX^m}.
\end{equation}
Considering the latest Planck observational data \cite{Planck:2018jri}, the spectral index of the primordial curvature perturbations takes the value $n_\mathcal{S}=0.9649\pm 0.0042 $
with $67\%$ C.L and the tensor-to-scalar-ratio r must be $r<0.064$ with $95\%$ C.L. Last but not least, the tensor spectral index has yet to be observed. Consequently, in the near future a positive tilted tensor spectral index may be observed by LISA or NANOGrav rectifying blue gravitational waves compatible with Einstein-Chern-Simons gravitational theory with exotic kinetic terms. At this stage we shall present the methodology to evaluate the observational
indices during the first horizon crossing.
A convenient way to evaluate the observational indices is to use the initial and the final values of the scalar field instead of use wavenumbers. First of all, the evaluation of the final value of the scalar field is necessary. The final value of the scalar field can be derived by equating the first slow-roll index
$\epsilon_1$ in equation (\ref{e1k}) to unity. As a result, the initial value can be evaluated from the $e$-folding number, which defined as
$N=\int_{t_i}^{t_f}{Hdt}=\int_{\phi_i}^{\phi_f}{\frac{H}{\dot\phi}d\phi}$,
where the difference $t_f-t_i$ signifies the duration of the
inflationary era. Recalling the definition of $\dot\phi$ in Eq.
(\ref{fdot}), one finds that the proper relation from which the
initial value of the scalar field can be derived is,
\begin{equation}
\centering
\label{efolds1}
N=-\int_{\phi_i}^{\phi_f}\frac{3H^2\alpha_0}{V'}d\phi.\,
\end{equation}
As it stands, the present phenomenology is only valid for the case of $\alpha_0=\pm1$ and not for the purely noncanonical case of $f(R,\phi,X)\sim-a X^m$ corresponding to $\alpha_0=0$. In such a scenario the expression of $\dot\phi$ and in consequence the e-folding number are altered. Such model, although plausible, is not studied in the present article. Note also that an extra non minimal coupling between the scalar field and the Ricci scalar should alter the overall phenomenology as well. Although it is not a difficult task to study such model, the overall number of degrees of freedom increase therefore we refrain from including such extra coupling between the scalar field and curvature.

In the following subsections two toy models are presented in order to ascertain the compatibility of such theory. As it turns out, the Chern-Simons scalar coupling function $\nu(\phi)$ can be chosen such that a blue tilted tensor spectral index can indeed be generated. Essentially this is the main difference between the pure k-essence model and the augmented by the Chern-Simons term. Let us now proceed with the subsequent models.

\subsection{Model with quadratic scalar potential}
The first proposed model involves a  slow rolling scalar field in a potential with quadratic form,
\begin{equation}
\centering
\label{pot}
V(\phi)=\lambda\left(\frac{\phi}{\kappa}\right)^2.
\end{equation}
The Chern-Simons scalar coupling function is considered to be an exponential function of the form,
\begin{equation}
\centering
\nu(\phi)=e^{-\gamma \kappa \phi},
\end{equation}
where $\gamma$ is a dimensionless parameter.
The slow-roll parameters of the model are given by the following expressions,
\begin{equation}
\centering
\epsilon_1\simeq \frac{2\alpha_0^3 \kappa^4-2.6  \alpha \lambda}{\alpha_0^4 \kappa^8 \phi^2},
\end{equation}
\begin{equation}
\centering
\epsilon_2\simeq \frac{2\kappa^4 \alpha_0^3(1-\alpha_0)-2.6\alpha \lambda }{\alpha_0^4 \kappa^8 \phi^2},
\end{equation}
\begin{equation}
\centering
\epsilon_3=0,
\end{equation}
\begin{equation}
\centering
\epsilon_4\simeq \frac{32 \gamma ^2 \lambda^2 (\gamma  \kappa  \phi -1)}{16 \alpha_0  \lambda^2 \gamma ^2 \kappa ^2  \phi ^2-9 \alpha_0^3 e^{2 \gamma  \kappa  \phi }}.
\end{equation}
The value of the k-essence field at the end of the inflationary era is derived setting the first slow-roll index into unity and therefore it reads,
\begin{equation}
\centering
\label{phif}
\phi_f\simeq\frac{\sqrt{2\alpha_0^3\kappa^4-2.6\alpha \lambda}}{\alpha_0^2\kappa^3}.
\end{equation}
Considering the form of the e-folding number in Eq.(\ref{efolds1}), the initial value of the scalar field is extracted and subsequently
the observed quantities. The initial value reads,
\begin{equation}
\centering
\label{phii}
\phi_i\simeq \frac{\sqrt{2\alpha_0^3\kappa^4(1+2N)-2.6\alpha \lambda}}{\alpha_0^{1/2}\kappa}.
\end{equation}
\begin{figure}[t!]
\centering
\label{plot1}
\includegraphics[width=17pc]{1ns.eps}
\includegraphics[width=3pc]{1nsdata.eps}
\includegraphics[width=17pc]{1r.eps}
\includegraphics[width=2.65pc]{1rdata.eps}
\caption{Contour plots of the spectral index of primordial
curvature perturbations (left) and the tensor-to-scalar ratio
(right) depending on parameters $N$ and $\lambda$ ranging from
[50,60] and [1,5] respectively. } \label{plot1}
\end{figure}
\begin{figure}[t!]
\centering
\label{plot2}
\includegraphics[width=20pc]{1nsr.eps}
\caption{Parametric plot of the spectral index of primordial
curvature perturbations as function of tensor-to-scalar ratio
 for the model with quadratic scalar potential for $N=60$ e-foldings. The parameter $\lambda$ for the indices is ranging from [0.1,30]. } \label{plot2}
\end{figure}

In order to ascertain compatibility with the latest observational data, in reduced Planck Units, the free parameters take the following values (N, $\gamma$, $\lambda$, $\alpha$, $\alpha_0$)=(60, -0.06, 1, -0.01, 1). As shown, the model is in good agreement with the experimental data \cite{Planck:2018jri} since, $n_\mathcal{S}=0.966$ and $r=0.0470219$. Furthermore, the tensor spectral
index takes the value $n_{\mathcal{T}}=0.018908$. The initial and the final numerical values of the scalar field are respectively $\phi_i=15.5572$ and $\phi_f=1.42361$ which means that the field decreases as time flows. The numerical values of the slow-roll indices are $\epsilon_1 =0.00837373$, $\epsilon_2=0.000110181$, $\epsilon_3=0$ and $\epsilon_4=-0.0177486$. Also, the model is free of ghosts since $c_A \simeq 1$. In Fig.\ref{plot1} the behaviour of the observed indices $n_{\mathcal{S}}$ and $r$ with respect to free parameters $N$ and $\lambda$ is shown from which it becomes abundantly clear that compatibility with Planck data can be achieved for a variety of values. Moreover, in Fig.\ref{plot2} the parametric plot between these two observed indices is depicted for a fixed e-folding number and running potential depth $\lambda$, from which one can easily extract the one to one correspondence between such parameters.

As expressed before, the tensor spectral index for such model turns out to be a positive number. This is a possible outcome for the k-essence model only if one admits the existence of a Chern-Simons coupling. In turn, this result can be connected to an enhancement in the intensity of the gravitational waves compared to the Einstein model, hence the reason such model is studied in the inflationary era, however to ascertain this a proper analysis of the late-time era for such scalar field assisted gravity is needed. Note also that due to the k-essence part, the field propagation velocity satisfies the relation $c_A\le1$ in order to respect causality and obtain a ghost free theory. Therefore the tensor to scalar ratio $r$ is always lesser, or at most equal to the expected result for the canonical scalar field. This can be used in order to effectively decrease the value of the tensor to scalar ratio if needed.

Finally, we
examine each approximation which was made in order to derive the previous results holds true. According to the previous set of parameters in reduced Planck units always, during the first horizon crossing, $\dot H \sim \mathcal{O}(10^{-1})$ and $H^2 \sim \mathcal{O}(10^{2})$ so the slow-roll assumption holds true. In addition, the kinetic term $ a_0X+\alpha mX^m  \sim \mathcal{O}(10^{-1})$ is negligible compared with the scalar potential $V \sim \mathcal{O}(10^{3})$ and lastly, $\ddot \phi=0$ and $3 H \dot \phi \sim \mathcal{O}(10^{2})$. Hence, the slow-roll conditions are valid.

\subsection{Model with trigonometric potential}
Suppose now that the potential of the scalar field is defined as,
\begin{equation}
V(\phi)=sin\left(\frac{\phi}{\phi_0}\right),
\end{equation}
where $\phi_0$ is a parameter of the model with $[\phi_0]=$ev and the potential amplitude was assumed to be equal to unity for simplicity. Note that the proper dimensions run with eV$^4$ for consistency. The Chern-Simons scalar coupling function is described by a simple power-law form,
\begin{equation}
\nu(\phi)=(\kappa \phi)^2,
\end{equation}
where again the prefactor was fixed to unity in order to avoid the appearance of additional irrelevant free parameters.

