text:
\section{Introduction}
\label{sec:intro}

Recently, gravitational waves (GWs) have been attracting more and more
attention.  So far, LIGO and Virgo
collaborations have succeeded in detecting GWs from merging black
holes~\cite{Abbott:2016blz,Abbott:2017oio}.  KAGRA is also expected to
detect GWs in a few years~\cite{Akutsu:2018axf}.  GWs provide a lot of
information about not only the nature and the origins of black holes,
but also about the early Universe.  Stochastic GWs induced by curvature
perturbations at second order are one of the cosmological GW sources
closely related to the study of the early
Universe~\cite{Ananda:2006af,Baumann:2007zm,Saito:2008jc,Saito:2009jt,Alabidi:2012ex}.
There are a number of recent studies about such induced
GWs~\cite{Espinosa:2018eve,Kohri:2018awv,Cai:2018dig,Bartolo:2018evs,Bartolo:2018rku,Unal:2018yaa,Byrnes:2018txb,Inomata:2018epa,Clesse:2018ogk,Cai:2019amo,Cai:2019jah,Wang:2019kaf,Ben-Dayan:2019gll,Tada:2019amh},
some of which are related to primordial black holes.  The induced GWs,
along with other GW backgrounds of astrophysical as well as
cosmological origins, can be investigated by the ongoing or future GW
projects, such as pulsar timing array observations
(EPTA~\cite{Lentati:2015qwp}, PPTA~\cite{Shannon:2015ect},
NANOGrav~\cite{Arzoumanian:2015liz},
SKA~\cite{Moore:2014lga,Janssen:2014dka}), ground based interferometer
experiments (advanced LIGO (aLIGO)~\cite{Abbott:2017xzg},
Virgo~\cite{virgo}, KAGRA~\cite{Akutsu:2018axf}, Einstein Telescope
(ET)~\cite{Sathyaprakash:2009xs,Moore:2014lga,ET_sense}, Cosmic
Explorer~\cite{Evans:2016mbw}), and space based interferometer
experiments
(LISA~\cite{Sathyaprakash:2009xs,Moore:2014lga,Audley:2017drz},
DECIGO~\cite{Seto:2001qf,Yagi:2011wg},
BBO~\cite{phinney2003big,Yagi:2011wg}).  Future measurements of
stochastic GWs can be a key to reveal the evolution history of the
Universe.

In this work, we focus on the relation between the induced GWs and an
early matter-dominated era (eMD era).  An eMD era is a period during
which the energy density of a massive field dominates the Universe
before the reheating.  Although the eMD effects on the induced GWs
have been discussed in
Refs.~\cite{Assadullahi:2009nf,Alabidi:2013wtp,Kohri:2018awv}, in our
accompanying paper~\cite{Inomata:2019zqy}, we find that if we
carefully take into account the evolution of the gravitational
potential, which is the source of the induced GWs, around the transition from an
eMD era to the radiation dominated era (RD era), the predictions for
the induced GWs can change.  In particular, we show that the induced GWs can
be significantly suppressed for a gradual transition, whose transition
timescale is comparable to the Hubble time at that time.  In some
cosmological scenarios (see Appendix~\ref{sec:model}) however, the
transition from an eMD era to the RD era is sudden, i.e. the timescale
of the transition is much shorter than the Hubble time at that time.
The purpose of this paper is to study the induced GWs in such sudden
transition cases.

The effects on the induced GWs of a sudden reheating mainly arise
during the RD era by the scalar perturbations that have already
entered the horizon during an eMD era.  Although GWs induced during an
eMD era have been studied in
Refs.~\cite{Assadullahi:2009nf,Alabidi:2013wtp,Kohri:2018awv}, GWs
induced during the RD era by the perturbations experiencing an eMD era
on subhorizon scales have not been investigated in the previous
studies.  However, we point out that, in sudden-reheating scenarios,
GWs induced during the RD era can be larger than GWs induced during an
eMD era by several orders of magnitude. Making use of this
enhancement, we might be able to determine the reheating temperature
by future GW detectors, as we discuss later.

We begin by reviewing the equations to calculate the induced GWs in
Sec.~\ref{sec:formalism}, and based on these equations we obtain the
power spectra for the induced GWs in Sec.~\ref{sec:gw_calculation}
assuming a sudden transition from an eMD era to the RD era. We explore
possibilities to determine the reheating temperature in
Sec.~\ref{sec:reheating _constraints} by making use of the enhancement
of the induced GWs associated with a sudden reheating, and
Sec.~\ref{sec:conclusions} is dedicated to conclusions. In Appendix
\ref{sec:model}, we discuss two models that can realize a sudden
transition from an eMD era to the RD era, and in Appendix
\ref{sec:analytic} we present approximate formulas for the induced GWs
in sudden-reheating scenarios.

\section{Formulas for induced gravitational waves}
\label{sec:formalism}

In the following, we briefly review the equations to calculate induced
GWs (see Ref.~\cite{Kohri:2018awv} for more details).  We assume that
an eMD era ended abruptly with the Universe entering into the RD era
at a conformal time $\eta = \eta_\text{R}$. Then the scale factor and
the conformal Hubble parameter are given by
\begin{align}
\frac{a(\eta)}{a(\eta_{\text{R}})} =& \begin{cases}
\left( \frac{\eta}{\eta_{\text{R}}} \right)^2          \\
2 \frac{\eta}{\eta_\text{R}} - 1
\end{cases},
&
\mathcal{H}(\eta)=& \begin{cases}
\frac{2}{\eta}                           &  \quad (\eta \leq \eta_\text{R}) \\
\frac{1}{\eta - \eta_{\text{R}}/2} & \quad  (\eta > \eta_\text{R})
\end{cases}.
\end{align}
We also assume that the curvature perturbations follow a Gaussian
distribution\footnote{GWs induced by the curvature perturbations with
  non-Gaussianity are discussed in
  Refs.~\cite{Nakama:2016gzw,Garcia-Bellido:2017aan,Cai:2018dig,Unal:2018yaa}}
and adopt the conformal Newtonian gauge\footnote{The gauge dependence
  of induced GWs is discussed in
  Refs.~\cite{Arroja:2009sh,Hwang:2017oxa}.} for simplicity.  Since we
focus on the effects of an eMD era, relevant to very small-scale
fluctuations
($k \gg k_\text{eq} = 0.0103\,
\text{Mpc}^{-1}$~\cite{Aghanim:2018eyx}),
in this paper we do not consider the enhancement of the induced GWs during
the late MD era ($z\lesssim 3400$)~\cite{Mollerach:2003nq,
  Baumann:2007zm}.

The energy density parameter of GWs per logarithmic interval in $k$ is given by
\begin{align}
\Omega_{\rm{GW}} (\eta, k) &= \frac{\rho_{\rm{GW}} (\eta, k) } { \rho_{\rm{tot}}(\eta)} \nonumber\\
&=
\frac{1}{24} \left( \frac{k}{a(\eta) H(\eta) } \right)^2
\overline{\mathcal P_{h} (\eta,k)} ,
\label{eq:gw_formula}
\end{align}
where $\overline{\mathcal P_{h} (\eta,k)}$ is the time averaged power spectrum of GWs.
It can be evaluated from the power spectrum ${\cal P}_\zeta$ of the
curvature perturbations by~\cite{Kohri:2018awv}
\begin{align}
\overline{\mathcal P_{h} (\eta,k)} = 4\int^\infty_0 \mathrm{d} v &\int^{1+v}_{|1-v|} \mathrm{d} u \left( \frac{4v^2 - (1+v^2 - u^2)^2}{4vu}  \right)^2 \nonumber \\
& \times \overline{I^2(u,v,k,\eta,\eta_\text{R} ) }\mathcal P_\zeta(u k) \mathcal P_\zeta(v k).
\label{eq:p_h_formula}
\end{align}
Here, $I(u,v,k,\eta,\eta_\text{R} )$, describing the time dependence of GWs, is given by
\begin{align}
I(u,v,k,\eta,\eta_\text{R} ) =& \int^{x}_0 \mathrm{d} \bar{x} \frac{a(\bar \eta)}{a(\eta)} k G_k(\eta, \bar \eta) f(u,v,\bar x, x_\text{R} ),
\label{eq:i_formula}
\end{align}
where $x$ and $x_\text{R}$ are defined as $x \equiv k\eta$ and $x_\text{R} \equiv k\eta_\text{R}$.
In this equation, $G_k$ is the Green's function being the solution of
\begin{align}
G_k''(\eta, \bar \eta) + \left( k^2 - \frac{a''(\eta)}{a(\eta)} \right) G_k(\eta, \bar \eta) = \delta (\eta - \bar \eta),
\label{eq:g_formula}
\end{align}
where a prime denotes differentiation with respect to $\eta$, not $\bar \eta$.
Note that the concrete expression of $G_k$ depends on the background evolution of the Universe, which is an eMD era or the RD era in our problem.
In addition, $f(u,v,\bar x, x_\text{R} )$ is the source function defined as
\begin{widetext}
\begin{align}
f(u,v,\bar{x}, x_\text{R} )=& \frac{3 \left( 2(5+3w) \Phi(u\bar{x})\Phi(v\bar{x})+4 \mathcal H^{-1} (\Phi'(u\bar{x})\Phi(v\bar{x})
 + \Phi(u\bar{x})\Phi'(v\bar{x}))
+ 4 \mathcal H^{-2} \Phi'(u\bar{x})\Phi'(v\bar{x}) \right) }{25(1+w)},
\label{eq:f_def}
\end{align}
\end{widetext}
where $\omega = P/\rho$ is the equation-of-state parameter with $P$
and $\rho$ being the pressure and the energy density, respectively.
$\Phi$ is the transfer function of the gravitational potential, which
satisfies $\Phi(x \rightarrow 0, x_\text{R} ) \rightarrow 1$, and a prime
denotes differentiation with respect to the conformal time, that is,
$\Phi'(u \bar{x}) \equiv \partial \Phi(u \bar x)/\partial \bar \eta =
u k \,\partial \Phi(u\bar x)/\partial (u \bar x)$.
The second argument of $\Phi$ is abbreviated  in
Eq.~\eqref{eq:f_def} for compact notation.  $\Phi(u \bar{x})$
actually means $\Phi (u\bar{x}, u\bar{x}_\text{R})$, and
$\Phi(v\bar{x})$ should be understood similarly.

