text:
\section{Introduction}
Neutrino oscillations \cite{MSW, Parkes, KuoPanta, Barger91a} are
considered to be the most likely solution to the longstanding Solar
Neutrino (SN) Problem \cite{Bahcall, Langack94, Langack97}. The
standard solution asserts that neutrinos have non-vanishing masses and
that there is mixing. Many extensions of the Standard Model (SM), such
as Left-Right Symmetric Models (LRSMs) \cite{LRSM} and Supersymmetric
Models without $R$-parity \cite{SUSY}, predict not only neutrino
masses but also New Physics (NP) neutrino interactions that are not
present in the SM.

\sp
The effects of NP on neutrino oscillations have been studied
previously in the literature \cite{Roulet, Guzzo, Barger91b, Fogli,
  KB97}.  In~\cite{Roulet} the effects of flavor changing neutrino
interactions on the Mikheyev-Smirnov-Wolfenstein (MSW) effect
\cite{MSW} were considered and it was demonstrated that, even in the
absence of neutrino mixing in vacuum, neutrino oscillations in matter
can be enhanced by flavor changing neutral currents (FCNCs).
In~\cite{Guzzo} it was shown that additional non-universal flavor
diagonal neutral currents (FDNCs) may allow for resonantly enhanced
neutrino transitions even if neutrinos have vanishing masses. Both
scenarios as well as the case of massive neutrinos with off-diagonal
and new diagonal currents were investigated thoroughly in
Ref.~\cite{Barger91b}. This analysis also determined the regions in
parameter space that gave consistency with the standard solar model
(SSM) and the then available solar neutrino data from the Homestake
\cite{HS} and Kamiokande \cite{KK} experiments.  The implications on
the allowed regions due to the more recent data from the two gallium
detectors, GALLEX \cite{GALLEX} and SAGE \cite{SAGE}, were discussed
in \cite{Fogli} for massive neutrinos and FCNCs (but no FDNCs).  More
recently also the solution to the SN Problem with both FCNCs {\it and}
FDNCs but with massless neutrinos was re-analyzed \cite{KB97}, this
time including the data from all four SN experiment and the latest
improvements to the SSM \cite{BP95}.

\sp
In this work we reconsider the combination of neutrino masses and
mixing with new flavor changing neutrino interactions (but without
significant non-universal FDNCs). We update the previous analyses of
this case by taking into account the most recent data from all four SN
experiments and by using the latest improvements to the SSM. We
present the updated combined allowed regions of the four SN
experiments for different strengths of the NP neutrino couplings. In
particular we include the effects due to the variation of the relative
NP strength that arises when the solar neutrinos scatter off quarks on
their way to the solar surface.  We show that for a certain range of
the NP coupling it is possible to solve the SN problem with
vanishingly small vacuum mixing. Moreover we reveal some interesting
analytic details of the MSW resonant conversion of solar neutrinos in
the presence of FCNCs.

\sp
The paper is structured as follows: In Section~\ref{formalism} we
introduce the formalism of neutrino oscillations with FCNCs. In
Section~\ref{lepFCNC} we explore the effects on the MSW resonant
conversion for purely leptonic NP and use our results in
Section~\ref{lepNPexps} to plot the MSW-contours for the three types
of SN experiments.  From this we obtain the combined allowed regions
for various NP-strengths in this sector.  In Section~\ref{quarkFCNC}
we discuss the new features arising when the neutrinos scatter off
quarks and we present the MSW-contours and the new allowed regions in
Section~\ref{quarkNPexps}.  Finally we conclude in
Section~\ref{conclusions} and discuss briefly how the NP couplings we
require are constrained by SM-forbidden decays.

\section{Formalism}
\label{formalism}

NP interactions may affect the neutrino propagation through matter.
In particular, the resonant conversion of electron neutrinos produced
in the center of sun is modified in the presence of FCNC neutrino
scattering off electrons and nucleons.

\spa%
To a good approximation the equation of motion for two neutrino
flavors $\nu_e$ and $\nu_\ell$ ($\ell=\mu, \tau$) in the presence of
matter induced FCNCs  is given by \cite{Roulet}

\begin{equation}
i\frac{d}{dt} \pmatrix{\nu_e \cr \nu_\ell} =
{\cal{H}}_N \pmatrix{\nu_e \cr \nu_\ell} =
\frac{1}{4E}
\pmatrix{-\Delta \cos2\theta + A & \Delta \sin 2\theta + B \cr
          \Delta \sin2\theta + B & \Delta \cos 2\theta - A \cr}
\pmatrix{\nu_e \cr \nu_x},
\label{eq-of-motion}
\end{equation}

\spa \nid%
where $E$ is the neutrino energy, $\Delta \equiv m^2_2 - m^2_1$ is the
mass-squared difference of the two vacuum mass-eigenstates and
$\theta$ is the vacuum mixing angle. (Note that in the presence of
non-standard neutrino interactions the weak eigenstates are not always
flavor eigenstates \cite{Yuval}.)  $A \equiv 2E \sqrt{2} G_F N_e$ is
the standard induced mass due to $W$-exchange in the reaction $\nu_e
e \to \nu_e e$ and the parameter

\begin{equation}
B \equiv 4E \sqrt{2} (G_N^e N_e + G_N^u N_u + G_N^d N_d)
\end{equation}

\spa \nid%
describes the FCNC contributions from neutrino scattering off
electrons and quarks in the sun. Here $N_f$ denotes the number density of
the fermion type $f$ and $G_N^f$ is the effective four-Fermi coupling
of the reaction $\nu_e f \to \nu_\ell f$. It is convenient to rewrite
this as

\begin{equation}
B  = 4E \sqrt{2} G_F N_e \left[\epsilon_e
          + 2 \epsilon_u + \epsilon_d
          + \left(\epsilon_u + 2\epsilon_d \right) \frac{N_n}{N_e} \right].
\label{Bdef}
\end{equation}

\spa \nid%
We introduced the parameters

\begin{equation}
\epsilon_f \equiv G_N^f / G_F
\end{equation}

\spa \nid%
and used the fact that the quark densities can be expressed in terms
of the neutron density $N_n$ and the electron density $N_e$ which
equals to the proton density $N_p$ for neutral matter like in the sun.

\spa%
In the following section we will first analyze the case where only
$\epsilon_e$ is non-vanishing. This case is the simplest and displays
most of the features we will encounter later when discussing the more
complicated case of FCNCs  from scattering off quarks.

