text:
\section{Introduction}

The accelerated expansion of the universe has led cosmologists
to postulate the existence of a mysterious dark energy
as an explanation, a fluid with exotic properties (very negative
pressure $P \simeq - \rho$, where $\rho$ is the energy density) \cite{AmendolaTsujikawa}. Alternatives
to this {\it ad hoc} dark energy have been proposed, including
the backreaction of perturbations on the cosmic dynamics \cite{Buchert, Buchert2, Rasanen},
living in a giant void \cite{Boleiko}, or
modifying altogether gravity at large scales \cite{Review1, Review2, Review3}.
Even if one accepts dark energy as an explanation,
there are a plethora of models and it is important
to design observational tests which can discriminate
between dark energy and modified gravity, or
between various dark energy models.

Recently,
the concept of turnaround radius has been proposed
as an interesting and promising way to test dark
energy. Since an accelerated cosmic expansion
opposes the collapse of local overdensities and the
formation of cosmological structures, it is not surprising
that, in an accelerating Friedmann-Lema\^itre-Robertson-Walker
(FLRW) universe with a \emph{spherical} inhomogeneity,
there is an upper bound to the radius of an
overdensity of a certain mass, beyond which
this matter cannot collapse but can only expand.
Assuming, for reference, that the universe in which
we live is approximately described by the standard
$\Lambda$-Cold Dark Matter ($\Lambda$CDM) scenario of General
Relativity with a cosmological constant or dark energy, it
has been suggested that the $\Lambda$CDM scenario can be
tested by studying whether the mass-radius relation
of structures in the cosmos respects a theoretical
prescription \cite{Souriau, Stuchlik1, Stuchlik2, Stuchlik3, Stuchlik4, Mizony05, Stuchlik5, Roupasetal, Nolan2014, PT, PTT}.

To be more precise, consider
a spherical configuration of mass in an accelerating FLRW
universe: when the outer layers of this material configuration
 reach zero radial acceleration and collapse under the self-gravity of the perturbation,
it is said that the perturbation has reached its \emph{turnaround
radius} (\cite{PT, PTT}, see also \cite{BlauRollier, DG1, DG2, DG3, DG4, DG5, DG6}). In a decelerated universe there is
no upper bound on the turnaround radius, but in a
de Sitter background with constant Hubble parameter $H=\sqrt{\Lambda/3}$
(where $\Lambda > 0$ is the cosmological constant), there exists the upper bound
\begin{equation} \label{turnaround-lambda}
R_c = {\left( \frac{3GM}{\Lambda} \right)}^{1/3}
\end{equation}
on the turnaround radius, where $R$ is the
areal radius of the Schwarschild-de Sitter (SdS) line element,
\begin{equation}
ds^2 = -\left(1- \frac{2M}{R} - H^2 R^2 \right) dt^2 + \frac{dR^2}{1- \frac{2M}{R} - H^2 R^2} + R^2 d\Omega^2 _{(2)}
\end{equation}
in static coordinates, $d\Omega^2 _{(2)} = d\vartheta ^2 + \sin^2 \vartheta d\varphi^2$ is the
line element on the unit 2-sphere, and $H=\sqrt{\Lambda/3}$ \cite{PT, PTT}.  In Fig.\ref{F:SdS} we plot the trajectories of test particles placed at various radii in the SdS spacetime, with initially zero \ref{sF:zero}, outgoing \ref{sF:out} and in-falling \ref{sF:in} initial velocities.
\begin{figure}
\centering
\subfigure[]{
\includegraphics[scale=0.37]{zero.eps}
\label{sF:zero}}
\subfigure[]{
\includegraphics[scale=0.37]{out.eps}
\label{sF:out} }
\subfigure[]{
\includegraphics[scale=0.37]{in.eps}
\label{sF:in}}
\caption{Radial trajectories of massive test particles in the SdS spacetime subject to zero \ref{sF:zero}, outgoing \ref{sF:out} and in-falling \ref{sF:in} initial velocities. The solid blue line is the location of the critical radius $R_c$ \eqref{turnaround-lambda}.   To make these figures we used the illustrative parameter values $M=1$ and $H=0.1$ for which both the cosmological and black hole horizons are present (dashed lines). $\tau$ is the proper time (an affine parameter) along the geodesics.  \label{F:SdS}}
\end{figure}
The figure shows that the critical radius is not an absolute boundary in the same way a horizon is since timelike geodesics can cross it in either direction. The critical radius is that point beyond which, if you cross outside of it in geodesic motion, you will never cross back without proper acceleration, and \textit{vice-versa}.  This one-way property is also directly visible from the geodesic equation for radial timelike trajectories, which can be shown to be given by
\begin{equation}
\ddot{R}(\tau)=\left(R^3-R_c^3\right)\frac{H^2}{R^2} \label{E:SdS_geodesic},
\end{equation}
where an overdot denotes differentiation with respect to the proper time $\tau$ parametrizing timelike geodesics. We see that for $R>R_c$ we have $\ddot{R}>0$ and for $R<R_c$ we have $\ddot{R}<0$. This is the defining property of the turnaround radius.\footnote{The other geodesic equation for radial motion is
\begin{equation}
\ddot{t}(\tau)-2\left(R^3-R_c^3\right)\frac{H^2}{R^2}\left(1-\frac{2M_\text{MSH}}{R}\right)^{-1}\dot{t}(\tau)\dot{R}(\tau)=0 ,
\end{equation}
where $M_\text{MSH}$ is the quasi-local mass of a sphere of radius $R$.
}

The concept of turnaround radius can be generalized
to arbitrary (but accelerating) FLRW universes \cite{PTT}.
In Ref.~\cite{PTT}, also a Lema\^itre-Tolman-Bondi metric
\begin{equation}
ds^2 = - dt^2 +\frac{R'^2(t,r)}{1+f(r)} dr^2 +R^2(t,r) d\Omega^2 _{(2)}
\end{equation}
is studied, where $f(r)$ is an arbitrary function
related to an initial density profile, and a cosmological
constant $\Lambda$ is present in addition to the usual dust fluid (a prime denotes differentiation with respect to $r$). The authors study shells of
areal radius $R$ and derive their radial acceleration
\begin{equation}
\ddot{R} = - \frac{G \mathcal{M}(r)}{R^2} + \frac{\Lambda R}{3} \,,
\end{equation}
obtaining a turnaround radius
\begin{equation}
R_c (t_c,r_c) = {\left( \frac{3G \mathcal{M}(r_c)}{\Lambda} \right)}^{1/3} \,.
\end{equation}
Here $\mathcal{M} (r) = 4 \pi \int ^R _0 R^2 \rho dR$ is the well-known Lema\^itre
mass and $\rho$ is the density of the cosmic dust in the Lema\^itre-Tolman-Bondi spacetime.

The Lema\^itre-Tolman-Bondi model is only one of the
possible choices to describe a spherical inhomogeneity
embedded in a FLRW universe: other choices exist, for
example the McVittie \cite{FaraoniJacques} and generalized McVittie \cite{McVittie}
metrics, which have been the subject of recent attention \cite{Kleban, Lake1, Lake2,
Roshina1, Roshina2, AndresRoshina, DSFG2012, DaSilvaGuarientoMolina2015, NiayeshDaniel, Horndeski, FaraoniGaoetc} and which describe a generalization of Schwarzschild-de Sitter spacetime to include a time-dependent Hubble parameter $H(t)$. The McVittie spacetime is described by the metric
\begin{equation}
ds^2=-\left(1-\frac{2m}{R}-H^2R^2\right)dt^2+\left(1-\frac{2m}{R}\right)^{-1}dR^2- \frac{2HR}{\sqrt{1-\frac{2m}{R}}} \, dtdR+R^2d\Omega^2_{(2)}
\end{equation}
with $H(t) \equiv \dot{a}(t)/a(t)$  the time-dependent Hubble parameter. The radial geodesic equation in McVittie spacetime is a generalization of eq.~\eqref{E:SdS_geodesic} and it can be shown to be
\begin{equation}
\ddot{R}(\tau)=\left(R^3-R_c^3\right)\frac{H^2}{R^2}+\dot{H}R\sqrt{1-\frac{2m}{R}}\,\dot{t}^2(\tau)
\end{equation}
Note that in the de Sitter case (when $a(t)=\exp(\mathcal{H}t)$ with $\mathcal{H}$ constant), the extra term proportional to $\dot{t}^2$ vanishes exactly.  Therefore, the turnaround property at $R=R_c$ is not an exact result in the McVittie case and the details depend on the precise evolution of the background as well as the time in which the sprinkling takes place. For power-law expansion $a(t)=t^p$ at the radius $R=R_c$ we have
\begin{equation}
\ddot{R}(\tau,R_c)\propto \frac{-1}{t^{8/3}(\tau)}\sqrt{1-\frac{2m}{R_c}}\,\dot{t}^2(\tau) \label{E:stricly},
\end{equation}
which goes to zero at late times, establishing that the sphere $R=R_c$ is critical at late times. In Fig.~\ref{F:McVitte_geodesics} we show congruences of timelike geodesic trajectories starting near the time-dependent radius $R=R_c$  and the (time-dependent) apparent horizons to illustrate this discussion for McVittie.
\begin{figure}
\centering
\subfigure[]{\label{sf:a}
\includegraphics[scale=0.35]{McVitte_captured.eps}
}
\subfigure[]{\label{sf:b}
\includegraphics[scale=0.35]{McVitte_above.eps}
}
\caption{Timelike geodesics with large positive (subfigure \ref{sf:a})  and small positive (subfigure \ref{sf:b}) initial velocities.  The critical radius is the solid blue line and the apparent horizons for McVittie spacetime with $a(t)=t^3$ are the dashed red and orange curves. t is the coordinate time.  \label{F:McVitte_geodesics}}
\end{figure}
The figure shows that it is possible to find geodesics which escape but are subsequently captured by the critical sphere. Note that the result \eqref{E:stricly} shows that the exact critical radius is strictly larger than $R_c$ since $\ddot{R}(t,R_c)$ is always negative inside the horizons.

In any case, when one decides to describe
a large-scale structure (assumed
to be spherical for simplicity) in a FLRW universe, the deviations of
the metric from an exact FLRW one are small (although the density contrast, {\em i.e.},
the ratio between the density of the local perturbation and the average
cosmological density can be large).
By adopting the conformal Newtonian gauge, the
perturbed FLRW metric is written as
\begin{equation}
ds^2 = a^2(\eta)\left[ - (1+2\phi)d\eta^2 +(1-2\phi)\left( dr^2 +r^2 d\Omega^2 _{(2)} \right) \right] \,,
\end{equation}
where $\eta$ is the conformal time of the FLRW background
(defined by $dt=ad\eta$ in terms of the comoving time $t$),
$a$ is the scale factor, and $\phi$ is a post-Friedmannian
potential describing the local inhomogeneity. Here we
neglect vector and tensor perturbations, as is customary
to first order, and we restrict our  discussion to
linear order in the metric perturbations, which
are assumed to be small everywhere. As usual,
the spatial derivatives of $\phi$ dominate over its time derivative,
and we confine ourselves to General Relativity (otherwise
two distinct potentials $\psi$ and $\phi$ would appear in the
metric coefficients $g_{00}$ and $g_{11}$).