The evolution equation for $\Phi$ is~\cite{Mukhanov:991646}
\begin{align}
\Phi'' +  3(1+w)\mathcal H \Phi' + w k^2 \Phi = 0.
\label{eq:phi_evo_eq}
\end{align}
By solving this equation, we find
\begin{align}
\Phi(x,x_\text{R} ) = \begin{cases}
1 & ( \text{for}\  x \leq x_\text{R}), \\
 A(x_\text{R}) \mathcal J(x) + B(x_\text{R} ) \mathcal Y(x)  & ( \text{for}\  x \geq x_\text{R}),
\end{cases}
\label{eq:phi_formula}
\end{align}
where we have dropped the decaying mode for $\eta < \eta_\text{R} $.
In this expression, $\mathcal J(x)$ and $\mathcal Y(x)$ are defined from the first and second spherical Bessel functions, $j_1(x)$ and $y_1(x)$, as
\begin{align}
\mathcal J(x) =& \frac{ 3\sqrt{3} \,  j_1\left(\frac{x-x_{\text{R}}/2}{\sqrt{3}} \right)}{x-x_{\text{R}}/2}, \\
\mathcal Y(x) =& \frac{3\sqrt{3} \, y_1\left( \frac{x - x_{\text{R}}/2}{\sqrt{3}} \right)}{x- x_{\text{R}}/2},
\label{eq:c_d_formula}
\end{align}
and the coefficients $A(x_\text{R} )$ and $B(x_\text{R} )$ are determined so that $\Phi(x)$ and $\Phi'(x)$ are continuous at $x=x_\text{R} $:
\begin{align}
\label{eq:a_formula}
A(x_\text{R} ) &= \frac{1}{\mathcal J(x_\text{R} ) - \frac{\mathcal Y(x_\text{R} )}{\mathcal Y'(x_\text{R} )} \mathcal J'(x_\text{R} )}, \\
\label{eq:b_formula}
B(x_\text{R} ) &= - \frac{\mathcal J'(x_\text{R} )}{\mathcal Y'(x_\text{R} )} A(x_\text{R} ).
\end{align}
In Appendix~\ref{app:sudden_reh_model}, we introduce a model realizing a sudden-reheating transition and check that the above analytic expression for $\Phi$ with these connection conditions coincides well with the numerical solution for $\Phi$ calculated for that model.

We can reexpress Eq.~(\ref{eq:i_formula}) as in Ref.~\cite{Kohri:2018awv} with a slight refinement of the time dependence of the scale factor:
\begin{align}
I(u,v,x,x_\text{R} ) =& \int^{x_\text{R}}_0 \mathrm{d} \bar{x} \left( \frac{1}{2(x/x_\text{R} ) -1} \right) \left( \frac{\bar x}{x_\text{R}} \right)^2 \nonumber \\
&\qquad \qquad
\times k G_k^{\text{eMD}\rightarrow \text{RD}}(\eta, \bar \eta) f(u,v,\bar x,x_\text{R} ) \nonumber\\
&
+ \int^x_{x_\text{R}} \mathrm{d} \bar x \left( \frac{2(\bar x/x_\text{R} ) -1}{2(x/x_\text{R} ) -1} \right) \nonumber \\
& \qquad \qquad
\times
k G^{\text{RD}}_k (\eta, \bar \eta) f(u,v,\bar x,x_\text{R} ) \nonumber  \\
\equiv& I_\text{eMD}(u,v,x,x_\text{R} ) + I_\text{RD}(u,v,x,x_\text{R} ),
\label{eq:i_formula_emd}
\end{align}
where $I_\text{eMD}$ and $I_\text{RD}$ represent the contributions
from GWs induced during an eMD era and the RD era, respectively. See our accompanying paper~\cite{Inomata:2019zqy} for the concrete expressions of the Green functions. We approximate $\overline{I^2(u,v,x,x_\text{R} )}$ in Eq.~(\ref{eq:p_h_formula}) as
\begin{align}
\overline {I^2(u,v,x,x_\text{R} )} \simeq \overline{I_\text{eMD}^2(u,v,x,x_\text{R} )} + \overline{I_\text{RD}^2(u,v,x,x_\text{R} )}.
\end{align}
Correspondingly, we approximately split $\Omega_\text{GW}$ into two parts as $\Omega_\text{GW} \simeq \Omega_\text{GW,RD} + \Omega_\text{GW,eMD}$,
where $\Omega_\text{GW,RD}$ and $ \Omega_\text{GW,eMD}$ are calculated from $\overline{I^2_\text{RD}}$ and  $\overline{I^2_\text{eMD}}$, respectively.

The
analytic formulas for $I_\text{eMD}$ and $I_\text{RD}$ are derived in
Ref.~\cite{Kohri:2018awv}. In this reference, we adopted an implicit
assumption that GWs induced during the RD era by the perturbations
having entered the horizon during an eMD era, which we focus on in
this work, are subdominant compared to the GWs 1)
which are induced during the eMD era and 2) which are induced by the
perturbations entering the horizon after the reheating.
However, this assumption is not true in realistic situations.  In our
accompanying paper~\cite{Inomata:2019zqy}, we consider a gradual
reheating transition and show that the contributions from
$I_\text{RD}$ play an important roll for the suppression of induced
GWs.  In addition, in a sudden-reheating scenario, the dominant contribution comes from $I_\text{RD}$ as we will show in
Sec.~\ref{sec:gw_calculation}.

During the RD era, the gravitational potential, the source of GWs,
decays on subhorizon scales, and therefore $\Omega_{\text{GW}}$
becomes constant after the gravitational potential has sufficiently
decayed.  Here, we define $\eta_c$ as the moment when
$\Omega_\text{GW}$ becomes constant.
Note that since we focus on small scales, where the effects of an eMD
era may leave traces, $\eta_c$ is well before the standard
matter-radiation equality time.  Taking into account the evolution of
GWs during the late MD era and the change in the effective
relativistic degrees of freedom, we can write the current energy
density parameter $\Omega_\text{GW}(\eta_0,k)$ as~\cite{Ando:2018qdb}
\begin{align}
\Omega_{\rm{GW}} (\eta_0, k)  = 0.39 \left( \frac{g_c}{106.75} \right)^{-1/3} \Omega_{\text{r},0} \Omega_{\rm{GW}}(\eta_c, k),
\label{eq:latetime}
\end{align}
where $\Omega_{\text{r},0}$ is the current value of the energy density
parameter for radiation. In this paper, we denote the effective
relativistic degrees of freedom by $g$, and $g_c$ in this equation is
its value at $\eta = \eta_c$.

\section{Calculations of induced gravitational waves}
\label{sec:gw_calculation}
Using the above equations and the analytic formulas in Ref.~\cite{Kohri:2018awv}, we calculate induced GWs.
To be specific, we assume the following power spectrum of the curvature perturbation:
\begin{align}
\mathcal P_\zeta (k) =  \Theta(k_\text{max} - k) A_s \left( \frac{k}{k_*} \right)^{n_s-1},
\label{eq:pzeta_def}
\end{align}
where $A_s$ is the amplitude at the pivot scale $k_*$, $n_s$ is the tilt of the power spectrum, and $\Theta$ is the Heaviside step function.
We introduce $k_\text{max}$ as the cutoff scale of the power spectrum. Since matter density perturbations grow in proportion to the scale factor during a MD era, perturbations may enter into the non-linear regime, depending on the amplitude of primordial fluctuations and the duration of an eMD era. If perturbations remain in the linear regime during an eMD era, the cutoff scale is the Hubble radius at the beginning of an eMD era. On the other hand if such nonlinearities arise, $k_{\text{max}}$ should be chosen as the wavenumber of perturbations that are entering the non-linear regime at the end of an eMD era, since our formalism is based on the linear theory.\footnote{
	There are works discussing GWs induced by non-linear perturbations, though the results inevitably involve some uncertainties~\cite{Jedamzik:2010dq,Jedamzik:2010hq}.
}
In this case, the smallest scale on which we can apply the linear theory is approximated as~\cite{Inomata:2019zqy}
\begin{align}
k_\text{NL} \sim 470 /\eta_\text{R} .
\label{eq:nl_scale}
\end{align}
Hence, to ensure the validity of our analysis, we limit our analysis to cases with $k_\text{max} \leq 450 /\eta_\text{R}$. That is, we do not take into account GWs that are generated from non-linear perturbations, and this means our analysis would lead to conservative estimations of the GW spectrum.

Figure~\ref{fig:emd_gw_profiles} shows the scale dependence of the spectrum of induced GWs.
In this figure, we take $n_s = 1$ for simplicity.  We can see that
$\Omega_\text{GW,RD}$ is much larger than $\Omega_\text{GW,eMD}$.
This is because the GWs induced during the RD era by the subhorizon
perturbations that entered the horizon during an eMD era, neglected
in the previous works but taken into account in this work, are
significant.  For comparison, we also plot the GW spectra induced by
the power spectra of
$\mathcal P(k) = \Theta(k_\text{max}-k) \Theta(k - 0.7
k_\text{max})A_s$
and
$\mathcal P(k) = \Theta(0.7 k_\text{max}-k) \Theta(k - 0.4
k_\text{max})A_s$ with blue and red lines.
As shown in the figure, the contributions from the smallest scales
(blue dashed line) are the dominant contributions to the total
spectrum (solid black line) except for the large-scale-side tail of
the sharp peak ($0.3 \lesssim k/k_\text{max} \lesssim 1$).  This sharp peak is due to the resonance effect, which
is a characteristic feature of GWs induced during the RD
era~\cite{Ananda:2006af}, when the gravitational potential oscillates.
The tail of the sharp peak is formed by the envelope of the resonance
effects on these scales (see the red dot-dashed line).  In this way,
the spectrum of the induced GWs is produced dominantly by the smallest
scales, and the resonant amplification plays a key role.  This
understanding becomes clearer in Appendix~\ref{sec:analytic}, where we
derive approximate analytic formulas for induced GWs for sudden-reheating scenarios.
On much larger scales, the contributions from the perturbations
entering the horizon after the reheating dominate induced GWs, whose
spectrum becomes scale invariant
$\Omega_\text{GW}(\eta_c,k) \simeq 0.8222
A_s^2$~\cite{Kohri:2018awv}.
This can be observed in the GW spectrum for $k<10^9$Mpc$^{-1}$ in
Fig.~\ref{fig:emd_induced_gws}, though in that figure a slightly
scale-dependent primordial spectrum is assumed, leading to a slight
scale dependence of $\Omega_{\text{GW}}$.