\section{FCNCs  in the Leptonic Sector}
\label{lepFCNC}

Assume that the NP relevant to the neutrino propagation appears only
in the leptonic sector, i.e.  $\epsilon_e \gg
\epsilon_d, \epsilon_u$.  When rewriting the Hamiltonian ${\cal{H}}_N$
in the equation of motion (\ref{eq-of-motion}) for the neutrino
propagation with matter induced FCNCs  as

\begin{equation}
{\cal{H}}_N =
\frac{\Delta_N}{4E}
\pmatrix{-\cos2\theta_N & \sin 2\theta_N \cr
         \sin2\theta_N & \cos 2\theta_N \cr}
\end{equation}

\spa \nid%
we obtain that the effective mixing is given by

\begin{equation}
\cos2\theta_N = \frac{(\Delta \cos2\theta - A)}
  {\sqrt{(\Delta \cos2\theta - A)^2 + (\Delta \sin2\theta + B)^2}}
\label{cos-theta_N}
\end{equation}

\spa \nid%
and the effective mass-squared difference is

\begin{equation}
\Delta_N = \frac{\Delta \sin 2\theta + B}{\sin 2\theta_N}.
\end{equation}

\spa%
For the range of the parameters $\Delta$ and $\theta$ relevant to the
MSW-effect there are typically many oscillations between the neutrino
production and a resonance, and again between the resonance and detection.
Hence the phase information from before and after resonance is easily
lost. In this case one may use the averaged probability for a neutrino
produced in the solar center to be detected as an electron neutrino
which is given by \cite{Parkes, KuoPanta}

\begin{equation}
P_N(\nu_e \to \nu_e) =
 \frac{1}{2} + (\frac{1}{2} - P_c) \cos 2\theta ~\cos 2\theta_N.
\label{Pee}
\end{equation}

\sn
If a neutrino is produced above the resonance ($A_{prod} \ge
A_{res}=\Delta \cos 2\theta$) then level-crossing can occur. This is
accounted for by the crossing probability $P_c$ in (\ref{Pee}) which
is well approximated by~\cite{Petcov, KuoPanta}

\begin{equation}
P_c=\Theta(A_{prod}-A_{res}) \times
    \frac{\exp \left[\pi \gamma_N F(\theta)/ 2 \right]-
          \exp \left[\pi \gamma_N F(\theta)/ 2 \sin^2 2\theta \right]}
         {1 - \exp \left[\pi \gamma_N F(\theta)/ 2 \sin^2 2\theta \right]}.
\label{Pc}
\end{equation}

\spa \nid%
If we assume that the electron density in the sun $N_e \propto
\exp(-r)$ then the parameter $F$ takes the value $F(\theta)=1-\tan^2
\theta$. The adiabaticity parameter $\gamma_N$ in (\ref{Pc}) is
defined as

\begin{eqnarray}
\gamma_N &\equiv& \left|\frac{\Delta_N/4E}{d\theta_N/dx}\right|_{res}
 \nonumber \\
 &=& \left|\frac{(\Delta \sin 2\theta + B_{res})}{4E}
           \frac{2 \Delta (\sin 2\theta + 2\epsilon_e \cos 2\theta)}
                {A_{res} ~(dN_e/dx)/N_e|_{res}} \right| \nonumber \\
 &=&  \gamma |1+2\epsilon_e \cot 2\theta|^2,
\label{gamma_N}
\end{eqnarray}

\spa \nid%
where the standard adiabaticity parameter is $\gamma=\frac{\Delta
  \sin^2 2\theta} {2 E \cos2\theta ~(dN_e/dx)/N_e|_{res}}$.
We used

\begin{eqnarray}
\frac{d{\theta}_N}{dx} &=&
     {\left(\frac{d{\tan 2\theta}_N}{d{\theta}_N}\right)}^{-1}
      \left(\frac{d{\tan 2\theta}_N}{dA}\right)
      \left(\frac{dA}{dx}\right) \nonumber \\
&=& \left(\frac{\cos^2 2\theta_N}{2}\right)
    \left(\Delta \frac{\sin 2\theta +
        2\epsilon_e \cos 2\theta}{(\Delta \cos 2\theta - A)^2}\right)
    \left(\frac{A}{N_e} \frac{dN_e}{dx} \right) \nonumber \\
&=& \frac{1}{2} \frac{\Delta (\sin 2\theta + 2\epsilon_e \cos 2\theta)}
        {(\Delta \cos 2\theta - A)^2 + (\Delta \sin 2\theta + B)^2}
    \left(\frac{A}{N_e} \frac{dN_e}{dx} \right)
\end{eqnarray}

\spa \nid%
and $\Delta_N|_{res} = \Delta \sin 2\theta + B_{res}$.  Note
that for purely leptonic FCNCs  the induced mass at the
resonance $A_{res} = \Delta \cos 2\theta$ is linear to $B_{res} =
2\epsilon_e \Delta \cos 2\theta$.

\spa%
From the expression (\ref{gamma_N}) for $\gamma_N$ one can see that
for $\epsilon_e \ \rlap{\raise 3pt \hbox{$>$}}{\lower 3pt \hbox{$\sim$}}\  \tan 2\theta$ there is a considerable modification
to the standard adiabaticity parameter $\gamma$.  Since the standard
non-adiabatic threshold energy
$E_{NA}=\frac{\pi \Delta \sin^2 2\theta}
             {4 \cos2\theta ~(dN_e/dr)/N_e)|_{res}}$
is proportional to the
adiabaticity parameter it has to be corrected by the same factor
\mbox{$|1+2\epsilon_e \cot2\theta|^2$}:

\begin{equation}
E_{NA}(\epsilon_e)=
\frac{\pi \Delta \sin^2 2\theta \times |1+2\epsilon_e \cot2\theta|^2}
     {4 \cos2\theta ~(dN_e/dr)/N_e)|_{res}}.
\label{E_NA_eps}
\end{equation}

\spa%
We have plotted the survival probability $P_N(\nu_e \to \nu_e)$
of Eq.~(\ref{Pee}) in the $\Delta - \sin^2 2\theta$ plane for a fixed
energy $E$ and different values of $\epsilon_e$. (See
Fig.~\ref{NP-monop} for positive and Fig.~\ref{NP-monom} for negative
$\epsilon_e$, the shading indicates the value of $P_N$: White
corresponds to $0.9 \le P_N \le 1.0$ and the darkest area
corresponds to $0.0 \le P_N \le 0.1$.) For $|\epsilon_e|$ as
small as $0.001$ the effects of NP are minor (compared to any standard
MSW-plot).  However already for $|\epsilon_e| = 0.01$ the triangular
shape is distorted and the originally diagonal band appears bent and
-- most striking -- has a ``gap" for negative $\epsilon_e$.  For even
larger $|\epsilon_e|$ these features remain, only the gap moves
towards larger $\sin^2 2\theta$. Our goal is to understand why these
changes arise.