In spherical symmetry $\phi = \phi(r)$ and it is possible to
introduce the areal radius
\begin{equation}
R(\eta,r)=a(\eta) r \sqrt{1-2\phi(r)} \,.
\end{equation}
The authors of \cite{PTT} derive the radial acceleration
of a spherical shell in comoving time
\begin{equation} \label{radial_acceleration}
\ddot{R} = - \frac{4 \pi}{3} (\rho_E +3P_E)R - \frac{G \mathcal{M}(r)}{R^2} = \frac{\ddot{a}}{a} R - \frac{G \mathcal{M}(r)}{R^2} \,,
\end{equation}
where an overdot denotes differentiation with respect to the comoving time of the FLRW
background, $\rho_E$ and $P_E$ are the energy density and pressure of the
dark energy propelling the cosmic acceleration, respectively,
\begin{equation}
\mathcal{M}(r) = 4 \pi \int ^r _0 r'^2 \rho(r') dr'
\end{equation}
is the mass contained within the shell of radius $R(t,r)$,
and the energy density $\rho$ includes both the homogeneous cosmological density
$\rho_E$ and the inhomogeneous density of the perturbation.\footnote{However, this expression for the mass is not written explicitly in \cite{PTT}.} It is then straightforward to
derive the radius $R_c$ corresponding to the situation
in which the two contributions, cosmological and
local, cancel out in the right hand side of eq.~(\ref{radial_acceleration}) \cite{PTT},
\begin{equation}
R_c = {\left( - \frac{3 \mathcal{M}}{4 (1+3w) \pi \rho_E} \right)}^{1/3} \,,
\end{equation}
where $w \equiv \frac{P_E}{ \rho_E} <-\frac{1}{3}$ is the equation of state parameter of
dark energy. This expression is taken as the
turnaround radius in a dark energy-dominated
FLRW universe in which $H=H(t)$. For $w=-1$ (the value corresponding to a de Sitter background),
it reduces
to the expression~(\ref{turnaround-lambda}). A similar expression defines the ``sphere of
influence'' used for the same purpose in the literature ({\em e.g.}, \cite{Bushaetal}).

Writing the perturbed FLRW metric in terms of the areal radius and the Misner-Sharp Hernandez quasi-local mass\footnote{We will introduce and motivate the quasi-local mass  more fully in section \ref{S:qlm}. Essentially, $M_\text{MSH}$ measures the total mass/energy inside a sphere of areal radius $R$, including gravitational contributions.}
\begin{equation}
M_\text{MSH}=-\phi R+\frac{H^2 R^3}{2}-H^2 R^3 \phi
\end{equation}
we have
\begin{align}
ds^2&=-\left(1-\frac{2M_\text{MSH}}{R}\right)dt^2+\left(1-\frac{2M_\text{MSH}}{R}+H^2R^2\right)^{-1}dR^2+R^2d\Omega_{(2)}^2\notag \\
&\hspace{25mm}-\frac{2HR}{1-\frac{2M_\text{MSH}}{R}+H^2R^2}\,dR dt
\end{align}
which is ``McVittie-like'', since the McVittie metric is written in terms of the quasi-local mass as
\begin{align}
ds^2&=-\left(1-\frac{2M_\text{MSH}}{R}\right)dt^2+\left(1-\frac{2M_\text{MSH}}{R}+H^2R^2\right)^{-1}dR^2+R^2d\Omega_{(2)}^2 \notag \\
&\hspace{25mm}-\frac{2HR}{\sqrt{1-\frac{2M_\text{MSH}}{R}+H^2R^2}}\,dR dt\, .
\end{align}
We see that the only difference is in the off-diagonal terms in the metric which could arguably be equal to the level of approximation we employ in the FLRW metric.\footnote{Since $M_\text{MSH}=\mathcal{O}\left(\phi\right)$ we have $H^2R^2=\mathcal{O}\left(\phi\right)$ and hence the numerator is $\mathcal{O}\left(\phi^{1/2}\right)$ and the denominator can be split into two products of the square root of itself, one of which contributes $1+\mathcal{O}\left(\phi\right)$ to the numerator and is therefore discarded.} As a linearized solution, however, the perturbed FLRW metric in ``McVittie form" should only be used far from the inner apparent horizon when it exists. Nevertheless, the geodesic structure near the critical radius and its approximate nature carry over from the McVittie case.

We note that:
\begin{enumerate}
\item There is a vast literature on the interplay between cosmological
expansion and local physics (see \cite{CarreraGiulini} for
a review), originating in the ``pure'' relativity community,
which seems to be mostly neglected by the more astrophysically-oriented community working on the turnaround radius
and studying real celestial objects. Here we attempt to bridge between these two
approaches and communities, in view of the fact
that the turnaround radius holds much promise for
testing the $\Lambda$CDM model.

\item Discussions relying on a particular gauge (such as the conformal Newtonian gauge) are gauge-dependent
and one would like, instead, to have gauge-invariant characterizations.

\item The ``mass contained within a sphere'' is defined
in a rather hand-waving way in the literature on the
turnaround radius: should this ``mass'' include
that of the cosmological fluid but not its pressure (as in
\cite{PTT})? Should it include the negative pressure of
dark energy? If not, why not? Should it include only
the local density ({\em i.e.}, energy density minus the cosmological density)? These
questions are not answered, nor asked explicitly, in the
literature on the turnaround test of $\Lambda$CDM.
It is clear, however, that the turnaround spheres considered
contain significant amounts of dark energy and
a relativistic definition of gravitating mass-energy
in them should be used. In other words, the universe
of cosmology is relativistic and regions sufficiently large
should {\em a priori} be treated with relativity and
not with Newtonian physics.
Indeed, the questions above are not trivial: researchers in General Relativity
have wondered for decades about the correct definition
of gravitating mass-energy for a given spacetime,
especially when the latter is not asymptotically
flat (as is the case in cosmology), and have come up
with several quasi-local approaches and mass
definitions (see \cite{Szabados} for a review). There is
now a large consensus that the ``correct'' notion is
the Hawking-Hayward quasi-local mass \cite{Hawking, Hayward}.
We have recently applied \cite{VMA}
the Hawking-Hayward quasi-local mass $M_\text{HH}$ construct to
cosmological perturbations, giving a covariant splitting of this quantity into ``local'' and
``cosmological'' parts which can be used
to separate the gravitational effects of local perturbations
and cosmological background. Although Ref.~\cite{VMA}
studied the growth of structures in the dust-dominated era,
the formalism presented in it is general and can be immediately adapted to the
accelerated era, which is what we set out to do here.
Ref.~\cite{VMA} is not restricted to
spherical symmetry, although it includes the spherically
symmetric case as an example.

\end{enumerate}

Our goals include clarifying the issue of mass within
a turnaround sphere and giving firmer foundations
to the concept of turnaround radius. Although, in practice,
there is at least a 10~--~30~$\%$ uncertainty in the determination
of masses and radii of the astronomical objects used
in the turnaround test of $\Lambda$CDM, vagueness
and uncertainty in the theory do not help
getting firm outcomes for the test.

It turns out that, in a FLRW universe dominated by
dark energy with equation of state parameter $w \simeq -1$,
the difference between the more rigorously defined
turnaround radius and the one used in the astronomical
literature is minimal. The ambiguities inherent in
the definition of ``mass'' are clarified (although the
astronomical uncertainties on the \emph{values} of these
masses, of course, persist). The ``mass''
is here defined in a completely gauge- and coordinate-independent
way (independent of the conformal Newtonian
gauge chosen at the outset for the perturbed FLRW metric).

\section{A rigorous definition of turnaround radius \label{S:qlm}}
Here we approach the issue of cosmological accelerated
expansion versus local physics and that of a rigorous
definition of turnaround radius using the Hawking-Hayward
quasi-local mass. Our assumptions are:

\begin{enumerate}
\item General Relativity is valid (otherwise the Hawking-Hayward
quasi-local energy is not defined and the perturbed FLRW metric is not
given by eq.~(\ref{CNG})).

\item We restrict ourselves to first order in the metric
perturbations (however, density fluctuations can be
large). The perturbed FLRW metric is written
in the Newtonian conformal gauge as
\begin{equation} \label{CNG}
ds^2 = a^2(\eta)\left[ - (1+2\phi)d\eta^2 +(1-2\phi)\left( dr^2 +r^2 d\Omega^2 _{(2)} \right) \right] \,,
\end{equation}
but our final results are gauge-independent. We neglect vector and tensor perturbations in the
metric to this order, and spatial derivatives $\partial_i \phi$
of the post-Friedmannian perturbation potential are
assumed to dominate over the time derivative $\partial_t \phi$.

\item The background is assumed to be a spatially flat
FLRW universe dominated by a single dark energy
fluid with energy density $\rho_E$, pressure $P_E$
and equation of state parameter $w \equiv \frac{P_E}{\rho_E} < - \frac{1}{3}$
(until stated explicitly, we do not assume
that $w$ is constant in time or redshift).

\item The spacetime is spherically symmetric, $\phi = \phi (r)$.
This last assumptions recurs in previous
literature \cite{PT, PTT} and is regarded
here only as a simplification to be relaxed at a later stage, whose
effects are discussed in \cite{Barrow}.
\end{enumerate}

These assumptions exclude the alternative explanations of the present acceleration of the universe mentioned in the Introduction and the present discussion is to be seen as a test of the $\Lambda$CDM model only. For example, even remaining within the context of General Relativity, if backreaction of inhomogeneities is invoked to explain the cosmic acceleration, the background metric is affected and is no longer given by eq.~(\ref{CNG}), and an effective turnaround radius would have to be introduced through an averaging of the physical variables (which we leave for future work).

\subsection{Hawking-Hayward quasi-local mass and its local and cosmological parts}
The physical, gravitating mass of a non-asymptotically
flat spacetime has been the subject of much debate
in General Relativity and, after extensive work on
quasi-local energies \cite{Szabados}, the community
seems to have settled on the Hawking-Hayward construct \cite{Hawking, Hayward}.
There is little doubt that
when a region of spacetime of size not entirely negligible
in comparison with the Hubble radius $H^{-1}$ is considered,
a relativistic (as opposed to Newtonian) mass-energy
causing gravitational effects needs to be employed.
The Hawking-Hayward quasi-local mass in defined as
follows \cite{Hawking, Hayward, Hayward2}. Let $S$ be a closed, orientable, 2-dimensional
surface. Let $\mathcal{R}$ be the induced Ricci scalar on $S$
and consider the outgoing and ingoing congruences of
null geodesics from $S$, which have expansion
scalars $\theta_\pm$ and shear tensors $\sigma_{ab} ^{(\pm)}$, respectively.
Let $\omega^a$ be the projection onto $S$ of the commutator
of the null normal vectors to $S$ (``anholonomicity''),
then the quasi-local mass of $S$ is
\begin{equation}
M_\text{HH} \equiv \frac{1}{8 \pi} \sqrt{\frac{A}{16 \pi}} \int \mu \left( \mathcal{R} + \theta_+ \theta_- -\frac{1}{2} \sigma_{ab} ^{(+)} \sigma_{(-)} ^{ab} - 2 \omega_a \omega^a \right) \,,
\end{equation}
where $\mu$ is the volume 2-form of $S$ and $A$ is its area \cite{Hawking, Hayward}.