The main reason why induced GWs are enhanced is that the gravitational
potential $\Phi$ with large $k$ ($\gg 1/\eta_\text{R} $) is constant until
$\eta = \eta_\text{R} $ and, after the reheating, it oscillates with the
timescale $\sim 1/k$, much shorter than its decay timescale
$\sim \eta_\text{R} $.
Due to the fast oscillations of perturbations with
unsuppressed amplitudes, which remained constant until the moment of the reheating, induced
GWs are significantly enhanced.\footnote{Although the perturbations entering the horizon during the RD era also oscillate with the timescale much shorter than their decay timescale well after (not soon after) the horizon entry, the amplitudes of the perturbations start to decay soon after the horizon entry, unlike during an eMD era, and therefore the enhancement is not caused by the perturbations entering the horizon during the RD era. }
Note that the dominant contributions come from the last term in Eq.~(\ref{eq:f_def}), which involves two time derivatives of the gravitational potential.
This is because, at the beginning of the RD era, the last term can be approximated as $\mathcal H^{-2} \Phi'\Phi' \sim (k\eta_\text{R} )^2\Phi^2 \gg \Phi^2$ for the perturbations that entered the horizon well before the sudden reheating. In other words, the factor $(k\eta_\text{R} )^2$ in the source term and the amplitude of $\Phi$ that remained constant until the reheating are the main causes for the enhancement.

In addition to numerical solutions, we also obtain approximate
analytic formulas of $\Omega_{\text{GW,RD}}$ in
Appendix~\ref{sec:analytic}, with $\Omega_{\text{GW,RD}}$ given by the
sum of Eqs.~\eqref{eq:Omega_GW_large-scale} and
\eqref{eq:Omega_GW_resonance}.  Using these expressions, the GW
spectrum is roughly expressed as
\begin{align}
\frac{\Omega_{\text{GW}}(\eta_c,k)}{A_{\text{s}}^2} \simeq &
\begin{cases}
0.8 & (x_{\text{R}} \lesssim 150 x_{\text{max,R}}^{-5/3}) \\
3 \times 10^{-7} x_{\text{R}}^3 x_{\text{max,R}}^5  &   (150 x_{\text{max,R}}^{-5/3} \lesssim x_{\text{R}} \ll 1) \\
1 \times 10^{-6} x_{\text{R}} x_{\text{max,R}}^5 & (1 \ll x_{\text{R}} \lesssim x_{\text{max,R}}^{5/6}) \\
3 \times 10^{-7}   x_{\text{R}} ^7 &     (x_{\text{max,R}}^{5/6} \lesssim x_{\text{R}}   \lesssim x_{\text{max,R}})  \\
\text{(sharp drop)} & (x_{\text{max,R}} \lesssim x_{\text{R}} \leq 2 x_{\text{max,R}})
 \end{cases},  \label{eq:Omega_GW_rough_behavior}
\end{align}
neglecting a logarithmic factor for the second line.

\begin{figure}
\centering
\includegraphics[width=0.48 \textwidth]{figs/gw_profiles5.pdf}
\caption{Energy density parameters of GWs, for each logarithmic interval of wavenumber, induced during the RD era ($\Omega_\text{GW,RD}(\eta_c,k)$) and during an eMD era ($\Omega_\text{GW,eMD}(\eta_c,k)$),
as well as the power spectrum $\mathcal P_\zeta(k)$ of curvature perturbations. They are normalized by $A_s^2$ or $A_s$, respectively, and
we take $\eta_\text{R} = 450/ k_\text{max} $.
The black lines are derived from $\mathcal P_\zeta(k) = \Theta(k_\text{max} - k) A_s$.
For comparison, the blue and red lines are also shown, which are derived from $\mathcal P_\zeta(k) = \Theta(k_\text{max} - k)\Theta(k - 0.7 k_\text{max}) A_s$ and $\mathcal P_\zeta(k) = \Theta(0.7 k_\text{max} - k)\Theta(k - 0.4 k_\text{max}) A_s$, respectively.
}
\label{fig:emd_gw_profiles}
\end{figure}

\section{Determination of reheating temperature}
\label{sec:reheating _constraints}

In the previous section, we have shown that the induced GWs can be
much larger than those previously
reported~\cite{Kohri:2018awv,Alabidi:2013wtp,Assadullahi:2009nf}.  In
the following, we consider the GWs induced by the almost
scale-invariant power spectrum, given in Eq.~(\ref{eq:pzeta_def}),
with $A_s=2.1\times 10^{-9}$, $k_* = 0.05$\,Mpc$^{-1}$, and
$n_s = 0.96$~\cite{Aghanim:2018eyx}.  Figure~\ref{fig:emd_induced_gws}
shows the sensitivity curves of current and future GW experiments and
plots for $\Omega_{\text{GW}}$ of the GWs induced by this power spectrum
with $k_\text{max}  = 10^{14}$Mpc$^{-1}$.  This figure shows that the induced
GWs associated with a sudden transition from an eMD era to the RD era
could in principle be observable by future projects.  Since the height
and scale of the peak are determined by the scale of the reheating and
the cutoff $k_\text{max} $, we discuss what range of the reheating
temperature could be probed by future observations searching for GWs.

\begin{figure}
\centering
\includegraphics[width=0.48 \textwidth]{figs/emd_gw_const_summary4.pdf}
\caption{Effective sensitivities to stochastic GWs of current and future experiments.
	Note that we plot $\Omega_\text{GW,eff} h^2 /\sqrt{T_\text{obs} f/10}$ as a sensitivity curve for each experiment.
	We consider the same experiments and take the same parameters as in Ref.~\cite{Inomata:2018epa}.
	In particular, we take the same parameter sets of observation time for each experiment: $T_\text{obs} = 18$ years for EPTA, $T_\text{obs} = 20$ years for SKA, and $T_\text{obs} = 1$ year for the other experiments.
	The shaded regions have already been excluded by the existing observational data.
	See Ref.~\cite{Inomata:2018epa} for more details about the sensitivity curve of each experiment.
	Black lines show the energy density parameters of the GWs induced by the power spectrum of $\mathcal P_\zeta(k) = 2.1\times 10^{-9} (k/0.05\,\text{Mpc}^{-1})^{-0.04} \Theta(k_\text{max}  - k)$.
	We take $k_\text{max}  = 10^{14}$Mpc$^{-1}$ for all these three lines and
	 $\eta_\text{R}  = 450 / k_\text{max} $, $\eta_\text{R}  = 200 / k_\text{max} $ and $\eta_\text{R}  = 100 / k_\text{max} $ for each line, respectively.
}
\label{fig:emd_induced_gws}
\end{figure}

We adopt an analysis similar to that in our previous
paper~\cite{Inomata:2018epa} (see also Ref.~\cite{Thrane:2013oya}).
We use the signal-to-noise ratio $\rho$ for GW interferometers given
by~\cite{Thrane:2013oya}.
\begin{align}
\rho = \sqrt{2T_\text{obs}} \left[ \int^{f_\text{max}}_{f_\text{min}} \mathrm{d} f \, \left(\frac{\Omega_\text{GW}(f)}{\Omega_\text{GW,eff}(f)}\right)^2 \right]^{1/2}.
\label{eq:rho_def}
\end{align}
Here, $T_\text{obs}$ is the observation time, and $(f_\text{min}, f_\text{max})$ is the range of observable
frequencies for each project.
$\Omega_\text{GW,eff}$ is the
effective sensitivity curve, which is calculated for each project (see
Ref.~\cite{Inomata:2018epa} for detail).  For pulsar timing array
(PTA) observations, we use
~\cite{Anholm:2008wy,Siemens:2013zla,Chamberlin:2014ria}
\begin{align}
\rho = &\sqrt{2T_\text{obs}} \left(\sum_{I=1}^M  \sum_{J>I}^M \chi^2_{IJ} \right)^{1/2} \nonumber \\
&\times \left[ \int^{f_\text{max}}_{f_\text{min}} \mathrm{d} f \, \left(\frac{\Omega_\text{GW}(f)}{\Omega_\text{n} (f) + \Omega_\text{GW}(f)}\right)^2 \right]^{1/2}.
\label{eq:pta_snr}
\end{align}
In this expression, $M$ is the number of the observed pulsars, $\chi_{IJ}$ is the Hellings and Downs coefficient, and $\Omega_\text{n}$ is the energy density parameter for noise of each pulsar. We take the same parameters and noise power spectrum as in Ref.~\cite{Inomata:2018epa} assuming that the noise is dominated by the white timing noise~\cite{Thrane:2013oya}.