The first two gravitational equations for this model are,
\begin{equation}
\centering
H^2 \simeq \frac{\kappa^2 sin(\frac{\phi}{\phi_0})}{3},
\end{equation}
\begin{equation}
\centering
\dot H \simeq -\frac{cos(\frac{\phi}{\phi_0})cot(\frac{\phi}{\phi_0})}{7\alpha_0 \phi_0^2}.
\end{equation}
Let us now proceed with the overall phenomenology.
The slow-roll parameters of the model are given by the following expressions,
\begin{equation}
\centering
\epsilon_1\simeq \frac{cot(\frac{\phi}{\phi_0})^2}{2\alpha_0 \kappa^2 \phi_0^2},
\end{equation}
\begin{equation}
\centering
\epsilon_2\simeq \frac{2\alpha_0+cot(\frac{\phi}{\phi_0})^2}{2\phi_0^2 \alpha_0},
\end{equation}
\begin{equation}
\centering
\epsilon_3\simeq -\frac{\frac{\alpha}{2}cot(\frac{\phi}{\phi_0})(cos(\frac{\phi}{\phi_0})+cot(\frac{\phi}{\phi_0})csc(\frac{\phi}{\phi_0}))}{\alpha_0^4\kappa^4\phi_0^4-\alpha_0\alpha \kappa^2 \phi_0^2 cos(\frac{\phi}{\phi_0})cot(\frac{\phi}{\phi_0})}   ,
\end{equation}
\begin{equation}
\centering
\epsilon_4\simeq \frac{16\kappa^6\phi cos(\frac{\phi}{\phi_0})^2(\phi-\phi_0 cot(\frac{\phi}{\phi_0}))}{16\alpha_0\kappa^8\phi^2\phi_0^2cos(\frac{\phi}{\phi_0})^2-9\alpha_0^3\phi_0^4} .
\end{equation}
Similar to the previous model, the value of the scalar field at the end of inflation is derived from the equation
$\epsilon_1=1$ however, due to the perplexed form of the equations they are omitted. A real value can be obtained in order to avoid complex valued scalar field, something which becomes apparent subsequently. Also, by making use of the definition of the e-folding number the initial value of the scalar field during the first horizon crossing is extracted. Obviously it depends of $N$ and $\phi_f$ however as in the case of $\phi_f$ it was deemed lengthy and thus unnecessary to be shown. Let us proceed with the numerical results and comparison with observations.

\begin{figure}[t!]
\centering
\label{plot3}
\includegraphics[width=17pc]{2ns.eps}
\includegraphics[width=3pc]{2nsdata.eps}
\includegraphics[width=17pc]{2r.eps}
\includegraphics[width=2.65pc]{2rdata.eps}
\caption{Contour plots of the spectral index of primordial
curvature perturbations (left) and the tensor-to-scalar ratio
(right) depending on parameters $N$ and $\phi_0$ ranging from
[50,60] and [8,15] respectively. } \label{plot3}
\end{figure}
Specifying the free parameters of the theory one could produce results compatible with the observational values for the
spectral indices and the tensor-to-scalar ratio introduced in Eq. (\ref{observed}). Assuming that (N, $\alpha_0$, $\alpha$, $\phi_0$)=(60, 1, -0.01, 8.9), in reduced Planck units, so for $\kappa^2$=1, the model at hand produces acceptable results, since $n_\mathcal{S}=0.964101$ and $r=0.0519585$ are both compatible with observations. Furthermore, the tensor spectral
index takes the value $n_{\mathcal{T}}=0.00736323$. The blue shifted tensor spectral index is again generated from the presence of
Chern-Simons term. The initial and the final numerical values of the scalar field are respectively $\phi_i=9.65185$ and $\phi_f=-0.705439$ which means that the field is decreasing with time. The numerical values of the slow-roll indices are $\epsilon_1=0.00176425$, $\epsilon_2=0.0143889$, $\epsilon_3\sim  \mathcal{O}(10^{-7})$ and $\epsilon_4 \simeq -0.00543937$. Also, the sound wave velocity is almost equal to unity and real, thus the model  respects causality and is also free of ghosts respectively. The aforementioned designation of free parameters is obviously not the only one capable of producing compatible with the observations results. In figures \ref{plot3} and \ref{plot4} we present the respective contour plots of the scalar spectral index of primordial primordial curvature perturbations and the tensor to scalar ratio and also the parametric plot. Both observed indices are shown as functions of auxiliary parameters $N$ and $\phi_0$ for the first while in the latter case it becomes clear that allowed pairs of viable $n_S$ and $r$ reside in a slim area of viability.

At this stage it should be stated that the sign of the tensor spectral index is not always positive however, in both k-essence models which we present, the auxiliary parameters were in an essence fine tuned in order to obtain such result. Obviously the fact that $n_{\mathcal{T}}$ appears to be positive is due to the existence of the Chern-Simons scalar coupling function $\nu(\phi)$ and appears whenever the condition $\epsilon_4+\epsilon_1<0$ is satisfied however to our knowledge there exists no universal behaviour that once satisfied, it guarantees that a blue tilted tensor spectral index shall be produced. In general, such result is entirely model dependent and therefore extra care is needed if one wishes to produce a positive tensor spectral index for the k-essence model since not only does one need compatible results with Planck data, but due to the existence of the non canonical kinetic term $\sim \alpha X^2$, a well behaved field propagation velocity is also needed. In both models, as demonstrated, such case is indeed possible.

Finally, let us discuss here and validate whether the approximations assumed in the section II hold true. First of all, we shall check the validity of the slow-roll approximations, $\dot H \sim \mathcal{O}(10^{-4})$ and $H^2\sim \mathcal{O}(10^{1})$ hence the approximation, $\dot H\ll H^2$ holds true. In addition the kinetic term of the k-essence scalar field is $a_0 X+\alpha mX^m \sim \mathcal{O}(10^{-4})$ while the scalar potential is  $V\sim\mathcal{O}(10^{-1})$, hence the condition $a_0 X+\alpha mX^m\ll V$ is valid. Lastly, comparing the term $\ddot \phi\sim \mathcal{O}(10^{-3})$ with the term $H \dot \phi\sim \mathcal{O}(10^{-2})$, it is clear that the condition $\ddot \phi\ll 3H\dot \phi$ is satisfied. Thus, all the approximations are valid.

\begin{figure}[t!]
\centering
\label{plot4}
\includegraphics[width=17pc]{2nsr.eps}
\caption{Parametric plot of the spectral index of primordial
curvature perturbations as function of tensor-to-scalar ratio
 for the model with quadratic scalar potential for $N=60$ e-foldings. The parameter $\phi_0$ for the indices is ranging from [3,20]. } \label{plot4}
\end{figure}

Therefore, both examined models serve as examples of viable k-essence model that admit blue tilted tensor spectral index. Although model dependent, such result when it manifests can lead to interesting results in subsequent cosmological eras.

\newpage
\section{THEORETICAL FRAMEWORK OF INFLATIONARY DIRAC-BORN-INFELD MODELS IN EINSTEIN-CHERN-SIMONS GRAVITY}
In this section we shall investigate the inflationary phenomenology of Dirac-Born-Infeld string-inspired models in Einstein-Chern-Simons gravity examining their viability. The gravitational action which is utilized in order to extract all the information about the primordial Universe is Eq.(\ref{action}). As k-essence models, Dirac-Born-Infeld models belong to a general class of $f(R, \phi, X)$ theories. Hereafter, the general form of the
$f(R, \phi, X)$ function is assumed to be the following,
\begin{equation}
\centering
\label{f2}
f(R, \phi, X)=\frac{R}{\kappa^2}-2K(\phi)^{-1}\sqrt{1+2K(\phi)X(\phi)}-2V(\phi),
\end{equation}
where once again R is the Ricci scalar, $K(\phi)$ is a function which depends from the scalar field and $V(\phi)$ is the scalar potential. It should be stated that the auxiliary function $K(\phi)$ must have mass dimensions of eV$^{-4}$ for the sake of consistency.
Substituting Eq.(\ref{f2}) into the equations of motion (\ref{motion1}-\ref{motion3}) the following equations arise,
\begin{equation}
\centering
\label{eq1dbi}
\frac{3H^2}{\kappa^2}=\frac{VK+\frac{1}{\sqrt{1+2KX}}}{K},
\end{equation}
\begin{equation}
\centering
\label{eq2dbi}
\frac{\dot H}{\kappa^2}=\frac{X}{\sqrt{1+2KX}},
\end{equation}
\begin{equation}
\centering
\label{eqdbi}
\frac{1}{\sqrt{1+2KX}}[\ddot \phi+3H\dot \phi+\frac{K'(1+KX)}{K^2}-\dot \phi(\frac{K'\dot \phi X+K \dot X}{1+2KX})]+V'=0.
\end{equation}
The above equations seem quite perplexed to be solved analytically. In order to proceed our analysis further approximations are required.
First of all, the factor $1/\sqrt{1+2KX}$ is expanded via a Taylor series by making the assumption that $KX\ll1$. In turn, the linear term which emerges is subleading compared to the scalar potential if one admits the slow-roll conditions are valid. During the inflationary era the slow-roll conditions are imposed as presented,
\begin{align}
\label{approx}
\centering
\dot H&\ll H^2,& X&\ll V,& \ddot\phi\ll3 H\dot\phi.\
\end{align}
As the contribution of the kinetic term X is minor, the products $KX$, $K'\dot \phi X$ and $K\dot X$ can be discarded from the above equations. Considering all the approximations,
the equations of motion are simplified further,
\begin{equation}
\centering
\label{eq1dbifinal}
H^2 \simeq \kappa^2 \frac{VK+1}{K},
\end{equation}
\begin{equation}
\centering
\label{eq2dbifinal}
\dot H\simeq \kappa^2 X,
\end{equation}
\begin{equation}
\centering
\label{eq3dbifinal}
3H\dot \phi +\frac{K'}{K^2}+V'\simeq 0.
\end{equation}
Solving Eq.(\ref{eq3dbifinal}) one can get easily,
\begin{equation}
\centering
\label{fdotdbi}
\dot \phi \simeq -\frac{1}{3H}\left(V+\frac{K'}{K^2}\right).
\end{equation}
As mentioned in k-essence case, the dynamics of Dirac-Born-Infeld inflation in the context of $f(R, \phi, X)$ gravity can be described in terms of the slow-roll parameters \cite{Hwang:2005hb}.
The first slow-roll index is given by the expression,
\begin{equation}
\centering
\label{e1dbi}
\epsilon_1 \simeq \frac{(3K'+K(1+KV)V')^2}{18\kappa^2(1+KV)^2},
\end{equation}
while the rest indices are given by quite perplexed equations. Last but not least, parameter E of the model is described by the following equation,
\begin{equation}
E=\frac{81 \sqrt{3}}{\left(\frac{K \left(K \left(27-(K V+1) V'^2\right)-6 K' V'\right)-\frac{9 K'^2}{K V+1}}{K^2}\right)^{3/2}}.
\end{equation}