In the geometry (\ref{CNG}), the Hawking-Hayward  mass of a surface $S$
corresponding to a sphere in the unperturbed FLRW
background was computed, to first order in the
perturbations, in Ref.~\cite{VMA}. The result becomes
particularly simple in spherical symmetry in which
the Hawking-Hayward mass reduces \cite{Hayward2} to the better
known Misner-Sharp-Hernandez mass \cite{MisnerSharp, HernandezMisner}.
The result is \cite{VMA}
\begin{equation} \label{MSH}
M_\text{HH} = ma + \frac{H^2 R^3}{2} \left( 1-\phi \right)
\end{equation}
where $m$ is the Newtonian mass obtained by
integrating $\phi$ over a sphere, $m= \int \nabla ^2 \phi \, d^3 \vec{x}$,
and is constant.
The physical mass scale of the perturbation described by $\phi$,
like physical length scales, is obtained
by multiplying by the scale factor (more on this later).
In units in which $G = c = 1$, $2 m$ gives the comoving Schwarzschild
radius scale of the perturbation, while the physical
scale is $2 m a$. Since $\phi \simeq - m/r \simeq - m a/R$
to first order, where
\begin{equation}
R = a r \sqrt{1- 2 \phi} \approx a r (1 - \phi)
\end{equation}
is the areal radius of the perturbed FLRW space in spherical
symmetry, we can make the approximation
\begin{equation} \label{approx}
M_\text{HH} \simeq ma + \frac{H^2 R^3}{2}
\end{equation}
to this order. Note that the factor $HR$, the ratio of
the size of a sphere of areal radius $R$ to the Hubble radius $H^{-1}$,
is small for the structures that we will consider, and it appears
to the second power in eq.~(\ref{MSH}). The decomposition (\ref{approx}) splits
the Hawking-Hayward/Misner-Sharp-Hernandez mass into
a ``local'' part $ma$ and a ``cosmological'' part $H^2R^3/2$.
It was shown in \cite{VMA} that this decomposition is
covariant and gauge-invariant to first order, in spite of starting with the
particular gauge (\ref{CNG}).

Eq.~(\ref{approx}) is particularly suited for quantifying the competition between cosmological
expansion and local physics, since the gravitational effects
are due to the physical gravitating masses of the local
structure and of the surrounding cosmology. The criterion
defining the {\it critical} (turnaround) radius for a system
on the verge of breaking down is now that for
such a system the two contributions to $M_\text{HH}$ are equal,
\begin{equation} \label{equal}
m a = \frac{H^2 R^3}{2}
\end{equation}
which yields
\begin{equation}
R_c (t) = \left( \frac{2 m a}{H^2} \right)^{1/3}
\end{equation}
for the critical radius. With this definition there are no
ambiguities in the concept of mass contained in the
sphere of radius $R_c$ (more about this later). Note that eq.~(\ref{equal})
equating the two contributions to $M_\text{HH}$ makes it explicit that
we are in an intermediate regime in which local
gravitational effects are comparable with cosmological ones.
This is the ``gray'' area lying in between the Newtonian
regime $R \ll H^{-1}$ in which cosmological effects are
negligible, and the FLRW regime $R \sim H^{-1}$ in which
relativistic cosmology dominates.
By using the Hamiltonian constraint
\begin{equation}
H^2 = \frac{8 \pi}{3} \rho_E
\end{equation}
for a spatially flat FLRW background dominated by dark
energy, one obtains
\begin{equation} \label{critical_radius}
R_c (t) = \left( \frac{3 m a}{4 \pi \rho_E} \right)^{1/3} \,.
\end{equation}
Let us assume now that the equation of state parameter $w$ is constant; then using the relations valid for the FLRW background
\begin{equation} \label{scale_factor}
a(t) = a_* t^{\frac{2}{3(1+w)}} \,, \qquad
\rho_E (t) = \frac{\rho_0}{a^{3(1+w)}} \qquad (w \neq -1) \,,
\end{equation}
where $a_*$ and $\rho_0$ are constants, the critical radius is seen
to vary with the scale factor as
\begin{equation}
R_c (a) =  \left( \frac{3 m }{4 \pi \rho_0} a^{3w + 4} \right)^{1/3} \equiv R_0 \, a^{\frac{3w+4}{3}}
\end{equation}
(which makes it clear that the ``critical sphere'' is not comoving)
and where the constant $R_0$ is
\begin{equation}
R_0 \equiv  \left( \frac{3 m}{4 \pi \rho_0} \right)^{1/3} =  \left[ \frac{9 m (1+w)^2}{2 a_* ^{3(1+w)}} \right]^{1/3} \,,
\end{equation}
where the relation
\begin{equation}
H = \frac{2}{3(1+w)t} = \frac{2 a^{\frac{3(1+w)}{2}}}{3(1+w) a_* ^\frac{3(1+w)}{2}}
\end{equation}
has been used. By showing explicitly the physical local mass $ma$,
one has instead
\begin{equation}
R_c (a) =  \left( \frac{3 m a}{4 \pi \rho_0} \right)^{1/3} a^{w+1} \,.
\end{equation}
As a function of time, the critical radius is
\begin{equation} \label{Rct}
R_c (t) = \left( R_0 a_* ^{\frac{3w+4}{3}} \right) t^{\frac{2(3w+4)}{9(w+1}}
\end{equation}
for $w \neq -1$. For $w=-1$, corresponding to a de Sitter background,
it is instead
\begin{equation}
R_c (t) = R_0 a^{1/3} = R_0 \, a_*^{1/3} \, \mbox{e}^{H_0 t/3} \,.
\end{equation}
The exponent $\frac{2(3w+4)}{9(w+1)}$ in eq.~(\ref{Rct}) is
\begin{itemize}
\item positive if $w < -\frac{4}{3}$ or $w>-1$,
\item negative if $-\frac{4}{3} < w <-1$,
\end{itemize}
and vanishes in a phantom universe with $w=-4/3$,
in which $R_c$ remains constant (a rather odd occurrence).
We can express $R_c$ as a function of redshift $z$ using
$a_0/a = z+1$, where $a_0$ is the present
value of the scale factor. The result is
\begin{equation}
R_c (z) = \left[ \frac{3 a_0 ^{3(w+1)}}{4 \pi \rho_0} ma \right]^{1/3} \frac{1}{\left( z+1 \right)^{w+1}} = \frac{R_c (0)}{\left( z+1 \right)^{w+4/3}}
\end{equation}
if we insist on using $ma$ as the local mass, where
\begin{equation}
R_c (0) = \left( \frac{3 m \, a_0 ^{3w+4}}{4 \pi \rho_0} \right)^{1/3} \,.
\end{equation}

By setting the present value $a_0$ of the scale factor to unity,
as customary, one obtains the equation of state parameter
of dark energy as a function of the redshift and the mass $ma$
\begin{equation} \label{w_z}
w(z) = -1 + \frac{1}{\ln(z+1)} \left\{ \ln \left[ \left( \frac{3ma}{4 \pi \rho_0} \right)^{1/3} \frac{1}{R_c (z)} \right] \right\} \,,
\end{equation}
which can be used to constrain $w$ if $ma$ and $R_c$ are known.

The Hawking-Hayward mass of a ``critical sphere'' of radius $R_c$ is
\begin{equation}
M_c \equiv M_\text{HH} (R_c) = ma + \frac{H^2 R_c^3}{2} = 2ma = H^2 R^3 _c = \frac{8 \pi}{3} \rho R^3 _c
\end{equation}
by definition, and it includes both the ``local'' mass
$ma$ due to the perturbation and the contribution of the energy
density of the cosmic fluid. When $m$ is constant,
$M_\text{HH} (R_c)$ is ``comoving'', while $R_c$ is not.

\subsection{Comparison with the previous definition of $R_c$}
We are now ready to compare our $R_c (t)$ with previous
definitions. Since the ``mass''  $\mathcal{M} (r)$ contained in a sphere
of areal radius $R$ is not clearly defined in previous literature,
care must be taken in this comparison. The authors
of \cite{PTT} obtain
\begin{equation}
R_c ^{(1)} = \left( \frac{3 \mathcal{M} (r)}{4 \pi |1+3w| \rho_E} \right)
\end{equation}
where it is argued that $\mathcal{M} (r) = 4 \pi \int _0 ^r r'^2 \rho(r') dr'$
and $\rho$ includes the homogeneous energy density (but not the pressure)
of dark energy and the density of the perturbation.
Based on our previous discussion, this would imply
the correspondence $\mathcal{M} \leftrightarrow 2ma$ and
\begin{equation} \label{ratio}
\frac{R_c}{R_c ^{(1)}} = \left( \frac{|1+3w|}{2} \right)^{1/3} \,.
\end{equation}
For $w \approx -1$ this ratio is almost unity. Therefore,
our calculation can be regarded as a rigorous justification
of the expression of $R_c$ previously obtained in \cite{PTT}
(with a small correction), plus an important clarification
of the meaning of ``mass in the sphere of radius $R_c$''.
Since the idea is to constrain $w$, however, it is best not
to assume the value of this quantity and to use eq.~(\ref{critical_radius}) for the value of $R_c$ and
eq.~(\ref{ratio}) for its relation with previous literature.

If the equation of state parameter $w$ is not constant, using
the covariant conservation equation
\begin{equation} \label{conservation}
\dot{\rho}_E + 3 H (P_E + \rho_E) = 0 \,,
\end{equation}
differentiating the relation $a_0/a = z+1$ to
obtain $dt = - \frac{a_0 dz}{\dot{a} (z+1)^2}$, and integrating eq.~(\ref{conservation}) yield
\begin{equation}
\int dz \, \frac{w(z) +1}{z+1} = \ln \left[ \left( \frac{3ma}{4 \pi \rho} \right)^{1/3} R_c ^{-1} \right]
\end{equation}
which, for $w=$~constant, reduces to eq.~(\ref{w_z}).

\section{Dynamics of the critical sphere}
Let us consider the ``critical sphere'' of radius $R_c (t)$, which
contains a system on the verge of breaking down under
the influence of the cosmic acceleration. Without assuming $w=$~constant,
the differentiation of eq.~(\ref{critical_radius}) yields, in conjunction with
the covariant conservation equation (\ref{conservation}),
\begin{equation} \label{rate}
\frac{\dot{R}_c}{R_c} = \left( w+ \frac{4}{3} \right) H \,,
\end{equation}
which quantifies the deviation of the critical sphere from
the comoving motion of the cosmic substratum.
In an accelerated universe with $w <- 1/3$, the critical
sphere grows slower than the cosmic substratum, while
it grows faster in a decelerated universe in which it is
easier for large structures to collapse. By further
assuming $w=$~const. and using the scale factor~(\ref{scale_factor}),
eq.~(\ref{rate}) becomes
\begin{equation}
\frac{\dot{R}_c}{R_c} = \frac{2(w+4/3)}{3(w+1)} \, \frac{1}{t}
\end{equation}
for $w \neq -1$, which tends to zero as $t \rightarrow + \infty$ and integrates to
\begin{equation}
R_c (t) = R_* t^{\frac{2(w+4/3)}{3(w+1)}} \,.
\end{equation}
In the de Sitter case $w=-1$, instead,
\begin{equation}
R_c (t) = R_* \exp \left[ \left( w + \frac{4}{3} \right) H_0 t \right]
\end{equation}
where $H_0 \equiv \sqrt{\Lambda/3} =$~const.