Using the effective sensitivity curves in Fig.~\ref{fig:emd_induced_gws}, we derive the cutoff scale to give $\rho=1$ for each project and reheating temperature.
The numerical results are shown in Fig.~\ref{fig:reh_const_kmax}.
When we derive the curves, we use the approximation formulas given in Eqs.~(\ref{eq:Omega_GW_large-scale}), (\ref{eq:Omega_GW_resonance}), and (\ref{eq:omega_gw_approximation}) to save the computational time.\footnote{
For simplicity, we use the formulas for the scale-invariant spectrum, given in Eqs.~(\ref{eq:Omega_GW_large-scale}), (\ref{eq:Omega_GW_resonance}), and (\ref{eq:omega_gw_approximation}), instead of those for the power-law spectrum, given in Eqs.~(\ref{eq:omega_tilt_ls})-(\ref{eq:omega_tilt_res}).
Since the enhancement of the induced GWs is mainly caused by the perturbations on the smallest scales ($k\sim k_\text{max}$) and the tilt of the power spectrum is small, we can approximately use the formulas for the scale-invariant spectrum whose amplitude is given by $A_s (k_\text{max}/k_*)^{n_s-1}$.
We have also numerically checked that the effect of the tilt with $n_s = 0.96$ around the smallest scale on the enhanced GW spectrum is negligible.}
In this figure, we take $T_\text{obs} = 20$ years for SKA and $T_\text{obs}=1$ year for the other projects and assume no foreground for simplicity.
When we obtain these plots, we have used the following relation between the conformal time and the temperature~\cite{Inomata:2018epa}\footnote{
To derive Eq.~(\ref{eq:eta_t_rel}), we use the relation $a_\text{eq}H_\text{eq} = k_\text{eq} (= 0.0103\, \text{Mpc}^{-1}$)~\cite{Aghanim:2018eyx,Ade:2015xua}.
This relation corrects the factor given in Ref.~\cite{Inomata:2018epa}.
}
\begin{align}
	\label{eq:eta_t_rel}
   & \frac{aH}{a_\text{eq} H_\text{eq}} = \frac{1}{\sqrt{2}}  \left(\frac{g_{s,\text{eq}}}{g_s}\right)^{1/3} \left( \frac{g}{g_\text{eq}} \right)^{1/2} \frac{T}{T_\text{eq}}, \nonumber \\   \Rightarrow \
   & \frac{\eta_\text{R} }{10^{-14} \text{Mpc}} = \left( \frac{g_s}{106.75} \right)^{1/3} \left( \frac{g}{106.75} \right)^{-1/2} \nonumber \\
   & \qquad\qquad\qquad\qquad\qquad
   \times  \left(\frac{T_\text{R} }{1.2 \times 10^{7}\text{GeV}}\right)^{-1},
\end{align}
where the subscript ``eq'' means the value at the late
matter-radiation equality ($z\sim3400$), and $g_s$ is the effective
degrees of freedom for the entropy density.  Note again that the peak
scale of the induced GWs corresponds to $k\sim k_\text{max} $, not
$k\sim 1/\eta_\text{R} $.
Figure ~\ref{fig:reh_const_kmax} shows that, in the case of $k_\text{max}\eta_\text{R}  = 450$, the ranges of reheating temperature that future observations could investigate are $T_\text{R}  \lesssim 7\times 10^{-2}\, \text{GeV} $ for SKA, $20\,\text{GeV}  \lesssim T_\text{R}  \lesssim 4\times 10^3\,\text{GeV} $ for LISA, $20\,\text{GeV}  \lesssim T_\text{R}  \lesssim 1 \times 10^7\,\text{GeV} $ for DECIGO, $20\,\text{GeV}  \lesssim T_\text{R}  \lesssim 2 \times 10^7\,\text{GeV} $ for BBO, and $4\times 10^5\,\text{GeV}  \lesssim T_\text{R}  \lesssim 2\times 10^7\,\text{GeV} $ for ET.

\begin{figure}
\centering
\includegraphics[width=0.48 \textwidth]{figs/kmax_etar.pdf}
\caption{\small
	Relation between the cutoff scale multiplied by $\eta_\text{R} $ and the reheating temperature that can be probed by the future observations.
	We take $T_\text{obs} = 20$ yr for SKA and $T_\text{obs}=1$ yr for the others.
	The curves correspond to the values of $k_\text{max}\eta_\text{R} $ required to reach the signal-to-noise ratio of unity ($\rho = 1$) for the experiments at each reheating temperature.
	The brown shaded region is already excluded by the big bang nucleosynthesis and the Planck data~\cite{deSalas:2015glj}.
}
\label{fig:reh_const_kmax}
\end{figure}

\section{Conclusions}
\label{sec:conclusions}

We have studied the effects of an eMD era on the induced GWs.  In
particular, we have focused on a sudden-reheating scenario, in which
the reheating completes on a timescale much shorter than the Hubble
time at that time.  Then, we have found that the induced GWs can be
significantly enhanced in such a scenario. The main contributions to
the enhanced GWs come from the GWs induced during the RD era by the
perturbations that entered the horizon during the eMD era.  This is
due to the fast oscillations of the perturbations after the sudden
transition.  This enhancement is qualitatively opposite to the
suppression of induced GWs in gradual-reheating scenarios, which we
report in our accompanying paper~\cite{Inomata:2019zqy}.  This means
that the eMD effects on the induced GWs strongly depend on how the
reheating takes place.

We have also numerically calculated the induced GWs with realistic
power spectra of curvature perturbations and discussed possibilities
of determining the reheating temperature observationally for sudden-reheating scenarios.
We have found that if an eMD era lasts for
$224 \eta_\text{eMD,start}$, where $\eta_\text{eMD,start}$ is the
conformal time at the start of the eMD era,\footnote{Note that the
  wavenumber corresponding to the horizon scale at
  $\eta_\text{eMD,start}$ satisfies $k_\text{eMD,start} \eta_\text{R} = 450$
  because
  $k_\text{eMD,start} = a_\text{eMD,start} H_\text{eMD,start} =
  2/\eta_\text{eMD,start}$
  and $\eta_\text{R}  = 225 \eta_\text{eMD,start}$ in this case (the duration is $\eta_\text{R} - \eta_\text{eMD,start} = 224 \eta_\text{eMD,start}$).} the
reheating temperatures in the range
$T_\text{R}  \lesssim 7 \times 10^{-2}$GeV or
$20 \, \text{GeV} \lesssim T_\text{R}  \lesssim 2\times 10^7 \, \text{GeV}$
could be probed by future GW projects, such as SKA, LISA, DECIGO, BBO,
and ET.  Note that, if an eMD era starts right after inflation era,
the duration of the eMD era of $\mathcal O(100) \eta_\text{eMD,start}$
corresponds to $\rho^{1/4}_\text{inf}/T_\text{R}  \sim \mathcal O(10^3)$,
where $\rho_\text{inf}$ is the energy density during the inflation
era.

Since the enhancement of the induced GWs we find is so significant,
one may wonder if it is consistent with some physical requirements.
Hence, we briefly mention some consistency checks.
Let us first discuss energy conservation and backreaction.
Note that the dominant part of the energy density of the induced GWs is generated soon after the reheating transition by the short-wavelength modes at around $k \sim k_\text{max}$, and the enhancement is stronger for $k_\text{max}$ closer to the non-linear scale $k_\text{NL}$.  By definition, the energy density of density perturbations at scales around $k_\text{NL}$ is comparable to the energy density of the homogeneous component. On the other hand, in Fig.~\ref{fig:emd_gw_profiles}, we have seen that the energy density of the induced GWs is $\Omega_\text{GW}(\eta_c) \sim 10^{12} A_s^2 \sim \mathcal O(10^{-6})$ even for $k_\text{max} \eta_\text{R} = 450$ ($k_\text{max} \sim k_\text{NL}$). The smallness of $\Omega_\text{GW}$ implies that the energy density of the induced GWs is much smaller than both the energy density of its source, namely the density perturbations, and the homogeneous component.  Thus, a
backreaction of the GW production to the thermal history of the
Universe would be negligible.

Another concern may be whether or not GWs induced at third order in
scalar perturbations are negligible, given the fact that the
second-order contributions have turned out to be significant.
In other words, one might wonder whether or not sources coming from third order scalar perturbations appear with many derivatives,
which can be larger than the dominant source in second order scalar perturbations, $\mathcal H^{-2} \Phi'\Phi'$, even when the perturbations are linear $(k\eta_\text{R} )^2 \Phi \lesssim 1$.
Complete evaluations of the third-order contributions are much more
complicated than those for the second-order analysis. Thus, we
estimate their orders of magnitudes by listing up possible third-order
terms that appear in the evolution equation for tensor perturbations
and are consistent with general covariance and the transverse
traceless condition.  Most of them turned out to be negligible
provided that we are in the linear regime, where the density
perturbations are less than unity. However, we need to carefully
evaluate the contributions involving the first-order scalar
perturbations multiplied by the second-order vector perturbations,
which are sourced by first-order scalar perturbations at second order,
similarly to the induced GWs we have studied. That is because
 the power spectrum of second-order vector perturbations is
larger than that of second-order tensor
perturbations~\cite{Saga:2015apa}.  Full evaluations of these
contributions are beyond the scope of this work, but we expect that
the third-order GWs can be subdominant as long as
$k_{\text{max}} \ll k_{\text{NL}}$.

In this paper, we do not take into account the gauge dependence of
the induced GWs~\cite{Hwang:2017oxa}, GW foregrounds due to other
astrophysical as well as cosmological sources, and the possible
contributions from non-linear perturbations~\cite{Jedamzik:2010dq,
  Jedamzik:2010hq}, which can arise depending on the length of the
eMD era and the amplitude of the small-scale primordial
fluctuations. Although these issues remain to be investigated, our
result shows that observations of GWs could possibly reveal the
reheating history of the Universe in the near future.

\acknowledgments

KI and TN thank KEK, Johns Hopkins University and Research Center for
the Early Universe, University of Tokyo, for hospitality received
during this work.
KI acknowledges Tomohiro Fujita, Teruaki Suyama, and Masahide Yamaguchi for useful comments.
This work was supported in part by World Premier
International Research Center Initiative (WPI Initiative), MEXT,
Japan, the JSPS Research Fellowship for Young Scientists (KI and TT),
JSPS KAKENHI Grants No.~JP18J12728 (KI), No.~JP17H01131 (KK), and No.~JP17J00731 (TT), MEXT
KAKENHI Grants No.~JP15H05889 (KK), No.~JP18H04594 (KK) and
No.~JP19H05114 (KK), and Advanced Leading Graduate Course for Photon
Science (KI).

redpajama_set_name: RedPajamaArXiv


Let us be totally honest here. Miike Snow's 'Animal' is one of the finest pop songs written in recent times. Of that we are not in doubt. What do you expect from a bunch of Swedes though? Anyway, they return today with a inter-country collaboration with Lykke Li. The track is part of an album which Miike Snow, Bloodshy & Avant and Andrew Wyatt are releasing in late March this year.
The track which features Lykke Li is 'Black Tin Box' and can be heard below.
The album they are releasing is called Happy to You and will be released through Downtown/Universal Republic on March 27 (via Pitchfork).


