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

 The recently discovered r-mode instability
\citep{andersson98:_new_class,friedman98:_axial_instab} might play a
significant role in setting the spin frequencies ($\nu_s$) of rapidly
rotating neutron stars
\citep{lindblom98:_gravit_radiat_instab,owen98:_gravit,andersson99:_gravit_radiat,bildsten98:gravity-wave,andersson99:accreting_rmode}.
The unstable regime for the r-modes in the neutron star (NS) core
depends on the competition between the gravitational radiation
excitation and viscous
dissipation. \citet{lindblom98:_gravit_radiat_instab} and
\citet{andersson99:_gravit_radiat} computed the dissipation due to
shear and bulk viscosities in normal fluids (not superfluids) and
found that gravitational excitation exceeds viscous damping in
all but the most slowly rotating stars. \citet{lindblom99:superfluid}
showed that superfluid mutual friction is also not competitive with
gravitational radiation unless the superfluid entrainment parameter
assumes a very special value. Hence, on theoretical grounds, r-modes
are expected to be unstable over much of the parameter space occupied
by newborn NSs, NSs in low-mass X-ray binaries (LMXBs), and
millisecond radio pulsars (MSPs) during spin-up.

However, observations pose challenges to this theoretical picture. The
existence of two $1.6$~ms radio pulsars means that rapidly rotating
NSs are formed in spite of the r-mode instability
\citep{andersson99:accreting_rmode}.  While it is not clear that their
{\it current} core temperatures place these MSPs inside the r-mode
instability region, current theory says that they were certainly
unstable during spin-up. For accreting NSs in LMXBs,
\citet{bildsten98:gravity-wave} and
\citet{andersson99:accreting_rmode} conjectured that the gravitational
radiation from an r-mode with a small constant amplitude could balance
the accretion torque.  This would possibly explain the preponderance
of $\approx 300$~Hz spins among LMXBs \citep{klis99:_millis}, which
would otherwise have been spun up to $>1000 \ {\rm Hz}$ during their
$\gtrsim10^9$~yr lifetime \citep{vanparadijs95:lmxb_distrib}.
However, for normal fluid cores, \citet{levin99} showed that the
temperature dependence of the shear viscosity makes this spin
equilibrium thermally unstable, leading to a limit cycle behavior of
rapid spin-downs after prolonged periods of spin-up.  For superfluid
cores, \citet{bu99:rmodes} showed that such constant-amplitude spin-up
is inconsistent with the quiescent luminosities of several known
LMXBs.

 All but the hottest NSs have solid crusts that occupy the outer
$\approx $~km of the star.  In this paper, we calculate a previously
overlooked dissipation: the viscous boundary layer between the
oscillating fluid core and static crust. The shear viscosity of NS
matter is relatively small and does not affect the r-mode structure in
the stellar interior. However, the transverse fluid motions of the
r-modes are very large at the crust-core boundary and must, of course,
go to zero relative velocity at the crust. The dissipation in the
resulting viscous boundary layer (hereafter referred to as the VBL)
substantially shortens (by typically $10^5$) the r-mode damping times.
Previous work
\citep{lindblom98:_gravit_radiat_instab,Lindblom99:2ndorder,andersson99:_gravit_radiat}
included damping from the shear viscosity acting only on the gradient
in the transverse velocity of the mode in the interior of the star (on
the length scale of the stellar radius, $R$).  The shear in the VBL
acts on a much shorter length scale, and is hence stronger.

 This new source of dissipation raises the minimum frequency for the
r-mode instability in NSs with a crust to $\gtrsim500$~Hz for
$T\approx10^{10}$~K, and even higher frequencies for lower
temperatures. It thus alleviates the conflict between the
accretion-driven spin-up scenario for MSPs and the r-mode instability and
significantly alters the spin-down scenario proposed by
\citet{owen98:_gravit} for newborn NSs.

\section{The Viscous Boundary Layer}
\label{sec:boundary-layer}

  The transverse fluid motions of an r-mode cause a time-dependent
``rubbing'' of the core fluid against the otherwise co-rotating crust
spinning at $\Omega=2\pi \nu_s$. In previous works, the boundary
condition applied at this location allowed the fluid to have
large-amplitude transverse motion. Neglecting viscosity is an
excellent assumption far away from the crust-core interface.  However,
there can be no relative motion at the boundary for a viscous fluid,
leading to a VBL where the transverse velocity drops from a large
value to zero (the ``no-slip'' condition). The VBL is mediated by the
kinematic viscosity, $\nu$, in the fluid just beneath the base of the
crust. The density there has most recently been estimated as
$\rho_{\rm b}\approx 1.5\times10^{14}{\rm~g~cm}^{-3}$ \citep{pethick95}.  We
use the values for $\nu$ as found by \citet{flowers79} and fit by
\citet{cutler87},
\begin{equation}\label{eq:viscosity}
\nu=1.8\times 10^4 {\rm~cm}^2 {\rm~s}^{-1}\frac{f}{T_8^{2}}.
\end{equation}
In this fit, three different cases are handled with the parameter $f$.
When both neutrons and protons are normal, the predominant scatterers
are neutrons, and $f=(\rho/\rho_{\rm b})^{5/4}$. If neutrons are superfluid
and protons normal, the viscosity is mediated by electron-proton
scattering, and $f=1/15$. Finally, when both protons and neutrons are
superfluid, electron-electron scattering yields $f=5 (\rho/\rho_{\rm b})$.

  We begin by assuming that the crust is infinitely rigid, and hence
the waves do not penetrate into the crust.  In an oscillating flow,
the thickness of the VBL, $\delta$, is found by setting the
oscillation frequency of the r-mode in the rotating frame,
$\omega=2m\Omega/l(l+1)=2\Omega/3$ ($l=m=2$), to the inverse of the
time it takes vorticity to diffuse across its width, i.e.
$\delta^2/\nu\sim \omega^{-1}$.  In the plane-parallel case,
\citet{landau59:_fluid_mech} show that the correction to the velocity
in the VBL of an incompressible oscillatory flow falls off
exponentially with a length
\begin{equation}\label{eq:bl-thickness}
\delta=\left(\frac{2\nu}{\omega}\right)^{1/2}\approx
3{\rm~cm~}\frac{f^{1/2}}{T_8}
\left(\frac{1{\rm~kHz}}{\nu_s}\right)^{1/2},
\end{equation}
much smaller than $R$.  This estimate neglects the Coriolis
force. When the VBL is determined by the balance between the Coriolis
force, $\sim2\Omega v$, and viscosity, $\sim\nu v/\delta^2$ (the Ekman
problem), then the thickness is $\delta\sim(\nu/\Omega)^{1/2}$,
roughly the same as eq.~(\ref{eq:bl-thickness}).  Hence, while the
Coriolis force will change the angular dependence of the velocity in
the VBL, it is unlikely to change its thickness.

The viscous dissipation can be handled quite simply for this thin VBL.
Since all of the kinetic energy there is damped in one
cycle, the $Q$ of the oscillation is roughly just the ratio of the
total volume to that in the VBL, or $Q\sim R/3\delta\sim 10^5 T_8
(\nu_s/1{\rm~kHz})^{1/2} /f^{1/2}$. The damping time is then a few
hundred seconds, thus competitive with the growth time from
gravitational wave emission, $\tau_{\rm gw}= -146{\rm~s~}
M_{1.4}^3 R_6^{-9} (\nu_s / 1{\rm~kHz})^{-6}$, where $M_{1.4}=M/1.4
M_\odot$ and $R_6=R/10 {\rm \ km}$, of the $l=m=2$ r-mode
\citep{owen98:_gravit,lindblom98:_gravit_radiat_instab}.

To calculate the damping more accurately, we use the dissipation per
unit area from \citet{landau59:_fluid_mech} and integrate over the
surface area at the crust-core boundary
\begin{equation}\label{eq:dEdt}
\frac{dE}{dt}=-\int\frac{\rho v^2}{2}
\left(\frac{\omega\nu}{2}\right)^{1/2} R^2 \sin\theta d\theta d\phi.
\end{equation}
The fluid velocity is given by $\vec v=(\alpha\Omega R)\vec
Y_{lm}^Be^{i\omega t}$, and $E=1.64\times10^{-2} M (\alpha\Omega
R)^2/2$ is the mode energy \citep{owen98:_gravit}.  Integrating and
using the mode frequency in the rotating frame, we find the damping
time due to rubbing
\begin{equation}\label{eq:tau-rub}
\tau_{\rm{rub}}=-\frac{2E}{dE/dt} \nonumber \\
	\approx100{\rm~s~}
	\frac{M_{1.4} T_8}{R_6^2 f^{1/2}}
	\left(\frac{\rho_{\rm b}}{\rho}\right)
	\left(\frac{1{\rm~kHz}}{\nu_s}\right)^{1/2},
\end{equation}
where $\rho$ is
the density at the crust-core boundary.

So far, we have assumed that the large-scale relative motion between
the oscillating core and the crust is simply set by the toroidal
motion of the r-mode. This is fine in the inviscid limit
($\nu=0$). The transverse displacement $\xi_\perp$ at the crust-core
boundary is then discontinuous, and the r-modes do not couple to the
crust's torsional modes, which have $\vec{\xi}=\xi_\perp
\vec{Y}_{lm}^B$. For $\nu=0$, r-modes can only couple to the crust via
their $\mathcal{O}(\Omega^2)$ radial motion.  However, the VBL exerts a
time-dependent shear stress, $\sigma_{r\perp}= (\omega\nu)^{1/2}\rho
v$ \citep{landau59:_fluid_mech}, that shakes the crust and can
potentially couple the crust to the core.  If this coupling can drive
the amplitude of the crustal motion $\xi_\perp$ to be comparable to
the transverse motions in the r-modes ($\xi_\perp=3\alpha R/2$ for
$l=m=2$), then our picture of the core rubbing against a static crust
would need to be reconsidered.  The energy in an r-mode oscillation is
$\sim10^{51}\alpha^2 (\nu_s/1{\rm~kHz})^2{\rm~ergs}$, while the
typical energy in torsional oscillations of the crust is roughly
$10^{48}\alpha^2{\rm~ergs}$ \citep{mcdermott88}. Hence, if the r-mode
could couple efficiently to the crust, it would have adequate energy
to drive crustal pulsations of comparable amplitude and potentially
break the crust.  We now estimate the magnitude of this coupling and
show that, under most circumstances, it should be quite small.