\section{Compatibility OF INFLATIONARY DIRAC-BORN-INFELD MODELS WITH OBSERVATIONS}
Compatibility with the latest Planck data is discussed extensively in section III. For Dirac-Born-Infeld models the equations of the observed indices  (\ref{observed}) remain the same. The sound wave velocity $c_A^2$ is given by the equation,
\begin{equation}
\label{dbica}
\centering
c_A^2=1-\frac{\left(3 K'+K (K V+1) V'\right)^2}{27K^2 (K V+1)},
\end{equation}
while the number of e-foldings is:
\begin{equation}
\centering
\label{dbiefoldings}
N=-\int_{\phi_i}^{\phi_f}  \frac{3 K (K V+1)}{3 K'+K (K V+1) V'}
d\phi.\,
\end{equation}
As shown, the field propagation velocity remains strictly lesser than unity if the condition $KV+1>0$ is satisfied. In this case it is expected that the model is free of ghost instabilities while simultaneously respects causality. Therefore both cases are described by the same condition. On the other hand the e-folding number seems to be depending on both noncanonical function $K(\phi)$ but also the scalar potential $V(\phi)$, along with their derivatives. This suggests that the overall phenomenology is expected to be quite perplexed. For that reason we shall limit our work to a single trivial example of constant scalar potential to simplify the expression of the e-folding number. The numerical results are available in the following subsection.

\subsection{Model with Dirac-Born-Infeld scalar field and constant potential}
It is presented inflationary phenomenology of Dirac-Born-Infeld scalar field with Chern-Simons string-corrections. The scalar potential is considered to be constant,
\begin{equation}
\centering
\label{dbipot}
V(\phi)=\Lambda,
\end{equation}
while the Chern-Simons scalar coupling function $\nu(\phi)$ and the function K are given by the exponential and power-law form respectively,
\begin{equation}
\centering
\label{cs}
\nu(\phi)=e^{\kappa \phi},
\end{equation}
\begin{equation}
\centering
\label{F}
K(\phi)=\kappa^6\phi^{2}.
\end{equation}
Note that while $\nu(\phi)$ is indeed dimensionless, the scalar potential, even though constant, must have mass dimensions of eV$^4$ therefore $[\Lambda]=$ev$^4$. Also, hereafter natural units are used for simplification therefore the replacement $\kappa=1=M_P$ is used.

The first two gravitational equations for the model are,
\begin{equation}
\centering
H^2\simeq \frac{1}{3} \left(\Lambda +\frac{1}{\phi ^2}\right),
\end{equation}
\begin{equation}
\centering
\dot H \simeq-\frac{2}{3 \left(\Lambda  \phi ^6+\phi ^4\right)}.
\end{equation}

The dynamics of the model is described by the following slow-roll parameters,
\begin{equation}
\centering
\epsilon_1\simeq \frac{2}{\left(\Lambda \phi ^3+\phi \right)^2},
\end{equation}
\begin{equation}
\centering
\epsilon_2\simeq \frac{6 \Lambda  \phi ^2+4}{\left(\Lambda  \phi ^3+\phi \right)^2} ,
\end{equation}
\begin{equation}
\centering
\epsilon_3 \simeq \frac{24 \Lambda  \phi ^2+12}{\left(\Lambda  \phi ^3+\phi \right)^2 \left(3 \Lambda  \phi ^4+3 \phi ^2-4\right)},
\end{equation}
\begin{equation}
\centering
\epsilon_4\simeq \frac{e^{2\phi } (6 -2 \phi )}{\phi ^2 \left( e^{2\phi }- \phi ^6/2\right) \left(\Lambda  \phi^2+1\right)} .
\end{equation}
Equating to unity the
first slow-roll index and utilizing the e-folding number $N$ in Eq. (\ref{dbiefoldings}), one obtains the following values for the scalar field,
\begin{equation}
\centering
\label{phif}
\phi_f \simeq \frac{\sqrt{\frac{\left(\Lambda -\sqrt[3]{27 \Lambda ^4+\Lambda ^3+3 \sqrt{3} \sqrt{\Lambda ^7 (27 \Lambda +2)}}\right)^2}{\Lambda ^2 \sqrt[3]{27 \Lambda ^4+\Lambda ^3+3 \sqrt{3} \sqrt{\Lambda ^7 (27 \Lambda +2)}}}}}{\sqrt{3}},
\end{equation}
\begin{equation}
\centering
\label{phii}
\phi_i\simeq \frac{\sqrt{\frac{3 \sqrt{\frac{\left(\Lambda  \sqrt[3]{27 \Lambda ^4+\Lambda ^3+3 \sqrt{3} \sqrt{\Lambda ^7 (27 \Lambda +2)}}+\left(27 \Lambda ^4+\Lambda ^3+3 \sqrt{3} \sqrt{\Lambda ^7 (27 \Lambda +2)}\right)^{2/3}+\Lambda ^2\right)^2}{9 \Lambda ^2 \left(27 \Lambda ^4+\Lambda ^3+3 \sqrt{3} \sqrt{\Lambda ^7 (27 \Lambda +2)}\right)^{2/3}}+8 \Lambda N}-3}{\Lambda }}}{\sqrt{3}}.
\end{equation}

\begin{figure}[t!]
\centering
\label{plot5}
\includegraphics[width=17pc]{3ns.eps}
\includegraphics[width=2.65pc]{3nsdata.eps}
\includegraphics[width=17pc]{3r.eps}
\includegraphics[width=2.65pc]{3rdata.eps}
\caption{Contour plots of the spectral index of primordial
curvature perturbations (left) and the tensor-to-scalar ratio
(right) depending on parameters $N$ and $\Lambda$ ranging from
[50,60] and [0.1,1] respectively. } \label{plot5}
\end{figure}
\begin{figure}[t!]
\centering
\label{plot6}
\includegraphics[width=20pc]{3nsr.eps}
\caption{Parametric plot of the spectral index of primordial
curvature perturbations as function of tensor-to-scalar ratio
 for the model with constant scalar potential for $N=60$ e-foldings. The value of the potential $\Lambda$ for the indices is ranging from [0.1,1]. } \label{plot6}
\end{figure}
The previous statement referring to difficulties in the overall phenomenology due to the presence of a noncanonical term $K$ stands corrected as for the trivial case of a constant scalar potential throughout the inflationary era, the expressions of the initial and final value of the scalar field as functions of the free parameters are quite complicated. This does not mean that other potentials are prohibited per se but rather $\phi$ dependent potentials manifest certain difficulties in the nature of the scalar field as complex numbers arise frequently. Let us proceed with the results of the model at hand.

Numerically speaking, let us assign the following values
to the free parameters, always in reduced Planck units ($N$, $\Lambda$)=(50, 0.4) the observational indices take the values $n_{\mathcal{S}}=0.966886$, $n_{\mathcal{T}}=0.0351517$ and $r=0.00495707$ which are compatible with the latest observations. The scalar field seems to decrease with time since $\phi_i=5.41455$ and $\phi_f=1.00644$. Also, the model is free of ghosts since $c_A\simeq1$, or the latter term in Eq. (\ref{dbica}) is positive but quite subleading. Furthermore, the slow-roll indices have the following numerical values
$\epsilon_1=0.000421172$, $\epsilon_2 \simeq 0.0156595$, $\epsilon_3\simeq 0.0000554044$ and $\epsilon_4 \simeq -0.017997$, therefore the respective slow-roll conditions are expected to apply in this situation.

The above designation as shown leads to a quite negative slow-roll index $\epsilon_4$ thus the tensor spectral index changes sign and becomes positive. Therefore the fact that the tensor spectral index can become blue tilted is not limited only in the k-essence models but applies to various models, either canonical or noncanonical, provided that $\epsilon_4+\epsilon_1<0$. Therefore, viability of Chern-Simons string inspired noncanonical theories have interesting implications in general as the generation of a blue tilted tensor spectral index may be indicative of theories that predict enhanced intensity of gravitational waves. As mentioned before, this can be ascertained once a proper study of the late-time era is performed.

The last step is to check whether the approximations considered in section IV holds true. According to the previous set of parameters in reduced Planck units always, during the first horizon crossing, $\dot H \sim \mathcal{O}(10^{-1})$ and $H^2 \sim \mathcal{O}(10^{-5})$  so the slow-roll assumption holds true. In addition $X \sim \mathcal{O}(10^{-5})$ while $V \sim \mathcal{O}(10^{-1})$ and lastly, $\ddot \phi \sim \mathcal{O}(10^{-3})$ and $3 H \dot \phi \sim \mathcal{O}(10^{-2})$. Hence, the slow-roll conditions are valid. All that remains is to ascertain the validity of the rest approximations. It turns out that the term $K'KX\sim \mathcal{O}(10^{-4})$ is negligible compared to the term $K'\sim \mathcal{O}(10^{-1})$ thus, our approximation $K'KX\ll K'$ holds true. Finally the term $\dot \phi(\frac{K'\dot \phi X+K \dot X}{1+2KX})\sim \mathcal{O}(10^{-5})$ is quite smaller in order of magnitude than $3H\dot \phi$ concluding that all our approximations are indeed valid.