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What the Globalists Refuse to Learn | Jake Scott
by Jake Scott · Published September 25, 2019 · Updated August 17, 2020
In June 2016, before the Brexit referendum, I predicted that Britain would vote to Leave the European Union. Mercifully, I wasn't alone; many people predicted such an outcome, and for many different reasons. Roger Scruton gave an eloquent speech in which he elaborated upon the differences between the continental and the common law traditions and the attitude each revealed towards governance: the essential difference being that the continental tradition was one of top-down, edictal governance in which the law is made according to a goal derived by the ruling class; and the common law tradition was one in which law was discovered, by the organic communities that lived with the consequences of these very laws.
My reasoning was not so high-flown. Mine was more to do with the attitudes I had noticed in the people around me, in conversations in pubs, classes and living rooms. The whole conversation surrounding the referendum had morphed into one of not being told what to do; the British people have always had a fine mind for liberty and freedom that they felt they could hold in their hands, and balanced by the law and order of self discipline, not the Puritanism of Cromwell, or the arrogance of socialism, and now the distance of the European Union. The same British people, however, have always had respect for authority where they feel it is deserved or earned. The old deference to the aristocracy might have passed away, but that was merely the content of the thing, not the actual form; in other words, the British people have found other elites to respect, but these remain local and community leaders.
So when the EU referendum was talked about as a rebellion, I was struck that the rebellion was not against elites per se, but the unknown (and unknowable) elites in Brussels, a distant place that most British people have never even been to, or perhaps point to on a map of Europe – not out of ignorance or lack of intelligence, but because for time immemorial they haven't needed to. We all know where London is, and who our MP is, but most British people don't know who their Member of the European Parliament is (not that they should – it's a paper-thin monument to vanity anyway); it currently sits at a staggeringly-low 5%, which is actually a decrease from 2014.
What this rebellion was against was the perceived nature of global elitism. Why should bureaucrats in Brussels have any say in the way British people live? Well, why should bureaucrats in Westminster have any say in the way Northerners should live? The answer is partly to do with that made by Scruton I mentioned at the beginning, and the structural nature of our laws, but also because bureaucrats in Westminster are by-and-large drawn from the common folk of Britain, and so know what problems face the British people.
This was a problem exacerbated when foreign bodies were brought in to "convince" the British people the right way to vote; it was the arrogance of this attitude that was bothering people. Obama talked about how Britain would be at the "back of the queue" for a deal; the International Monetary Fund (IMF), staffed by people drawn from all over the world, warned of a recession; and of course, the Eurocrats rallied to defend their project. That's not to say that pessimism was a purely foreign attitude, and the British really had the "spirit of Dunkirk" – after all, Cameron's famous prediction that Brexit could threaten the peace in Europe will never be forgotten – but when the people fighting for British independence were almost exclusively British, you couldn't help but notice the natural appeal to patriotism that stokes the hearts of all people. As the character Bert Cooper put it in Mad Men, "some people have no confidence in this country".
Three years on, and the globalists haven't learned. Recently, the United Nations (one of the great globalist institutions) heard two undeniably significant speeches: one by the activist Greta Thunberg; and the other by President Donald Trump. As a side note, it wasn't long ago the Left was decrying globalism as a form of Western imperialism reborn; how quickly the tide turns when the tools are in their hands.
Thunberg, a Swedish sixteen year-old, raged at the impotency of Western nations to reverse the climate change caused by generations of industrialism and pollution, and the "stolen future" of her generation, followed by a formal complaint of five nations for their lack of action. None of this is true, of course: of the five most polluting nations, one is in the West (the United States); none of those indicted were in that list; the ozone is repairing; and the Earth is greener now than it was twenty years ago. Now I'm not saying no action needs to be taken, that's not the point of this article – this topic has been dealt with by better people than I. What I think needs to be pointed out, is that the globalists are using the same tactics; Americans will not respond to a Swedish girl coming to their country and telling them what to do, the same as the Swedes probably don't want an American to go there and tell them how to live.
Which was, importantly, the point of the second speech made. This time, Trump told the UN that the "future belongs to patriots and nations" not global institutions. The reason politicians like Donald Trump are winning is because he and others have noticed the sea-change that has taken place across the West; a rejection of the globalisation process that has not benefited the people whose politicians support it.
The globalists will not succeed, so long as they continue to do the same thing; lecture the people who have no connection to the global institutions that have been built, but will live with the consequences of their existence.
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Google+ is an online sharing and social platform with elements in common with Facebook. One of the main differences however is that you can have 1 profile and manage many different types of interactions with ease. Pages is the business version and is similar to Google places.
The question we are asked is - is it worth me setting-up yet another online profile for my business?
With all the different platforms out there at the moment this is a very valid point. In fact we built our own page a little over a week ago and to be honest it does currently feel a little like talking to myself, out loud and in public! Getting true engagement I feel will take a little time and effort.
However the effect on our online profile and most importantly our natural search results seems to be very positive and almost immediate! So if you are able to get adding some content at least a couple of times a week (and you don't mind talking to yourself!) what have you got to lose?
Largest search platform brings out a sharing and social platform - in my mind it's worth a bit of time to see where it goes.
Oh, and just so that I don't have to keep talking to myself please add PinkJelly Marketing to your circles!


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And because cable internet is so widely available already, DOCSIS 3.1 will bring blazing fast internet speeds to more households than ever before. Something fiber has struggled to do thus far.
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Enables a significant increase in network capacity with the ability to transmit up to 50 percent more data over the same spectrum, on existing HFC networks.
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DOCSIS 3.1 technology improves the spectral efficiency of the HFC network and thus increases the capacity significantly. While DOCSIS 3.0 technology supports up to 256 QAM (8 bits/symbol), DOCSIS 3.1 technology supports up to 4096 QAM (12 bits/symbol) thus providing the potential to drastically increase the system capacity.
Do you need to deploy DOCSIS 3.1 technology in the upstream and downstream simultaneously?
No, DOCSIS 3.1 technology is backwards compatible to DOCSIS 3.0 technology. A DOCSIS 3.1 downstream can operate with a DOCSIS 3.0 upstream and a DOCSIS 3.1 upstream can operate with a DOCSIS 3.0 downstream channel.
Do you need to upgrade the cable plant to deploy DOCSIS 3.1 technology?
No, DOCSIS 3.1 technology does not require any upgrades to the HFC plant in order to operate. DOCSIS 3.1 technology can capitalize on HFC network upgrades to increase network capacity.
Do you need to expand the upstream to deploy gigabit service in the downstream channel?
The current 5-42 MHz upstream channel provides sufficient capacity to deploy gigabit services in the downstream.
Could you deploy DOCSIS 3.1 technology in the existing plant, and then reduce the downstream service group size and/or expand the downstream/upstream spectrum capacity?
DOCSIS 3.1 technology can be deployed on the current HFC network with any required modifications. DOCSIS 3.1 technology provides great flexibility in defining the channel spectrum and the group sizes.
Will DOCSIS 3.1 modems run in DOCSIS 3.0 systems?
Yes, DOCSIS 3.1 devices are backwards compatible and will operate on a DOCSIS 3.0 system.
Will DOCSIS 3.1 modems require dedicated spectrum?
DOCSIS 3.1 downstream channel will require dedicated spectrum to operate, while the DOCSIS 3.1 devices can share the upstream spectrum with DOCSIS 3.0 devices.
Will DOCSIS 3.0 modems need to be upgraded when DOCSIS 3.1 technology is deployed?
DOCSIS 3.1 technology is backwards compatible to DOCSIS 3.0 technology; thus DOCSIS 3.0 devices will not need to be upgraded when DOCSIS 3.1 technology is deployed.
How does DOCSIS 3.1 technology compare with FTTH?
DOCSIS 3.1 technology was designed to support multiple Gbps of line capacity while maintaining economical deployment and maintenance costs on the current HFC infrastructure, thus delivering Gbps performance to the masses in contrast to the limited deployment of FTTH solutions.


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Ever since Tony Yang (楊祐寧) ended his relationship with Amber Kuo (郭采潔) in 2015, his love life has seemingly been barren. However, the truth is that the All is Well <都挺好> star has secretly been dating for the last two years! Two years ago, Tony participated in Mainland variety show Divas Hit the Road <花兒與少年> and Jing Boran (井柏然) was able to trick him into accidentally revealing that he had a girlfriend. He did not immediately deny at the time, but paparazzi has never been able to get concrete evidence of his girlfriend's existence.
On May 14, a woman with a long ponytail was witnessed entering an upscale Japanese restaurant with a middle-aged lady. When exiting the restaurant, paparazzi were able to confirm that the middle-aged woman was Tony's mother and the lady in the ponytail was Tony's rumored girlfriend, Melinda. The paparazzi also recognized that his girlfriend had previously dated singer Eric Chou (周興哲), who was six years her junior!
The trio ordered an Uber car and after dropping off his mother, Melinda got off at a condo nearby. After 20 minutes or so, another Uber car arrived with Tony Yang in it. He stood at the entrance of the condo seemingly trying to remain inconspicuous before entering. It seems that their relationship has reached a stage of co-habitation.


Lock in a great price for Limak Limra Hotel - Kids Concept – rated 8.2 by recent guests!
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Staff were so responsible and helpful. All facilities were like the pictures and as well as we expected. Night club and disco was amazing. At the end of my stay I received a discount card for my next stay and I like to try it again.
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This 115 ft² family room has garden view. Certain rooms of this type has a balcony with pool view. Air conditioning and kettle are also provided.
This twin/double room features a satellite TV, mini-bar and air conditioning.
These rooms are located in the annex building across the street.
This twin/double room has a balcony, mini-bar and air conditioning. Nonalcoholic drinks can be enjoyed at the hotel's bars and restaurants during the stay.
This twin/double room features air conditioning and mini-bar. Limitless nonalcoholic drinks can be enjoyed at the hotel's bars and restaurants for free, during the stay. This room is located in the annex, located across the main building.
Resort is family-friendly and offers lots of free facilities & activities for its visitors such as free internet access in the room and in general areas, delicious food at main restaurants, good snacks, A La carte restaurants, buffet restaurant, local and import good alcoholic drinks, safe box in the room and reception, free kettle with tea & coffee set up. A wellness center will let you get out of tiredness of the year with its special packages such as relaxation, rejuvenation, Turkish bath etc. with reasonable prices. A Turkish bath (Hamam), Sauna and Fin bath are opened all a year long. Beach towels, sun beds, sun umbrellas are provided around the pool and on the beach free of charge. Central air condition is being set up according to weather conditions.Clean beach provides a playground for kids. A very tasty breakfast is available at late breakfast restaurant between 10:00- 11:00 o'clock. Housekeeping gives a daily excellent service for a clean rooms and bathroom.
Area Info – This neighborhood is a great choice for travelers interested in mountains, nature and relaxation – Check location Great location - show map Guests loved walking around the neighborhood!
House Rules Limak Limra Hotel - Kids Concept takes special requests – add in the next step!
Limak Limra Hotel - Kids Concept accepts these cards and reserves the right to temporarily hold an amount prior to arrival.
Strong smell in sauna. Yet it was not bad, just strong.
We had a room in the park hotel and i have to say it was little, old and not smell good, i had the feeling i was at a cheaper pension... İn the hotel they where still every where working so lots of noice. You guys say the hotel is Kids concept but there was nothing special even the 2 swings in the play park the plastik was broke. The food was also not great this time, 3 the time we was coming limak limra and that was now also the last time.
The reception desk staff were unfriendly and unwelcoming, both on check-in and checkout. There was little or no vegetarian food amongst the hot dishes at lunches and dinners.
Garden can be decorate better , pedestrian could renew.
Wifi was terrible. Would have been nice to have squash rackets available for rent (they only had one). Tennis rackets needed more tape. All food that is not salad was very oily (but not more oily than the average in Turkey). Music in the nightclub was too loud (They even have signs up claiming it is unhealthy) But besides all that it was great value (+$ 30euro/night/pp) in November and we had much better things to do than surfing the web all the time. Also it would have been nice to have other beers than Efes on offer. Efes tastes like water.
The beds were awful, hard as bric! They should absolutely spent som money on new beds!! If you dont like cats this i not a hotel for you, there where cats everywhere inside as well, but they feed them and take good care of them!
The food was very good! The outdoor area was very nice! The beach was nice, but not suitable for children, a lot of big waves and deep water instantly.