The physical volume $V_c$ of the critical sphere, of course, obeys
\begin{equation}
\frac{\dot{V}_c}{V_c} = 3 \, \frac{\dot{R}_c}{R_c} = \left( 3w+4 \right) H \,.
\end{equation}
The Hawking-Hayward/Misner-Sharp-Hernandez quasi-local
mass contained in the critical sphere is
\begin{equation} \label{Mc}
M_c = \frac{8 \pi}{3} \rho_E R_c ^3 = H^2 R_c ^3
\end{equation}
and its time derivative is easily found to be
\begin{equation} \label{Mc_dot}
\dot{M}_c = ( H R_c)^3 = \frac{6ma}{H^{-1}}
\end{equation}
using eqs.~(\ref{conservation}) and (\ref{rate}) and without assuming $w=$~const.
Thus, $R_c$ is the fraction $(\dot{M}_c)^{1/3}$ of the Hubble radius
$H^{-1}$. Taking the ratio of eqs.~(\ref{Mc_dot})
and~(\ref{Mc}) yields
again the result that $M_c$ is comoving, $ \dot{M}_c/M_c = H$, which
we already know since it was previously established
that $M_c = 2ma$.

\section{Conclusions}

The mathematical splitting of $M_\text{HH}$ gives nearly the same
numerical result as previous literature for the turnaround radius.
This is reassuring since it inspires confidence in the
use of the formal quantity $M_\text{HH}$ in astrophysics, because
its application reproduces almost exactly results obtained with less formal reasoning based on the motion of test and
gravitating particles and fluids, but puts those
results on a firmer theoretical ground. Thus far (with the exception of Ref.~\cite{VMA}), the Hawking-Hayward mass has been used only in formal contexts and computed only
for analytical solutions of the Einstein equations, but is should be useful also in more practical and astrophysically relevant situations.

We have shown that the spherically symmetric perturbed FLRW metric is equivalent to a McVittie spacetime and we have provided an exact analysis of the turnaround radius in the latter case. We note that the McVittie metric is a good approximation to the FLRW metric near the turnaround radius as defined by our quasi-local mass splitting, which sits well inside the inner apparent horizon at late times when one exists.

Following previous literature, we have considered only
spherical symmetry in this work. The limitations of this
assumption and the quantitative effects of non-sphericity
have been debated in the literature \cite{Barrow}. A background-free discussion without specifying a FLRW background or requiring spherical symmetry should be possible on the lines of Refs.~\cite{Buchert}-\cite{Boleiko}.   The
splitting of the Hawking-Hayward quasi-local mass in
\cite{VMA} is general, and will be applied to non-spherical
situations in future work.

\acknowledgments
This work is supported by the Natural Science and Engineering Research Council of Canada and by Bishop's University.


text:
Q: Infinte sum, find value that makes it converge I think that this is pretty basic, but I just can't seem to figure it out. I've tried all of the approaches that I can think of, and I can't seem to find the expression for the Nth sum. The Sum is given by:
$$\sum_{n=1}^\infty \frac{1}{(a^n+1)}$$
And I have to find the values of $a>0$ that makes this sum converge, but I can't figure out how to do this. I thought about comparing it with the sum for $1/a^n$ because I guessed that this would converge for $|x|<1$, since we have learned that this goes for $x^n$ but I'm not sure whether it goes for $x^{-n}$ too, but that didn't seem to work. And I tried to see if the integral of $f(x)$ would converge but them there appeared a lot of $\ln(a^t)$ that would end up as $\ln(0)$. But I am guessing that I have to split it into the case where $a<1$ and $a>1$. A hint would be really nice :)

A: If $a = 0$ or $a = 1$ the series is obviously divergent.
If $a>1$ we write
$$\frac{1}{a^n+1} = \frac{1}{a^n}\frac{1}{1+a^{-n}}\le\frac{1}{a^n}.$$
This shows that the series converges for $a>1$.
If $0<a<1$ we have that the sequence $a^n$ is decreasing, so that $\tfrac{1}{a^n+1}$ is bounded below and the series cannot converge.

For $a<0$, we split the sequence into terms with $n$ even and $n$ odd, and check convergence for both separately:
$$\sum_{n=0}^\infty\frac{1}{a^n+1} = \sum_{k=0}^\infty\frac{1}{b^{2k}+1} + \sum_{\ell=0}^\infty\frac{1}{1-b^{2\ell + 1}}$$
where $b=|a|$. By what seen above, the first term converges if, and only if $b>1$. For the second term, we rewrite
$$\frac{1}{1-b^{2\ell + 1}} = \frac{1}{1-b}\frac{1}{1+b+\ldots+b^{2\ell}}\le\frac{1}{1-b}\frac{1}{1+b^{2\ell}}.$$
Again by what we have seen above, this gives convergence in the case where $b>1$.

In conclusion, we have that the series converges if, and only if $|a|>1$.

A: Hint: Try to split it into two cases:

*

*$ 0 < a\le 1$. Think of the divergence test.

*$a >1$. Then $a^n > 1^n = 1$. Then try to use comparison test.

redpajama_set_name: RedPajamaStackExchange


text:
Russell C. Stinnett, 90 Set 2 P.M. Thursday
Published 4:44 pm Tuesday, August 17, 2010
BUCKINGHAM, Oct. 27 – Russell Coleman Stinnett, 90, of Buckingham, died Saturday, October 24, 2009 at the McGuire VA Medical Center in Richmond.
He was born May 23, 1919 in Monroe, a son of the late Russell A. and Ida C. Stinnett. He served in the United States Army for nine years. During World War II, he was in five major battles including the Battle of the Bulge. He was later employed by AMF in Richmond.
Surviving are his wife of 56 years, Sarah Stinnett of Buckingham; a daughter, Georgianne Stinnett of Richmond; and nieces and nephews. In addition to his parents, he was preceded in death by three sisters; four brothers; and nieces and nephews.
The family will receive friends at Dunkum Funeral Home on Wednesday from 7-9 p.m.
A funeral service will be conducted at Antioch Union Baptist Church at 2 p.m. on Thursday with burial in the Wright family cemetery.
Memorial gifts can be made to Antioch Union Baptist Church, 2810 Greenway Road, Wingina, VA 24599, or the Buckingham County Volunteer Rescue Squad, P.O. Box 444, Dillwyn, VA 23936.
Dunkum Funeral Home, Dillwyn, is in charge of arrangements.
Jane B. Chapman, 89
OCTOBER 27 – Jane Barr Chapman, 89, of Farmville, passed away, Friday, October 23, 2009 in Farmville.<br /> Mrs. Chapman... read more

redpajama_set_name: RedPajamaCommonCrawl


After reading the Sydney Morning Herald and many SEO/SEM blogs, It seems to be confirmed that Google has performed a new Page Rank Update over the last couple of days.
Many search engine marketing blogs and major newspapers (Washington Post, Forbes etc..) and publishing network (Weblog Inc) have been penalised with a Page Rank drop.
SEO Sydney Blog has however noticed a serious improvement from a PR:0 to PR:3 and seems to confirm the effectiveness of our link building strategy.
The last major Google Algorithm update took place in Mid-July and aimed at decreasing the value of links originating from 'bad neighborhood' and irrelevant websites.
* Paid Linking : The easy excuse is that they're targeting paid links, but not all sites which experienced the drop sell or buy links.
* Mass Linking : Do we link out to too many sites via Blog Rolls? Does Linkbait just result in TOO MANY links, even if they are natural. Do blog networks use influential linking to their advantage? I think PageRank has been spread too thin and Google is changing its PageRank formula to address the mass publishing which has taken place over the past 2 years.
* Devalue PageRank : PageRank is seen by many as the end all value of a web site. Our PageRank dropped but we are receiving more Google search traffic than ever. PageRank does not define site rankings in Google or traffic and it should not be mistaken as so.
More accurate explanation should emerge in the next couple of days.


It's One Shoe's 9th anniversary!
Exactly nine years ago Floris Derksen and Michel van Velde started One Shoe.
Since the launch of One Shoe in 2006 (at their coffee table) we have grown to our current operations as a fully integrated advertising and digital agency in our present building on Janskerkhof.
The hard work of our team put us on the map and our commitment to high-end creative innovation keeps us there. Because we have been working with Drupal for more than 9 (!) years, it is time to look back on our efforts for the Drupal community.
And... we'll keep on going! We have set some exciting new challenges for us and we look forward to the next nine years!


I've been to the Sea Isle City workshop. I highly recommend it. Check out other workshop opportunities on the web site below.
and make the marble younger.
Who guessed stones were prone to age?
who Verna was infatuated with at 14.
and has an affinity for gray cats.
of salt in the bowl.
and I screwed open too easily.
after I made the bed.
the audition to be Job's wife.
Have you seen the latest issue of Arbella? If not, you should. Tom's included some really interesting writing, photographs and drawings. I especially love the back cover photograph by Andrew M. Daddio, "The Loraine Diner Series/#18-End of the Meal."
Television Daddy is in the 13th row, 4th book in. Or snail mail the order form below.
____ Enclosed is my check, payable to Finishing Line Press for $ ____________.
Ed Galing's poetry, through the use of simplistic form and language, tackles subjects that are complex and extremely relevant today, given our current economic climate. Galing is 91 years old and is still writing. He is an inspiration and a talented poet. I had asked him to read for PoetsWednesday a couple of years ago, but the trip from PA was too much for him. I read several of his poems at the Barron Arts Center and they were well received. With the permission of Iniquity Press/Vendetta Books, Dave Roskos was gracious enough to let me print these three poems from Buying A Suit On Essex Street. I hope you enjoy these poems as much as I do. My childhood was somewhat similar. I, too, grew up in a cold water flat. I understand all that is related to that lifestyle such as warming yourself near the kitchen stove, heating stones in order to warm the sheets before bed, and very discretionary spending. Ed Gailing has a gift. He finds beauty in places that most people refuse to look, and is at home where no one wants to live. That's poetry.
bagels at an early age.
pay some attention to her.