Let us look at a toy problem of a simple harmonic oscillator (i.e.,
the crust) with a mode frequency $\omega_0$ and weak damping
$\gamma\ll\omega_0$ driven by a harmonic force per unit mass $f_0
e^{i\omega t}$.  Away from resonances with crustal pulsation modes,
the response of the crust is then just $\xi_\perp\approx
f_0/(\omega_0^2-\omega^2)$. Ignoring Coriolis force, the fundamental
$l=2$ torsional mode has a frequency $\sim 40\rm{~Hz}$, while the
overtones have frequencies $\sim500n\rm{~Hz}$, where $n\ge1$ is the
radial order of the overtone \citep{mcdermott88}.  Damping times of
these oscillations are on the order of days to decades
\citep{mcdermott88}, so the resonances are narrow.  The spacing
between the crustal modes, $\sim500$~Hz, is comparable to the r-mode
frequency, so on average, $\omega_0^2-\omega^2\sim\omega^2$.  Mass
per unit area in the crust is $M_{\rm{crust}}/4\pi R^2=\rho h$, where
$h\sim1$~km is the scale height at the base of the crust. Therefore,
$f_0=\sigma_{r\perp}/\rho h$ and, in the likely situation that the
r-mode frequency is not in
resonance with a normal mode frequency of the crust, we find
$\xi_\perp/R\sim\alpha(\delta/h) \approx10^{-4}\alpha/T_8$.

This simple model (and a preliminary calculation) shows that the
induced toroidal displacements in the crust are much smaller than the
r-mode displacements. In other words, even though the r-mode has
plenty of energy to drive crustal pulsations, it cannot effectively
shake the crust.  Hence, neglecting the coupling should not invalidate
our estimate of the damping time $\tau_{\rm rub}$.

\begin{figure*}[t]
\begin{minipage}[t]{3.5in}
\begin{center}
\epsfig{file=fig1.eps}
\end{center}
\vskip -0.15in
\figcaption{
\label{fig:instability} Critical spin frequencies for the
r-mode instability.  Solid line shows the critical frequency set by
the viscous boundary layer and internal dissipation, for a star with
normal nucleons in the core.  The shading around the solid line
displays the effect of core superfluidity.  The dashed line shows the
critical frequency as calculated previously, neglecting the boundary
layer friction.  The LMXBs reside in the rectangular shaded region.
The arrows show the frequencies and the upper limits on core
temperatures (obtained, as in \citealt{andersson99:accreting_rmode}
from \citealt{reisenegger97} and \citealt{gudmundsson82}) of the two
fastest known MSPs.}
\end{minipage}
\hfill
\begin{minipage}[t]{3.5in}
\begin{center}
\epsfig{file=fig2.eps}
\end{center}
\vskip -0.15in
\figcaption{
\label{fig:evolution} Evolutionary scenarios for rapidly
rotating neutron stars with crusts.  The thick solid line shows the
critical spin frequency for the r-mode instability, including boundary
layer friction.  The two thin solid loops show the evolution of a
neutron star in an LMXB, accreting at $10^{-8} M_\odot$~yr$^{-1}$, for
two different values of the r-mode saturation amplitude $\alpha_s$, as
marked on the plot.  The dotted line shows the spin-down and cooling of
a newborn rapidly rotating neutron star.}
\end{minipage}
\end{figure*}

\section{The R-mode Instability}
\label{sec:instability-strip}

We now find the region in $(\nu_s,T)$ space where a NS is unstable to
the r-mode instability by balancing the viscous damping with the
excitation due to gravitational radiation. When the crust is present,
the r-mode is unstable for $\tau_{\rm rub}<|\tau_{\rm gw}|$, or
\begin{equation}\label{eq:nu-min}
\nu_s\gtrsim1070{\rm~Hz~}\frac{M_{1.4}^{4/11}}{R_6^{14/11}}
	\frac{f^{1/11}}{T_8^{2/11}}
	\left(\frac{\rho}{\rho_{\rm b}}\right)^{2/11}.
\end{equation}
However, other viscous mechanisms in the core also contribute to the
damping. In Figure~\ref{fig:instability} we show the critical spin
frequency where $1/\tau_{\rm gw}-1/\tau_{\rm rub}-1/\tau_{\rm
visc}=0$, where we use previously published calculations of shear
\citep{lindblom98:_gravit_radiat_instab} and bulk
\citep{Lindblom99:2ndorder} viscous r-mode damping for the interior
viscous damping time $\tau_{\rm visc}$.  The solid line corresponds to
the case where all nucleons are normal ($f=1$), while the shading
around it represents the range in frequencies when either neutrons or
all nucleons are superfluid.  For comparison, the dashed line shows
the instability curve that neglects the effect of the viscous boundary
layer.  Our curves presume that the crust is present for all
temperatures less than $\sim2\times 10^{10}$~K. For temperatures
higher than that, the bulk viscosity is the dominant damping mechanism.

The shaded box in Figure~\ref{fig:instability} indicates the region of
the $(\nu_s, T)$ space where the observed LMXBs
($250{\rm~Hz}\lesssim\nu_s\lesssim600{\rm~Hz}$,
$T\sim(1-8)\times10^8$~K; \citealt{brown98}) reside. The arrows on the
left-hand side of the plot show frequencies and the upper limits on
the core temperatures for the two fastest MSPs. Clearly, the strength
of the VBL dissipation means that r-modes are not excited in the
accreting and colder ($T\lesssim10^9$~K) NSs.  This result removes the
discrepancy between the existence of $1.6$~ms ($625$~Hz) millisecond
pulsars and the r-mode instability \citep{andersson99:accreting_rmode}
and alleviates the disagreement between the observed and predicted
quiescent luminosities of NS transients \citep{bu99:rmodes}.

 We now re-examine the thermogravitational runaway scenario for LMXBs
\citep{levin99} .  The two closed loops in Figure \ref{fig:evolution}
show the evolution of the spin and temperature of a NS accreting at
$10^{-8} M_\odot$~yr$^{-1}$ (i.e, same as in \citealt{levin99}), but
including the VBL damping.  The evolution is qualitatively the
same. First, the star spins up until it reaches the instability
line. The r-mode amplitude then grows until saturation (at amplitude
$\alpha_s$), heating the star, and then spins it down due to
gravitational wave emission. The r-mode eventually stabilizes and the
star cools down. For the chosen $\alpha_s$, the thermal runaway spins
the star down to $200-400$~Hz.  The final frequency is not sensitive
to the initial temperature of the star, but only to the assumed
$\alpha_s$. The duration of the active r-mode phase is $< \ {\rm yr}$, while
the duration of the cool-down at constant spin is $\sim10^5$~yrs. The
spinup from $\sim400$ to $\sim1100$~Hz takes roughly
$5\times10^6$~yrs.

Therefore, in agreement with \citet{levin99}, we do
not expect that any of the currently observed LMXBs are in the active
r-mode phase. Moreover, this evolution cannot explain the clustering
of LMXB spins around $300$~Hz \citep{klis99:_millis}, since the
duration of the cool-down at constant spin phase (horizontal leg in
Figure~\ref{fig:evolution}) is much shorter than that of the spin-up
phase (the vertical leg). Other mechanisms, such as mass quadrupole
radiation from the crust \citep{bildsten98:gravity-wave} can likely
explain such clustering.

What about newborn NSs? NSs born in supernovae are thought to rotate
near breakup, and have initial temperatures $T_i\approx10^{11}$~K.
They quickly cool, roughly according to $T_9=(t/\tau_c)^{-1/6}$ for
$T\ll T_i$, where $\tau_c\approx1$~yr is the Urca cooling time at
$10^9$~K \citep{shapiro83}.  During the initial cooling stage, the
r-mode instability line is as calculated previously (dashed line in
Figure~\ref{fig:instability}), and the spin-down evolution proceeds
according to the scenario described by \citet{owen98:_gravit}.
However, a solid crust forms when the NS has cooled to $T_{\rm
m}\sim10^{10}$~K (the exact temperature depends on the composition),
after which we expect the evolution to be significantly altered.

The dotted line in Figure~\ref{fig:evolution} shows the evolution of
$\nu_s$ and $T$ of a newborn NS, computed as in
\citet{owen98:_gravit}, with initial spin $\nu_{s,i}=1320$~Hz, but
including the VBL and the heating from it.  The star cools from
$T_i=10^{11}$~K and enters the instability region.  The r-mode then
grows, saturates at $\alpha_s=1$, and spins the star down.  We find
that the final spin frequency of the star is $\nu_f=415$~Hz including
the VBL, rather than $120$~Hz \citep{owen98:_gravit}.  The spindown is
also of shorter duration, lasting only $10^4$~s, rather than the
$\sim1$~yr of the original calculations of \citet{owen98:_gravit}.
For shorter Urca cooling time $\tau_c$, the final frequency is
somewhat higher.  The effect of the heating due to the VBL on the
cooling time is negligible.  In our simulation, the r-mode amplitude
grows only by a factor of 3 from its initial value by the time the
star cools to $T_{\rm m}$, so we do not expect the presence of the
r-mode to affect crust formation. In general, the rapid spindown phase
begins when the Urca cooling time at the current temperature,
$T/(dT/dt)\propto T^{-6}$, exceeds the gravitational wave spindown
time, $\Omega/(d\Omega/dt)\propto\alpha_s^{-2}$. Therefore, unless
$T_{\rm m}$ is much less than $10^{10}$~K, the crust will form while
the r-mode amplitude is still rather small.

The strain amplitude is a very shallow function of $\nu_s$ during the
spin-down stage, $h_c\propto\nu_s^{1/2}$ \citep{owen98:_gravit}.
However, most signal-to-noise ($S/N$) in a
gravitational wave detector is accumulated at low $\nu_s$, where the
source spends most of its time. Hence, the total $S/N$ depends
sensitively on the low-frequency cutoff of the spin-down evolution.
Using the results of \citet{owen98:_gravit}, we find that raising
the cutoff frequency to $415$~Hz from $120$~Hz reduces the $S/N$ from
$\sim8$ to $\sim2.5$ for ``enhanced'' LIGO and a NS at a distance of
$20$~Mpc, where the event rate is expected to be a few per year.

\section{Conclusions and Future Work}
\label{sec:conclusions}

 Our initial work on the viscous boundary layer between the
oscillating fluid in the core and the co-rotating crust shows that the
dissipation there is very large, making it the predominant r-mode
damping mechanism when the crust is present.  The smallest spin
frequency which allows the r-mode to operate is about 500 Hz, nearly a
factor of five higher than previous estimates. This substantially
reduces the parameter space for the instability to operate, especially
for older, colder NSs, such as those accreting in binaries and
millisecond pulsars.  It resolves the discrepancy between the
theoretical understanding of the r-mode instability and the
observations of millisecond pulsars and LMXBs.