\spa%
Note that for a given $E_{NA}$ and small vacuum mixing angle we have
\mbox{$\Delta \propto 1/|\sin 2\theta + 2\epsilon_e \cos 2\theta|^2$}.
For $\epsilon_e = 0$ this yields the diagonal contours in a
double-logarithmic plot in the $\Delta - \sin^2 2\theta$ plane
known as the non-adiabatic band.  However for non-vanishing
$\epsilon_e$ these contours are not diagonal, since $\Delta$ is not
proportional to $\sin^2 2\theta$ anymore. For $\epsilon_e > 0$ the
contours are below the original diagonals and approach a constant
for $\sin^2 2\theta \to 0$. For $\epsilon_e < 0$ the behavior of the
non-adiabatic band is more complicated. For large mixing the new
contours are above the standard diagonal and diverge at

\begin{equation}
\tan 2\theta_{div} = -2\epsilon_e,
\label{tan_div}
\end{equation}

\spa \nid%
where the correction-factor $|1+2\epsilon_e \cot2\theta|^2$ vanishes and
hence also $E_{NA}(\epsilon_e) = \gamma_N = 0$. This implies that --
independently of $\Delta$ -- almost all the electron neutrinos
which were produced above the resonance mainly as the heavier
mass eigenstate  will ``cross over" at the resonance to the lighter mass
eigenstate and therefore leave the sun as electron neutrinos. Hence the
survival probability is very large, which explains why the contours
split at $\sin^2 2\theta_{div}$. Due to the absolute value in
Eq.~(\ref{E_NA_eps}), the contours are symmetric in the region
around $\sin^2 2\theta_{div}$. For very small vacuum mixing $\sin^2
2\theta \ll \sin^2 2\theta_{div}$ the contours approach the same
constant values as in the case of positive $\epsilon_e$.

\sp
To understand how the contours split it is instructive to display
the survival probability (\ref{Pee}) as a function of the energy $E$
for fixed $\sin^2 2 \theta$ and $\Delta$ as shown in
Fig.~\ref{NP-probs}. The solid curves show $P_N(E)$ for some negative
$\epsilon_e$, while the dashed curves indicate $P_N(E)$ for
$\epsilon_e = 0$. Note that when $\epsilon_e$ approaches the value
where $\sin^2 2\theta \simeq \sin^2 2\theta_{div}$, the ``valley"
disappears -- due to the decrease of the non-adiabatic threshold
$E_{NA}(\epsilon_e)$ -- and hence almost all electron neutrinos
survive. Also note that the left side of the valley corresponding to
the adiabatic threshold is almost unaffected by NP interactions. Thus
the adiabatic (horizontal) solution is not shifted.  Moreover if
the vacuum mixing is large ($\sin^2 2\theta \approx \tan^2 2\theta \gg
\epsilon_e$) then the NP correction factor becomes negligible
($|1+2\epsilon_e \cot2\theta|^2 \simeq 1$) with the result that the
large-angle solution is inert to NP.

\section{Solar Neutrino Experiments and $\nu_e-e$ FCNCs }
\label{lepNPexps}
Once we have found the new survival probability $P_N(E)$ [see
(\ref{Pee})], it is straightforward to predict the effects of NP on
the MSW-plots for the three kinds of SN experiments in the presence of
NP.  In order to obtain the suppression rate $\rho$ at any point in the
$\Delta - \sin^2 2\theta$ plane the survival probability $P_N(E)$ has
to be convoluted with the neutrino energy spectrum times the
sensitivity of each experiment. (For all plots we use the SSM predictions
of Ref.~\cite{BP95} (including Helium and heavy metal fusion)
and the experimental results as summarized in Table~I of
Ref.~\cite{Langack97}. We neglect day-night effects \cite{daynight}.)
Fig.~\ref{NP_all_e} shows the contours for
$\epsilon_e = \pm 0.05$ for Kamiokande, Homestake and the Gallium
experiments, respectively. The plots exhibit basically the same
behavior as those we showed for a discrete energy (Fig.~\ref{NP-monop}
and Fig.~\ref{NP-monom}). The only difference is the distortion
produced by the energy spectrum, as known from the standard
MSW-effect.

\spa%
Finally we have plotted the allowed regions determined by the ratio $\rho$
between the expected and measured neutrino fluxes for the three types
of SN experiments. We present the individual 95\% C.L. contours (dotted for
the combined gallium experiments, dashed for the Homestake and solid for the
Kamiokande experiment) together with the {\it combined} allowed regions
(shaded) for positive and negative $\epsilon_e$ in Fig.~\ref{AR_NP_pe} and
Fig.~\ref{AR_NP_me}, respectively. For very small $\epsilon_e = \pm 0.001$
and $\epsilon_e = \pm 0.01$ the small-angle solution appears a little
shifted, but it does {\it not} disappear.  Note that the NP neutrino
interactions do not change the allowed value for the mass difference, which
is fixed at $\Delta \approx 10^{-5} \rm eV^2$ due to the adiabatic solution
of the Gallium experiments.  For larger values $\epsilon_e = \pm 0.05$
and $\epsilon_e = \pm 0.1$ the effects are more dramatic.  One can see
that for $\epsilon_e = \pm 0.05$ the combined allowed regions include
{\it all} vacuum mixing angles for which $\sin^2 2\theta \ \rlap{\raise 3pt \hbox{$<$}}{\lower 3pt \hbox{$\sim$}}\  3
\times 10^{-4}$. This means in particular that in the presence of NP
interactions there may be a solution to the SN problem with
vanishingly small vacuum mixing.  Moreover for $\epsilon_e = -0.05$
there appears a second solution at $\sin^2 2\theta \simeq 3 \times
10^{-2}$, which is due to the gap for negative $\epsilon_e$.  Finally
for $\epsilon_e = +0.1$ there is {\it no} overlap of the small-angle
allowed regions, while for $\epsilon_e = -0.1$ there are two solutions
at $\sin^2 2\theta \simeq 10^{-2}$ and $\sin^2 2\theta \simeq 7 \times
10^{-2}$ on both sides of the gap. Moreover -- as we expected -- the
large-angle solution ($\sin^2 2\theta \simeq 0.6-1.0$ and $\Delta
\simeq 3 \times 10^{-6}-10^{-4}~{\rm eV}^2$) is inert to NP for all
$\epsilon_e$.

\section{FCNCs  in the Quark Sector}
\label{quarkFCNC}

So far we have restricted our discussion to the case of purely
leptonic interactions. However electron neutrinos which have been
produced in the core of the sun may as well scatter off protons and
neutrons when propagating to the solar surface. Without NP
interactions this only gives rise to additional weak neutral currents
via $Z$-exchange which do not alter the resonant conversion. But in
the presence of NP there can be FDNCs and FCNCs which may affect the
neutrino propagation. We only consider flavor changing neutrino
interactions which correspond to non-vanishing $\epsilon_u$ and/or
$\epsilon_d$ in~(\ref{Bdef}). In this case a new parameter, the ratio $R
\equiv N_n/N_p$ plays a role. If $R$ were constant, we would only need to
replace $\epsilon_e$ of Section~\ref{lepFCNC} by

\begin{equation}
\epsilon(R) = \epsilon_e + 2 \epsilon_u + \epsilon_d +
(\epsilon_u + 2\epsilon_d)~R
\label{eps_R}
\end{equation}

\spa \nid%
and could then use all the results we obtained so far.  However $R$ is
in fact {\it not}\/ a constant, but changes from a value of about
$0.48$ at the center of the sun to $0.16$ at its surface according to
the SSM predictions~\cite{Bahcall}. Taking into
account that $^4$He is four times heavier than $^1$H and neglecting
the contributions from heavier elements, whose abundances are much
smaller, we obtain that

\begin{equation}
R \simeq \frac{X(^4{\rm He})}{2X(^1{\rm H})+X(^4{\rm He})}.
\end{equation}

\spa \nid%
The isotopic abundances $X(^1$H) and $X(^4$He), the ratio $R$ and the
electron density $N_e$ are shown as functions of the distance to the
solar center $d_c$ (in units of the solar radius) in
Fig.~\ref{sun_data}.  In the following we discuss the subtleties that
arise due to the fact that $R$ is a function of the distance to the
solar center.