strategies to get Super Rich in the opportunity market.
Each pretty morning, while most of the people are still sleeping, I look up my email account And earn the benefit of my C- Concept business: Hundrets of new subscribers Have come to my blogs. They start as subscribers, then develop As donators, authors and editors. Few, I can set later to be administrators. They create value by Publishing own essays and articles, Leading to their landing pages For goods, services and value content.
using scientific advertizing will bring You much benefit. Three masterplan strategies shall be scored out here.
I founded my company ROSARY in 2004 (the video stream shows my friend and social charity club founder Pastor John Chacko and my mother in Law, Martha Ringwald (+).) to hold the patent rights of my invention ROSARY Ridgebed Roundabout. This is registered as a low-profit- company. The maximum amount of real Pure Leverage after Taxes shall be under 23,000 € that equals 25,000 $ a- Year!- This gives freedom to make easy bilances to build accountable income streams online.
Use Your medieval PureLeverage.com network to generate a Big list of subscribers.


text:
The Amalgamated
Charles Parkman
San Diego Music Awards nominates The Amalgamated for Best World Music Album
The Amalgamated have been nominated for their album "Premium Quality". The album was recorded at After Hours Studio in Ramona, CA. Released in September 2018 it is a collection of some of the great songs that inspired the sound of the band.
The Best Album categories are not voted on by the listening public, the San Diego Music Awards enlists a large group of experts known as "The Academy". This is a stellar collection of Musicians, Venue owners, Bookers, Promoters, Journalists, Radio and Television personalities. These individuals are very knowledgeable and involved in the San Diego Music Scene.
The Awards Ceremony is at 6 pm on March 11 at The House of Blues, San Diego. Tickets can be purchased through the SDMA website.
Proceeds from ticket sales go to The San Diego Music Foundation. They are partnering with Taylor Guitars to get more musical instruments in San Diego Schools.
We are incredibly honored to be nominated and hope to see you at the awards show. We would like to thank everyone who has supported the band since 2007.
Mad Caddies with The Amalgamated and Jon Gazi
On October 25th, Mad Caddies will be at Brick by Brick as part of their west coast tour with John Gazi and The Amalgamated!
Get your tickets here


The optical module is intended for advanced authenticity verification of passports, ID cards and other travel documents, visa stamps and seals, including but not limited to entry permits, banknotes, driving licenses, vehicle registration certificates and other vehicle related documents, signatures and handwriting fragments, revenue and special stamps, securities and other documents with security features.
Regula 4178 is a compact USB device constructed in plastic body in the form of a base for a spectral luminescent magnifier Regula 4177. The device power supply, control, displaying and processing examination results are carried out via a PC and Regula Forensic Studio software.
The optical module widens the spectral luminescent magnifier field of view. The device is equipped with additional light sources.
security fibers, planchetes, security threads, holograms, foil stamping, pole feature, transparent vanish coating, etc.
intaglio: texts, guiloche frames, rosettes and vignettes, microprinting, latent images and moire patterns, signs for the visually impaired, blind embossing, colour shifting ink, including OVI with embossing and latent images, etc.
letterpress: serial numbers, texts, barcodes, etc.
offset printing including Orlov and rainbow printing: texts, microprinting, moire patterns, background and anti-copy patterns, etc.
screen printing: security features with optically variable effects, etc.


text:
Q: Как можно решать ряды подобного типа? Есть вот такой ряд, каким образом в цикле можно добавлять блоки (a + 1) к знаменателю в формуле?

double result = 0;

for (int i = 1; i < n; i++)
{
    result += factorial(i) / Math.Pow(a, i + 1);
}

Этот код подходит только для первой части этой серии, как при следующей итерации я могу добавить в формулу блок (a + 1)?

A: Поделите i-ое слагаемое на (i-1)-ое, получится
d_i = i!/ ((i-1)! a (a + 1) ... (a + i - 1)) = i/(a (a + 1) ... (a + i - 1))

для i >= 1.
Имея первое слагаемое и зная d_i, можно последовательно вычислять следующие слагаемые и накапливать сумму.
Теперь, как подсчитать d_i? Числитель у нас есть, а на знаменатель h_i = a (a + 1) ... (a + i - 1) можно составить аналогичное итеративное соотношение:
h_i / h_(i-1) = a + i - 1

для i >= 2.
Таким образом, на каждом шаге находите h_i, потом d_i, потом текущее слагаемое.
Код не даю, поскольку это явно учебное задание.


text:
Europs bilineatus es una especie de coleóptero de la familia Monotomidae.

Distribución geográfica
Habita en Nicaragua.

Referencias

Bilineatus
Coleópteros de Nicaragua

redpajama_set_name: RedPajamaWikipedia


text:
Wildlife given clear path with new overpass in Yoho National Park
Michael Franklin CTVNewsCalgary.ca Senior Digital Producer
@CTVMFranklin Contact
Published Thursday, June 7, 2018 5:26PM MDT Last Updated Thursday, June 7, 2018 6:54PM MDT
Crews are now putting the finishing touches on a large scale project in Yoho National Park aimed at reducing the risk of wildlife deaths on the Trans-Canada Highway and helping populations thrive.
Since spring 2017, workers have been building a $6.6M, 60 metre wide wildlife overpass, the largest structure of its kind in the mountain parks and very first for Yoho.
Officials say the pathway will help animals easily cross the highway to access food sources and intermingle with other populations that would otherwise be inaccessible without the risk of being hit by vehicles.
Trevor Kinley, a biologist, says placement of the overpass was carefully planned.
"We put it in this location because it's near to a goat lick and we are trying to encourage long term for those goats that move across but also to encourage use by all other species."
He says that the only way they were able to build such a project was that the Trans-Canada Highway was being twinned at the same time.
"We don't build many of these; they are challenging to build. Our one chance to build them is when we are twinning the highway. We kind of go all-out when we get the opportunity."
The idea of overpasses built specifically for wildlife isn't new. The structures have enjoyed quite a bit of success in the Bow Valley with six of them built in Banff National Park.
Kinley says the bridges are just one part of the wildlife crossing network.
"One is the actual structures, the overpasses and underpasses, and the other part is the fencing. What keeps animals from getting killed on the highway is the fencing but of course, if you just build fencing it would block all that movement."
Seth Cherry, a wildlife pathologist, says specific things needed to be taken into account when it came to building the overpasses.
"In choosing this location, we look at a number of things. First we look at modelling animal movement on a large landscape scale that's even broader than Yoho National Park. We look at where animals are likely to be moving long distances and where they are crossing the highway so we get a general idea of our high potential crossing areas."
He adds that a lot of work is also done to make sure that wildlife, specifically those species sensitive to the racket of a busy highway, aren't disturbed while crossing.
To do that, workers installed a berm on either edge of the crossing and filled it with native trees, grasses, rocks and vegetation to make the man-made structure appear exactly as the park itself.
"Our hope is that eventually an animal will be able to stand where I am right now and look around and it will be very difficult to tell that it is on a man-made structure and not just part of the natural landscape."
Once the landscaping is finished in the next few weeks, monitoring cameras will be installed and the overpass will be completely sealed away from human contact, to avoid any scents that would scare off wildlife.
"We don't want the scents of people up here for wildlife that might deter them from crossing. Once this is open to wildlife, it's only for wildlife," Cherry says.
The wildlife crossing network is made up of 38 underpasses and six overpasses in Banff and three underpasses in Yoho.
There are no plans to build further wildlife crossing pathways further west at this time.
(With files from Kevin Green)
The 60 metre wide wildlife crossing was made possible by a twinning project for the Trans-Canada Highway.
Crews are landscaping the surface of the wildlife overpass to make it seem exactly as the park around it.
The overpass was specially designed to prevent noise from the Trans-Canada Highway from disturbing the animals using it.
Calgary hospitals filling as COVID count climbs


The company was founded back in 1989, by Peter Tribeman, in Boston, Massachusetts. Since then, Atlantic Technology has become one of the largest specialist THX loudspeaker manufacturers in the world.
Peter had already become one of the most important innovators and engineers in the then new field of Home Cinema. Peter was the leading engineer on a project undertaken with Lucasfilm to develop a home decoder for the groundbreaking surround audio track on The Empire Strikes Back. Since then he has become one of the most influential designers in the home cinema scene; every product reinforces his commitment to high performance and high value.
Unlike most speaker companies that package together five random speakers and a sub-woofer and call it a matched 'Home Cinema System', they design, engineer, and build integrated multichannel speaker systems.
So if you are after a perfectly matched, voiced and high quality freestanding speaker system, or want the perfect flat screen speaker system with acoustically matched rear/surround in-ceiling speakers (and a sub to complement) - then look no further than Atlantic Technology.


We provide the first cross-sectoral description of local consumption markets. Detailed credit card data show consumers have limited mobility and manage the spatial dimension of their transactions. In more frequently purchased sectors, expenditure declines faster with distance; further, the spatial distribution of transactions becomes more concentrated with income and less affected by travel cost shocks. We propose a simple theory of storability/durability of a sector's output as a new dimension affecting local consumption markets, and provide evidence that consumer mobility influences local employment, establishment density, and establishment size differentially across sectors. Consumers' spatial behavior appears important for analyzing local shocks.


The club has been profiled on a double centre spread in this week's Gaelic Life newspaper. An interesting read!
Ballyhegan Park will host St Oliver Plunkett's Primary School Blitz next Thursday 31st May 2012 starting at 10am. If anyone is available to help or support, please do!
If there is anyone interested in representing the club refereeing GO games (U12s), please get in touch. Training is provided! This opportunity is open to everyone, young (good for your CV) and old, male & female!


The rfc HTTP Connections to ABAP System(XI_INTEGRATIONSERVER) fails with error 'HTTPIO_PLG_CANCELED' in one client while the same rfc connection is executed successfully in other client of the same system.
The HTTP communication of this application server is not functioning correctly.
Please suggest how to rectify this rfc error.
I believe this is an issue with your ICM parameters.
Whats the value of icm/server_port_0? is HTTP active in SMICM?
But in the same system, when i test the http rfc connection in other client, it is getting finished successfully.
Will the the port be different for different clients in the same system?
btw, i tried to telnet the target server, it was unsuccessful.
There were Global Proxy setting activated in HTTP services for the specific client in the sap system. Thus HTTP communication was failing.
Now the issue has been resolved.


text:
F20 è la sigla che identifica la versione a 5 porte della seconda generazione della Serie 1, un'autovettura di segmento C prodotta dal 2011 al 2019 dalla casa automobilistica tedesca BMW. La variante a 3 porte, subentrata in un secondo momento nella gamma, ha preso la sigla di F21.

Storia e profilo

Debutto

La presentazione ufficiale al pubblico, avvenuta al Salone di Francoforte nel settembre 2011, è stata anticipata dalla presentazione alla stampa, avvenuta il 5 giugno dello stesso anno.

Design ed interni

In generale va detto che della precedente Serie 1 vengono mantenute le proporzioni tra i volumi della carrozzeria: si ritrovano così caratteristiche come il lungo cofano motore che fa da contraltare all'abitacolo arretrato, il tutto volto a dare slancio alla linea. Gli spigoli vivi della prima generazione della compatta bavarese si sono fatti più smussati ed arrotondati, una tendenza stilistica dettata non più da Chris Bangle, dimessosi un paio d'anni prima dalla BMW, ma dal suo successore Adrian van Hooydonk, subentrato al designer statunitense.Il frontale della F20 rivela alcune tra le principali novità, come per esempio i gruppi ottici, sempre a doppia parabola, ma dal taglio triangolare che conferisce una particolare personalità alla vettura che fin dal suo esordio ha diviso nettamente tra sostenitori e detrattori. Un'altra particolare caratteristica del frontale della F20 sta nella calandra inclinata leggermente in avanti, un aspetto che sembra ricordare le BMW degli anni settanta. Ed ancora, il cofano motore è solcato da quattro nervature diagonali che confluiscono verso la calandra. La vista laterale evidenzia linee più dolci degli spigoli rispetto all precedente modello, mantenendo nel contempo quella tendenza a creare i particolari giochi di luci ed ombre che hanno reso così particolari le BMW dell'ultimo decennio.