In our estimates we presumed that the boundary layer is laminar.  Of
course, turbulence in the VBL would increase the viscosity there and
move the instability to higher rotation frequencies.  We also showed
that the r-modes induce some transverse motions in the crust, though
these motions appear to be negligibly small compared to the r-mode
amplitude.  The Coriolis force is likely to change the details of the
eigenfunctions in the boundary layer, but it is unlikely to change its
gross structure.  Finally, based on the large conductivity contrast
between the core and the crust, we have presumed that the VBL heating
evenly spreads throughout the isothermal core.  This may be an
oversimplification, and a more detailed time-dependent calculation of
the heat transport will yield the radial temperature profile.  This
is especially important for the accreting systems, where the crust
melting temperatures are lower because of the smaller mean nuclear
charges \citep{haensel90b}.

Can a weak magnetic field substantially change our arguments?  The
Ohmic diffusion time across the VBL is many years, much longer than
the oscillation period. Hence, any magnetic field protruding into the
fluid from the crust will be pulled and sheared in a nearly ideal MHD
response. The field produced by the shear is $\delta B/B\sim\alpha
R/\delta$, and hence the magnetic field does not compete with viscous
shear when $B\ll(\rho\nu\Omega)^{1/2}\approx
10^{11}{\rm~G~}(\nu_s/1{\rm~kHz})^{1/2}/T_8$.  The surface dipole
field strengths in LMXBs and MSPs are lower than this value. If the
same can be said about the $B$ field at the base of the crust, then
the viscous boundary layer we have discussed should apply. Of course,
for younger and potentially much more magnetic neutron stars, the
story will be modified, as the restoring force from the stretched
field lines needs to be self-consistently included.

\acknowledgements
We thank Andrew Cumming, Yuri Levin, and Lee Lindblom for helpful
conversations.  L.B. is a Cottrell Scholar of the Research Corporation
and G.U. is a Fannie and John Hertz Foundation Fellow. This work was
supported by the National Science Foundation through Grants
AST97-31632 and PHY 94-07194.

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text:
You are here: Home / Action Alerts / Action Alert: Vote on Abortion Clinic Inspection and Voter ID
Action Alert: Vote on Abortion Clinic Inspection and Voter ID
May 9, 2011 By Diane Leave a Comment
Issues (check corresponding number in 'Details' and 'Action' Sections)
1.) Vote on Abortion Clinic Inspection Bill
2.) Combating Voter Fraud
3.) How Did Senator Casey Vote on Confirmation?
1.) HB 574 will amend the Health Care Facilities Act to require abortion facilities to meet the same standards as Ambulatory Surgical Facilities. The passage of such legislation would significantly reduce the number of abortions, abortion facilities and abortionists in Pennsylvania. Pro-abortion forces are claiming that such legislation will result in the closure of 17 of the approximately 20 free-standing abortion chambers in Pennsylvania and increase the cost of an abortion by $1,000.
2.) HB 934 was introduced by State Representative Daryl Metcalfe on March 4th. If passed, this bill would require voters to present a valid photo ID when they vote. Such a bill passed several years ago, but was vetoed by Governor Rendell. HB 934 currently sits in the House State Government Committee which Representative Metcalfe chairs. In an orchestrated effort last Thursday all members of the House State Government Committee received emails from the League of Women Voters of Pennsylvania and the County Commissioners Association of Pennsylvania asking them to oppose the bill.
3.) Last Wednesday the Senate voted to confirm John McConnell, Obama's nominee to the U.S. District Court for Rhode Island. McConnell was the Director of the Planned Parenthood Abortion Clinic in Providence Rhode Island from 1997 to 2001. He was the director of the George Wiley Center with not only close ties to ACORN, but it was named after one of ACORN's founders! McConnell's results-oriented lawsuits have stretched legal theories far beyond the fringe of reason, and who, at best, misled the Senate Judiciary Committee (and at worst lied in his written answers to their inquiries), and was not suited for a lifetime appointment to the Federal Judiciary. But, guess what, that didn't stop Senator Bob Casey, Jr. from voting for confirmation!
1.) Many weakening amendments from State Representatives Chris Ross and Dan Frankel are expected TODAY. While Representatives Stephen Barrar and Bryan Barbin will introduce amendments today that would strengthen HB 574. Contact your State Representative and ask him or her to oppose any weakening amendments and support amendments to strengthen HB 574. Ask your State Rep to support a strong HB 574 in the final vote on Tuesday May 10th. Click here for contact information.
2.) It is especially important that you contact your State Rep if he or she is on the House State Government Committee because if the bill doesn't get out of this committee it dies! Contact your State Representative and express your support for HB 934 and the need to reduce voter fraud. Click here for contact information.
3.) If Senator Casey's vote to confirm radical judicial nominee John McConnell concerns you, give his office a call. Click here for contact information.
Filed Under: Action Alerts, Life Issues, Politics Tagged With: abortion, Abortion clinics, Ambulatory Surgical Facilities, confirmation, inspection, John McConnell, Senator Bob Casey Jr., voter fraud

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Lavelle said we can pick up our final exam in 3034 Young Hall Week 3 of Spring Quarter!
Yes, and remember that an irreversible reaction will always require less work.
Topic: What does unique rate of reaction mean?
Re: What does unique rate of reaction mean?
The unique rate is a rate of a reaction divided by its stoichiometric coefficient. A unique rate will be the same for each reactant or product but the product will be a negative value.
Very intriguing questing Nathan Tran. I am glad you asked this to further facilitate the conversation of Kinematics.
Half life reactions are just 1st order reactions!
Free energy is a state function!
If Gibbs Free Energy is negative, it is spontaneous.
The reaction will eventually stop when there are no more ions trading off.
For redox reactions you have to do both, balance, like we learned in high school, and make sure the charges are even.
The anode and the cathode are deemed right and left just as a formality so you can tell where the reactions are taking place. An anode is the oxidation part of the reaction and the cathode contains the reduction part of the reaction.
Yes, when delta G is negative it is spontaneous and when delta G is positive it is not spontaneous. When delta. G is 0, it is at equilibrium.
When do we use this equation to find internal energy? And where does the 3/2 come from for this equation?
In a closed system, heat can still travel in and out of it, but in an isolated system nothing can affect the internal energy(that is why U=0 for a closed system).
In lecture Lavelle defined degeneracy as the number of ways of achieving a given energy state, and it can help us find entropy.
I am terrible at explaining, but here is the video I watched: https://www.youtube.com/watch?v=54n1XppP-lA and I got confused with the example at 25:46 when the initial concentrations of the products were not 0.
Condensations is an exothermic process!
If there are the same number of moles on both sides of the equation and you increase/decrease the volume then does the equation shift to the left or right?
I was watching a YouTube video, and I got a bit confused on a topic. If you are given initial concentrations and the Kc value, and the Qinitial>Kc then do you switch the x signs for change in molarity when doing the ICE table to find the final equilibrium concentrations? If so, then why?
Solving for Q is the same as solving for K. When Q is less than K, forward reaction is favored. When Q is greater than K, reverse reaction is favored.
We can know if a reaction is endothermic when heat is absorb and in contrast an exothermic reaction is when heat is released. This is how one can environmentally tell if a reaction is exothermic and endothermic. Other than that, I think one has to know if delta H is negative or positive.
What does it mean when "expansion occurs" on a certain reaction?
When using the ICE box, you can use partial pressure and molarities/concentrations.
When converting to Kp and Kc, you use the ideal gas law, P=concRT, and you use the concentrations given to find pressure in atm.
Kc is specifically the molar concentration [P]/[R], and K is just an overall equilibrium constant.
Homework questions are 7 points a week (70 points per quarter) and the 3 chemistry community posts are 3 points a week (30 points per quarter).
Topic: Solids do not have concentrations?
Re: Solids do not have concentrations?
Yes, you are correct, solids do not have concentration, and neither do pure liquids; therefore, they cannot be used to calculate for K.
Yes, a lone pair is considered a region of electron density and therefore you will count it to find hybridization.
Can someone elaborate what polar power is? And why a high charge and a low volume affect it?
A stands for the central atom!
Yes! Everything that was not covered on the midterm!
The center atom would be oxygen because if you look at the periodic table it has the lowest ionization energy.
Dr. Lavelle said it depends on if we are behind or ahead.
The degeneracy of a 4p orbital will be 3 because they all have the same energy level.
The mass composition percentage has to add up to 100%.
Why do we choose the atom with the lowest ionization energy as the central atom for Lewis Dot Structures?
The change in energy can be negative(exothermic) or positive(endothermic). In this case the change of energy is exothermic in which energy is released, so the value will be negative.
Yes, a nodal plane is in a region of zero electron probability meaning the planes are perpendicular to the internuclear axis. For example, the S orbital has no internuclear axis; therefore, it has no nodal planes.
I would round the answers to the significant figures towards the end because it would provide the most accurate answer. Throughout the problem I would use the most amount of decimal places in order to obtain a precise number until the end.
For this upcoming test, I would memorize the formulas needed, for there are not that many. We will get a periodic table for the molecular masses though.
Usually the problem indicates what units should be utilized for the answer. If not, stick to your standard metric units of measurement, such as liters, grams, and meters. These are additionally the units employed in most chemistry concepts like molarity and quantum chemistry.


text:
module Rushmate
  # Rushmate::Exit provides a list of methods for exiting
  # a command and changing the output type in Textmate
  #
  # For instance if you specified the command to be
  # output: Discard
  # it may be benificial to show a tooltip if the command
  # could not do what it was tasked to do
  #
  # Example:
  #
  #   Rushmate::Exit.show_tool_tip("could not find file")
  module Exit
    class << self
      def discard
        exit 200
      end

      # changes output to replace selected text
      def replace_text(out = nil)
        print out if out
        exit 201
      end

      # changes output to replace selected document
      def replace_document(out = nil)
        print out if out
        exit 202
      end

      # changes output to insert text at editor position
      def insert_text(out = nil)
        print out if out
        exit 203
      end

      # changes output to insert a snippet at editor position
      def insert_snippet(out = nil)
        print out if out
        exit 204
      end

      # changes output to show html
      def show_html(out = nil)
        print out if out
        exit 205
      end

      # changes output to show a tool tip
      def show_tool_tip(out = nil)
        print out if out
        exit 206
      end

      # changes output to create a new document
      def create_new_document(out = nil)
        print out if out
        exit 207
      end
    end
  end
end

redpajama_set_name: RedPajamaGithub


The Free Software Foundation (FSF) runs a website to organize meetings related to free software/open source. It's a wiki so anyone can update it.
I'm using it to organize the Toronto Free Software Group/LibrePlanet Ontario meetups. If anyone's interested in free software and lives in Toronto or across Ontario, we'd be happy to have you subscribe to the mailing list!