\spa%
In order to find the adiabaticity parameter $\gamma_N$ [see
Eq.~(\ref{gamma_N})] we have to calculate

\begin{equation}
\frac{d{\theta}_N}{dx} =
     {\left(\frac{d{\tan 2\theta}_N}{d{\theta}_N}\right)}^{-1}
      \left(\frac{d{\tan 2\theta}_N}{dx}\right).
\end{equation}

\spa \nid%
Taking the derivative with respect to $x$ (henceforth denoted by a
prime) we find that

\begin{eqnarray}
\frac{d{\tan 2\theta}_N}{dx}
&=&  \frac{d}{dx} \left(\frac{\Delta \sin 2\theta + B}
                             {\Delta \cos 2\theta - A} \right) \nonumber \\
&=&  \frac{B'(\Delta \cos 2\theta -A) - (\Delta \sin 2\theta + B)(-A')}
                  {(\Delta \cos 2\theta - A)^2}.
\end{eqnarray}

\spa \nid%
Computing

\begin{eqnarray}
B' &=& 4E \sqrt{2} G_F N_e' \left[\epsilon_e
     + 2 \epsilon_u + \epsilon_d
     + \left(\epsilon_u + 2\epsilon_d \right) R(x) \right] + \nonumber \\
   &~& 4E \sqrt{2} G_F N_e  \left[ \left(\epsilon_u + 2\epsilon_d \right)
            R'(x) \right]
\label{B-prime}
\end{eqnarray}

\spa \nid%
one can see that {\it a priori} $B'$ is not proportional to $A'$ as in
the case of purely leptonic NP, due to its dependence on $R(x)$.
But to a very good approximation the second term in
(\ref{B-prime}) can be neglected, since the change of the ratio $R$
between neutron and proton density is much smaller than the change of the
electron density, i.e. $R'(x) \ll N_e'/N_e$ (see Fig.~\ref{sun_data}). Then
$B'$ does not depend on $N_e$, but only on $N_e'$ (like $A'$) and we obtain
that

\begin{equation}
B=2 \epsilon(R) A \hspace{1.4cm} \mbox{and} \hspace{1.4cm} B'=2 \epsilon(R) A',
\end{equation}

\spa \nid%
where $\epsilon(R)$ is defined in Eq.~(\ref{eps_R}). Hence we have
recovered the same formal relation between the parameters $A$ and $B$
as in the case of purely leptonic NP, only that now the proportionality
factor depends on the distance $x$ traveled by the neutrino. For the
adiabaticity parameter $\gamma_N$, which is defined at the resonance,
this implies that we can take over our previous result
(\ref{gamma_N}) (since now $B' A=B A'$) provided that we replace
$\epsilon_e$ by $\epsilon(R_{res})$:

\begin{equation}
\gamma_N(R) = \gamma |1+2\epsilon(R_{res}) \cot 2\theta|^2
\end{equation}

\sn
The position of the resonance for a neutrino produced in the center of
the sun depends on its energy. We have to compute $R_{res}$ as a
function of the critical density which is given by

\begin{equation}
N_e^{crit}=\frac{\Delta \cos 2\theta}{2\sqrt{2} G_F (E_\nu)_{prod}}.
\label{Nc_E}
\end{equation}

\spa \nid%
Thus the new adiabaticity parameter $\gamma_N(R)$ introduces an
additional energy dependence which is however not large since $R <
\frac{1}{2}$. Fig.~\ref{R_Ne} shows $R$ as a function of the electron
density $N_e$.  The dashed curve is a fit to the data points from
Ref.~\cite{Bahcall} by a parabola

\begin{equation}
R(y) \simeq 0.1624 - 0.0851 y + 0.4227 y^2,
\label{R_y}
\end{equation}

\spa \nid%
where $y \equiv N_e/(100 N_A)$ and $N_A = 6.023 \times 10^{23}$ is the
Avogadro number.

\spa%
The effects of NP neutrino interactions enter the survival probability
$P_N(E)$ [see (\ref{Pee})] via the crossing probability $P_c$ [through
$\gamma_N(R)$] and via the matter mixing $\cos 2\theta_N$ [see
(\ref{cos-theta_N})]. For $P_c$ we have to calculate $B$ (and
therefore $R$) at the resonance which gives rise to the additional
energy dependence as discussed above. The factor $\cos 2\theta_N$ in
(\ref{Pee}) has to be taken at the production point of the neutrino.
For the intermediate and high-energy neutrinos, which are mainly produced
close to the solar center, we have $R_{prod} \simeq 0.4-0.5$. Only for
the low-energy neutrinos, a substantial fraction
is produced with $R_{prod} < 0.4$.

\spa%
To summarize: To a good approximation all FCNC-effects due to quarks
on the neutrino propagation may be accounted for by replacing
$\epsilon_e$ with $\epsilon(R_{res})$ in the crossing probability
$P_c$ and with $\epsilon(R_{prod})$ in $\cos 2\theta_N$. The change in
$P_c$ introduces a further energy dependence which is due to the fact
that $R_{res}$ depends on the neutrino production energy.