Would you wear a race shirt from a race you didn't run?
Years ago, when I first starting running races I wondered whether or not I should run in my race shirt. I was told by some of my more seasoned runner friends that it would be a big mistake and I would look like an amateur if I did, so I never ran in one. Truth be told it wasn't because other runners told me not to it was because I was terrified to run in anything I hadn't pre-tested because I didn't want any surprises on race day.
For a few years anytime I ran a race I'd hang the t-shirt up in closet and never think about it again. It sort of became like a race medal, a prize that you hang up and notice occasionally but you don't actually wear.
I don't know why it happened but at one point MacGyver and I were in a thrift store and I noticed brand new race shirts on the racks. I bought some to use during training because I figured at 1.99 they were cheaper than most of the running shirts I usually bought and they were moisture wicking so it was a win-win. It never occurred to me that I had some perfectly good running shirts hanging in my closet because in my mind those were trophies.
Wearing participant shirts that you got in a thrift store also presents a problem because inevitably someone will see the shirt and ask is you liked the race, or when you ran it, or how many times, and since you bought the shirt at a thrift store you can't answer most of the questions. I would usually say, 'I bought this shirt at a thrift store but I plan on running it this year' or something like that.
I think it was MacGyver who actually asked me why I ran in participant shirts from the thrift store but now my own and it was about that time I realized I should go ahead and pull them out of the closet and add them to my rotation. Of course by that time some of them had yellowed a bit.
It didn't take me long to choose my favorites. Living in Florida and the fact that I tend to get really hot, I typically run in tanks, but in the fall and winter I do add some of the short sleeves into my rotation, both my own participant shirts and ones from the thrift store.
The long sleeve shirts are worn much less often. Typically I wear them about 10 days when running in Florida and I take some of them with me whenever I head to any destination north of here.
I still buy participant shirts at the thrift store but these days I typically only buy them when I'm visiting another state and I find cool ones that I would normally never have the chance to acquire and I also run in them too.
People still ask me if I ran the race and when, because let's face it most of the people who live in Florida aren't from Florida and the person asking is usually from the state you got the shirt from. No matter, I still think it's the most affordable option for running shirts and for finding cool running shirts with awesome slogans and graphics.
One of my favorites participant shirts has a bible verse on the back, it reads, "2 Chronicles 15:7 But as for you, be strong and do not give up, for your work will be rewarded." I like to think that it gives encouragement to anyone running behind me and I don't think about the fact that I never ran the race for which it was given out.
Do you wear your participant shirt when you run a race?
Would you wear a shirt from a race you didn't actually run?
Do you wear your old race t shirts to train?
What do you do with your race shirts?
This entry was posted in Uncategorized and tagged participant shirts, race shirts, what to do with race shirts by flowerjovia. Bookmark the permalink.
The only race shirt that I own from a race I didn't run is from the Boston marathon. I did actually qualify that year, but was cut due to my time. So, when my husband ran it that year, he gave me the shirt 🙂 That scored big points with me!
That would score big points with me too but that would never happen in my world because MacGyver is a biker and hates running, big sigh….
Like you, I never wear the shirt for the race that day. I don't think I've worn a race shirt during any race. I think I have about 50 shirts after 6 years and I keep them folded in a large basket, along w my running tanks. (I prefer sleeveless too.) I would never wear a shirt I didn't "earn" – it just would feel like I was cheating. Also, there's some great quilt making places for running shirts that you can find online or at race expos. Easier than doing it yourself – it's quite an endeavor. Good luck!!
OMG I literally was looking at how to make a t-shirt quilt last night (which would be actually this morning for day time people lol)! I was looking at no sew options but they were all tie methods. I might do Stitch Witch or maybe just get a sewing machine at a thrift store. The quilt would be for decoration mostly. But it's mostly straight stitches so….
I've worn a race shirt during a race maybe twice. I've got a 5k Sat morning and it's a LS shirt so I might wear it.
I don't wear a(n over) shirt when I run except when it's under 60. I don't really like the "technical" shirts. I think they are hot and don't breathe. My St Pete Run Fest shirt is cotton (blend I assume) and I'd wear that over my sports bra.
Are you going to run Gasparilla?
Also, I saw a shirt from Raw Threads that said running is horrible oh look there's a race. I was tempted but I don't wear t shirts much.


Hello all my Lovelies..Happy Monday!! Hope you all are great and your weekend went quite well.
This is what I wore when I went for shopping this weekend. I simply love this color combination – Mint Green and Blue. I feel these colors are made for each other.
My weekend was awesome as it included some shopping.. and some coffee.. and yummy food..!
Actually, it was love at first sight for these sandals. I love how the vibrant color match my jeans.
What do you think of this outfit.. Please drop those lovely comments below.


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Meet Amber Salzman, the Female CEO to Helm Bay Area's Adverum Biotechnologies
By Alex Keown, BioSpace.com Breaking News Staff
MENLO PARK, Calif. – Shortly after taking over the helm of new gene therapy company Adverum Biotechnologies, newly-dubbed Chief Executive Officer Amber Salzman has delayed enrollment of patients in the Phase 1/2 clinical trial for ADVM-043 until the fourth quarter of 2017.
When Adverum launched earlier this year, following a merger plan after Avalanche Biotechnologies acquired the French company Annapurna, the plan had been to begin its first dosing trials by the end of 2016. In a statement, the company said it "decided to upgrade the ADVM-043 manufacturing process by implementing its proprietary baculovirus-based production system and plans to transfer the third-party contract manufacturing for ADVM-043 to a large-scale contract manufacturer." The company said the upgrade is intended to increase the production scale of the gene therapy aimed at treating Alpha-1 Antitrypsin (A1AT) Deficiency, a genetic disorder that can lead to serious respiratory and liver disease. By increasing the production scale, Adverum said that will allow the company to comply with industry standards so "that the same production process is used from clinical trials through commercial stage."
In a statement, Salzman said the company plans to meet with the U.S. Food and Drug Administration (FDA) in early 2017 to review the modified plans and prepare for the dosing trial to being at the end of 2017.
"We are committed to advancing this novel gene therapy for patients with A1AT deficiency, and are planning to be ready to deliver this potential product through a robust commercial-ready manufacturing process," Salzman said in a statement.
That shift in strategy seems to have made investors happy, as pre-market shares of Adverum are up more than 8 percent, hitting $3.99, up from Thursday's closing price of $3.67 per share.
Salzman's CEO spot was announced this morning after serving as chief operating officer of the company following the merger. She served as co-founder, president and chief executive officer of Annapurna Therapeutics prior to the merger, according to her bio on the company website. Before founding Annapurna, Salzman held various roles at various pharmaceutical companies, particularly those with a focus on rare diseases. She also helmed Cardiokine Inc. before that company was acquired by Cornerstone Therapeutics. She also served as a member of GlaxoSmithKline 's R&D executive team where she "planned and managed drug-development projects and clinical trials comprising more than 30,000 patients worldwide," according to her bio.
Former CEO Paul B. Cleveland was named executive chairman of the company's board of directors. He said after 10 months helming the newly formed company it was time to turn over the reins of the company.
Avalanche, the parent company of Adverum, ran into problems last year when analysts began to question its wet AMD drug, AVA-101. Analysts questioned if there was truly any statistical difference between the drug and placebo. Those questions sent share prices of Avalanche down the mountain and Cleveland stepped in to right the company through the questions and the renaming into Adverum.