A motion to modify disposition or revoke supervision can be filed against your child if he or she has violated the terms and conditions of his or her original probation. This is a serious matter. Depending on the nature of the original charge, this can be the first step in the state of Texas removing your child from your home and placing him or her outside your home in a residential setting or in a Texas Juvenile Justice Department (TJJD) facility.
Generally, depending on your child's supervision guideline level, a violation of his or her probation can result in an increase to a higher level, an extension of his or her probation term or the addition of other conditions of probation. Allow the law office of J. Michael Price II, located in Dallas, Texas, to guide your child through the process.
If your child is facing a motion to revoke his or her probation, please call us immediately at 214-765-8000 to schedule a consultation with our attorney. All hope is not lost. We have been very successful at keeping our juvenile clients on their same probation terms and not allowing the state or judges to remove our client from his or her home. Even in impossible situations, I have been successful in keeping kids from being sent to TJJD.
We put more than 15 years of proven success behind your child's case and work to eventually seal juvenile records to make sure mistakes today don't become a burden as adult.
Practicing exclusively in criminal and juvenile defense, and recognized by organizations including Martindale-Hubbell, and has been named in Texas Super Lawyers®, a Thomson Reuters service, from 2005-2018, as published in Texas Monthly Magazine, we stand ready to provide reliable and effective representation for all juvenile crimes. Contact our office today or call us directly at 214-765-8000 to schedule an initial consultation.


As Vice President of Preconstruction at JC&A, Michael offers twenty years of construction industry experience. He is responsible for the daily operations of estimating and pre-construction services and for overseeing the daily operations of the company's estimating department. Mike possesses a wealth of experience in construction management, with expertise in estimating, procurement and cost control.
Michael earned a Bachelor of Science degree in Civil Engineering with a Minor in Engineering Management from Tufts University. His professional experience encompasses the involvement in multiple projects (ranging in size up to $300 million) with extensive experience in hard bid/lump sum, GMP and conceptual estimates as well as value engineering and risk assessment analysis.
His experience spans from large heavy/highway transportation projects to corporate, residential and retail/restaurant markets.
Mike lives in Braintree, MA with his wife, Kara and their 3 children Matthew, Sammy and Kelcey.


If you're doing loads of exercise, eating well and still struggling to lose weight, this is for you. In this episode, I interview Personal Trainer and Nutritionist Ash Lane. Ash helps women learn to eat more, train less, build muscle and lose fat.
Looking for real food recipes and tips to help you lose weight, get more energy and thrive? You've come to the right place! I'm Fran, a Functional Nutritionist. Learn more about me here.
READY TO LOSE WEIGHT, GET MORE ENERGY & THRIVE?
Schedule your free 20 minute Functional Nutrition Strategy today. Available by phone or Skype.
Grab your free copy of Cloud Nine, your 8 step guide to a blissful night's sleep.


text:
'Moana' is a feast for the soul
Directed by Ron Clements, Don Hall, John Musker, and Chris Williams
Somewhere along her wayfinding journey, Moana tells Maui, "I am not a princess." While nobody can claim that "Moana" doesn't find some inspiration in Disney's 80-year history of princess stories, it definitely finds a way of setting itself apart.
On the island where Moana (Auli'i Cravalho) lives with her parents and pet pig, everything they need is within arm's reach. They find coconuts on their trees, fish in their bays. There's no need to go beyond the reef. But Moana feels called to the sea. Her crazy grandmother (Rachel House) encourages her adventurous spirit, but her father, the chief (Temuera Morrison), tries to protect her by keeping her under his wing. Soon, though, the island will be plagued. The fish leave, the coconuts dry up. Moana will need to sail the ocean to find the demi-god Maui (Dwayne Johnson), the only one who can bring her island back to life.
Auli'i Cravalho, welcome to your bright and exciting future. The then-14-year-old Hawaiian high school student sent in an audition tape that impressed her friends, but one she feared wouldn't stack up to the hundreds of others who wanted the coveted lead role. Thankfully for her and for us, it impressed the directors. Her spunky spirit bleeds through the colorful, vibrant animation and brings Moana (both the character and the movie) to life. And her vocals capture the emotions in Lin-Manuel Miranda's lyrics. Just last week, People named Dwayne Johnson their Sexiest Man Alive. His cocky character Maui would would have relished that. Johnson is a great choice for the character. His energy helps drive the movie ahead with full steam. Although his song, "You're Welcome," isn't the movie's best, it is remarkable for a man whose only prior singing experience is pulling out a guitar and serenading "Stone Cold" Steve Austin during a wrestling match.
Lin-Manuel Miranda's genius was always his writing. I've never seen "Hamilton," but I've seen him act and sing elsewhere…while I appreciate his efforts, his real talent is writing the words and the scenes, not reciting them. So when I heard he would be composing original music and lyrics for Disney's "Moana," I got excited. I'm sure you did, too. Well, it's worth all the hype. Miranda's music propels the story forward, clues you in on what's going on, and breaks up long stretches at the right time—the music always comes just when you're hoping it will. But not only is it good in context, it's wonderful alone, too. Future generations of Disney-lovers can expect to find "How Far I'll Go" (both Cravalho's movie version and the soundtrack version by Alessia Cara) on their Disney compilation albums. I've listened to it on Spotify more than a few times already.
The wise mentor, the "chosen one," the trickster, the protective parent, and the animal sidekick are all characters we've seen rehashed hundreds of times before. But "Moana" also pulls from a rich multi-cultural storytelling tradition, using an ethnically and racially diverse cast. Moana is very decidedly not like other Disney princesses and "Moana" not like other Disney princess movies. It's a beautiful tapestry of color and sound that will fill your heart after Thanksgiving fills your stomachs. Go see this movie.
Posted in Film Review, MovieTagged 2016, Auli'i Cravalho, Cravalho, Dwayne Johnson, film, Maui, Moana, Moana movie review, movies, Rachel HouseBy Logan BurdLeave a comment
← 'Lilo & Stitch' and its sequels shouldn't be forgotten
'Manchester by the Sea' : Tide change marked by this cinematic effort →


White House News Photographers Association invites ASMP members to Eyes of History Gala. Discounted tickets available to ASMP members.
The 2018 Eyes of History Gala will be held on Saturday, June 16 at the Ritz-Carlton in Washington, DC. The annual event honors the best in visual journalism from the winners of the annual Eyes of History contests. Join us as we celebrate the 97th anniversary of the WHNPA!
The black tie gala kicks off at 6:30pm with a Cocktail Reception, followed by Dinner at 8:00pm and drinks and dancing until 1:00am.
ASMP members will receive the WHNPA member price for tickets.


We love teaching as much as eating! Get in touch for personal or group cooking classes in Creole, Cajun, and Sushi. We will work with you to create a truly unique experience that you can bring home with you, and share with your family and friends...or bring them along with you!
Below is an example of one of our classes, if this looks like something you'd be interested in get in touch with us to plan your own class. We enjoy working with our guests to create unforgettable experiences, let us know if you have any requests beforehand so we can design the perfect class!
We'll start the day with a Partridge Berry Tea and get started prepping and cooking. Once our boulettes are formed, our bread pudding is soaking and our gumbo is simmering, Terrence will take you out for a mini foraging expedition. You'll grab some goodness to garnish our dishes and enjoy the surroundings. When you return, replenish yourself with a home brewed ginger ale. We'll finish our dishes, set the table and enjoy what we have prepared.
Newfoundland Style Sushi - You've never had Sushi like this!
Our locally sourced sushi is one of our most popular dishes, and you can come and learn all about it! Weather permitting you can harvest seaweed yourself, learn the process of preparing it and the other ingredients as well as the basics of sushi rice and how to make sushi rolls. Terrence incorporates local ingredients such as candied scrunchions, locally dried seaweed, minced dried capelin and of course seafood. Once completed you will enjoy the meal you have prepared as well as the confidence in knowing you have new skills to share with family and friends back home!


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Being in a new home, the improvements and decorating are never ending. But, we are taking it slow. It takes quite a bit to make a house a home. And when you become a homeowner some of the strangest things might tickle your fancy and make you happy. For me it's awesome, functional home appliances….


text:
/*
    DOM module handler, compatible with @pod-point/module-loader

    All modules export `init` methods.

    DOM modules:
        - Can be initialised multiple times per page.
        - Can optionally export a `destory` method.
        - Are destroyed between page transitions.
        - Initialised by adding the imported module name to an element's
            `data-js-module` attribute. Multiple names can be added and are
            space-delimited.
*/
import { select, nodesToArray } from '@pod-point/dom-ops';

const DATA_TAG = 'data-js-module';

var activeModules = [];
var domModules = {};
var definedDataTag = '';

function init() {
    var moduleElements = nodesToArray(select(`[${definedDataTag}]`));

    activeModules = [];

    if (moduleElements) {
        moduleElements.forEach(element => {
            let modulesToLoad = element.getAttribute(definedDataTag).split(' ');

            modulesToLoad.forEach(name => {
                let module = domModules[name];

                if (module && module.init) {
                    module.init(element);
                    activeModules.push(module);
                }
            });
        });
    }
}

function refresh() {
    activeModules.forEach((module) => {
        if (module.hasOwnProperty('destroy')) {
            module.destroy();
        }
    });

    init();
}

export default function (modules, dataTag = DATA_TAG) {
    domModules = modules;
    definedDataTag = dataTag;
    return { init, refresh }
}


text:
Colorado HealthOP Folds: What Consumers Need To Know
HealthOp workers in Denver encourage the public to get health coverage under the Affordable Care Act in this March 2014 photo.
Colorado HealthOP collapsed. The state Department of Insurance says the financial viability of HealthOP was in jeopardy when it found out it would receive only about $2 million in federal reimbursements this year, after expecting about $16.2 million. The shortfall meant HealthOP's rainy day fund would be erased, and would likely go into the red to the tune of about $34 million by year's end.
How many people are affected?
HealthOP says it had 82,785 members as of Sept. 15. Of those, 79,877 held individual policies and another 2,908 are covered under small group policies.
What happens to them?
All individual policy holders will be covered until their existing 2015 policies expire, as long as they pay their premiums. Small group policies will be effective until the anniversary date of the policy. After that, HealthOP customers will have to look for new health insurance.
Do they need to keep paying premiums?
Yes. HealthOp customers must also continue to pay deductibles, co-payments and co-insurance when required.
What about claims?
HealthOP will keep paying claims for current members. If HealthOP can't pay, the Colorado Life & Health Insurance Protection Association, a nonprofit will step in and pay claims.
What are the deadlines?
Individual policy holders must choose another carrier during open enrollment, which starts Nov. 1 and goes through Jan. 31. They can work with Connect for Health Colorado, the state's insurance marketplace, or find coverage off the exchange. Small group policy holders have until their anniversary date of their policy.
Can consumers still see their doctors and other health care providers?
Yes, for both medical and pharmacy needs. Anyone who experiences problems should contact Colorado HealthOP member services at 866-915-6619.
What about the tax credit?
If you get a tax credit for your 2015 Colorado HealthOP individual coverage, it will continue through the end of the policy. The insurance department is reminding all consumers that health insurance tax credits are only available if coverage is purchased through Connect for Health.
For every one else, the calculations on advance premium tax credits will likely change since since the Colorado HealthOP was the carrier with that second-lowest Silver premium in many areas . The APTC is calculated based upon the second-lowest Silver plan in an area, says the Colorado Division of Insurance.
Are any other health care providers in trouble?
The DOI says no other carriers are affected.
More questions? Here's contact information:
The Colorado Division of Insurance regulates the insurance industry and assists consumers and other stakeholders with insurance issues. For more information call 303-894-7499 / toll free 800-930-3745.