\section{Solar Neutrino Experiment and FCNCs  in the Quark Sector}
\label{quarkNPexps}

In this section we present the MSW-contours and the combined allowed
regions for the three types of solar neutrino experiments in the
presence of FCNCs  in the quark sector. We have used the same
method as described previously, only that now we have included the
necessary corrections due to the energy dependence of the ratio
$R=N_n/N_p$. We have investigated the three cases of having

\begin{itemize}
\item{only $\nu-u$ FCNC $(\varepsilon \equiv \epsilon_u \ne
    \epsilon_d = 0) \Longrightarrow \epsilon(R)=\varepsilon (2 + R)$}
\item{only $\nu-d$ FCNC $(\varepsilon \equiv \epsilon_d \ne \epsilon_u
    = 0) \Longrightarrow \epsilon(R)=\varepsilon (1 + 2R)$}
\item{both $\nu-u$ FCNC and $\nu-d$ FCNC $(\varepsilon \equiv
    \epsilon_d = \epsilon_u \ne 0) \Longrightarrow \epsilon(R)=3\varepsilon (1 +
    R)$.}
\end{itemize}

\spa \nid%
As an example for the MSW-contours we show in Fig.~\ref{NP_all_u},
Fig.~\ref{NP_all_d} and Fig.~\ref{NP_all_b} our results for the three
types of solar neutrino experiments with $\epsilon_u = \pm 0.05$,
$\epsilon_d = \pm 0.05$ and $\epsilon_u = \epsilon_d = \pm 0.05$,
respectively.  Comparing with the contours for
$\epsilon_e$ (see Fig.~\ref{NP_all_e}) one can see that for positive
$\varepsilon$ the changes are minor, while for negative $\varepsilon$
the region where the contours are split (at $\theta_{div}$) is
somewhat tilted.  This results from the fact that the effective
$\epsilon(R)$ of Eq.~(\ref{eps_R}) is energy dependent.  Thus the
position of the gap $\sin \theta_{div}$ is not fixed, but varies as a
function of $\Delta$. Since $N_e^{crit} \propto \Delta$, for larger
$\Delta$ also $R(N_e^{crit})$ is larger [see Eqs.~(\ref{Nc_E})
and~(\ref{R_y})]. This slightly increases $\sin \theta_{div}$
[according to (\ref{tan_div}) with $\epsilon_e$ replaced by
$\epsilon(R)$] when $\Delta$ takes larger values.  This effect is most
pronounced for $\varepsilon \equiv \epsilon_d$ (see
Fig.~\ref{NP_all_d}), since in this case the relative change
in $\epsilon(R)=\epsilon_d(1+2R)$ due to $R$ is most significant.

\spa%
As the changes in the contours due to the energy dependence of
$\epsilon(R)$ are small also the combined allowed regions for the
three cases of FCNCs  in the quark sector do not differ significantly
from the results we obtained in the case of having only $\nu-e$ FCNC.
The individual and combined allowed regions at 95\% C.L. are shown
in Fig.~\ref{AR_NP_mu}, Fig.~\ref{AR_NP_md} and Fig.~\ref{AR_NP_mb} for
some negative $\varepsilon$. Again we have the interesting phenomena
that for a certain $\varepsilon$ there exist solutions to the SN
Problem with vanishingly small vacuum mixing. This occurs for
$\epsilon_u=\pm 0.02$, $\epsilon_d=\pm 0.03$ and
$\epsilon_u=\epsilon_d=\pm 0.01$, respectively. (For positive
$\varepsilon$ the qualitative behavior of the contours is similar to
that of $\epsilon_e > 0$ as shown in Fig.~\ref{AR_NP_pe}. For very
small $\sin^2 2\theta$ the contours coincide with those of negative
$\varepsilon$.) Note that for $\varepsilon \equiv
\epsilon_u=\epsilon_d=-0.1$ the effective $\epsilon(R) \simeq
0.35-0.45$ is so large that also the large angle solution is affected.

\section{Conclusions and Discussion}
\label{conclusions}

We have studied the effects of FCNCs  on the resonant conversion of
solar neutrinos. Our main results are presented in
Fig.~\ref{AR_NP_pe}, Fig.~\ref{AR_NP_me}, Fig.~\ref{AR_NP_mu},
Fig.~\ref{AR_NP_md} and Fig.~\ref{AR_NP_mb}. We learn that the changes
to the MSW-solution could be dramatic for a NP coupling strength $G_N
\ \rlap{\raise 3pt \hbox{$>$}}{\lower 3pt \hbox{$\sim$}}\  10^{-2} G_F$, in particular if the sign of $G_N$ is negative.

\spa%
There remains a question of whether couplings in the relevant range
can arise in explicit models of NP. Left-Right symmetric models
\cite{LRSM} and supersymmetric models without $R$-parity \cite{SUSY}
give rise to the purely leptonic flavor changing neutrino scattering
$\nu_e e \to \nu_\ell e$ ($\ell=\mu, \tau$).  However
model-independently these reactions are related by $SU(2)_L$-rotations
to the SM-forbidden decays $\ell^\pm \to e^\pm e^\pm e^\mp$.  The
experimental bounds on the branching ratios (BR) of these reactions
\cite{PDG} (BR$(\mu \to 3e) < 10^{-12}$ and BR$(\tau \to 3e) < 3.3
\times 10^{-6}$) imply that $\epsilon_e \ \rlap{\raise 3pt \hbox{$<$}}{\lower 3pt \hbox{$\sim$}}\  10^{-6}$ for $\ell=\mu$
and $\epsilon_e \ \rlap{\raise 3pt \hbox{$<$}}{\lower 3pt \hbox{$\sim$}}\  10^{-3}$ for $\ell=\tau$.  Since we found in
Section~\ref{lepNPexps} that for $\epsilon_e \ \rlap{\raise 3pt \hbox{$<$}}{\lower 3pt \hbox{$\sim$}}\  10^{-3}$ the
modifications to the MSW-contours are very small (see
Fig.~\ref{AR_NP_pe} and Fig.~\ref{AR_NP_me}), we conclude that the
purely leptonic FCNC effects on the MSW-mechanism (in particular for
$\ell=\mu$) are not likely to be significant for solar neutrinos.

\spa%
For the semi-hadronic neutrino scattering $\nu_e q \to \nu_\ell q$ the
$\nu_e \to \nu_\mu$ transitions are severely constrained by the
decay $\mu \to e \gamma$.  The experimental bound \cite{PDG}, BR$(\mu
\to e \gamma) < 4.9 \times 10^{-11}$, implies $\epsilon_q \ \rlap{\raise 3pt \hbox{$<$}}{\lower 3pt \hbox{$\sim$}}\
10^{-6}$ ruling out significant changes to the MSW-solution. However
for $\nu_e \to \nu_\tau$ oscillations the most stringent bound comes
from BR$(\tau \to \rho^0 e) < 4.2 \times 10^{-6}$, which is much
weaker and gives $\epsilon_q \ \rlap{\raise 3pt \hbox{$<$}}{\lower 3pt \hbox{$\sim$}}\  10^{-2}$.  We note that a relaxation
to our estimated bounds on $\epsilon_f$ could be achieved by $SU(2)_L$
breaking effects. However, since we consider NP at or above the
electro-weak scale, the effective four-Fermi couplings related to
$\nu_e f \to \nu_\ell f$ and $\ell \to f \bar{f} e$ differ at most by a
factor of a few.

\spa%
We conclude that for $\nu_e q \to \nu_\tau q$, the strength of the
coupling in NP models could be in the range where it gives interesting
effects for solar neutrinos. Supersymmetry without $R$-parity is an
example of a model where such a coupling (for $q=d$) exists. In view
of the interesting results presented in Ref.~\cite{KB97} and in this
work, a detailed analysis of the bounds on flavor changing and new
flavor diagonal neutrino interactions in such models is called for.