Overall, the Dirac-Born-Infeld model is capable of producing compatible with the Planck data results while simultaneously it manifests a blue tilted tensor spectral index provided that a Chern-Simons scalar coupling function is present.

\section{Conclusions}
In the present article the viability of certain noncanonical scalar theories of gravity in the presence of string corrective term was studied. Initially, the case of k-essence models was examined by introducing the proper phenomenology. By making use of the slow-roll conditions and simplifying in accordance the equations of motion we found that the inflationary era can manifest compatible with the observations results. The inclusion of a Chern-Simons scalar coupling function does not spoil compatibility with the Planck data however as showcased previously, it can lead to a blue tilted tensor spectral index $n_{\mathcal{T}}$ something which is impossible in the case of $\nu(\phi)=0$. Subsequently, a second noncanonical model and in particular a Dirac-Born-Infeld model was studied. Considering a trivial substitution on the scalar potential and admitting a constant value during the inflationary era, compatible results can once again be generated with the tensor spectral index being again positive. Although there exists no universal condition which guarantees a blue tilted tensor spectral index if it is satisfied, apart from the condition $\epsilon_4+\epsilon_1<0$, the results even though model dependent are in agreement with the latest Planck data. The fact that a blue tilted tensor spectral index can be manifested, although it has yet to be observed, makes a powerful prediction about the behaviour of the overall theory and also gravitational waves. A blue tilted tensor spectral index can be connected to an enhcanced signal in the gravitational waves relative to the expected one from GR which in principle could be observed in the near future by LISA or NANOGrav for instance. To ascertain whether such enhancement is feasible, a proper analysis of the late-time era is needed by keeping the same values of the free parameters that produce a viable inflationary era. Truthfuly the overall model may be altered by assuming for instance the existence of an $f(R)$ function which receives two contribution, a linear contribution as in GR which is dominant mainly in the inflationary era and an additional one which, although subleading in the early era, dominates the late time era. This is an interesting scenario for non canonical theories scalar-tensor theories in general, augmented by a Chern-Simons scalar coupling functions and we leave this study for a future work.

redpajama_set_name: RedPajamaArXiv


>I direct you to this blog, by Elizabeth of Ontario. I wish to point out the picture in the post named "Anguish". Here is how I feel. Here is my deepest self. Here is the anguish of illness. Made visible for all to see. Elizabeth, whom I only know through blogging comments, is a remarkable woman, it seems. Please view her blog.
This entry was posted in CFS Fibro Illness by excentric. Bookmark the permalink.


Elsie's Holiday by Martha Finley Audiobook Download - Christian audiobooks. Try us free.
Eight-year-old Elsie Dinsmore is enjoying Christmas with her family when a terrible crisis arises. She believes that obeying a request her father has made would violate her conscience, and she must refuse him. Elsie clings to her faith in God as, one by one, all the things she holds dear are taken from her, including even her father's presence.


text:
Temperature dependence of coherence in transmon qubits — •Steffen Schlör1, Jochen Braumüller1, Oleksandr Lukashenko1, Hannes Rotzinger1, Martin Sandberg2, Michael R. Vissers2, David P. Pappas2, Martin Weides1, and Alexey V. Ustinov1 — 1Physikalisches Institut, KIT, 76131 Karlsruhe, Germany — 2NIST, Boulder, CO 80305, United States
Superconducting qubits are a promising field of research, not only with respect to quantum computing but also as highly sensitive detectors and due to the possibility of using them to study fundamental implications of quantum mechanics. The requirements for qubits that can be used as building blocks in a potential quantum computer are challenging. Modern superconducting qubits like the transmon are strong candidates for achieving these goals. The main challenge here is to increase the coherence of prepared quantum states. Here, we experimentally investigate the influence of temperature variation on relaxation and dephasing of a transmon qubit. Our goal is to understand decoherence mechanisms in material optimized circuits. Aiming at longer coherence, in this case peaking over 50 µs for T1 and T2, our samples are fabricated at NIST using two different materials. Low-loss TiN was used for the shunt capacitance as well as the resonator, combined with shadow evaporated ultra-small Al-AlOx-Al Josephson junctions. We will present temperature-dependent data on qubit relaxation and dephasing times as well as power spectra. Our data will be compared to previously obtained temperature dependent data for other types of qubits.

redpajama_set_name: RedPajamaCommonCrawl


A cooktop is an important kitchen appliance when it comes to the preparation of simple meals as well as complicated ones. With the plethora of cooktop models coming with different price tags, finding the best cooktop for your kitchen can be a difficult task.
To get the best you need to consider some factors such as your needs as well as the cooktop models available on the market today. These are just but a few of the things you should consider, but in this article, we have shared important things you should consider when choosing your kitchen cooktop.
•	A kitchen cooktop is flexible in design: You can place it anywhere you feel convenient for you.
•	A kitchen cooktop minimizes heat: A kitchen cooktop produces less heat.
•	Provides sufficient storage space: A cooktop offers you more storage space below it where you can store pots and pans.
Usually, cooktops come in the range of 30-36 inches with at least four or five burners. This is just enough for most cooking tasks in the kitchen. However, if you want to use the cooktop in a busy kitchen to prepare more complicated meals, then you will want to consider a cooktop with several burners and so a large cooktop would be the best option for you, though it is pricier.
This also means sparing enough space in your kitchen, since a larger cooktop will take up space on the counter. If you just want to replace your old cooktop, you may just use the dimensions for the old one so that it becomes easy to install the new one. In this case, you must get the dimensions of the old unit or search online for similar models to get the precise dimensions.
Any appliance you have in your kitchen is an investment and you do not want to go back to the shop every now and then buying something you bought just recently. Similarly, a cooktop is an investment and it should be durable enough to last.
Usually, electric coil cooktops are considered the cheapest but are also long lasting, unlike electric smooth-top cooktops. However, when it comes to the durability of the cooktop, the brand can make a big difference in how long the appliance can last.
Village-bakery advises people to research to find out how credible and reliable the brand is by checking customer reviews. Find out what type of maintenance is required for your kitchen cooktop before you buy it.
Of course, you will want to clean your kitchen cooktop regularly and this is not optional. Well, some cooktops are easier to clean than others; for instance, smooth-top electricity and induction cooktops. These appliances are flat which makes them easier to wipe down when cleaning. However, you need to prevent spills, else smooth-top though easy to clean, you will find it hard to clean them.
On the other hand, gas and coil cooktops have parts that you must detach when cleaning them to get good results. This means you will have to spend some time and effort. So, if ease of cleaning is a high priority for you then induction cooktops would make the best option for you and not gas and coil cooktops.
An induction cooktop is considered the safety appliance since it is capable of cooking without dispensing more heat to the surface. On the other hand, gas cooktops create open flames,so you must take caution on the items you place close to the appliance when cooking. Gas cooktops and electricity cooktops can be dangerous when not used properly.
The kitchen is one of the sensitive places and so safety should be the topmost thing anytime you are preparing meals.
Different cooktops cost differently, for instance, expects a large cooktop to be costly than a small one. Also, an electric cooktop designed with advanced features is costly. Induction cooktops also come with a hefty price tag as well. In this case, you must decide how much you are willing to spend and your needs as well.
If you are thinking of buying a new kitchen cooktop, then be prepared to choose from a number of options. With plenty of brands out there, it's imperative to consider the above-mentioned factors so that you get the best appliance.


text:
Q: Attributes sent from link_to to create action is not saved I have the following link_to in my index.html.erb. Whenever I click on the link, it will create a new record in retrieval_requests table but for some reason user_id and package_id was not saved.
I'm not sure on how to go about this. I would appreciate any help.
Thanks.
index.html.erb
.
.
<%= link_to "Retrieve this package", retrieval_requests_path(user_id: current_user.id, package_id: item.package.id), :method => :post %>
.
.

retrieval_requests_controller.rb
class RetrievalRequestsController < ApplicationController
  def index
      @items = Item.where(:user_id => current_user.id)
  end

  def create
    @retrieval_request = RetrievalRequest.new(params[:retrieval_request])
    if @retrieval_request.save
      redirect_to retrieval_requests_path, notice: "Successfully created retrieval request."
    else
      render :new
    end
  end
end

A: Since you're using a link and not a form, you're going to have to create the record with the individual params.
So instead of using params[:retrieval_request] (which don't exist), use params[:user_id] and params[:package_id].
When you pass parameters to a link helper, such as:
retrieval_requests_path(user_id: 3, package_id: 26)

It will create a URL that looks something like the following, depending on how you set up your routes:
"/retrieval_requests/3/26"
# or with no user_id or package_id set in routes:
"/retrieval_requests?user_id=3&package_id=26"

Then in your controller you need to grab those params separately.

redpajama_set_name: RedPajamaStackExchange


Want to add a little extra something to your pedicure? The paraffin pedicure is a truly relaxing experience. This comes with everything in our signature pedicure, but we add a hot paraffin wax dip to keep those feet smooth as silk long after your pedicure ends.
Do your feet need a little extra care? Are you the more athletic type? Or maybe you're constantly on your feet. We have just the pedicure for you! Includes everything that our signature pedicure has plus a little extra heel therapy.
Treat yourself in this indulgent pedicure, you know you deserve it! This is 75 mins of pure relaxation and bliss. Not only do you get your cuticles trimmed, buffed and shaped, heels scrubbed, and a massage, but we also add on a hot towel treatment, foot mask, and more exfoliation.