Last month, we all got a good view of what the Metro update would look like, and for the most part it's pretty sleek. It ditches rows in favor of a single gridded box per category, which gives tiles of featured content that feels less cramped, making it easier to navigate the choices.
They've also integrated the Kinect sensor into a fully functional hands-free remote, taking us one step closer to clicker-free television. And now everyone can surf the web directly from their Xbox with the Bing search function.
Microsoft continues to work on the Metro update for Xbox, and the latest sneak peak can be seen in a slightly blurry leaked video in French. Though it's not in English, you can still get the picture, as it gives us a taste of the Xbox Live Marketplace, the Bing search page, and the new Metro UI. It's not the best of videos, but it does show you what to expect when the rumored November 15th update comes to consoles everywhere.
I'm still wondering if Netflix will get a new look and functionality, because I find it quite difficult to navigate. Maybe having the ability to search Netflix, Hulu Plus and Zune all at once with Bing is a good thing, but I doubt I'll ever get to taste the whole shebang, since I'll be cancelling my Netflix subscription soon.


text:
Cruise Line News
Follow @Cruise_TT
Celebrity Cruises Launches New 'Captain's Club' Program
Cruise news, forum and port timetables and schedules. Lists which ships are in what ports for upcoming days.
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CruiseTT
Enhanced loyalty program features two new tiers, with greater recognition and rewards
Celebrity Cruises is excited to announce improvements to its Captain's Club loyalty program.
Guest feedback helped define the new program features, which include two new, additional levels of status and rewards beyond the existing "Elite" level, which is the highest level of membership in the brand's current four-tiered program.
Effective on sailings commencing after November 25, 2013, the new Captain's Club will offer a six-tier program. The Club's current levels of "Preview," "Classic," "Select" and "Elite" will remain, with two new tiers -- "Elite Plus" and "Zenith" -- each with their own unique set of benefits and privileges.
Members who achieve the new Elite Plus status will receive an even higher level of recognition and broader benefits, including additional beverage and specialty dining discounts, complimentary 200-minute Internet packages, complimentary cappuccinos, lattes and more.
Members who achieve Zenith status will receive benefits and perks befitting this ultimate level of membership, such as access to Michael's Club Lounge (available fleetwide in 2014), a complimentary premium alcoholic beverage package, complimentary laundry, a 1,600-minute Internet package, and other benefits.
Celebrity's guests now can accelerate their progression through the loyalty tiers with a new Club Points system which recognizes the stateroom category as well as the days spent onboard. Members' previous cruise credits will be automatically converted into Club Points, and members will retain all of the benefits they earned in the program to-date – with no expiration. In many cases, guests may automatically become charter members of Celebrity's new Elite Plus or Zenith tier. It is important to note that no current members will lose any of the benefits they have come to expect and enjoy today. Full program details are available at www.celebritycruises.com/captainsclub
Another new enhancement is the ability to quickly access special pricing exclusively for Captain's Club members through the Captain's Club portal on the Celebrity Cruises website. By simply entering their name and Captain's Club member number on the site, they can instantly see available loyalty pricing.
"At a time when many loyalty programs are cutting back on benefits or making it more difficult to redeem rewards, we're thrilled to do just the opposite," said Celebrity's Director of Loyalty Lee Moreau. "Guest loyalty is the cornerstone to any successful business, and that's why, at Celebrity Cruises, we make our guests the center of our attention. We hope this reinvigorated program will even more vividly show our guests how much we appreciate their loyalty, and allow us to welcome them back onboard even more frequently."
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Year Before The Cruise (Votes: 17)
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Last Minute (Votes: 2)
Your Cruise Ship And Port Timetable


text:
Why are we seeing outbreaks of mumps in Texas?
April 21, 2017 April 21, 2017 Momentum 1 Comment Dr. Peter Hotez, mumps, National School of Tropical Medicine, pediatrics, Texas
Dr. Peter Hotez, dean of the National School of Tropical Medicine at Baylor College of Medicine.
Texas has seen a record number of mumps cases in 2017. The Texas mumps outbreaks began in 2016, with almost two hundred cases in that year, most of them occurring towards the end of the year. We have seen more than 200 cases this year. According to some reports, this represents the largest mumps surge in more than two decades. Such numbers are in contrast to 2015 when only 20 cases were reported in Texas.
Within the last few weeks, I have received a number of calls from science journalists asking if the new rise in mumps is related to a corresponding rise in a powerful and outspoken Texas anti-vaccine movement. Indeed, I have recently predicted that Texas could soon be affected by breakthrough infectious disease outbreaks, especially measles virus epidemics, due to high rates of non-medical exemptions in our state.
It is possible that pockets of non-medical exemptions, due to the Texas anti-vaccine movement, have a role in the 2016-17 mumps surge. We'll learn more in the coming weeks as the Texas Department of State Health Services conducts investigations. But in the case of mumps there could be other explanations.
Shown in Figure 1 is a representation prepared by the U.S. Centers for Disease Control and Prevention (CDC) for the total number of mumps cases between 1968 and 1977. It shows that mumps cases declined precipitously after a vaccine was introduced in 1967 and then again in 1977 when mumps vaccination became routine.
Fig. 1. Mumps cases in the United States between 1968 and 2011. Graph courtesy of the CDC.
What's interesting about this chart is the inset that magnifies the increased number of cases beginning in the 1980s and another increase in 2006 and 2010. We are now seeing yet another uptick in cases. According to the CDC, there were only about 200 mumps cases reported in all of 2012, but then in 2016 there were more than 5,000 cases. So far this year from Jan. 1 to March 25, there have been nearly 2,000 cases.
So why is 2016-17 another big mumps year similar to 2006 and 2010? I don't think we really know the answer. This year's outbreak in Texas seems to have originated in the neighboring state of Arkansas, which is experiencing even a bigger outbreak. Missouri is also seeing a surge in cases (see Figure 2). So this is mostly a south-central U.S. mumps epidemic.
However, the most recent Texas outbreak appears to be occurring on South Padre Island and may be related to spring break. It's unclear what the relationship is, if any, between the South Padre Island and Arkansas mumps outbreaks. It's also interesting to note that there are a significant number of cases in Washington state, which also has a vigorous anti-vaccine movement.
Fig. 2. Mumps cases in the United States between Jan. 1, 2017 and March 25, 2017. Graph courtesy of the CDC.
A number of virus and vaccine experts, including Dr. Paul Offit at the Children's Hospital of Philadelphia, have pointed out that of the three vaccines contained in the MMR vaccine (measles, mumps, and rubella) the mumps component is the weakest in terms of inducing high levels of protection. By some estimates a single dose of the mumps vaccine induces only about 75 percent protective immunity, while even two doses induce less than 90 percent protection.
Therefore, our state and federal response to the 2016-17 mumps outbreak could be to recommend a third dose of the mumps vaccine in the areas experiencing outbreaks, such as the one that occurred two years ago at the University of Illinois Urbana-Champaign. Alternatively there may be a rationale for setting a new national policy around recommending three mumps vaccinations routinely.
We'll need to follow the Texas mumps epidemic closely. In the meantime, view the CDC's detailed Q&A for mumps patients and their families.
-By Dr. Peter Hotez, dean of the National School of Tropical Medicine at Baylor College of Medicine and Endowed Chair in Tropical Pediatrics at Texas Children's Hospital
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One thought on "Why are we seeing outbreaks of mumps in Texas?"
The exemption rates in the heavily affected Arkansas counties were hugely disproportionate and absolutely compromised herd immunity. In the Springdale school district, which straddles Washington and Benton counties, there were more than 1500 philosophical exemptions. There's a link to the county-by-county list in this news article:
http://m.arktimes.com/ArkansasBlog/archives/2015/02/05/where-the-unvaccinated-are-northwest-central-arkansas


Guest blog by EDA Member and GreenDOC Gold Certified Dr. Thomas Gent of SoLa Dental. Located in Austin, Texas, SoLa Dental focuses on the health and well-being of patients as well as the planet. Learn more about SoLa Dental on their website.
Your mouth is a mirror that reflects your overall health and well-being. It's also a key determinant of your nutritional status and your self-esteem. "Oral health means more than sound teeth. Oral health is integral to overall health," says Donna E. Shalala in the Surgeon General's Report on Oral Health.
But what is oral health?
First of all, the word "oral" refers to the mouth, which includes not only the teeth and gums and their supportive tissues, but also the roof and the floor of the mouth (the hard and soft palate), the tongue, the lining of the mouth and the throat (called the mucosa), the lips, the salivary glands, the upper and lower jaws, and the chewing muscles. Oral health also involves the branches of the nervous system, the immune system and the vascular system (blood vessels) that serve this part of the body.
The health of the oral tissues is indicative of the health of organs and systems throughout your body. Your dentists and other healthcare providers can gather an enormous amount of information about your overall health simply by examining these tissues.
A thorough oral exam can uncover nutritional deficiencies, microbial infections, immune disorders and some forms of cancer.
Clues to a disease can be discovered by analyzing saliva under a microscope.
Facial nerves have counterparts elsewhere in the body.
The jaw bones and jaw joint function like other musculoskeletal regions of the body.
Regular dental visits allow many problems to be prevented, and the rest to be treated the most successfully and conservatively. Don't wait until you are in pain! By then it is usually a much bigger problem. Remember, we care about your overall health and well-being, not just your teeth.