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HomeWelcome!Past Events (2009-2018)2013 Past Events
Development of Guidelines for School Area Traffic Safety in Manitoba (and Annual Business Meeting)
By Jennifer Chapman, MIT
The December 2013 meeting of the ITE Manitoba Section will be held on Thursday, December 12th starting at 12 noon at the Round Table Steak House and Pub located at 800 Pembina Highway.
Our presenter this month is Jennifer Chapman, P.Eng. Jennifer is a Professional Engineer with the Traffic Engineering Branch at Manitoba Infrastructure and Transportation. In that role, she is responsible for pedestrian crossing issues, capacity analyses, and overseeing MIT's traffic collision database. Prior to joining MIT, Jennifer was employed with ND Lea (now MMM Group). She is the current Treasurer for the ITE Manitoba Section and also sits on a working group committee for the Green Action Centre`s Active and Safe Routes to School Program.
Jennifer`s presentation is entitled, "The Development of Guidelines for School Area Traffic Safety in Manitoba". This recently-completed Guideline was undertaken for MIT by MMM Group. The presentation will give an overview of the Guideline document, which consists of a procedural manual and toolkit and provides direction for both transportation authorities and school divisions to effectively and consistently address traffic safety issues within Manitoba school areas. The Guideline is applicable to rural, urban and suburban school areas.
Following the technical presentation, we will hold a short business meeting to discuss two administrative issues. First, we will seek approval of our budget for 2014. Second, we will discuss our Section Charter and Bylaws. CITE has informed the Manitoba Section that we do not currently have official Charter and Bylaws documents on file with ITE. The ITE Manitoba Executive has therefore developed these documents based on model documents provided by ITE. Where possible, we have drafted them to reflect current practice for ITE Manitoba. There will be an opportunity for discussion at the meeting and then we will ask the membership to approve these documents, at which point we will forward them for approval by CITE.
You may review the draft budget and Section Charter and Bylaws on the Section webpage.
Please note that the price of the luncheon is $20.00 for members and friends and $15.00 for students. Fees will be collected at the luncheon.
Meeting with CITE President
The President of CITE, Peter Truch, P.Eng. PTOE, FITE will be meeting with the ITE Manitoba Executive on November 20th, 2013, 12:00 pm at Brooklyn's Bistro, 177 Lombard Avenue.
ITE Members are invited to join and participate in a discussion on the future of CITE, what we're doing right, and what we can improve on. Peter is doing similar events across the country to help shape a strategy for the next few years.
If you are an ITE Member and interested in participating, please RSVP to David Wiebe at dwiebe@dillon.ca by November 15th. We would love to have you join us. Note that meal costs are not covered by ITE Manitoba.
Transit Oriented Development and the Winnipeg Context
By David Marsh, Dillon Consulting Limited
The November 2013 meeting of the ITE Manitoba Section will be held on Thursday, November 14th starting at 12 noon at the Round Table Steak House and Pub located at 800 Pembina Highway. The cost for regular members and guests is $20. The cost for students is $15.
Our presenter this month is David Marsh, AICP MCIP. Mr. Marsh is a Planner with Dillon Consulting in their Winnipeg office. David is member of the Canadian Institute of Planners and the American Institute of Certified Planners with a Masters degree in Urban Planning from McGill University. Prior to joining Dillon, David was a Principal Planner with the City of Winnipeg and was involved in the development of the Winnipeg Transit Oriented Development (TOD) Handbook, the Complete Communities Direction Strategy, the Yards at Fort Rouge TOD project, and the Southwest Transitway. David is currently the Vice President of IAP2 Canada Prairies Chapter, and is actively involved in Stage II of the Southwest Transitway and several TOD projects.
David's presentation is entitled "Transit Oriented Development and the Winnipeg Context: Key Considerations for Transportation & Planning Professionals". The presentation will provide an overview of what TOD is, the Winnipeg TOD Handbook project, and its relationship with the City's new development plan OurWinnipeg. TOD core principles, and key considerations in terms of transportation infrastructure, trip generation, modal splits, parking, and urban form will be highlighted.
Safety Aspects of Proper Signage and Pavement Markings
By Diane Robinson, 3M
The October 2013 meeting of the ITE Manitoba Section will be held on Thursday, October 10th starting at 12 noon at the Round Table Steak House and Pub located at 800 Pembina Highway. The cost for regular members and guests is $20. The cost for students is $15.
Diane's presentation will include the safety benefits of durable sign sheeting and matched components for traffic control and work zones. She will discuss the use of technology and environmental design to improve road safety, the difference in classifications of reflective sheeting, factors affecting sign performance and ideas from other jurisdictions across Canada.
Diane Robinson represents 3M Canada Traffic Safety and Security Division including retro reflective. She is based in Edmonton and works with the provincial and municipal jurisdictions in the three prairie provinces.
ITE Manitoba Golf Tournament
4th Annual! See the 2013 Golf Tournament page for details.
Tuesday, June 18th, 2013 at 5:00 pm
ITE Manitoba Summer BBQ!
ITE Manitoba is moving outdoors for our final event before a summer break. Please join us at Site 3 of Crescent Drive Park and bring the family!
Details are available here!
By Fiona Blackley, MA (Hons) MSc MCIHT MILT
The May 2013 meeting of the ITE Manitoba Section will be held on Thursday, May 16th starting at 12 noon at the Round Table Steak House and Pub located at 800 Pembina Highway. The cost for regular members and guests is $20. The cost for students is $15.
Fiona's presentation is titled Mobility Management. The presentation will describe this concept which sees the future of urban mobility as being user-focussed, seamless and valued by customers. Mobility Management aggregates the complete transport offer within a city to allow delivery of personalized, customer-oriented services which integrate with the lifestyle needs of the user. Adopting a Mobility Management approach allows cities to create mobility products which are valued and therefore used by its citizens.
Mobility Management products may respond to specific strategic city challenges, address the needs of key market segments or facilitate lifestyle and behavioural change in sectors such as health or tourism. The presentation will build on work being carried out at present in Vancouver and Brisbane where the concept of Mobility Management is being translated into commercial mobility products that together begin to form a system where all transport modes including transit, walking and cycling fit together as part of the future mobility mosaic.
Winnipeg's first Roundabout Corridor – Almost – Bison Drive in Waverley West
By Bob Kurylko, P. Eng. and Brad Cook, P.Eng.
The April 2013 meeting of the ITE Manitoba Section will be held on Thursday, April 25th starting at 12 noon at the Round Table Steak House and Pub located at 800 Pembina Highway. The cost for regular members and guests is $20. The cost for students is $15.
The presentation will highlight some of the considerations in the design development, approval process and detailed features for the design and construction of the first roundabouts on a City of Winnipeg Arterial street, the first two lane roundabout in Winnipeg and the median centered staged construction of two lanes of a four lane divided street. Bob Kurylko and Brad Cook from Stantec will walk the audience through the process that resulted in the construction of the Bison Corridor in Waverley West.
Kean Lew Memorial Student Paper and Presentation Competition Winner
By Mark Reimer
Our presenter this month is Mark Reimer, the winner of the Kean Lew Memorial Student Paper and Presentation Competition. The prize is awarded for an outstanding student paper/presentation submitted to ITE Manitoba. It is given in memory of Mr. Kean Lew,P. Eng., a graduate of the Civil Engineering program at the University of Manitoba and active member of ITE Manitoba, who tragically lost his life in 2009. The award is generously supported by members of ITE Manitoba.
Mark Reimer is currently enrolled as a graduate student in transportation engineering at the University of Manitoba, pursuing a Master of Science degree. His research focuses on freight movement and the transportation systems serving specific industries, namely the petroleum and agriculture industries. Mark's work will benchmark the magnitude and characteristics of industry-related transportation in the prairie region which will help clarify future impacts of policy and transportation network developments that promote, rather than hinder, regional economic development. Aside from his own research, Mark is gaining valuable experience in transportation engineering through research projects with the University of Manitoba Transport Information Group. Mark is also the founding president of the first Canadian student chapter of the American Railway Engineering and Maintenance-of-Way Association (AREMA).
Mark's presentation is titled A Hybrid Approach for Clustering Vehicle Classification Data to Support Regional Implementation of the Mechanistic-Empirical Pavement Design Guide. Emerging infrastructure design practices require an increasingly detailed representation of traffic and loading characteristics. This presentation provides a hybrid approach for analyzing vehicle classification data to develop a set of regional truck traffic classification groups (TTCGs) for use in the Mechanistic-Empirical Pavement Design Guide (MEPDG). The hybrid approach is unique in that it enables analysts to receive the joint benefits of analytical rigor and industry-oriented pragmatism. Benefits of such an approach on regional datasets include: improved statistical strength, datasets that reflect the diversity of truck traffic in a given region, and an improved ability to capture future shifts in truck traffic characteristics. This approach to data analysis can be applied to a variety of challenges involving traffic characteristics and expanded to multi-dimensional analyses.
Wednesday, February 13th, 2013
TAC Pedestrian Crossing Control Guidelines
By Dr. Jeannette Montufar, P. Eng.
Our presenter this month is Dr. Jeannette Montufar, P. Eng., of the University of Manitoba. Dr. Montufar's presentation is on the new TAC Pedestrian Crossing Control Guidelines for Canada.
Dr. Montufar is a professional engineer registered in Manitoba and Alberta, and Associate Professor in Civil Engineering at the University of Manitoba. She is also Principal of Montufar Group, a transportation consulting firm specializing in road safety and freight transportation. Dr. Montufar has done extensive work in the U.S. and Canada on projects dealing with road safety, freight transportation, the application of advanced technologies to commercial vehicle operations, truck size and weight policy, goods movement in urban areas, traffic information systems, and the automation of data collection systems. She has worked for the Battelle Memorial Institute in Columbus, Ohio; the Texas Transportation Institute in College Station, Texas; and the University of Michigan Transportation Research Institute in Ann Arbor, Michigan.
Dr. Montufar is the President of the Canadian Institute of Transportation Engineers.
Whose Fault Is It?
By Lori Garet, P.Eng.
Lori Garet, P.Eng., is a Professional Engineer registered in Manitoba. Prior to completing her degree in 2006 she received a Business Administration Diploma from Red River College as well as a Certificate for Building Construction Technician. She worked in the trucking industry before heading back to school. While in University she made a move into construction, and with her degree finished she started out in the structural field. However, the lure of Transportation was too great and she started with MIT in 2009 and moved to the City of Winnipeg Public Works Department in December of 2010, taking over the role of Traffic Studies Engineer in the Transportation Division.
Lori was a member of the local Arrangements Committee for the CITE conference held in Winnipeg in 2012 and is on the Board of Directors for WAPSO.
Lori's presentation this month is entitled Whose Fault Is It?. Based on the title, it promises to be a tongue in cheek overview of the various branches within the Transportation Division, how things get done, and who to blame when it doesn't!


Human Revolution Clothing (HRC) is a Hawaii-based company founded by Lauren Adelman. Turning her life into one complete mission, Lauren has set out to create a sustainable company, which features organic, GMO free, fair-trade clothes along with hand woven khadi scarves, dresses as well as hand stitched trucker hats. This all started when she had the idea to make organic underwear for yogis and began what she thought was some innocent research into the textile industry. What Lauren discovered was an industry that has been unregulated and unmonitored, leaving it second to oil as the dirtiest industry in the world. Add the fact that more than 90% of the world's cotton is currently genetically modified, signifying cotton as the most chemically intensive crop which requires more toxic carcinogenic insecticides and pesticides than any other crop, left Lauren with a life mission and passion to help change the way clothing is made, seed to shirt.
Before making any products or starting HRC, Lauren went to India to meet many farmers and their families after learning about the mass suicides in the "cotton belt" in India. Over 300,000 farmers in India have committed suicide in the past decade due to increasing costs and low yields of seed and chemicals required for use by genetically modified cotton farming. It is very hard to step away from GMO cotton farming in India, but many small farmers are seeing that is the only way to survive and many of these farmers work harder just to discontinue chemical farming in efforts to save their land and their families.
From over five years of research, HRC was born along with a business model that aligns itself with nature - every part of HRC business is to be done to the best of their abilities and created with every bit of integrity and respect. With that in mind, Lauren hopes to develop the company into a lifestyle brand that focuses on sustainable, organic and recycled materials. Lauren also hopes to start a foundation to help farmers in India purchase drip irrigation, which is a necessity for growing consistent yields of cotton.