Dalla vista laterale si osserva l'altro l'arrivo di un particolare stilistico e funzionale, quale l'indicatore di direzione integrato nel retrovisore esterno. Sono presenti elementi ormai immancabili, come l'Hofmeister-Knick e la nervatura laterale che passa in corrispondenza delle maniglie porta. La linea di cintura alta ed il tetto digradante nella zona posteriore, danno un aspetto di maggiore sportività. Vista posteriormente, la F20 mostra la sua sportività grazie ai passaruota leggermente bombati ed al piccolo spoiler sul tetto. I fari quadrangolari dagli spigoli smussati sono a led con grafica a strisce orizzontali.

L'abitacolo della F20 è una rivisitazione in chiave modernizzata dei concetti di ergonomia, eleganza e sportività necessari in una vettura appartenente al sotto-segmento premium. Ormai tipici ed irrinunciabili sono il cockpit orientato verso il conducente e la presenza della manopola dell'iDrive in una porzione del tunnel separata stilisticamente dal resto del tunnel stesso, una soluzione che ricorda molto da vicino la ben più grande Serie 6 introdotta pochi mesi prima. Non mancano tuttavia soluzioni prettamente razionali, come il buon numero di tasche e vani portaoggetti. L'abitabilità da parte dei passeggeri è leggermente aumentata grazie al passo cresciuto di 3 cm, ma soprattutto è la capacità del bagagliaio ad aver beneficiato di un significativo aumento, portandosi a 360 litri.

Struttura, meccanica e motori

La seconda generazione della Serie 1 nasce su un pianale progettato e realizzato per fare da base, con opportune modifiche ed adattamenti, anche alla sesta generazione della Serie 3, siglata F30. Questa base meccanica, dall'ottimale ripartizione dei pesi, comprende carreggiate allargate di 5.1 cm anteriormente e di 7.2 cm posteriormente, sospensioni anteriori realizzate in lega di alluminio, con geometria a doppio snodo, ed un retrotreno multilink a 5 bracci. L'impianto frenante prevede dischi su tutte e quattro le ruote, ed è corredato dai dispositivi ABS, DSC ed ESP. Lo sterzo si avvale di un servocomando elettromeccanico che a richiesta può essere integrato con un dispositivo in grado di variarne l'incidenza in funzione della velocità.Al suo debutto, la F20 è equipaggiata con cinque motorizzazioni, due a benzina e tre a gasolio, tutte con sovralimentazione di tipo twin scroll e distribuzione bialbero in testa con fasatura variabile Bi-VANOS ed alzata variabile Valvetronic:

116i: motore N13 da 1598 cm³ della potenza di 136 CV;
118i: stesso motore della 116i, ma con potenza portata a 170 CV;
116d: motore N47D20 turbodiesel common rail da 1995 o 1598 (dal 2013) cm³ di cilindrata e con potenza massima di 116 CV;
118d: stesso motore della 116d, ma con potenza portata a 143 CV;
120d: stesso motore della 118d, ma con potenza portata a 184 CV ed altri accorgimenti come iniettori e turbine più prestanti.

Il cambio è normalmente manuale a 6 marce, ma in opzione è possibile avere il cambio automatico ad 8 rapporti e, come ulteriore opzione, è possibile averlo con leve al volante.

Allestimenti e dotazioni

In Italia, la F20 debutta in tre livelli di allestimento, tutti abbinabili a qualsiasi motorizzazione tra quelle disponibili:

base, allestimento di attacco la cui dotazione di serie prevede: doppio airbag frontale, airbag laterali anteriori, airbag per la testa, climatizzatore manuale, ABS, DSC, ESP, computer di bordo, retrovisori esterni regolabili elettricamente e riscaldabili, sedili anteriori regolabili in altezza, volante regolabile in altezza e in profondità, cerchi in lega da 16", divano posteriore frazionabile, autoradio con lettore CD, vetri elettrici anteriori e posteriori, poggiatesta posteriori;
Sport: allestimento superiore leggermente improntato in chiave sportiva, grazie ad elementi come gli inserti in nero lucido sulla carrozzeria. La sua dotazione di serie prevede: cerchi in lega da 16", volante in pelle e sedili sportivi;
Urban: livello di allestimento improntato maggiormente verso il lusso, ma sprovvisto di alcune caratteristiche presenti nelle versioni Sport, come i sedili sportivi e gli inserti in nero lucido, che in questo caso lasciano il posto ad inserti cromati.

Evoluzione

La produzione della nuova Serie 1 è stata avviata subito dopo la presentazione alla stampa, nella sola configurazione a 5 porte, mentre la commercializzazione è stata avviata il 17 settembre del 2011. Lo stabilimento di produzione è quello di Ratisbona, come nel caso della precedente Serie 1 a 5 porte.

Nel marzo del 2012, la gamma si amplia con l'arrivo di tre modelli, sempre a 5 porte: da una parte la 125i, spinta da una variante potenziata del 2 litri turbo N20, e che in questo caso raggiunge una potenza massima di 218 CV; un'altra novità per il marzo 2012 è rappresentata dalla 116d Efficient Dynamics, spinta dallo stesso motore 1598 della 114d, ma dotata di misure atte a contenere ulteriormente emissioni, consumi e maggior potenza. In questo modo, tale modello diviene la prima BMW a scendere sotto la soglia dei 100 grammi di CO2 per ogni chilometro percorso. La terza novità del marzo 2012 è invece la 125d, equipaggiata con il 2 litri biturbo N47 in grado di raggiungere 218 CV di potenza massima. Inizialmente, tali novità non sono state proposte su tutti i mercati, ma solo su alcuni mercati tra cui quello tedesco e quello austriaco. In Italia, per esempio sarebbero arrivate solo tre mesi dopo. Nel mese di giugno viene avviata la produzione della F21, ossia della versione a 3 porte, che sancisce la scomparsa dai listini della precedente 3 porte conosciuta con la sigla E81. In tale occasione la gamma motori viene ampliata con l'arrivo del modello di base, la 114i (spinta da un 1.6 sovralimentato a bassa pressione e con potenza di 102 CV) e della versione di punta, la M135i (equipaggiata dal potente 3 litri turbo da 320 CV, montato anche sulle F12 ed F13). Non solo, ma anche un'altra novità tecnologica ha fatto la sua comparsa, vale a dire la trazione integrale xDrive, la quale per la prima volta va ad applicarsi ad una BMW di segmento C. I modelli previsti con tale nuova soluzione tecnica sono due: la top di gamma M135i e la 120d, le quali possono però essere sempre ordinate anche con trazione posteriore. Nell'autunno dello stesso anno, un'altra versione di base, questa volta a gasolio, è andata ad arricchire la gamma: la 114d, spinta dallo stesso motore dei modelli 116d Efficient Dynamics, ma depotenziato da 116 a 95 CV.Gli aggiornamenti successivi si sono avuti nel luglio del 2013, quando a listino compare la 118d xDrive: con questo modello la trazione integrale fa la sua comparsa anche nella fascia bassa della gamma F20. Il motore è lo stesso della normale versione a trazione posteriore.

Il restyling del 2015

Al Salone di Ginevra del 2015 è stato presentato il restyling della F20: gli aggiornamenti prevedono un nuovo design del frontale, che adotta una nuova calandra e nuovi gruppi ottici con nuove luci diurne ad anello. Anche la parte posteriore è stata rivista ed ora monta nuovi fari posteriori dal disegno ad "L" rovesciata, in modo da uniformarsi allo stile delle restante gamma BMW. Anche i gruppi ottici posteriori integrano la tecnologia a LED.

Novità consistenti anche per quanto riguarda la gamma motori, dove la top di gamma M135i vede la propria potenza salire da 320 a 326 CV, ma soprattutto dove si ha il debutto di nuove ed inedite (per la Serie 1) motorizzazioni a 3 cilindri, B38 a benzina e B37 a gasolio. In particolare, la precedente 114i è stata sostituita da una nuova 116i sotto il cui cofano viene montato un tre cilindri da 1.5 litri con potenza massima di 109 CV. La precedente 116i viene invece ribattezzata 118i, ma nei primi mesi mantiene il vecchio motore da 136 CV, sia pur leggermente aggiornato. Solo nell'estate del 2015, ad esso subentra il nuovo 1.5 turbo da 136 CV. Quanto alla vecchia 118i da 170 CV, essa viene sostituita dalla 120i con motore da 177 CV. Quest'ultima mantiene invece il vecchio 1.6 N13 senza ulteriori tentennamenti. Anche sul fronte diesel è presente un tre cilindri, sempre da 1.5 litri, con potenza di 95CV per la 114d e di 116 CV per la 116d. Quest'ultima, tra l'altro, viene ancora una volta proposta anche nella "pulita" configurazione EfficientDynamics. I motori diesel a 4 cilindri sono a loro volta derivati dal tre cilindri diesel e consistono nel nuovo 2 litri a gasolio B47 declinato in tre livelli di potenza: 150 CV per la 118d, 190 CV per la 120d e 224 CV per la 125d. Le prime due sono anche disponibili con trazione integrale, mentre per avere la trazione integrale con un motore a benzina, l'unica possibilità resta ancora quella di optare per il motore 3 litri turbo N55 della M135i xDrive.

Nell'estate del 2016 si hanno alcuni aggiornamenti per quanto riguarda i motori a benzina: i modelli 120i e 125i vedono infatti l'arrivo dei nuovi motori modulari a 4 cilindri B48, rispettivamente da 184 e 224 CV. Al vertice della gamma, invece, la M135i cede il passo alla M140i, equipaggiata con il nuovo 3 litri modulare B58, ancora una volta sovralimentato mediante turbocompressore con potenza massima di 340 CV. Anche la M140i, come il modello che l'ha preceduta, può essere a trazione posteriore o integrale.

Restyling del 2017 e fine produzione
Nel maggio 2017 la vettura viene sottoposta a un ennesimo aggiornamento, un secondo restyling, questa volta meno marcato e rivoluzionario rispetto a quello del 2015. Esteticamente vi sono cambiamenti di dettaglio con nuovi inserti neri per la carrozzeria e fari bruniti sia anteriori che posteriori; le variazioni più consistenti vi sono negli interni che presentano una nuova plancia e cruscotto ridisegnati con nuovi materiali e finiture. Nessuna novità invece per quanto riguarda la gamma motori.