BEIRUT (AP) — Jamal Khashoggi, the Saudi journalist who disappeared last week after a visit to his country's consulate in Turkey, was once a Saudi insider. A close aide to the kingdom's former spy chief, he had been a leading voice in the country's prominent dailies, including the main English newspapers.
A graduate of Indiana State University, Khashoggi began his career in the 1980s, covering the Soviet occupation of Afghanistan and the decade-long war that followed for the English-language daily Saudi Gazette. He traveled extensively in the Middle East, covering Algeria's 1990s war against Islamic militants and the rise of Islamists in Sudan.
Khashoggi rubbed shoulders with the Saudi royal family and supported efforts to nudge the kingdom's entrenched ultra-conservative clerics to accept reforms. He served as an editor for nine years on the Islamist-leaning al-Madina newspaper and was frequently quoted in the Western media as a reformist voice and expert on Islamic radicals.
He was fired from his post as an editor at Al-Watan, a liberal paper founded after the 9/11 terror attacks, just two months after he took the job in 2003. The country's ultra-conservative clerics had pushed back against his criticism of the powerful religious police and Ibn Taymiyah, a medieval cleric viewed as the spiritual forefather of Wahhabism, the conservative interpretation of Islam that is the founding tenant of the kingdom.
Khashoggi then served as media adviser to Al-Faisal, the former spy chief, who was at the time the ambassador to the United States.
Khashoggi returned to Al-Watan in 2007, where he continued his criticism of the clerics as the late King Abdullah implemented cautious reforms to try to shake their hold. Three years later, he was forced to resign again after a series of articles criticizing Salafism, the ultra-conservative Sunni movement from which Wahhabism stems.
Khashoggi's final break with the Saudi authorities followed the Arab Spring protests that swept through the region in 2011, shaking the power base of traditional leaders and giving rise to Islamists, only to be followed by unprecedented crackdowns on those calling for change. Siding with the opposition in Egypt and Syria, Khashoggi became a vocal critic of his own government's stance there and a defender of moderate Islamists, which Riyadh considered an existential threat.
He also criticized his government's diplomatic break with Qatar and war in Yemen as well as Riyadh's policy toward its archenemy, Iran, whose influence has grown in Yemen and Syria.
Before his disappearance, Khashoggi had been living since last year in the U.S. in self-imposed exile, after he fled the kingdom amid a crackdown on intellectuals and activists who criticized policies of Crown Prince Mohammed Bin Salman.


The multi axis inertial measurement unit is a modular concept scalable up to six degrees of freedom (6DoF). Yaw, roll and pitch rate are measured in a scalable range up to 300 deg./sec. The acceleration is detected in longitudinal, lateral and vertical direction. The multi axis inertial measurement unit enables and/or optimizes intelligent safety and comfort systems which are inconceivable without inertial sensor systems.


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Home » Healthy Florida » Most Populated County in Florida 2023
Most Populated County in Florida 2023
The most populated County in Florida 2023 is Miami-Dade County. The county is located in the southeastern part of the U.S. state of Florida. Furthermore, it is the 7th most populated county in the United States. Miami-Dade County is heavily Hispanic, and was the most populous majority-Hispanic county in the nation. Did you know that the earliest evidence of Native American settlement in the Miami region came from about 12,000 years ago?
Miami-Dade Land Area – Most Populated County in Florida 2023
Miami-Dade is also Florida's third largest county in terms of land area, with 1,946 square miles. Only Collier County and Palm Beach County are larger. According to wikipedia "the northern, central and eastern portions of the county are heavily urbanized with many high-rise buildings along the coastline, including Miami's Central Business District in Downtown Miami.
Southern Miami-Dade County includes the Redland and Homestead areas, which make up the agricultural economy of the county. Agricultural Redland makes up roughly one third of Miami-Dade County's inhabited land area, and is sparsely populated, a stark contrast to the densely populated, urban portions of the county northern sections.
The county also includes portions of two national parks. To the west, the county extends into the Everglades National Park and is populated only by a Miccosukee tribal village. Biscayne National Park and the Biscayne Bay Aquatic Preserves are located east of the mainland in Biscayne Bay."
Miami-Dade Fortune 500 Companies
The following 5 companies are based in the metropolitan area
"Lennar (Miami), $16.4 billion
Office Depot (Boca Raton), $12.1 billion
World Fuel Services (Miami), $11.3 billion
AutoNation (Fort Lauderdale), $11 billion
Ryder System (Miami), $5 billion"
The 5 Most Populated Counties in Florida 2023
Rank County Population
1 Miami-Dade County 2,757,592
2 Broward County 1,969,099
3 Palm Beach County 1,518,152
4 Hillsborough County 1,520,529
5 Orange County 1,481,321
A Word from healthylifestyleflorida.com
Miami-Dade county is the most populated county in Florida 2023. Miami is also the most expensive city in Florida. If you prefer to avoid the crowds check Liberty County. It is the least populous county in Florida with just 8,000 people. But there is more in between and something for everyone. Move to the sunshine state! You will love what you can be!
25 Best Places to Live in Central Florida
The 22 Richest Neighborhoods in Florida
What City In Florida Has The Most Billionaires 2023?
Best Fly-In Community Florida
Antje Diana Baumgarten
I believe that the things we do and the products we use determine our lifestyle. Whether your ultimate goal is to optimize your health, fitness or well-being. I introduce you to content that has the true potential to make a significant difference to how we live, love, perform, learn, look, exercise, travel, relax, sleep, work and more.
Pros and Cons of Concierge Medicine
What Love Means – 5 Aspects Everyone Should Know
Self-Care Statistics 2023- Fascinating Facts
How To Strengthen Veins and Arteries – A Perfect Guide
Swimming Pool Statistics 35+ That Blow you Away
Best 10 Tips How To Pack For A Move
Find The Best Gifts Today
Best Gifts For a 70 Year Old Woman
Check our Gifts Guide here


Finding the right projector lamp needn't be a hassle. Here at BT Shop, we bring together a huge range in the same place - and all at value-for-money prices. Ensure high display quality and vivid colours with projector lamps from BT Shop. We've got an extensive selection for you to choose from, with a range of different wattages and devices from some of the leading manufacturers in the field - including NEC, Panasonic and Hitachi. Shop the full range of projector lamps here at BT Shop today.


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Q: Finding probability of bivariate random variable from joint probability density function I have a Bivariate continuous random variable (X,Y) with joint probability density function
$ f_{X,Y}(x,y) = \{{6(y^2-x^2)}$ for $ 0 < x < y < 1$  (0 otherwise)
I want to work out $P(X + Y > 1) $
I have done $$\int_{1/2}^{1} \int_{1-y}^{1} 6(y^2-x^2) dx dy$$
$$ = \int_{1/2}^{1} (4y^3+6y^2-6y)dy$$
$$ = \frac{7}{16} $$
Is this right or have I made a mistake?

A: The OP and the suggestion in the comment by @Zhanxiong are both wrong.
Draw a diagram of the non-zero density region 0 < x < y < 1 and of the region x + y > 1. It will be the box with vertices (0,0),(0,1),(1,0),1,1) with the non-zero density region being the northwest triangle formed in the box from the diagonal line y = x.  This must be intersected with the region x + y > 1 which is the northeast triangle formed in the box from the diagonal line x + y = 1.  Intersecting these regions is thus the upper triangle formed from the two diagonal lines.
The OP is missing part of this upper triangle by integrating x from 0 to 1, which given y going from 1/'2 to 1 is equivalent to integrating x from 0 to 1/2, and therefore missing the term from the right-hand side of the upper triangle, i.e., for x > 1/2.  The correct integration is for x from 1-y to y and y from 1/2 to 1.  Or equivalently, form an additive term for each half of the upper triangle; the left half being for x from 1-y to 1/2 and y from 1/2 to 1, and the right half being for x from 1/2 to y and y from 1/2 to 1. Either way produces the answer of 5/8 (OP missed the 3/16 contribution from the right half of the upper triangle.

redpajama_set_name: RedPajamaStackExchange


Enjoy first-run movies in a locally owned and operated, comfortable and clean theater. Aurora Cineplex features 10 screens with the best picture in town using Sony 4k projection, 3D capabilities, stadium-style, high-back-rocker seating, and unmatched customer service. Located on the lower level of Roswell Town Center Mall behind Big Lots at the corner of Holcomb Bridge and Alpharetta Highway.
This location features 9 auditoriums outfitted with the latest digital projection as well as a full-service bar and lounge perfect meeting up before the movie or a nightcap afterwards. Choose from fresh house favorites or heart-healthy choices on our American Grill Menu, and over 60 premium spirits at the bar. Friendly service is available at the push of a button for an unmatched cinema-dining experience.
The ultimate entertainment center with high speed SuperKarts, 2 European style tracks, arcade with over 120 games, indoor ropes course, rock wall, zip line, comedy club and Andretti Grill Restaurant. Over 10,000 SF of event space!
Area 51/The Fringe Mini Golf offers two beautifully sculpted 18-hole mini golf courses. A family friendly miniature golf course fun for hours and great for any size group! Located right next to Aurora Cineplex!
Good times and open lanes await you. Fun at its best! Something for everybody: bowling, video games, food, and drink. A great way to get out, cut loose and grab some smiles. Monday – Wednesday, 9 AM – Midnight, Thursday, 10 AM – 1 AM, Friday – Saturday, 9 AM – 2 AM, Sunday, 9 AM – 1 AM.
Batting cages and sports facility for training, instruction, birthday and team parties, baseball, softball, basketball, lacrosse, cheer, speed and agility boot camps. Mon. – Thurs. 4 – 10 p.m.; Fri by reservations only; Sat. 8 a.m. – 6 p.m.; Sun. 12 – 6 p.m.
State-of-the-art indoor shooting range and retail facility featuring the finest technology available and offering 24 spacious shooting lanes divided into 3 bays of 8 lanes with clear ballistic stalls and digital target retrieval systems. An unparalleled venue for firearms education, training and enjoyment. Mon. – Fri. 11 a.m. – 8p.m.; Sat. 10 a.m. – 8 p.m.; Sun 10 a.m. – 6 p.m.
Indoor trampoline park, providing fun and fitness for all ages.
The Roswell Recreation & parks Department offers sports activities, games and tournaments throughout the year.
War Games is a tactical laser tag facility. Dedicated to making the game real! We offer high tech realistic simulated weaponry and objective based gameplay. Corporate team building, birthday parties and more. Open Monday & Tuesday by reservation only. Open for walk‐ins Wednesday & Thursday, 3 PM ‐ 9 PM. Friday, 4 PM ‐ 11 PM. Saturday, 11 AM ‐ 11 PM. Sunday, 12 PM ‐ 9 PM.
A mixture of track ball and 5 on 5 basketball with a whiffle ball all at the same time, oh, did we mention you're in a bumper car? Try one of the most unusual games out there + it's incredibly fun and hilarious to watch. 2 courts allow up to 20 people playing at the same time.


income from property, savings and dividends.
You can find out more about income tax at www.hmrc.gov.uk/incometax. You can get help and advice about taxes and completing tax forms from the HMRC self-assessment helpline, on 0845 300 0627, and the HMRC website at www.hmrc.gov.uk.
Employees have their National Insurance Contributions deducted from their pay by their employer. People who are self-employed need to pay National Insurance Contributions themselves. Anyone who does not pay enough National Insurance Contributions will not be able to receive certain contributory benefits such as Jobseeker's Allowance or a full state retirement pension. Some workers, such as part-time workers, may not qualify for statutory payments such as maternity pay if they do not earn enough.
Further guidance about National Insurance Contributions is available on HMRC's website at www.hmrc.gov.uk/ni.
A non-UK national living in the UK and looking for work, starting work or setting up as self-employed will need a National Insurance number. However, you can start work without one. If you have permission to work in the UK, you will need to telephone the Department for Work and Pensions (DWP) to arrange to get a National Insurance number. You may be required to attend an interview. The DWP will advise you of the appropriate application process and tell you which documents you will need to bring to an interview if one is necessary. You will usually need documents that prove your identity and that you have permission to work in the UK. A National Insurance number does not on its own prove to an employer that you have the right to work in the UK.
You can find out more information about how to apply for a National Insurance number at www.gov.uk.