\spa%
\spa%
\begin{center}
\bf Acknowledgments
\end{center}

\spa \nid%
I am indebted to Y. Nir and Y. Grossman for many useful discussions
and valuable comments on the manuscript. I also thank E. Nardi for his
comments and J.N. Bahcall for useful communications.

\spa%
\spa%

redpajama_set_name: RedPajamaArXiv


Explore the healing going on in Indian country.
There is pain in these stories and there is loss. There is death, but there is also rebirth, and there is always the search from each of the narrators for personal truth. Readers will recognize Larry Sole from "The Lesser Blessed" in his story "How I Saved Christmas", but there are new voices here, new secrets, from new characters in communities across the north and the south, yet they are all linked by themes of hope, the spirit of friendship, and hunger.


text:
Triple win for Hayfield: Crowned Housebuilder of the Year 2021
Press release: 22.11.2021
A young West Midlands based housebuilder has reached the pinnacle of British housebuilding, taking home the industry's biggest prize – the title of Housebuilder of the Year 2021 – alongside Gold in the Best Medium Housebuilder category and Gold in the Best Public Realm category at The WhatHouse? Awards.
Hayfield's enterprising story is one of swift growth. It was only two years ago that the Solihull business success story won gold in the Best Small Housebuilder category of the WhatHouse? Awards. Now, at just five years old, Hayfield has succeeded in out doing far bigger national competitors to take home the ultimate crown.
Triple winner Hayfield will deliver more than 300 homes across its Middle England heartland of Oxfordshire, Bedfordshire, Cambridgeshire, Buckinghamshire and Wiltshire this year, representing over £100m turnover, and has contributed over £10m to local schools, sports clubs and charities through planning contributions, as well as further charitable donations. The award-winning builder is a green champion for the region, with the first 'Green Revolution' scheme including air source heat pumps, underfloor heating, EV charging points and ultra-fast broadband in a development of 101 eco-homes, and the creation of new native woodlands and wildflower meadows aplenty.
Mark Booth, co-founder and chair of Hayfield, said: "I am so delighted with how far Hayfield has come in five years. This business is all about the strength of its people and I could not be any prouder of how all the team has risen to the daily challenge of delivering outstanding, multi-award-winning homes. We have progressed so much in the past 12 months in particular and are as excited about the future as we have ever been."
The judges said: "Hayfield, based in Solihull, West Midlands, brims with enterprise and integrity, handpicking sites and handcrafting homes, while looking through consumers' eyes, always knowledgeable about its markets and the land opportunities, choosing the right locations to mould their new communities with deference to the heritage and sensitive to the local environment. 'We take what's good and make it great' is a mantra and a worthy one. It is a rare to see such a young housebuilder evolve such a distinctive brand so swiftly, shaking up its bigger competitors. Young of building age, but with bags of industry experience with the senior management team having previously worked together at Banner Homes. The trust in the people and the processes is clear to see, while onboarding new talent to fuse onto the experience and in training and nurturing staff."
The Whathouse? Awards - dubbed the Oscars of the housebuilding industry – showcases and celebrates the brightest stars in the housing sector, honouring those who build Britain's best homes. Now in their 41st year, the glittering ceremony took place at London's JW Marriott Grosvenor House Hotel, where the winners of the 21 categories were announced.
The complete Judges Report can be viewed here
About WhatHouse?
Whathouse.com is the UK's leading new home audience platform. For more than 30 years' its aim has been to inspire UK homebuyer decisions around new property. With a comprehensive directory of over 7,000 new homes, from the UK's most celebrated housebuilders, WhatHouse? makes it easy for buyers to consider the diverse range of property developments available and to find their perfect new home match.
The annual WhatHouse? Awards have been running for 41 years. Dubbed 'the Oscars of the housebuilding industry', the awards are the biggest accolades in British housebuilding and sponsored by the leading names in the new build supply chain.
Contact our press team:
WhatHouse? Online Press Centre
Call Jill Willis: 07855 409970
Contact our press team
Call Jill on: 07855 409970
Images >
New Homes Index >
WhatHouse? Facts
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New Homes Help to Buy Part Buy/Rent Retirement

redpajama_set_name: RedPajamaCommonCrawl


In Valley Stairs, the Commonwealth Court addressed the issue of the date a claimant's workers' compensation benefits become payable, under Section 406.1(d)(6) of the Workers' Compensation Act in connection with an employer's issuance of a Notice Stopping Temporary Compensation Payable (NSTCP), followed by a Notice of Denial (NCD).
The claimant in Valley Stairs alleged a date of injury of Friday, March 27, 2015. Claimant discontinued work on March 27, 2015 and reported to the hospital for his alleged injuries. On April 12, 2015, employer issued a Notice of Temporary Compensation Payable (NTCP), indicating the March 27, 2015 date of injury and that the 90-day period under Section 406.1(d)(6) of the Pennsylvania Workers' Compensation Act (Act) ran from Monday, March 30, 2015. On June 28, 2015, employer filed a NSTCP and a NCD. The Bureau issued a Notice of Conversation of Temporary Compensation Payable. Claimant then filed a Penalty Petition, alleging that the employer violated the Act by stopping payment of compensation benefits after the NTCP had converted.
The Workers' Compensation Judge found that even though claimant's injury caused him go out of work on Friday, March 27, 2015, because claimant received his full pay on that date, claimant's disability commenced on Monday, March 30, 2015, the day he began receiving indemnity benefits pursuant to the NTCP. The WCJ concluded that the employer's NSTCP was filed within 90 days of claimant's disability and that the conversion issued by the Bureau was void. Therefore, the WCJ concluded that claimant did not establish that employer violated the Act to warrant an award of penalties.
Claimant appealed to the Workers' Compensation Appeal Board (WCAB), arguing the WCJ erred in determining that claimant's first date of disability was March 30, 2015, because the injury caused his disability on Friday, March 27, 2015 and, therefore, the NTCP conversion was appropriate as the NSTCP and NCD were not filed within 90 days of March 27, 2015. The WCAB reversed the WCJ's Decision based the Commonwealth Court's holding in Galizia v. WCAB (Woodloch Pines, Inc.), 933 A.2d 146 (Cmwlth. Ct. 2007), which stated "the date of the 90[-]day period begins on is [sic] the first date that Claimant was entitled to receive disability benefits as a result of the work injury." Therefore, claimant was eligible for benefits as of March 27, 2015 and the 90-day period expired on June 25, 2015. Because the employer did not issue a NSTCP prior to that time the NTCP property converted. The WCAB remanded the matter to the WCJ for an appropriate penalty amount.
In applying this regulation, the Commonwealth Court reasoned that Friday, March 27, 2015 was the first day claimant suffered a loss of earning power because on that date, claimant was injured, transported to the hospital and did not return to work; however, because claimant received his full wages on March 27, 2015, the first day of the NTCP 90-day period began the following work day, which was Monday, March 30, 2015 as was indicated on the NTCP.
In Valley Stairs, the Commonwealth addressed an alleged violation of the Pennsylvania Workers' Compensation Act, pertaining to the issuance of a NTCP, which provides defendants with an avenue to temporarily accept a claim for a period of up to ninety (90) days, for further investigation of the claim to determine the existence of defenses. The case is also a good reminder to defendants of the requirements surrounding the duration of the temporary period, to ensure timely stopping if a defense is available. Counsel for claimants have been increasingly challenging the issuance of NTCPs for various reasons and, interestingly, are resorting to the filing of Penalty Petitions in lieu of a Claim Petition, which would otherwise put the burden of proof on claimant that he or she was disabled from a work-related injury during the temporary period or beyond.