text:
Undefined / Crying in H Mart
Crying in H Mart
From the indie rockstar Japanese Breakfast and author of the viral 2018 New Yorker piece, a deeply moving memoir on identity and belonging, grief and joy.
ISBN: 9781529033779 Author: Zauner, Michelle	Publisher: Picador Publication Date: 5th August 2021	Imprint: Picador Cover: Hardback	Dewey: 782.42166092 (edition:23) Pages: 256	Language: English	Readership: General - Trade / Code: K Category: Undefined Subjects: Autobiography: arts & entertainment, Coping with death & bereavement, Ethnic minorities & multicultural studies, Memoirs, Migration, immigration & emigration
From the indie rockstar Japanese Breakfast, an unflinching, powerful, deeply moving memoir about growing up mixed-race, Korean food, losing her Korean mother, and forging her own identity.
'As good as everyone says it is and, yes, it will have you in tears. An essential read for anybody who has lost a loved one, as well as those who haven't.' Marie–Claire
In this exquisite story of family, food, grief, and endurance, Michelle Zauner proves herself far more than a dazzling singer, songwriter, and guitarist. With humour and heart, she tells of growing up the only Asian-American kid at her school in Eugene, Oregon; of struggling with her mother's particular, high expectations of her; of a painful adolescence; of treasured months spent in her grandmother's tiny apartment in Seoul, where she and her mother would bond, late at night, over heaping plates of food. As she grew up, moving to the east coast for college, finding work in the restaurant industry, performing gigs with her fledgling band – and meeting the man who would become her husband – her Koreanness began to feel ever more distant, even as she found the life she wanted to live. It was her mother's diagnosis of terminal pancreatic cancer, when Michelle was twenty-five, that forced a reckoning with her identity and brought her to reclaim the gifts of taste, language, and history her mother had given her.
Vivacious and plainspoken, lyrical and honest, Michelle Zauner's voice is as radiantly alive on the page as it is onstage. Rich with intimate anecdotes that will resonate widely, Crying in H Mart is a book to cherish, share, and reread.
Crying in H Mart quantity
Liberty in the Things of God
Ten Poems About Art
The Guitar in Georgian England


The news of Changi's budget terminal closure on 25th September 2012 should have been known to all frequent travelers of budget airlines, which incidentally does not include Air Asia in its ranks. I traveled through Air Asia more often than other airlines, but I did peruse the service of Tiger Airways once in a while, so I was still well acquainted with this wayward terminal situated at the fringe of its 3 larger cousins.
The announcement of the end of Changi's budget terminal service on 25th Sept 2012.
Let not the terminal's name fool you. Budget it may be, it was rather clean and orderly, in the typical Singaporean way. Changi's budget terminal's cousin in Malaysia, LCCT, could learn a lot here. My visit to the latter never yielded any good impression.
Maybe it was my fellow Malaysian drivers who could not wait at designated areas, preferring their own convenience over others, clogging the traffic lanes. Or maybe it was the lighting which never seemed bright enough. Or maybe it was even the unpaved and dirty walkway from the airstrip to the terminal's arrival hall.
All in all, a flight from Changi's budget terminal to LCCT just gave me a sigh of exasperation, disappointed on how Malaysia could even expect to reach a first world mentality when her own citizens wish not to change their own thinking. Maybe it is easier to just blame it on the government or authorities, when simple acts like not clogging the lane felt just too daunting to us. There are only that much blame we could place on others before the finger has to point back to ourselves.
Approaching the Arrival Hall from the bus terminal. Compared to its bustling cousins, sometimes the budget terminal could be quite peaceful.
A shot of the cab pickup area.
Another quiet shot of the surroundings. If it were on Fridays, I believe it would not be this quiet. The terminal may not be as spacious as LCCT, but it definitely beats the latter hands down when it comes to cleanliness.
When it comes to convenience, the budget terminal had as much convenience as could be expected from one with the term 'budgetary' hooked to it. Fast food joints and other small cafeterias served travelers with a quick bite before departure or upon arrival. Other than that, there wasn't anything exciting about the place, apart from its cleanliness.
Unlike its other 3 big cousins, the budget terminal needed to be accessed through a shuttle bus, which although ran for free, did not make a traveler convenient. That was one of the biggest sigh of relief when the budget airlines were transferred to Terminal 2 (T2). The bus stop at the budget terminal was non-air conditioned, which sometimes could be unbearable when the sun was high up in the sky.
The arrival hall looked a lot cleaner and brighter than the one in LCCT. The only thing lacking in numbers was the amount of seats available.
The bus waiting area was not air-conditioned. When the sun shone high in the sky, it could get more than just warm waiting in the area. Fortunately, there were not many cars fuming their exhaust waiting for the arrival of their loved ones.
The three main terminals were served by a skytrain, making traveling from the MRT to the terminals easy and convenient. More than a few first-timers almost missed their flight departing from the budget terminal because they were not aware of the fact the they needed to board the shuttle bus to the budget terminal.
With the budget terminal serving its last customer on the 25th Sept 2012, it is no longer possible now to visit it, although I wonder why anyone would like to do that, given that they will need to board the shuttle bus to reach there. Still it would be nostalgic for those who had departed and debarked from the little terminal numerous times. I hope that these few photos will serve as a memory to all the hard work the terminal endured during its service, and that the new terminal will be an improvement over it.
Environment: A quiet terminal at the fringe of its bustling terminal cousins.
Address: 75 Airport Boulevard, 819664 Singapore.
Getting there: Just take the East-West MRT line (Green line) and disembark at Terminal 2 (T2). Look for the signs pointing you to the skytrain bound for T1, and you will see the twins nearby the check-in counters.


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My time has come to set sails again. People in Europe and Asia are waiting for me to return on my Voicycle to bring wonderful live-music to their cities.
While being in Asia I will stay in Thailand for 3 months and record my original acoustic album.
At this point of time I do not know yet when I will be back in Australia. Still, if you have a wedding coming up, send me an email and I will let you know how the chances are for me to return in time.
If you travel Europe this summer, make sure to stop by at wonderful La Rochelle (France) sometime between July September. You can then also get my latest CD.
Oh, and here is a video from my last street performance in Sydney with the beautiful Opera House in the background. Enjoy!
Tuesday, 25th October 2011 - I will be back!
After 6 months of cycling 8.500km all over the US west-coast and Europe I will return to Sydney to enjoy the Australian sun and of course entertain you all solo and with "The Full House" on King St (Newtown), at Darling Harbour and Circular Quay.
If you have are holding a function - be it a wedding, a backyard party, a corporate event, or any other occasion - between November 2011 and May 2012, I would be more than happy to entertain you and your guests.
In the coming six months I will collect more ideas to then finally roll all those moments of the last years into my first original album. I will record it in the beautiful north of Thailand.
I am also extremely excited that "Julien Mueller and The Full House" are again chosen to be the main act at next year's "Annual Jazz Festival" at Eryldene Historic House in Gordon on Sunday 11 March 2012 !
If everything goes well during the flight, if I can settle in quickly and if I can still remeber all those jazz lyrics, "Julien Mueller & The Full House" will have their welcome-back-performance at Darling Harbour on Sun 6 Nov 2011 at 5pm. Bring your friends and family, enjoy the music the sunshine and many bicycle stories.
I am looking forward to seeing you all again so soon!
Hi everyone! It's time for me to go on a new and exciting journey on a bicycle throughout the US, Canada and Europe. I will leave on March 15th but not without a great last show together with The Full House.
We will perform at the on Sunday, Mar 13th from 5pm. The gates will open at 4pm. We are going to make the night shine with 3 hours of finest live vocal jazz and swing live music.
All details about this event and booking information can be found here . You can also download the flyer.
This night will be great to spend a day with family and friends, have a glass of wine or simply a nice picnic. We'll make sure to have CDs with us and we will also stay around after the show.
For those who would like to watch us perform on the street for the last time: Come to Circular Quay on Fri, 11th Mar at around 7.00pm. All details can also be found here.
Thanks everyone for your support! We are looking forward to a great event with lots of fun.
Sunday, 18th July 2010 - I Made It !!!
My heart was racing, all my hopes concentrated on some words, which sound like: "And the Winner is..."
When they finally announced me as the Winner of this year's Sydney Eistedfodd Contemporary Singer of the Year 2010 Competition (NSW) all the efforts and training of the last year seem to pay out all in one second.
After the announcement I really wanted to talk to those people who came to the event since they believed in me and wanted to support me by attending the show. But after the first "thank you"s a photographer came up to me to take some pictures of me and some sponsors.
Coming back home to my lovely place in the Inner West I finally realized how lucky I was and what a great job I had done over the past weeks. I could hardly fall asleep that night. Everything just felt like heaven!
Thank you so much everyone for supporting me in so many ways!
Special Thanks also go to Sydney Eistedfodd for supporting young upcoming artists!
Monday, 5th July 2010 - I made it to the Finals!
I made it, I made it!I will have about 2 weeks time from now to prepare myself and pick three amazing songs. Can't wait for the big show!
My passion for Gospel singing made me want to try the 'Gospel' Category of this year's Sydney Eistedfodd - Contemporary Singer of The Year Competition 2010.
This time I brought my guitar and Jeremy Camp's 'Who Am I' .
I almost missed my performance due to bad restroom timing (I always warm up before the performance and come out to the stage when I was announced)! Fortunately my name was called out twice and so I made it just in time! When coming up the stairs of the stage I almost fell with my guitar. What a great start of a performance!
The most important part of the performance went pretty well though.
Enthusiastic and inspiring adjudicator Francince Bell later on announced the results for this Category. Last year's Contemporary Singer of The Year Amy Walton came first. I was runner up and happy to go home with a silver medal.
Just one day after my success in the Contemporary Singing Category I tried my best in the 'Jazz or Blues Singer' Category of this year's Sydney Eistedfodd - Contemporary Singer of The Year Competition 2010.
I brought a backing track to sing to and an apple to calm me down before the performance.
With the song 'Me and Ms Jones' which has become widely popular by Canadian Jazz singer Michael Bublé I earned myself the 3rd place.
Well, it was not really was I was aiming for (of course I was aiming for no.1 haha) but I was still satisfied to be awarded with a medal.
Thanks everyone who came down to watch and support me!
If you have a second check out amazing Liam Burrows who ranked 2nd and is extremly talented for his age of only 16 years!
Monday, 21st June 2010 - Placed 1st in the category 'Contemporary Singing'!
I just came home from a singing competition held at the Petersham RSL club. I was performing among Sydney's top vocalists in the category 'contemporary singing' of this year's Sydney Eistedfodd - Contemporary Singer of The Year Competition 2010.
To this competition I brought my guitar, my voice and a lot of excitement.
I was the 10th person to perform among 60 other contestant and sang 'Plane' by Jason Mraz. After everyone had their go, the judges took a few minutes to choose the winner. I couldn't wait for the results!
A few minutes later I was relieved and incredibly happy to be announced WINNER of this category with a very satisfiyng score of 98 out of 100 points! This will also enroll me for the semi-finals of the main category of this competition! Also I would like to congratulate my friend Miranda Hayman who came 2nd! Good job!
Thank you everyone for cheering for me and for supporting me today.
What a joyfull week that was! Julien the TuxGuy made it into the Daily Telegraph with a photo. Thank you Joel Christie for keeping the eyes open on a Saturday night, taking photos and then writing the article. We hope everyone interested in watching Julien perform found him by searching for "Tux Man".
On Friday Julien performed with his new Jazz Band (Jazz Guitar, Bass) in Newtown and had a blast! The songs are working better and better and very soon you might end up seeing Julien with a whole Big Band busking at Circular Quay.
Julien would like to thank everyone for supporting him and his band in Newtown on Friday and Saturday night. With your support he can live his dream. And for him, that is worth lot!
Next show will be Fri 11th June with the Band playing in Newtown in front of the DENDY Cinema at around 7pm.
Today Julien performed with his new Jazz Band on King St a second time. The guitarist (Francisco Ferreiro) and the bass player (Marcos Gil) are amazing. Next performance dates will be announced shortly.
Julien says thanks to Laisa and Daniel for having him at a private party in Earlwood. He would also like to thank everyone else who was busy dancing, taking photos and enjoying the show.
More content will be added to the TuxGuy website shortly.
The new website is almost finished. You will find all completed information and some songs shortly. If you like to see Julien perform tonight come to Favela in Kings Cross.