Side skirt made by Jet Stream that is 2 pieces (side step & rear side diffuser) that provides a nice look and better aerodynamics to the NB (1998-2005) MX-5 Miata. It follows the lines of the vehicle very nicely and will sure turn heads. Please note that the vehicles on the pictures are equipped with Jet Stream Aero Front Fenders, but it will also work with OEM fenders.
Jet Stream Clubman GT Side Steps should be ordered at REV9 Autosport https://rev9autosport.com/jet-stream-clubman-gt-side-steps.html as they provide the best service and speed we've seen so far!


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Q: Google maps API v3 - How are client loads detected? I have a small and low key website what features Google Maps using the v3 Javascript API.
Not that I am expecting to get over 25,000 loads per day, but how does Google detect people loading the map on my site? My site uses the the following code http://maps.google.com/maps/api/js?sensor=false without any API key, and as it is rendered in the clients browser, how does Google relate it to my site?
Is the loads worked out through the http headers/referrers or are the loads based on how many times each client/IP loads the map?
In essence, the code for the map is rendered on my clients/users browsers and thus how do Google know how many people are using the map on my site?
Finally; although I have Google web master tools; is it worth creating & using a API key, or will it just make it possible for Google to track how many people are using the map on my site and thus apply the limit of 25,000?

A: The API sends a request to google which contains the URI of the page that contains the map(when you inspect the network-traffic inside the dev-tools you'll see a request to https://maps.googleapis.com/maps/api/js/QuotaService.RecordEvent ) . This request will be sended when a Maps-instance has been created successfully.
The benefit of using a key: google is able to contact you when there are issues(e.g. may send a notice when you have reached any limits and give you a chance to react/solve the issue before they restrict the API-access for your domain/account).


text:
Black Bears sweep season series against Coshocton
Both Coshocton and River have eyes set on deep playoff run, but River View won Thursdays match up 3-1
Black Bears sweep season series against Coshocton Both Coshocton and River have eyes set on deep playoff run, but River View won Thursdays match up 3-1 Check out this story on coshoctontribune.com: http://ohne.ws/1RLgcyG
Cameron Teague Robinson, Reporter Published 9:06 p.m. ET Oct. 15, 2015
River View's Danielle Muhleman dribbles down the middle of the field, while Coshocton midfielder Skylar Hasseman works back in defense.(Photo: Cameron Teague Robinson)
COSHOCTON — Outside of the bragging rights, Thursday's matchup between the River View and Coshocton girls soccer teams didn't mean much; both teams have top four seeds in their District brackets, and they both have their focus on at least a district final appearance.
That's a feat both can accomplish, but before that run can begin, they took the field for the conclusion of their season series. The series, which River View coach Dave Kridler said the two have split for the last four years, was won by River View after their 3-1 victory Thursday at Kids America.
"It means a lot to them to beat Coshocton twice in one year," Kridler said.
Coshocton coach Craig Hamilton said that despite the loss, he liked what he saw from his team.
"This was a great finish to our season to get ready for the tournament because I don't see anybody being as talented as this River View team for at least the first round," Hamilton said.
In the first half, River View dominated in possession as Coshocton dropped an extra defender in to alleviate the pressure they knew they would have in the middle. That was something Kridler said he and the Black Bears anticipated, but he didn't think they adjusted well.
"We did not react well to what was given to us," Kridler said. "Our finishing decisions were poor. We got impatient. When we did build up, we did fine, but we made some bad calculations in the final third. We just kept them in the game."
The Black Bears did jump out to an early lead, though. With five minutes gone, sophomore Jesse Vandenbark scored. Fifteen minutes later, freshman Lexi Fry capitalized on a deflection in the six-yard box, scoring to make it 2-0 in favor of the Black Bears.
"I talked to our defense. I thought the few mistakes that we make cost us a couple goals," Hamilton said. "Then it's a different game because I really thought we played well today considering they dominated possession."
Later in the first half, a goal by Jensen Hocter, which would have made the score 3-0, was called back because of a handball. That left the score at 2-0 entering the halftime break.
The second half brought more of the same, but Coshocton was able to counterattack more than they did in the first 40 minutes, which led to a goal by Tyra Woods with 22 minutes to go in the game.
That goal kindled the intensity of both teams.
"That shouldn't have to happen," Kridler said of the extra energy that came after Coshocton's goal. "Credit her, we knew what we were dealing with, but she still got in on us. If you don't put away a team when you have the chance and you are sitting on a lead, which is considered the most dangerous lead in soccer because complacency can set in, and if they get the next goal then the momentum swings to them. It was the classic scenario," Kridler said.
But leave it to Vandenbark — who has been on a scoring tear since her three goal game against Coshocton on Sept. 24 — as she scored with 6:58 remaining to seal the win for the Black Bears.
"To have her beat the sweeper on the first touch was crucial," Kridler said. "We were taking a lot of first touches away from the goal, and that time she did the right thing and just muscled it in."
River View held on for the win and will host the winner of Steubenville and Dover at 6:30 Wednesday to begin its playoff run.
"I just told them it's not good enough. It's not good enough to win more than one game next week when we have our sights set on more," Kridler said. "We will come to practice in the cold on Saturday and try to get prepared to be better."
Coshocton has a week off before the team hosts Edison at 4:30 Thursday to start its run.
"This gives me a lot of confidence for these girls. We have a couple injuries, but I think everybody is really playing well," Hamilton said. "I definitely think we are good enough to get to district finals this year and probably meet Rosecrans again."
cteaguerob@gannett.com
Twitter: @cj_teague


Your enrollment in the HealthSelectsm Medicare Rx (PDP) plan is linked to your enrollment in an ERS health plan. ERS has specific rules that tell you when you can change or disenroll from your health plan. Please contact ERS for more information about enrolling or disenrolling in an ERS health plan.
UnitedHealthcare administers the HealthSelect Medicare Rx plan.
If you were enrolled in the HealthSelect Medicare Rx in January 2018, you remained enrolled and automatically transitioned to UnitedHealthcare .
If you do not want to enroll in this plan, you must follow ERS' instructions for opting out of coverage. Instructions will be included in your ERS retirement notice. If you decline coverage for this plan, you will not have any prescription drug coverage through the Texas Employees Group Benefits Program (GBP).
For more information, or to opt-out by phone, call ERS toll free at (866) 399-6908 or go online ers.texas.gov.
What am I enrolled in?
You are enrolled in the HealthSelect Medicare Rx (PDP) plan. To learn more about your plan details, review plan benefits and costs.
We'll review your information and eligibility.
After you're verified, your application will be sent to the Centers for Medicare & Medicaid Services (CMS) for approval. Approval may take up to one week.
Once CMS approves your enrollment, you'll be sent a confirmation letter and your plan member ID card.
Soon after, you'll receive your Member Kit in the mail. It includes details about your specific health plan benefits.
You can attend ERS Fall Enrollment Benefit fairs. You'll learn more about your benefit options and get important updates.
Watch for your Annual Notice of Changes, which is mailed to you every year you're a plan member. It describes your benefits, and any changes to them, for the next calendar year.
For additional questions about your enrollment or the opt-out process, call 1-877-275-4377 or 800-735-2989. TTY users, call 711. Or, contact us.


AgencyAnalytics accepts guest posts from passionate marketers, SEO experts, and agency professionals. Our blog is focused towards marketing consultants and agency owners. We want to help agencies increase productivity, deliver better results to clients and make more money. We are NOT looking for the same old SEO basics (boring rehashed content).
Casual tone, feel free to be funny!
We'd also love to get agency owners on the blog. If you would like to share your experience starting and scaling a marketing agency – please get in touch – I'd like to interview you!
Think you've got what it takes ?
Marketing Director at AgencyAnalytics. Rebecca is based in Fort Collins, CO. When she's not focused on marketing, you'll find her skiing or hiking in the Rockies.


... a collection of discographies of record labels and jazz musicians covering music from the late 1950's through to the 2000's. Each discography list comprises albums released on a specific label or albums that include a particular musician. Track lists and musician details are given for the majority of albums.
The site started as a Grant Green discography in about 2000. Lists for a number of soul jazz musicians were added in 2005 and 2006 and the site was moved to www.organguitardrums.com to reflect the temporary focus on soul jazz and organ trio musicians. Also during this period the first lists of albums released on specific record labels were added. Lists of compilations were added to fill in gaps.
By 2011 many more label lists had been added and the soul jazz focus had become a bit restrictive. The site name changed again - this time to www.jazzlists.com. Many more record label lists have been added since that time.
In 2014 a new series of musicians lists started, focussing initially on pianists. Sections covering selected saxophonists, trumpeters and trombonists have been added during 2014 and 2015. Further label lists have also been added during this period.
Please note that the copyright in any of the LP/CD/cassette covers, LP labels, posters and book covers reproduced in the discography rests with the record/CD-issuing companies, artists or book publishers. They are reproduced here for information only.
Jazzlists.com is a participant in the Amazon Services LLC Associates Program, an affiliate advertising program designed to provide a means for sites to earn advertising fees by advertising and linking to amazon.com.