text:
Apachai Hopachai
アパチャイ・ホパチャイ
Apachai is known as the Muay Thai "Shinigami" and Muay Thai master at the Ryozanpaku. He is also shown to have been trained in Muay Boran, though practices it at night only for the sake of upholding the traditional of the fighting style, and even tries not to show it to Kenichi to protect him because it is very dangerous.
Despite his lethal skills, Apachai has a very childlike nature, which is why he is good with kids and animals (he also happens to have the unique ability to communicate with animals). However, when it comes to fighting, Apachai lacks the ability to hold back, and often nearly kills Kenichi (one incident from chapter 24, Kenichi had to be revived with CPR due to cardiac arrest from an attack by Apachai). The reason for this is because Apachai has been fighting life or death battles in the ring since he was very young, therefore striking with deadly force has become a reflex for him. Since he was saddened by the fact that Kenichi was scared to train with him, he eventually learns how to hold back his strength, though he still sometimes knocks out Kenichi when he enters his fighting mode.
Apachai is shown to have looked up to Agaard Jum Sai as an older brother. He has also mentioned several times that he has trouble understanding Japanese which may be another reason why he never holds back despite how much everyone tells him to, though this may extend to languages in general when he is told by Agaard to hold back or that he has not seen the terrifying effects of it until he started to teach Kenichi.
When Apachai talks he frequently says "Apa," sometimes even yelling out "Apapapapa" whilst fighting or training. He also answers the phone with a "We have your child hostage." rather than a normal "Hello," presumably because of his past in working with child traffickers.
Apachai is also a big eater, especially of hamburgers, voraciously gulping down large amounts of food and will occasionally steal some from Sakaki. This stems from his past when he had his dinner taken away by his boss whenever he broke his training equipment.
Shijou Saikyou no Deshi Kenichi OVA
Shijou Saikyou no Deshi Kenichi Specials
Ranking: View
First appearance: Battle 7
Type: Dou
Type: Katsujin Ken
Martial Arts: Muay Thai and Muay Boran
MALAPI


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text:
// Provides control sap.m.ColumnListItem.
sap.ui.define([
	"sap/ui/core/Element",
	"sap/ui/core/library",
	"./library",
	"./ListItemBase",
	"./ColumnListItemRenderer",
	"sap/ui/thirdparty/jquery",
	// jQuery custom selectors ":sapFocusable", ":sapTabbable"
	"sap/ui/dom/jquery/Selectors"
],
	function(Element, coreLibrary, library, ListItemBase, ColumnListItemRenderer, jQuery) {
	"use strict";

	// shortcut for sap.m.ListType
	var ListItemType = library.ListType;

	// shortcut for sap.ui.core.VerticalAlign
	var VerticalAlign = coreLibrary.VerticalAlign;

	/**
	 * Constructor for a new ColumnListItem.
	 *
	 * @param {string} [sId] Id for the new control, generated automatically if no id is given
	 * @param {object} [mSettings] Initial settings for the new control
	 *
	 * @class
	 * sap.m.ColumnListItem can be used with the cells aggregation to create rows for the sap.m.Table control.
	 * The columns aggregation of the sap.m.Table should match with the cells aggregation.
	 *
	 * Note: This control should only be used within the sap.m.Table control.
	 * The inherited counter property of sap.m.ListItemBase is not supported.
	 *
	 * @extends sap.m.ListItemBase
	 *
	 * @author SAP SE
	 * @version ${version}
	 *
	 * @constructor
	 * @public
	 * @since 1.12
	 * @alias sap.m.ColumnListItem
	 */
	var ColumnListItem = ListItemBase.extend("sap.m.ColumnListItem", /** @lends sap.m.ColumnListItem.prototype */ {
		metadata : {

			library : "sap.m",
			properties : {

				/**
				 * Sets the vertical alignment of all the cells within the table row (including selection and navigation).
				 * Note: vAlign property of sap.m.Column overrides the property for cell vertical alignment if both are set.
				 * @since 1.20
				 */
				vAlign : {type : "sap.ui.core.VerticalAlign", group : "Appearance", defaultValue : VerticalAlign.Inherit}
			},
			defaultAggregation : "cells",
			aggregations : {

				/**
				 * Every control inside the cells aggregation defines one cell of the row.
				 * Note: The order of the cells aggregation must match the order of the columns aggregation of sap.m.Table.
				 */
				cells : {type : "sap.ui.core.Control", multiple : true, singularName : "cell", bindable : "bindable"}
			}
		},

		renderer: ColumnListItemRenderer
	});

	/**
	 * TablePopin element that handles own events.
	 */
	var TablePopin = Element.extend("sap.m.TablePopin", {
		ontap: function(oEvent) {
			// prevent the tap event if selection is done within the popin control and mark the event
			if (oEvent.isMarked() || ListItemBase.detectTextSelection(this.getDomRef())) {
				return oEvent.stopImmediatePropagation(true);
			}

			// focus to the main row if there is nothing to focus in the popin
			if (oEvent.srcControl === this || !jQuery(oEvent.target).is(":sapFocusable")) {
				this.getParent().focus();
			}
		}
	});

	// defines tag name
	ColumnListItem.prototype.TagName = "tr";

	ColumnListItem.prototype.init = function() {
		ListItemBase.prototype.init.call(this);
		this._bNeedsTypeColumn = false;
		this._aClonedHeaders = [];
	};

	ColumnListItem.prototype.onBeforeRendering = function() {
		ListItemBase.prototype.onBeforeRendering.call(this);
		if (this._oPopin && this._oDomRef) {
			this.$Popin().off();
		}
	};

	ColumnListItem.prototype.onAfterRendering = function() {
		if (this._oPopin && this.isActionable(true)) {
			this.$Popin().on("mouseenter mouseleave", function(oEvent) {
				this.previousSibling.classList.toggle("sapMPopinHovered", oEvent.type == "mouseenter");
			});
		}

		ListItemBase.prototype.onAfterRendering.call(this);
		this._checkTypeColumn();
	};