Cofense Intelligence™ uncovered a resurgent Sigma ransomware campaign on March 13, 2018 following a noted three-month hiatus of the malware. Although many aspects of this campaign—including its anti-analysis techniques—are consistent with previously analyzed Sigma samples, its return is in and of itself atypical.
So far, it's been a very exciting 2018 here at Cofense, with our recent acquisition and announcement of our new name and brand. We continued performing well as a company and launching numerous new features across our products.
On February 27th 2007, while on the phone with my friend and co-founder Rohyt Belani, I typed the name phishme.com into GoDaddy™. We couldn't believe our good luck and immediately registered it. As the co-founder who named this company PhishMe®, the emotional attachment is real. Somewhere in the pile of entrepreneurial startup books, I have a branding book that suggested your name is a vessel that should be big enough to carry your future products and services. We outgrew that boat quite some time ago.


Welcome to Times Square Hotel Service! We look forward to the opportunity to assist you in booking your hotel stay in exciting New York City.
All hotels are rated by AAA and Mobil Travel Guide. In addition, our hotels have been inspected by our staff for quality and comfort. Please also check our our new Yahoo map feature for quickly locating hotels in the Times Square area.
Times Square has it all. You can find first class lodging, all varieties of dining, entertainment, as well as tours of all parts of the city, shopping and nightlife in this exciting, vibrant and historic landmark in New York City. There are always events and attractions to be seen in Times Square, in the heart of the City that never sleeps.


Well, I have something special for you today!
Something us runners think about frequently is hydration and fueling our runs. It is totally key. I have run into dehydration issues more times than I can count. But hydrating is more than just making sure you drink 8 oz of water for ever 20 minutes you sweat or whatever rule of thumb you follow. AND it's especially hard this time of year when the weather is getting colder and you aren't reaching for an ice cold water to cool ya down.
During cold weather seasons, we may be at an increased risk for dehydration because it's not hot out and we may not feel as thirsty, but can't actually tell how hydrated we are by how thirsty we feel. For many of us, by the time we start to feel thirsty, we're already dehydrated, but just how much water is enough when it comes to staying hydrated? Keep a running tally of how much fluid you're getting and aim for half of your body weight in ounces of fluid per day, plus an extra 16 ounces for every pound of sweat lost during exercise. If you're really not in the mood for cold water, try leaving a pitcher of water out on the counter – allowing it to get to room temperature may make it easier to drink.
Staying well-hydrated is essential for maintaining optimal energy levels, preventing muscle cramping and headaches. But that doesn't mean you have to force down gallons of water or bottles of sugary sports drinks. Any type of alcohol-free beverage can count toward your fluid intake – and even some foods! Some of the top electrolyte-rich, hydrating foods include all types of fresh fruit, soups loaded with vegetables – even fall and winter foods like sweet potatoes and kale can provide much needed fluids.
For years, the widely held belief was that caffeinated beverages were dehydrating. Research has proven otherwise, however. The amount of caffeine typically found in standard servings of tea, coffee and soft drinks appears to have little diuretic effect. Meaning that these beverages don't cause us to lose more fluid than they provide. Drink a variety of beverages every day and remember all fluids, including those in foods you eat, contribute to daily water requirements.
I was fortunate enough to receive samples of some Crystal Light Pure from Kraft Foods to try for myself. Honestly, I was kind of skeptical because since I quit diet sodas and all soft drinks I have steered clear of anything that might remotely trigger that desire. The Pure product was surprisingly really good and I am SO HAPPY it does not have any fake sugars in it! YAY! The artificial sweeteners are what typically drive me away from a product like this.
I drank some after my work out today. Intervals on the elliptical and then stair master repeats, it was HARD and I was fiercely thirsty when I got home. I tried the strawberry-kiwi flavor and it really hit the spot. Plus it has electrolytes. WIN!
Did ya know that women who drink Crystal Light drink 20% more water? That's kind crazy.
How do you get your water in?
What is your favorite water add-in?
Have you tried Crystal Light Pure?
Disclaimer: The aforementioned review reflects my own opinions, Kraft Foods provided me with samples to review here on The Bosky Blog. The opinions above are my own and no one else's...like anyone could tell me what to do? Am I right?
How do you make your playlists?
There are few things in this world that buffalo wings can't solve.
Thursdays are my busiest day, so sorry for the late posting! I was pooped when I finally got home last night and passed right out.
Well let's see, yesterday I kind of had this epiphany that I am OVERLY negative. Not just lately with the injury, but I am naturally cynical, prone to impatience and negativity. So much of my energy is wasted getting worked up over silly things that don't matter, and I really don't think that kind of mindset is conducive to healing, or conducting a healthy-happy life.
So adding to my never-ending list of things I am trying to work on is: Cultivating a positive attitude. It sounds pretty hip and like something I should already be doing.
I did a HARD hill interval work out on the bike today. It got me sweating fast and it felt so good. The muscles on the bike next to mine kept looking over at my console and I could see him eyeing my calories burned, and in my mind I could see him speeding up trying to get his burn near mine. The resistance is key bro, resistance bro.
Blue cheese or Ranch dressing?


A tax-free payment to compensate for the costs incurred by an eligible member or former member needing assistance with household running and maintenance (such as cooking, house cleaning, laundry and gardening) because of an injury or disease for which liability is accepted.
he or she needs help with household tasks which they are no longer able to do because of the accepted injury or disease.
The above rate of payment is applicable as at 1 July 2014 and is indexed annually on 1 July.