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News @ UVU
UVU Magazine
UVU to Celebrate Earth Day with Live Discussions on Sustainability
OREM, Utah — This Earth Day, UVU is proving that green is more than just its school color with a special celebration to showcase the university's sustainability efforts. On Wednesday, April 22, 2020, the celebration will include a live Microsoft Teams webinar at 1 p.m. and an Instagram live Q&A at 2 p.m. on the account @sustainability.uvu.
Despite the COVID-19 health and safety precautions that have shut down most of campus, the UVU Sustainability Committee felt that it was important to recognize, even if it is remotely, the ongoing and new campus initiatives for the year.
"With all of the heavy news surrounding the pandemic, it's important that we celebrate things like Earth Day," said Jim Murphy, assistant dean of UVU's College of Science and co-chair of UVU's Sustainability Committee. "UVU continues to be committed to furthering a sustainability community both here on campus and throughout the world."
"By proactively addressing the issue of sustainability, UVU has a great opportunity to demonstrate our core values of exceptional care, accountability, and results," said Genevieve Richards, UVU Sustainability Coordinator. "As we take action to reduce energy consumption and quantify our environmental footprint, UVU becomes more accountable to key stakeholders in areas of fiscal, environmental, and social concern."
There are a wide variety of UVU sustainability projects in the works, many of which started when the main campus was constructed. For example, did you know:
UVU currently offers over 40 sustainability-related courses?
UVU's main campus is built on top of a natural aquifer, giving the campus a geothermal heating and cooling system?
The Facility Complex generates more electricity annually than the building consumes thanks to its 45 kilowatt-per-hour solar array?
The buildings at Capitol Reef Field Station, managed by UVU in partnership with Capitol Reef National Park, use solar chimneys and white roofs instead of air conditioning units to maintain interior temperatures?
With social distancing in place, UVU's students, staff, and faculty are encouraged to incorporate some of the university's sustainability efforts in their own homes.
Richards recommends taking small steps to reduce environmental impact like:
Unplugging electronics when not in use
Adjusting your thermostat
Using reusable bags while shopping
Running only full loads in your dishwasher and washing machine
"Advocate for sustainability in your home, workplace, place of study, and polling station," Richards said. "Discuss the issues with your friends and family. Most people don't talk about sustainability and climate change, and we can't promote change without talking about it. We hope that our Earth Day events can spark that discussion for people, whether they be students, staff, faculty, or community members and leaders."
With all of the heavy news surrounding the pandemic, it's important that we celebrate things like Earth Day.
— UVU assistant dean Jim Murphy
Return to News Home
Follow UVU News
lshumway@uvu.edu


text:
Камаз () насеље је и општина у јужној Француској у региону Миди Пирене, у департману Тарн која припада префектури Кастр.

По подацима из 2011. године у општини је живело 288 становника, а густина насељености је износила 37,5 становника/-{km²}-. Општина се простире на површини од 7,68 -{km²}-. Налази се на средњој надморској висини од 609 метара (максималној 653 -{m}-, а минималној 410 -{m}-).

Демографија

График промене броја становника у току последњих година

Види још
 Списак општина у департману Тарн

Референце

Спољашње везе
 База података: -{Insee}-
 Cammazes на страници Националног географског института Француске
 Cammazes на страници организације -{INSEE}-
 Најближа насеља (километража, правац и координате)
 План насеља Cammazes на мапи (-{Mapquest}-)

Департман Тарн у Француској
Википројект географија/Насеља у Француској

redpajama_set_name: RedPajamaWikipedia


Can Frank Wachowski provide this information? What is Chicago's greatest temperature variation measured on a particular calendar day from one year to the next?
He sure can. Huge temperature variations are part of our meteorological DNA. The Christmas periods in 1982 and 1983 could not have been more different and set the bar for same-day temperature changes in consecutive years. In 1982, driven by a strong El Nino, temperatures soared into the 60s, while in 1983, a roaring Siberian Express sent the mercury plunging far below zero. Wachowski noted that the 83-degree span between the 62-degree high and the low of minus 21 on December 21 is the greatest, closely followed by an 81 degree difference on Christmas Day ranging from a high of 64 to a low of minus 17.


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Q: Validation Symfony2 Entity Choice Field I'm trying to validate a form in a symfony 2.3 project,
So I have a 'Customer' field :
$builder
    ->add('customer',
          'entity',
           array('property'=> 'item',
                 'multiple' => true,
                 'expanded' => true,
                 'class' => 'OrdersBundle:Customer',
                 'required' => true, 'empty_value' => '',
                 'query_builder' => function(\Ella\OrdersBundle\Repository\CustomerRepository $er) {
            return $er->createQueryBuilder('q')->andWhere("q.is_delete = 0")->orderBy('q.item', 'asc');
        }));

I'm trying to return an error when user didn't select anything, so i do this :
properties:
    customer:
        - Choice: { min: 1, minMessage: 'message' }

Or
 properties:
    customer:
        - NotBlank:
            message: message

and other things, but nothing works , an idea of what I'm doing wrong ??
In the doc they say we could use an array, but this doesn't work either ...
Actually Symfony return :

Either "choices" or "callback" must be specified on constraint Choice

A: For the Choice validator you either need to specify an array with the available allowed choices or a callback function, from the docs:

This constraint is used to ensure that the given value is one of a given set of valid choices. It can also be used to validate that each item in an array of items is one of those valid choices.

What you could use may be the Count validator:
customer:
        - Count:
            min: 1
            max: 99
            minMessage: "Min message"
            maxMessage: "You cannot specify more than {{ limit }}"


Progressive Corp. (PGR) didn't just lose a fight with a blogger last week; it also lost customers.
More than 1,000 people on Twitter claimed to have dropped Progressive as their insurer in a four-day span last week, an analysis by social-media tracking firm Crimson Hexagon shows. Another 1,600 or so expressed a desire to not do business with the company, according to the analysis, which was conducted at the request of Dow Jones Newswires.
The dissatisfaction. . . . .


Legends Rocking horses - photos and information on this page for identification and interest.
There are many rocking horse makers who have manufactured rocking horses in recent times including todays market & Legends Rocking Horses deserve a mention.
Their designs are truly exquisite with great attention to detail.
They pride themselves on crafting Victorian & Georgian replica rocking horses as well as Carousels from hardwoods using traditional carving tools & time served tecniques. Bespoke models are their speciality including the Pharlap rocking horse, The Arab horse & the trotting horse... all very individual in design.
Their horses come in a variety of finishes, including traditional dapple grey, a natural realistic dapple & also wood finishes including Cherry wood & Oak.
Reknowned for their beauty and also strength they are often purchased not only for their beauty & design but also usability.
This particular rocking horse crafted by Legends has been given a bespoke finish in a dappled steel grey. He has the usual quality saddlery in a fixed style & sits on a hardwood swingstand. Take note of his detailed muscle carving to his legs and neck.
Here is a close up showing the stunning carving to the head of this Legends rocking horse.
Another angle showing the beautifully carved flared nostrils and kind eye expression on this bespoke Steel dapple grey Legends rocking horse. Also note the neck muscle carving .
Finished with a long flowing mane & tail in horsehair completes the look to this bespoke crafted rocking horse by Legends. this was one that was previously offered for sale & quickly found a new home!
This is another fabulous example of a wooden rocking horse carved by Legends.
This time in a lighter traditional dapple grey with blonde mane & tail.
He is presently for sale at a very reasonable price - click on the photo to be taken to his advert.


Tor and I have been struck down by something fluey this week. It featured lots of coughing.
Now, coughs in themselves have a raison d'etre - they expel mucus and get rid of muck in the lungs. So I don't like medicating them. In case you need further discouragement, commercial cough medicines have been found to possibly cause more harm than good.
The production and disposal of drugs is also deleterious on the environment.
On the other hand, it can really make life easier to have a few remedies, just to soothe throats and calm the spasms. Fortunately the pantry can supply quite a few.
Note: with discretion, these can be used for babies - however, medical advice cautions against giving honey to under-ones. You can use rice malt syrup or sweeten with stevia drops instead. However, real honey is really the best thing for coughs, and even out-performs commercial preparations.
This is really soothing and works to moisten up a dry cough. Slice up a raw onion and a few cloves of good-quality pungent garlic. The stronger the smell, generally the stronger the antibacterial quality. Simmer these on low heat in a cup of milk until onion is soft. Strain, add raw honey, and give a few spoonfuls between meals.
When you have a lot of phlegm coming up, thyme can be a great expectorant. (Thymol, an extract, is one of the active ingredients in the popular Vicks brand chest rub). Brew a generous sprig of thyme (or a half teaspoon dried herb) in a covered cup of boiling water, for ten minutes. Serve with half a teaspoon honey. You can add any leftover tea to baby's bath.
My Japanese 'mother' gave me this time-tested remedy which is well-known in Japan. It's antibacterial and helps break up phlegm. Peel and dice a Japanese 'daikon' radish (the long white kind). Put the pieces in a jar and cover with honey. Keep it in the fridge, shaking daily, at least overnight, and if possible for three days. The juice of the daikon will come out into the honey, making a thin syrup. Strain and give a teaspoon to children when a cough is keeping them up at night. You can use the cubes of daikon as a condiment to curry - sweet and crunchy, delicious!
Turmeric is feted in India for many qualities, and one of them is as an aid for dry and frequent coughing. Toast a pinch of tumeric in a dry skillet, mix with a teaspoon of honey and feed from the spoon, or add a pinch of the spice to warmed milk.
I'll follow this up soon with a recipe for flu soup!


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The 50 MW wind farm began working in January 2019.
"Alternative power engineering, which we have started developing more than three years ago, is still an important industry for us. Wind-power engineering is of particular interest; we have created a full-scale cluster, which includes wind farms, production of components for the wind power industry, and research and academic aspects. We will continue this work. With the new platform, the total amount of electric power received from renewable sources will make 85 MW. The region has at least three more platforms. By developing them, we will be able to increase the volume of generated green energy up to 500 MW", – the Governor Sergey Morozov noted.
The wind farm built by Fortum-RUSNANO Wind Development Investment Fund has 14 wind turbines with the capacity of 3.6 MW each. Local content of the equipment installed at the Ulyanovsk wind farm and confirmed by the Ministry of Industry and Trade of the Russian Federation exceeds 55%. Construction of the second wind farm began last summer, and installation of wind turbines was completed in November.
The first 35 MW wind farm built by Fortum was put into operation in January 2018. Both venues are located near the village Krasnyj Yar, Cherdaklinsky District.
At the same time, the Ulyanovsk region continues development of alternative power engineering. Negotiations are currently under way with a number of companies about construction of new wind and solar farms, as well as equipment for the wind and solar industry.
According to Sergey Vasin, CEO of the Ulyanovsk Region Development Corporation, power engineering will become the new promising sphere for the region. Vestas already has a project here to produce blades for wind generators. Last December, an investment agreement was signed with Green Source for construction of a photovoltaic module plant.
"To make components for the power engineering industry, we will use both enterprises working in the region and competences in the sphere of composite production, as well as learning facilities that we are changing for the needs of the renewable energy sector and power engineering", – Sergey Vasin said.