Nel maggio del 2019 è stata svelata la terza generazione della Serie 1, ragion per cui, tra il giugno e il luglio dello stesso anno, la F20 ha cominciato a scomparire gradualmente dai listini europei. La F20 è stata l'ultima BMW di segmento C con motorizzazioni 6 cilindri, con una variante a 3 porte e con trazione sulle ruote posteriori: il nuovo modello condividerà il pianale con le più recenti Mini, dalle quali erediterà anche lo schema meccanico di tipo "tutto avanti".

La Serie 1 Sedan

Costruita e venduta dal febbraio 2017 solo per il mercato cinese, nell'estate del 2016 è stato annunciato il lancio di una nuova variante denominata BMW Serie 1 Sedan (con nome in codice BMW F52) e che in pratica si propone come una versione a tre volumi della segmento C bavarese, come fatto dalla Mercedes con la CLA e dalla Audi con la A3 Sedan. L'auto viene prodotta dal costruttore cinese Brilliance, che attraverso una joint-venture con la casa, la produce nella fabbrica di Shenyang. Creata in sinergia tra il centro stile BMW e la casa orientale, la Sedan dimensionalmente si va a collocare tra l'omonima due volumi e la Serie 3, con una lunghezza di 4.456 mm, una larghezza di 1.803 mm e un'altezza di 1.446 mm con un passo assai generoso di 2.670 mm in rapporto alla vettura. Le motorizzazioni, tutte a benzina e turbocompresse, vanno rispettivamente dalla 118i (1,5 litri con 3 cilindri da 136 CV), alla 120i (2.0 litri con 4 cilindri da 192 CV) e alla 125i (2.0 litri con 4 cilindri da 231 cavalli).

In realtà, sul piano tecnico la vettura non ha niente in comune con la ben più nota 2 volumi a 3 o a 5 porte, in quanto la base tecnica deriva da quella utilizzata dalla Mini di terza generazione ovvero la piattaforma UKL, della quale vengono mantenute soluzioni tecniche come la trazione anteriore ed il motore trasversale. Tale pianale aveva già cominciato ad essere utilizzato nella produzione BMW, anche in quella prevista per il vecchio Continente, come il lancio, avvenuto nel 2014 e 2015 delle monovolume Serie 2 Active Tourer e Gran Tourer e della seconda generazione del SUV X1, anch'essi con schema tutto avanti. In questo senso, la Serie 1 Sedan va a rappresentare la prima berlina classica della casa dell'elica ad annoverare le ruote anteriori motrici e con propulsore trasversale.

Riepilogo caratteristiche

Di seguito vengono riepilogate le caratteristiche delle varie versioni previste per la gamma della BMW F20 in Europa.

Note

Voci correlate
BMW Serie 1

Altri progetti

Collegamenti esterni

F20


After reading this post from Schoolgirl Style I decided it was time to update my classroom decor. Don't get me wrong, I love my color scheme! It's the same as I have for my blog (teal, aqua, lime green, and brown) and it coordinates with a lot of the existing colors of the furniture and built-ins in the room. No, what this post got me thinking about was the idea of consistency. I wasn't going to change my palette; I needed to bring more consistency to my classroom decor. And that meant changing out my bulletin board borders.
As much as I like my Trend rainbow swirly star borders, I've had them since my second year at this school. My rainforest border and planet borders have followed me from my previous school...and before that, when I taught preschool. I felt I was justified in my decision to splurge in the name of change!
Before I show you the end result, I wanted to talk about the issues and process of mounting my borders. See I don't just use them on normal bulletin borders; I have them covering two different problem areas.
1. The front and back of my classroom is a weird mix of whiteboards mounted on top of chalkboards and framed by thin panels of cork boards. This may work for some teachers, but I decided early on to hide everything but the whiteboards under shower curtains instead of butcher paper. This way I don't have to change it out every year. It's worked well so far! I just have to tape in the chalkboard spots and staple in the cork board spots.
2. I have 6 closet doors that I use as bulletin boards. Three of them are actual bulletin board, and the other 3 are more chalkboards. Once again I covered them all, this time with fabric. Not only does it resist fading like the shower curtains, the fabric also helps to dampen the sound in the room a little. I've also found that my borders really last a long time if I laminate them. Before I did that they'd get shredded and fall off with use (kids opening and closing the closet doors every day).
In the past I used Velcro to adhere the fabric to the chalkboards and then stapled the border to the fabric. It works pretty well! There is some sagging, so I've had to replace the Velcro in places, but it's not a bad system. However, since I splurged on all new borders, I decided to try a new approach. My idea was to use those tiny Command hooks at the top only. This way they'd hold the weight of the laminated border and fabric, and the Velcro left on the sides would be more to prevent it from swinging than holding it up.
1. After taking down the old stuff and cleaning the area where the hooks would hang, I stuck one hook in each corner and two in the middle.
2. I carefully hole punched the fabric so it could hang on the hooks. Take your time to line up the hook with the area you hole punch! It helped to have sticky spots to hold the fabric in place during this process, so if you're starting with a clean slate either enlist a partner's help or tape it temporarily.
3. Create frames out of your border. You're NOT attaching the border to the wall or fabric in this step. To do this, hold the border up to the top and trim it to the size you need (if you make 2 for each door, use one for the top and one for the bottom. Put the bottom aside to save for the final step). Then, staple the sides to the perfectly measured border. I needed just over 2 strips to equal the height of the door. Of course you want to overlap the strips to staple the ends together (line them up for a continuous ripple pattern).
4. Hole punch the top of this border frame the same way as you did the fabric, starting from the hook in one corner. DO NOT staple the top of the border to the fabric. If you do, you have more of a chance that the border or the fabric will pucker. Just let the hook hold things up and gravity straighten things out below.
5. Start stapling this unfinished border frame to the fabric. Again, at this point gravity should have straightened the sides out for you. As long as your sides are perpendicular with the top of your frame, this step should be easy (if not, you can detach and re-attach the sides from the top).
6. Finish up your frame by stapling on the bottom of the fabric.
Although I felt a little sad when I took down the old stars (more so than the Jungle and planets borders) I'm very pleased with how my doors look now!
They flow not just with each other, but with the whole room. I can't wait to be finished with the cleaning and organizing so I can see how it all looks together! It's already looking a lot more cohesive and calming. I'll have more pictures of the rest of the room up hopefully at the end of the month, and as the year goes on I'll try to remember to update you on how the Command hooks "hold up."
I've already made headway with several of the other projects in my summer series, (as you can see above the Teacher's Bulletin Area is pretty much set) which I'll post next week. Sadly, once that's done it's on to filing paperwork, which is sadly more like ACTUAL work! At least being in an updated, pretty room will help me feel renewed. That and hitting the beach once the building shuts each afternoon for as long as the sun will let me! If you're still on vacation, I hope you're finding a good balance between preparing and relaxing.
Also, I'm linking up with Swimming Into Second for her Show Off Your Space linky! If you love to check out classroom design there are some great ideas here.


← Come on, let's go for a run. Yes, right now.
Those chairs that hold us and our babies are precious!
I had one almost exactly the same. It isn't just furniture that I have trouble letting go of though, it's ALL their old stuff!
I loved your post and all the nostalgic feelings you recall with that loved chair!
thank you. i really don't like to let things go.
This is really nice. I'm glad that your sister-in-law has the chair now for rocking her baby. That kind of furniture is meant to be shared and to gather memories of a family.
thank you. i know, the rocker just becomes part of the family, or a sweet part of a time that is hard to give up.
Yay. I bet the chair is soo happy to be needed again. I love the way you wrote it as a marker for all those important moments with a young child. And we went through three copies of Brown Bear, Bear Bear with my oldest. He was obsessed with that one.
there were so many… and each had their own favorites…i passed on a lot of the baby books, but i've kept the favorites. i can't quite let them go..
We are cleaning out things and there are certain children's books and certain clothes I just can't part with yuet.
you gotta to keep the real special ones.
Awwww! This is so sweet. I never had a special chair to rock my babies, but I totally get how you feel about it.
We have that rocker EXACTLY – maybe in a different color? But I love the slide action so much. The kids have drawn all over it and laid claim to it, and it was my comfy spot until Caroline claimed it.
i might steal it back when he babies are grown… that way i can rock myself and my memories when i'm old.
Been totally suffering from baby fever over here and this post did not help me one little bit, thank you very much! So lovely to think back on when our children were tiny and squishy. I felt the bittersweet in your words.
haha! it's such a sweet time, but then again, it's all pretty sweet.
Hankie alert! That was so sweet, and I'm so glad that well-loved chair has a new home.
me too. although she might find me curled in it, clutching on to one of my full grown kids, when i visit.
Wow! My rocking chair looks like a replica of yours. My husband wanted to get rid of it last year. But, like the crib, I was reluctant to part ways. Guess it's a good thing because now we can use the rocker for baby #3!
rock on, baby! and enjoy those moments, they're so just so sweet.
I recently did a post on my kitchen table not nearly as nostalgic…not even close…but Im sorry I didnt go there with it. I love your take on this piece of furniture. It was a real reflection of your life.
For me it was the Dr. Seuss book Horton Hears a Who. My mother read it to me; I read it to all my kids, and I bought a copy for my son so he could read it to my first grandchild.
I love love love this and it makes me miss rocking my babies. I gave my chair to a friend whose roommate was young, single and pregnant. I know she needed it more than i did but i miss it.
it's true. it's so nice to pass on things like that. we have to. i guess it's part of growing up.
We have a very similar chair that evokes similar emotion in me. Mine sits in my attic, not ready to move on, but not needing to be used. Great piece, here, nice emotion in it.
You described very beautifully in this post just how memories and life can make a simple piece of furniture so important. You can be so attached to these, right!
I'm glad your chair found a new home, where it will continue to soothe others in the twilight hours. I got a bit teary-eyed when we packed up the baby swing. I was frightened that he might never nap again without it, and I was a little sad that those newborn days were over.
it is sad, but i look at the growing bodies of my boys, still such babies but also big boys, and i know i'll miss these days even more!
Oh, I could almost have written this myself! I have the same chair, three kids, same attachment to inanimate objects. I burst into tears when my husband sold our Maya wrap!
I love how something like a rocking chair can be imbued with so many memories and provide such comfort. I rocked my own daughter in the same chair my mother rocked me. It's so much more than just a chair.
me too. it's amazing how we attach ourselves to these things. but they hold so much history.
Oh my god how I love this. My chair is now in the basement, in the corner of my oldest's room. I think I might go rock for awhile now, considering how sentimental I've felt of late. Beautifully written.
thank you. yes! go rock for me. and hum, you are my sunshine, while you do it.
Ah… Absolutely love this. From the flip-side, the only memory I have of my paternal grandfather is sitting on his lap in a rocking chair. There was no better feeling!
Love this! This story totally reminds me of my boyfriend — his mother still has the rocking chair that she nursed and soothed both boys. Every time we head to their house and find ourselves in the living room chatting, he gravitates towards it, claiming it as his spot. That was a very generous gift to give!
thank you. i really like to pass everything on, but some things are a little harder than others.
i like that… pass on the chair and keep the memories. nice.