I used to adore cooking, way back when my husband was just my boyfriend. The process fascinated me, and because I'm a bit of a purist, every night I'd happily make things the correct way, using the right ingredients. Restaurant dining was our passion, and we'd happily drop way too much money on a meal in a michelin star joint, or be there in the opening week when another hot spot opened up in London. Food and wine - I used to read about it, research it, do courses on it, plan travel arrangements based on it. My particular fascination was South East Asian food.
Then we got married, moved countries and built a house, and we more or less stopped going to restaurants and I became more interested in spending money on furniture. Then we had babies, and it suprised me to find that the spicy and exotic kind of things I wanted to cook was not the kind of thing they wanted to eat. Good Sydney restaurants were something we could splurge on only a few times a year, and sometimes the logistics and guilt associated with childcare arrangements outweighed the pleasure of going out at all.
After a few years of having my culinary efforts rejected night after night by the palates of the under fives, I came to view the evening meal as a horrible chore, one that only produced unnecessary washing up, and very little by way of appreciation. So I kind of abandoned my own food preferences, and just made what they'd eat, and what was easy, and my love of cooking and food stagnated into a distant memory of what seemed like someone else's life.
But now that they're older, and a lifetime of exposure to good tucker has led them to have relatively educated palates, I'm kind of drifting back into cooking.
So, in the absence of any knitting progress, let me share with you one of my kitchen adventures. There is a very cheap and cheerful studenty Asian restaurant here in Wollongong, called Chef's Choice. I'd thouroughly recommend it to any visitor looking for a cheap and decent Asian meal, complete with free jasmine tea from an airpot.
When I go there, I usually have Hainanese Chicken Rice. I remember getting all excited when Po made it on Masterchef, because by complete co-incidence I had bought it for dinner that very night. Last Saturday night I had a go at making it, using a mash up of Po's recipe from the Masterchef website, and the sbs food recipe here.
I got all the ingredients out.
The first step involves making a chicken stock.
The fat from the chicken skin is used to coat the rice in a pan, and then it is cooked in the stock. The local asian grocer that seems to have been bought by an indian family since last time I was there, and the rice selection was completely different. This par-boiled rice is something I haven't seen in there before, it had been hand poured into plastic bags with a label stuck on. It was a little strange, but worked really well, the grains were long and separated perfectly. But they had a completely different texture - almost like a risoni pasta. It reminded me of the old rice a riso we used to get when we were kids, and the purist in me was not impressed.
The eating part of the chicken is poached in aromatic acidulated water. Plenty of ginger, which is my favourite spice.
It was about this time that I set fire to the recipe by accident, so there was a bit of excitement when I had to put out a little fire in the sink!
The dipping sauce is full of ginger and garlic, and is so yummy Adriano Zumbo should make a macaron flavoured with it. Mine didn't turn out quite as perfect as the one at the restaurant though - and to me it is the best part.
By now it felt like hours had past, and I was pretty over the whole freaking thing. My parents rang and asked if the kids wanted to go to their house for a bonfire, sausage sizzle and marshmallow toasting - and no amount of hainanese chicken rice coaxing would talk them out of it.
So it ended up being a meal to go.
And then they ate so many sausages and marshmallows that they weren't interested in it anyway. Husband has always been rather ambivalent about it. Dad only liked the rice. Mum wouldn't touch 'that kind of thing' in a fit, and besides I made it, so it elicited a curled upper lip. So it was really only me who liked it.
Next time I feel like Hainanes Chicken Rice I will remember that for $7.50 someoene else will bring it to me AND do the washing up. And the rest of the family can bite me.
you can make me hainanese chicken any day. also, i would pay you $7.50 at least to see you set fire to something in the kitchen.
This made me giggle, especially setting the recipe on fire - it isn't an episode of Masterchef unless something is set in fire heh heh!
I too would be happy to eat your h.c. rice! And if you like, I will bake something nice for dessert, since I infinitely prefer to bake than cook!
I'm anther Hainanese chicken rice devotee and have just been eating it around Malaysia. Perfect comfort food. In the unlikely event you're ever in Ipoh (tourists about half a dozen a year) go to a restaurant called Hainam. Yum. About $12 for two including a bottle of Tiger beer. I've also, in my past cooking days, made it myself several times. It has to be the most labour-intensive apparently simple dish ever.
I discovered the joys of Hainanese chicken rice earlier this year, impressing the old Chinese lady at my local who told me that "white people never order this". I did have a go at making it myself (adapted a recipe from the NYTimes website) which was quite tasty, but really it's so much easier to just let the experts make it for me! Chicken + rice is my number 1 comfort food.
You did a great job of the Chicken Rice & I am sure it's yummy. I make this dish regularly as my girls love it.
I love Chef's choice....and yes it is better and easier to sometimes just get it from the restaurant. The bonfire looks really good.
oh well atleast you can say you've made it. i like it now that my kids are older and eat anything. but their favs are baked goodies, esp with anything that has chocolate. they demolished an entire choc mud cake last night.


SWANSEA are interested in a loan deal for Liverpool striker Iago Aspas, but chairman Huw Jenkins has rubbished claims that Blackpool winger Tom Ince is set to join the club.
The Swans have been linked with a move for Ince in January, with wingers Pablo Hernandez, Nathan Dyer and Roland Lamah all currently sidelined by injury.
And while Ince is a player Swansea are looking at, Jenkins has played down suggestions a deal is close.
"Looking at young British players, Tom is one of them and he performs well with the England Under-21s," Jenkins told talkSPORT.
"At our club, at our level, we always look for young players we can possibly add to the squad but whether we get any further with Tom Ince or other players remains to be seen.
"At the moment it is pure speculation, but young players are always great to bring in, to see their careers develop, and we feel our club is right for that."
Michael Laudrup is also considering a loan move for Aspas, who has been on the fringes of the Liverpool squad this term.
But Jenkins suggested that there will not be a flurry of January activity at the Liberty Stadium.
"At Swansea we try our best to do our business in the summer and to make sure our squad is more or less right," he said.
"There are times now and again when bringing in the odd player in January can boost morale, boost the team and get results and there's no doubt there are going to be a few clubs that do that before the window ends."


Audi teases the world with its 700HP hybrid Quattro Sport e-Tron concept by showing its sketches ahead of the Frankfurt Motor Show. Now what we have here is another luxury supercar with the all-new Mercedes-Benz GLA-Class, the images leaked ahead of the German motor show.
The design clearly foretold that it's based on CLA four-door coupe aggressively designed. The GLA will use same 2.0 Liter Turbo in FWD or AWD and it's expected to be priced a higher than the CLA that will be a direct competition in line with the new Audi Q3 and BMW X1. Probably this will also inline with the company's own GLK –unless we are near on seeing another leak for a much bigger and expensive GLK model.
Looking forward we are expecting the German floor will be filled with stunning luxury super cars. What are your favorites? The floor might be flavored with luxury range coming from the veterans: BMW, Audi and Mercedes-Benz. Let just see who will steal the show.


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Q: Перевод из одной системы счисления в другую в WindowsForms
Есть конвертер разных систем счисления. Я реализовал перевод с decimal в любую из четырех. Но как сделать перевод с остальных в остальные? Есть ли встроенные функции для этого, именно для Visualc++ & windowsforms? То как сделать такое просто в консольном приложении я знаю, а вот как тут следует сделать - нет.

A: Если вводимое пользователем значение является строкой, то вам подойдет следующий пример для получения dec hex и oct, при этом для каждой системы исчисления необходимо будет модифицировать поток соответствующими флагом (std::dec, std::hex, std::oct):
std::string foo = "0xff";
unsigned bar;
std::stringstream stream;
stream << std::hex << foo;
stream >> bar; // теперь bar хранит число 255.

Вот случай для bin:
std::string foo = "01011011";
std::bitset<32> bar(foo);
unsigned baz = bar.to_ulong(); // теперь baz хранит число 91.

Таким образом, вы получаете число типа unsigned для любого вида строк вводимых пользователем.
Далее передайте полученное ранее число типа unsigned в поток stringstream с соответствующим модификатором (заданным пользователем) и выведете результат на экран.
unsigned foo = 255;
std::string bar;
std::stringstream stream;
stream << std::hex << foo;
stream >> bar; // теперь bar хранит строку "ff".

Подробнее с модификацией строковых потоков можно ознакомится здесь в разделе Format flag manipulators.

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Lescaut in "Manon Lescaut" at La Scala
On March 31, 2019, Massimo Cavalletti will return to La Scala in a new production of Manon Lescaut by David Pountney, singing Lescaut. Riccardo Chailly will conduct. Maria José Siri will sing Manon, Marcelo Álvarez / Roberto Aronica Des Grieux, and Carlo Lepore Geronte. There will be nine performances, running through April 27, 2019.
Cavalletti has sung Lescaut at the world's most esteemed opera houses. Highlights include debuting the Richard Eyre production at the Metropolitan Opera, which was broadcast in HD internationally, as well as appearing as Lescaut at the Deutsche Oper.
Upcoming engagements include the premiere of David McVicars' new production of I masnadieri at La Scala, for which Cavalletti will sing Francesco. Later on in the season, he will reprise that role in the same production at the Savonlinna Opera Festival.
Information about Manon Lescaut at La Scala:
Manon Lescaut; Maria José Siri; Des Grieux: Marcelo Álvarez / Roberto Aronica; Geronte: Carlo Lepore; Edmondo: Alessandro Scotto Di Luzio;
Riccardo Chailly, conductor; David Pountney, stage director
Performances: 31 March; 3, 6, 9, 13, 16, 19, 24, 27 April 2019
news	22:03 , 14/03/2019


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