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It's that time of the year where cities across the globe see a significant increase in fatbergs and subsequent sewer overflows. During the winter months, and especially around the holidays, people are cooking larger meals and then rinsing items they shouldn't (cooking fats, oils and grease) right down their kitchen sink drain and unknowingly creating a major environmental hazard—fatbergs.
Fatbergs are mounds of congealed cooking fats, oils and grease that collect items such as wet wipes and other non-flushable items that get sent into the sewer network, to form a huge blockages that restrict the flow of raw sewage—thus, sending it back up into homes, neighborhoods and the environment through sewer overflows. These blockages become hard as concrete and frequently have to be removed by hand. The sheer mention of fatbergs will send a chill down any sanitation worker's spine.
Here are six facts about fatbergs you need to know. The more you know, the more you can work to help prevent them.
Fatbergs can be huge.
To date, London holds the record for the largest fatberg. In 2017, The Beast or Whitechapel Fatberg, as it has become known, weighed in at 143 tons, or 286,000 pounds, and stretched for an astonishing 820 feet, or two and a half football fields. It took crews, operating 24 hours a day, nine weeks to remove, to the tune of several million dollars. (Whisper)
In 2019, a giant fatberg, longer than the Leaning Tower of Pisa, was found lurking under a seaside town in Sidmouth, Devon. It was a 64 meters-long monster that took eight weeks to remove from the sewer.
While these are just two examples of "monster fatbergs" found, a fatberg doesn't have to be big to cause big issues.
Odd items are often found in fatbergs.
Fatbergs are always made up of the same culprits, cooking fats, oils, grease, wet wipes, tampons and dental floss however, sometimes there can be some very strange items hiding within. Children's toys, screwdrivers, drink cups and lids, drug paraphernalia, medical containers and eye glasses are just some items that have also been found and leave you scratching your head as to how and why they made it into the sewer network. (Hull Live)
Fatbergs smell terrible.
"A fatberg smells like rotting meat mixed with the odor of a smelly toilet," said said Alex Saunders, sewer network manager at Thames Water. (BBC)
It's not easy to remove fatbergs.
Fatbergs are hard to remove and it's expensive. Most fatbergs must be removed by hand since they are as hard as concrete. A special water jet is used to break the fatberg up into smaller pieces and then those pieces are removed from the pipe by manual excavation and powerful vacuumation tanker units.
Thames Water in London spends over £1m ($1.4 million) a month removing fatbergs from across their network.
New York City spends approximately $20 million annually to clear and repair damage from fatbergs. (Water & Wastes Digest)
A fatberg was put on display in London.
The Museum of London put a piece of the infamous Whitechapel fatberg on display in 2018. The samples that were on display, which were air-dried, looked like clumps of moonscape or a small asteroid. "Lean in and you'll see a tiny piece of a Double Decker chocolate bar wrapper poking out of one grayish blob. Lean in even closer and you'll see the small flies that hatched when the samples were in quarantine." (Washington Post)
You, yes you, can help stop fatbergs.
One simple way to help stop fatbergs from forming is to properly dispose of your cooking fats, oils and grease after cooking a meal. Never rinse them down the kitchen sink drain. Another easy way to make an impact, is to be mindful of what you flush down the toilet.
Grease Hero is a convenient and hassle-free way of disposing of cooking fats, oils and grease after cooking a meal. The environmentally friendly drain guard is made of recycled materials and quickly absorbs the fats, oils and grease that you pour into it directly from your cooking pan. You then simply dispose of the entire drain guard into your trash or upcycle it at your city's recycling facility. This keeps that harmful fats, oils and grease contaminants out of your plumbing, city sewers and prevents sewer overflows into the environment.
Grease Hero: Responsible & Sustainable Manufacturing
'Taste of Home' Feature | Grease Hero
Earth Day 2021 | Restore Our Earth
Cooking, Environment, Fatbergs, GreaseHero
Bacon Grease – How do you dispose of it?
A Peek Behind-the-Scenes of Grease Hero
Start Living an Eco-Friendly Lifestyle Today
The Financial & Environmental Costs of FOG
Grease Hero Drain Guards Retail Partners List
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If the governments made a real effort to manage waste and to inform people about where to "upcycle it at your city's recycling facility" (since very few people know where to go), we could begin to manage trash problems instead of letting them grow into fatbergs & floating trash isles.


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Applications are invited for a PhD position in bioinformatics to join Technical University of Denmark, Denmark. Successful candidate will have funding to work and study for 3 years in Denmark. Applications should be sent before January 01, 2019.
A PhD position is available in the 'T cells and Cancer' group headed by Professor Sine Reker Hadrup, DTU Nanotech, the Technical University of Denmark, Kgs. Lyngby.
The 'T cell recognition and Cancer' group is currently consisting of 25-30 people, including Postdocs, PhD students, Technicians and undergraduate students.
The overall aim of the research group is to gain novel insight to T cell recognition of cancer and autoimmune diseases, through use and development of novel technologies.
Please submit your online application no later than1 January 2019 (local time). To apply, please open the link "Apply online", fill out the online application form. The following must be attached in English: Candidates should have a two-year master's degree (120 ECTS points) or a similar degree with an academic level equivalent to a two-year master's degree.The scholarship for the PhD degree is subject to academic approval, and the candidate will be enrolled in one of the general degree programmes at DTU. For information about our enrolment requirements and the general planning of the PhD study programme, please see the DTU PhD Guide The assessment of the applicants will be made by professor, Sine Reker Hadrup.DTU is a leading technical university globally recognized for the excellence of its research, education, innovation and scientific advice. We offer a rewarding and challenging job in an international environment. We strive for academic excellence in an environment characterized by collegial respect and academic freedom tempered by responsibility.The appointment will be based on the collective agreement with the Danish Confederation of Professional Associations. The allowance will be agreed upon with the relevant union. The period of employment is 3 years.You can read more about career paths at DTU here Further information may be obtained from Professor Sine Reker Hadrup, sirha@dtu.dk Please submit your online application no later than. To apply, please open the link "Apply online", fill out the online application form. The following must be attached in English Excel sheet with translation of grades to the Danish grading system (see guidelines andExcel spreadsheet here) Candidates may apply prior to obtaining their master's degree, but cannot begin before having received it.
From January 2019, DTU Nanotech will cease to exist in its present form, and become part of a new department for Health Technology. With approximately 300 researchers from various departments, DTU Health Technology will be able to offer optimal conditions and facilities for health technology research. The aim is to become an international-class research platform capable of fostering new technology and new solutions that can improve the quality of patient care and public health and well-being.


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Dois romances de Nico Horta é um romance literário do escritor brasileiro Cornélio Penna (1896-1958), publicado em 1939. O romance narra a história de Nico Horta, personagem protagonista, que desde o nascimento sofre com a indiferença dos pais, que dão preferência ao seu irmão gêmeo, Pedro. Nico vive um conflito existencial durante toda a narrativa. A dedicatória do livro é dada à "melhor amiga do escritor", Itabira do Mato Dentro, que é a antiga cidade do escritor.

Enredo

O romance inicia com a história de D. Ana, que durante a infância fora amedrontada pela presença do pai, que nunca a machucou, mas o temia, e de sua mãe, mulher resignada e covarde, de seus irmãos que batiam nela e do amigo de seus irmãos, Nico, onde vem a casar-se com ele. Casada, ela se sentia escravizada, e ele a batia como seus irmãos a bateram quando vivia com eles. Mas, esperava-o:  O marido falece, deixando-a grávida, e ela casa-se novamente e da a luz gêmeos. Nomeia o primeiro filho de Antônio, que será conhecido pelo diminutivo de Nico, nome do pai, e do segundo filho de Pedro, nome do marido atual. A nomeação dos gêmeos gera um conflito entre os dois, pois os pais dão preferência a Pedro e trata Nico com indiferença. Para distingui-lo do morto todos o chamavam de Nico Horta. Quando recebiam visitas, o pai lhe chamava de seu segundo filho. Assim, as crianças crescem com uma certa rivalidade. E Nico ao tornar-se um homem, vive atormentado e passa a falar consigo mesmo e a ver fantasmas.  Não suporta a presença do irmão que desde que nasceram era o preferido, e apaixonasse por Maria Vitória, mas é enciumado com o irmão que também a corteja. Sua mãe pede-lhe que vá a fazenda pois estava tudo atrasado, e ele sente que irá derrotar Pedro, pois ele não administrara bem a fazendo Rio Baixo. Contudo, Pedro é levado para cidade para ser internado em um hospício. Sua estadia na fazenda ele tem visões mais constantes de fantasmas, depois de um período na fazenda ele parte para cidade, pois achava que precisava finalmente viver, sentia que a sua vida ia se esvaindo. E a sua grande luta é encontrar um sentido maior para viver, mas as alucinações não o abandonam.

Protagonista

Nico Horta, ao nascer era o mais franzino e seu irmão gêmeo, Pedro, o mais forte.  Sua infância foi cercada de desprezo que os pais nutriam por ele. Quando seu irmão parte para ser tratado na cidade, Nico corre para o quarto sentindo-se livre da presença do irmão. Tem um romance com Maria Vitória, mas parte para cidade como fuga de seu tormento interior, pois sentia-se diferente dos outros, mas tinha o desejo de ser semelhante aos outros. Dizia a si mesmo: Ao perceber que estava só, ele teria que se debater sozinho na companhia de seus fantasmas habituais, o medo e o remorso de viver. Ele tinha uma espécie de visitas noturnas: A vida para ele não fazia sentido, as pessoas que conviviam com ele as compara com os fantasmas que via, sentia que sua vida estava prestes a desfalecer. Na cidade o tabelião, amigo de sua família, oferece-lhe trabalho no cartório, o mesmo aceita, e ao conhecer a filha do tabelião, Rosa, a moça mostra-lhe interesse e ele passa a frequentar a sua casa e a família apoia o noivado. Nico fica confuso, ele havia sido vítima do duplo, no caso do irmão, dos dois pais, duas mães, a senhora Ana e a ama que cuidara dele durante toda a infância, e agora ele tornou-se o criador do dupla entre Maria Vitória e Rosa. Ele retorna para fazenda, casa-se com Maria Vitória e Rosa se suicida.  Ele sentia que alguém o perseguia, mas era um fantasma, sua aparência era de um homem forte. E ele vê muitos outros. Mas, diante das alucinações é levado para o hospital, ao ver sua mãe, sua esposa e o tabelião, afirma:  Após essa afirmação quando finalmente Nico Horta reconhece aos outros e a si mesmo diante do desejo de viver ele morre. Encontrou o seu lugar no mundo, mas já era tarde demais.

Romances

redpajama_set_name: RedPajamaWikipedia


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Mawangdui (馬王堆) est un site archéologique chinois exceptionnel datant des Han Occidentaux (~190-168 ).