The Permanent "I'm Leaving/Back Thread"
Re: The Permanent "I'm Leaving/Back Thread"
Sorry I've been so inactive recently! College has been far more time intense than I imagined. Apparently learning to read both Hebrew and Greek is time consuming? Anyway I am still around, but I'm probably only getting on every three or four days so if you respond to me don't worry if it takes time for me to get back to you! On the other hand I have no idea when normal service will resume.
I don't know how to start this.
I haven't logged in here for so long, a lot has happened and a lot hasn't.
I was going through some very terrible time in my life for the past few years and I only have myself to blame for that, my ill-disciplined lifestyle to be exact.
My performance in university was very poor, I am 22 now and still in my 2nd year of a 5 year degree.
Last year I actually gave my best, or at least what I think was my best, but I had to pass at least 14 subjects out of a total of 18 in order to progress to the next year and I only managed 10.
I was hit by depression at many points during the past few years.
Anime helped for some reason it had a major positive influence on me in the past months.
Videos of J.Peterson helped greatly as well.
This is embarrassing but I don't care.
I can't really promise that I'll be here a lot and I am sorry if this is not the place for such a post but I somehow wanted to write this today so I just went with what my heart wanted.
Who the hell do you think I am?!
I don't mean to be harsh, actually trying to help but did you really give your best? I notice a lot of people say they did to give themselves comfort. It's just because you mentioned your ill disciplined lifestyle. Sounds like a contradiction. I don't think you should ever aim to pass an exam. I get the impression that's your approach. You should aim for a first class mark then at worst you should at least pass. The best way to succeed in an exam is an organised approach and practice questions as you go along to continually test that you're understanding the material. University exams are all about practicing relevant questions. The examiner has to ask you certain types of questions, if you practice enough you can prepare for anything. You should be able to access past exam papers. I found that's one one of the best ways to prepare. Sometimes they are really lazy and ask you the exact same questions as a year or two before.
You are not being harsh at all actually.
That thought definitely crossed my mind and I confronted myself with the question "Did you really give your best?".
A part of me thought that maybe there was more, I was afraid I was just comforting myself with thinking that I gave my all and that it was my brain's defence mechanism at work to prevent me from going insane. But, no I am really convinced that there wasn't anything that I could've done and didn't do.
The part about my irresponsible and rather wild lifestyle refers to my life before that, let's say before the earlier months of 2018.
I didn't go with the mindset that I just had to pass. That was the case for around the first month but then I decided I should aim for a decent mark at every subject. Still, 18 subjects in a single study year (two terms) is quite overwhelming, at least by Syrian universities standard and my previous record didn't help me at all, it stood in my way.
That is true about benefiting from past exam papers, it definitely helps and sometimes they are that lazy that they just copy one exactly as is.
Don't get the wrong impression here.
My previous post was not motivated by self-pity, I am way past that.
It was just something I wanted to write at the time.
Indeed, welcome back Hussam! In my first year at university I stopped submitting essays at Christmas, got to the end of the year with 7 still due. I understand what its like to put yourself in a corner with no idea on how to get out. Being open is a good first step in dealing with it. If you want any advice or help then we will happy to offer it. Alternatively if you just need a safe space we can provide that as well!
Thank you Dong Zhou. It was mainly my own decisions that led me to that path. My habits are way better than they used to be now and I still have a chance at this.
My depression wasn't diagnosed but I am pretty sure I had one, I never believed it existed before it actually happened to me.
I am going to find a way, I have redeeming qualities that will help me find a way.
Sun Fin wrote: Indeed, welcome back Hussam! In my first year at university I stopped submitting essays at Christmas, got to the end of the year with 7 still due. I understand what its like to put yourself in a corner with no idea on how to get out. Being open is a good first step in dealing with it. If you want any advice or help then we will happy to offer it. Alternatively if you just need a safe space we can provide that as well!
Thank you Sun Fin, I really appreciate it.
Is that a common attitude in Syria?


Requiring little or no defrosting: a frost-free refrigerator.
"frost-free." YourDictionary, n.d. Web. 16 April 2019. <https://www.yourdictionary.com/frost-free>.
As with watermelons, you can either start the seeds indoors a few weeks before the last frost-free date, or plant seeds directly into the garden once the daytime temperatures hit 80 degrees consistently.
Keeping a gardening journal will help you pinpoint which natural events, such as frog calls, the return of particular birds or the leafing out of trees will coincide with frost-free days in your region.


Sosia by Sangiacomo reinterprets in a contemporary way the "Art Deco" drawer units, their particular forms and gentle curvatures of the fronts. The Oak, in different shades and chiaroscuros, dominates the collection interpreting a simple and elegant furnishing style, destined to live beyond the fashion. The Sosia bedsides and storage units, characterized by a slight curvature of the fronts, have horizontal grain. Veneered in heat-treated oak, white lacquered oak, ash (cenero), brown or grey oak, or lacquered oak in sampled colors.
Heat-treated Oak, the protagonist of the Cloe bed and the Sosia chest of drawers, is characterized by an effect of light grains that stand out on the base of the dark wood. The high temperatures at which the wood is subjected, determine the difference in color between the hardest and the softest parts of the wood, giving these pleasant light and shade random effects.
San Giacomo Sosia Dresser is made from class E1 particle board panels with low formaldehyde content (7/8" thick for the frame) in hollowed MDF panels on the front part (7/8" thick). The front panels are made from curved plywood (7/8" thick for tops) coated with stained and brushed oak veneer with open-pore varnish or lacquered oak with open-pore varnish. The sides of the drawers with bottom 3/8" thick are made from panels 5/8" thick with synthetic jute weave effect finish. They are mounted on high sliding runners with end-of-run buffer and soft closing mechanism (blumotion). Opened using the front panel which overhangs the side of the structure. Sosia can be anchored to the wall which prevents overturning and has optional counter-weights available for both the bedside tables and the dresser. Adjustable feet made of black plastic.


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Q: What is this Pokémon Go event I've heard about? I've been hearing about a Pokémon Go event that's happening this week for Halloween. What exactly is going to happen?

A: According to the official Pokémon site, there will be many bonuses for players who play Pokémon Go between October 26th and November 1st (it looks like it's safe to assume UTC, based on this post, which says the event has not started in New Zealand yet, despite being October 26th there, as well as noting the fact that Ingress events used UTC), mostly revolving around candy.

*

*Transferring Pokémon will reward you with 2 candies instead of 1.

*Catching Pokémon will reward you with 6 candies instead of 3.

*Hatching Pokémon will reward you with double the candy you would normally receive. For reference, an answer here says that you will normally get 5-15 candy for a 2km egg, 10-21 candy for a 5km egg, and 16-32 candy for a 10km egg. This means that during this event, you will receive 10-30 candy for every 2km egg, 20-42 candy for every 5km egg, and 32-64 candy for every 10km egg.

*Buddy Pokémon will find candy 4x as fast as they normally do. (0.25km, 0.75km, and 1.25km instead of 1km, 3km, and 5km)
In addition to the above candy bonuses, Pokémon in the Drowzee, Gastly, and Zubat lines will be more common during this event. The full list of Pokémon is:

*

*Drowzee

*Hypno

*Gastly

*Haunter

*Gengar

*Zubat

*Golbat

In addition to those listed above, some unannounced Pokémon are spawning much more frequently, namely Meowth and the Cubone line, which include:

*

*Meowth

*Cubone

*Marowak

Aside from personal experience, this post and this post express the same thing.
Note: Apparently, Persian is not a Halloween Pokémon, even though Meowth is. This post has a list of Halloween Pokémon that does not include Persian. (Anecdotally, I have not encountered a single wild Persian during this event)


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CONVALESCENT-PLASMA THERAPY FOR TREATING COVID-19: NEW POSSIBILITIES AND NEW CHALLENGES
It is hypothesized that antibodies to SARS-CoV-2 (the virus that causes COVID-19) in convalescent plasma may reduce severity of infection and reduce mortality in other sick patients who could not adequately develop this antibody response themselves.
Home / About / News & Events / Blog /
Published by Dr. Ruchika Goel on Tuesday, June 16, 2020 in Blog
presentation objectives
To trace the historical role of Convalescent Plasma therapy as an emergency application in times of epidemics and critically review the data showing current usage, safety and efficacy in SARS-COV-2.
To outline the collaborative community effort in successfully setting up a regional convalescent plasma program: the combined patient/donor, hospital and blood center initiative.
Discuss the current treatment protocols and standardized workflow.
Watch the presentation below to learn more.
Convalescent plasma is the yellow liquid that is separated from blood donated by a patients who has recently recovered from an infection. Convalescent plasma is being investigated for the treatment of severe COVID-19 infection. It is hypothesized that antibodies to SARS-CoV-2 (the virus that causes COVID-19) in convalescent plasma may reduce severity of infection and reduce mortality in other sick patients who could not adequately develop this antibody response themselves.
Given the dearth of effective treatments for COVID-19, convalescent plasma has gained serious attention. While this treatment is not a cure, it might help alleviate the symptoms patients experience with COVID-19. Recent promising data from China supports convalescent plasma use for early recovery of some of the sickest patients. It is important to note however, that majority of these data are observational and warrant cautious optimism. This approach requires evaluation in randomized clinical trials and initial clinical trial data on efficacy of CCP (although very prelim) looks promising. Further investigation is still necessary to determine if convalescent plasma might significantly shorten the 1) duration of illness, 2) reduce disease related morbidity, or 3) prevent mortality associated with COVID-19. Given this is a huge public health emergency, as a huge support, FDA has facilitated the access to COVID-19 convalescent plasma for use in patients who have serious or life-threatening COVID-19 infections as a single patient emergency Investigational New Drug Applications for individual patients.
Use of convalescent plasma has previously and more recently been studied in outbreaks of other respiratory infections, including the 2009-2010 H1N1 influenza virus pandemic, 2003 SARS-CoV-1 epidemic, and the 2012 MERS-CoV epidemic with varying degree of success. However, the idea of using blood (effective component is plasma) from disease survivors, also known as convalescent-plasma therapy, dates back to actually the late 19th or early 20th century. Doctors have transfused the blood of recovered patients into those who continued to be sick with the 1918 Spanish flu, measles, polio, chickenpox, and Ebola—all to varying degrees of success.
It is important to note that this potential therapeutic option can be a two-edged sword as convalescent plasma comes with all baseline and inherent risks with any plasma transfusion. Plasma transfusions are associated with adverse events ranging from mild fever and an allergic reaction like hives to life-threatening anaphylaxis, transfusion-related acute lung injury, and transfusion associated circulatory overload in patients with underlying cardiorespiratory disorders. However, safety data from first 20,000 products transfused nationally has been very promising with CCP being well tolerated with minimal side effects. There is also a very rare residual risk of infectious disease transmission like HIV and HCV (<1 per million transfusion events). There is no evidence of transfusion transmission of coronavirus through any blood products. Lastly, even if useful this will require ramping up of testing to find those who recovered and their goodwill to donate blood.
Dr. Goel is the Medical Director for Mississippi Valley Regional Blood Center, an Assistant Professor of Pediatrics and Internal Medicine in Hematology Oncology, Simmons Cancer Institute at SIU School of Medicine and an Adjunct Assistant Professor in Blood Banking and Transfusion Medici
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