Le site
Situé à Wulibei (五里牌) à quelques kilomètres à l'est de Changsha dans la province du Hunan. Signalé par deux tumuli en forme de selle (mawang est une corruption de ma'an 馬鞍 "selle"), le site fut fouillé en urgence de 1972 à 1974 à la suite d'un jet de gaz enflammé (le méthane résultait de la décomposition de toutes les matières organiques de la chambre funéraire). On y découvrit trois tombes datant des Han Occidentaux (~190-168 av. J.-C.) contenant les momies du marquis de Dai (軼侯), de sa femme Xin Zhui et de son fils. Celle de la marquise, qui survécut à sa famille, est dans un excellent état de conservation. Décédée entre 168 et 145 av. J.-C., elle reposait dans la tombe n° 1 dans une chambre funéraire en bois, enveloppée de 20 épaisseurs de tissu fixé par neuf ceintures, et placée dans quatre cercueils emboîtés et entourés de compartiments pour le mobilier funéraire.

Recouvertes de 16 à 20 m de terre pilée, les tombes étaient entourées de couches de charbon et d'argile blanche qui ont maintenu un degré d'humidité constant, assurant la préservation, très rare sur une durée si longue, d'objets en bois laqué (coffrets de toilette tripodes, vases, cuillères, louches, coupes et gobelets, cruches, plateaux, éventails) et de pièces de soie.

La tombe n°1

Organisation
Il s'agit d'une fosse verticale de 16 m de profondeur, surmontée d'un tumulus entre 50 et 60 m de diamètre à la base ouvrant au nord. La fosse funéraire rectangulaire (où se trouve la chambre funéraire) présente en son sommet un élargissement de quatre gradins auquel elle est reliée par une sorte d'entonnoir. L'accès se fait par une rampe qui descend jusqu'au fond.

La chambre funéraire elle-même fait environ 7,60 × 6 m, et accueille un cercueil contenant six cercueils intérieurs (les trois premiers sont laqués et le quatrième renfermait le corps de la défunte). Le cercueil extérieur était recouvert de vingt-six nattes de bambou couvertes de charbon et de kaolin (pour la protection). La défunte était étendue sur le dos, la tête tournée vers le nord, et était enveloppée dans des bandelettes de soie. Entre les différents espaces des cercueils se trouve disposé le mobilier funéraire.

Mobilier funéraire

Le mobilier de la marquise Xin Zhui est composé de plus de 1400 objets, dont un grand nombre d'objets en terre cuite laquée (pour le service de la défunte), des mingqi (figurant musiciens, danseuses, suivantes, etc.), des imitations de lingots d'or, des pièces de soie, etc. On ne trouve aucun bronze et aucun jade, à l'exception d'un miroir.

Parmi ces 50 pièces de soie brodée, des vêtements et surtout une bannière funéraire peinte exceptionnelle tant par le fait qu'il s'agit de la plus ancienne peinture sur soie conservée mais aussi par son format, en T suspendu sur un bambou par une cordelette, et par son sujet. Il s'agit en effet de la représentation du voyage de l'âme de la défunte marquise.

Il s'agit d'une peinture à destination du rituel funéraire mais on peut en considérer les qualités formelles dans l'approche du monde des représentations qu'elle évoque. Si l'on prend en considération le fait que la soie a été teinte en vermillon et le style très nerveux du trait de pinceau, un rapprochement peut se faire avec l'aspect des laques qui accompagnent les offrandes. Les laques donnent déjà le « la » au traitement du bronze depuis les Royaumes Combattants et ceci grâce au traitement graphique que la technique de la peinture à la laque permet (la laque incisée n'est pas pratiquée à cette époque). La bannière est composée en différents registres superposés, depuis le monde souterrain des Sources Jaunes (évoqué par deux poissons entrelacés) en bas jusqu'au monde céleste (où est accueillie la défunte) en haut. Deux paires de dragons placés en symétrie sur les deux côtés verticaux impulsent comme une circulation entre ces niveaux. Mis en relation avec les anciens Canons, cette division semble correspondre au monde du cadavre et à celui du "corps dans sa demeure éternelle". Sur les deux poissons serpentiformes entrelacés repose une atlante soutenant la plate-forme du monde terrestre (évoqué en partie médiane). Sur cette plate-forme se déroule, sous un dais suspendu à un disque bi, un banquet sacrificiel rendu en l'honneur de la marquise défunte. Au niveau du premier tiers les dragons se lient en comblant le vide au cœur du disque bi (symbole ? de l'univers « terrestre »). Sur le « plateau » que le disque supporte par l'intermédiaire d'animaux fantastiques la défunte appuyée sur une cane, dont la silhouette expressive évoque le grand âge et la faiblesse, est accompagnée par trois suivantes et reçoit les hommages de deux personnages accroupis. C'est peut-être une illustration de la cérémonie de rappel de l'âme. En dessous, deux oiseaux à tête humaine appelés Mille Automnes (qianqiu) ainsi que des tortues et des hiboux constituent autant de signes de la longévité espérée, autour des offrandes disposées dans les récipients rituels. Au-dessus, deux émissaires de l'Empereur céleste  l'attendent, comme à un passage : l'espace s'élargit. Plus haut, deux cavaliers aux traits félins hissent ce qui fait penser à un brûle-parfum. Le ciel est symbolisé par le crapaud  et le lièvre de la lune (dans l'angle gauche) et le corbeau, associé au soleil (dans l'angle droit).

Toujours sur soie : de nombreux rouleaux manuscrits (boshu 帛書) se rattachant pour la plupart au courant taoïste, dont les plus anciens documents connus concernant la médecine chinoise ainsi que  Daodejing (deux exemplaires) et le Yijing. Accompagnaient également le corps des provisions, des herbes médicinales, des instruments de musique (cithare, orgue à 22 tuyaux, cornemuses), 162 figurines de bois et des maquettes funéraires.

Notes et références

Notes

Références

Annexes

Bibliographie et ressources en ligne
 . Les trésors de Mawangdui en constituent la part la plus brillante avec la bannière, les tissus, les cartes...
  Ouvrage de référence, bibliographie et Sites Internet.
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Articles connexes
 La tombe du prince He de Changyi
 Lamelles de bambou de Tsinghua

Liens externes

 Site du Musée du Hunan :, le jeu d'échecs au complet.
 Wikimedia the free Encyclopedia :  :en:Mawangdui Silk Texts : les textes sur soie de Mawangdui.

Site historique et culturel majeur protégé au niveau national au Hunan
Dynastie Han
Hunan


Argyris, C. (1991). Teaching Smart People How to Learn. Harvard Business Review, (May-June).
City, E., Elmore, R., Fiarman, S., & Teitel, L. (2009). Chapters 4-6. In Instructional rounds in education: A network approach to improving teaching and learning (pp. 83-131). Cambridge, Mass.: Harvard Education Press.
Lieberman, A. (2000). Networks as Learning Communities: Shaping the Future of Teacher Development. Journal of Teacher Education, 221-227.
Design projects and data are not familiar language to educators, even though (hopefully most) teachers are literally engaged in design every day as they modify the local learning environment to fit the needs of their students. We rarely see it as such, though, as the emphasis is on students and their work in relation to the teacher's design, not the reflection on our own thinking. This mirrors Argyris' single-loop vs. double-loop learning. As Argyris notes, he was working with people who were "well-educated, high-powered, high commitment professionals," which I think would describe a lot of graduate students in education. Argyris (1991) writes, "People can be taught how to recognize the reasoning they use when they design and implement their actions." When faced with a design project that tests our thinking, where the likelihood of failure is high, fear creeps in.
It is through the very act of design, feedback, and failure that requires us to bypass our own interpretations because we've literally put our thinking outside of our heads. This act of dissociation of our emotional, judgmental selves from our practice is exactly what City et al. (2009) refer to as separating the practice from the person. Likewise feedback systems, whether they be user testing in design or observational notes in the classrooms, are what bring in the feedback, or data, on our design. When we can use the feedback to redesign, rather than defend, we can learn.
As we have heard in many readings this semester and again this week, professional community stems from "conversations about their work" (Lieberman, 2000), but clearly these conversations need data about practice, not about teachers, and the people conversing need guidance in using the data. City et al. (2009) refer to the "culture of nice" as an improvement-impeding norm, because it clouds the distinction between practice from person. People are unwilling to offer feedback for fear that it will be taken as criticism and elicit defensiveness, so they just avoid the conversation all together. The Instructional Rounds protocols offer such guidance for school leaders on how they help teachers in "learning to see, unlearning to judge" and offer clear expectations for how to discuss practice in a way that pushes people to think rather than defend.
On a more practical note, for the field work we are just beginning for the DRP class and on personalization in practice, I found many things helpful in the Instructional Rounds piece. At least for me, it will help me orient myself to conducting an observation: keeping it descriptive rather than evaluative, asking open questions to kids, not discussing with fellow researchers in the hallways but waiting for a time to debrief, and examining my own assumptions or biases about what good teaching and learning looks like.


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Q: Is there a way to determine what the rpm file permissions should be? I am working on hardening an instance of Fedora CoreOS and I am using OpenSCAP to perform a security scan to enumerate issues that need to be fixed.  One of the issues is that some of the permissions are not as expected for various RPM packages.
The recommended fix is to use sudo rpm --setperms PACKAGENAME to fix issues.  However, with CoreOS it fails for several files because /usr is a read-only file system by design.  The proper way to fix this would be to update the CoreOS ignition file to set the mode during deployment.
Is there any way to extract what sudo rpm --setperms PACKAGENAME is trying to do so I can use those to build my ignition file by hand?  Essentially I want to see what mode the package is expecting files to have but for the life of me I cannot figure out how to get that information.

A: I figured out how to do this by using tags for the --queryformat option as follows:
rpm -q --queryformat="[%{FILEMODES:perms} %{FILENAMES}]" PACKAGENAME

Where PACKAGENAME is the name of the package you're querying.  If you want to get every file for all packages you can use -ql like this:
rpm -ql --queryformat="[%{FILEMODES:perms} %{FILENAMES}]"