	ColumnListItem.prototype.exit = function() {
		ListItemBase.prototype.exit.call(this);
		this._checkTypeColumn(false);
		this._destroyClonedHeaders();

		if (this._oPopin) {
			this._oPopin.destroy(true);
			this._oPopin = null;
		}
	};

	// remove pop-in from DOM when setVisible false is called
	ColumnListItem.prototype.setVisible = function(bVisible) {
		ListItemBase.prototype.setVisible.call(this, bVisible);
		if (!bVisible && this.hasPopin()) {
			this.removePopin();
		}

		return this;
	};

	// returns responsible table control for the item
	ColumnListItem.prototype.getTable = function() {
		var oParent = this.getParent();
		if (oParent && oParent.isA("sap.m.Table")) {
			return oParent;
		}
	};

	/**
	 * Returns the pop-in element.
	 *
	 * @protected
	 * @since 1.30.9
	 */
	ColumnListItem.prototype.getPopin = function() {
		if (!this._oPopin) {
			this._oPopin = new TablePopin({
				id: this.getId() + "-sub"
			}).addDelegate({
				// handle the events of pop-in
				ontouchstart: this.ontouchstart,
				ontouchmove: this.ontouchmove,
				ontap: this.ontap,
				ontouchend: this.ontouchend,
				ontouchcancel: this.ontouchcancel,
				onsaptabnext: this.onsaptabnext,
				onsaptabprevious: this.onsaptabprevious,
				onsapup: this.onsapup,
				onsapdown: this.onsapdown,
				oncontextmenu: this.oncontextmenu
			}, this).setParent(this, null, true);
		}

		return this._oPopin;
	};

	/**
	 * Returns pop-in DOMRef as a jQuery Object
	 *
	 * @protected
	 * @since 1.26
	 */
	ColumnListItem.prototype.$Popin = function() {
		return this.$("sub");
	};

	/**
	 * Determines whether control has pop-in or not.
	 * @protected
	 */
	ColumnListItem.prototype.hasPopin = function() {
		return this._oPopin;
	};

	/**
	 * Pemove pop-in from DOM
	 * @protected
	 */
	ColumnListItem.prototype.removePopin = function() {
		this._oPopin && this.$Popin().remove();
	};

	/**
	 * Returns the tabbable DOM elements as a jQuery collection
	 * When popin is available this separated dom should also be included
	 *
	 * @returns {jQuery} jQuery object
	 * @protected
	 * @since 1.26
	 */
	ColumnListItem.prototype.getTabbables = function() {
		return this.$().add(this.$Popin()).find(":sapTabbable");
	};

	/**
	 * Calculates and returns the bounding client rectangle
	 * of the drop area taking the popin area into account.
	 * @private
	 */
	ColumnListItem.prototype.getDropAreaRect = function() {
		var oPopin = null;
		var oDomRef = this.getDomRef();
		var mDropRect = oDomRef.getBoundingClientRect().toJSON();
		if (this._oPopin && (oPopin = this.getDomRef("sub"))) {
			var mPopinRect = oPopin.getBoundingClientRect();
			mDropRect.bottom = mPopinRect.bottom;
			mDropRect.height += mPopinRect.height;
		}

		return mDropRect;
	};

	ColumnListItem.prototype.getAccessibilityType = function(oBundle) {
		return oBundle.getText("ACC_CTR_TYPE_ROW");
	};

	ColumnListItem.prototype.getContentAnnouncement = function(oBundle) {
		var oTable = this.getTable();
		if (!oTable) {
			return;
		}

		var aOutput = [],
			aCells = this.getCells(),
			aColumns = oTable.getColumns(true);

		aColumns.sort(function(oCol1, oCol2) {
			var iCol1Index = oCol1.getIndex(), iCol2Index = oCol2.getIndex(), iIndexDiff = iCol1Index - iCol2Index;
			if (iIndexDiff == 0) { return 0; }
		    if (iCol1Index < 0) { return 1; }
		    if (iCol2Index < 0) { return -1; }
		    return iIndexDiff;
		}).forEach(function(oColumn) {
			var oCell = aCells[oColumn.getInitialOrder()];
			if (!oCell || !oColumn.getVisible() || (oColumn.isHidden() && !oColumn.isPopin())) {
				return;
			}

			var oHeader = oColumn.getHeader();
			if (oHeader && oHeader.getVisible()) {
				aOutput.push(ListItemBase.getAccessibilityText(oHeader) + " " + ListItemBase.getAccessibilityText(oCell, true));
			} else {
				aOutput.push(ListItemBase.getAccessibilityText(oCell, true));
			}
		});

		return aOutput.join(" . ").trim();
	};

	// update the aria-selected for the cells
	ColumnListItem.prototype.updateSelectedDOM = function(bSelected, $This) {
		ListItemBase.prototype.updateSelectedDOM.apply(this, arguments);

		// update popin as well
		if (this.hasPopin()) {
			this.$Popin().attr("aria-selected", bSelected);
		}
	};

	ColumnListItem.prototype.onfocusin = function(oEvent) {
		if (oEvent.isMarked()) {
			return;
		}

		if (oEvent.srcControl === this) {
			this.$().children(".sapMListTblCellDup").find(":sapTabbable").attr("tabindex", -1);
		}

		ListItemBase.prototype.onfocusin.apply(this, arguments);
	};

	// informs the table when item's type column requirement is changed
	ColumnListItem.prototype._checkTypeColumn = function(bNeedsTypeColumn) {
		if (bNeedsTypeColumn == undefined) {
			bNeedsTypeColumn = this._needsTypeColumn();
		}

		if (this._bNeedsTypeColumn != bNeedsTypeColumn) {
			this._bNeedsTypeColumn = bNeedsTypeColumn;
			this.informList("TypeColumnChange", bNeedsTypeColumn);
		}
	};

	// determines whether type column for this item is necessary or not
	ColumnListItem.prototype._needsTypeColumn = function() {
		var sType = this.getType();

		return this.getVisible() && (
			sType == ListItemType.Detail ||
			sType == ListItemType.Navigation ||
			sType == ListItemType.DetailAndActive
		);
	};

	// Adds cloned header to the local collection
	ColumnListItem.prototype._addClonedHeader = function(oHeader) {
		return this._aClonedHeaders.push(oHeader);
	};

	// Destroys cloned headers that are generated for popin
	ColumnListItem.prototype._destroyClonedHeaders = function() {
		if (this._aClonedHeaders.length) {
			this._aClonedHeaders.forEach(function(oClone) {
				oClone.destroy("KeepDom");
			});
			this._aClonedHeaders = [];
		}
	};

	// active feedback for pop-in
	ColumnListItem.prototype._activeHandlingInheritor = function() {
		this._toggleActiveClass(true);
	};

	// inactive feedback for pop-in
	ColumnListItem.prototype._inactiveHandlingInheritor = function() {
		this._toggleActiveClass(false);
	};

	// toggles the active class of the pop-in.
	ColumnListItem.prototype._toggleActiveClass = function(bSwitch) {
		if (this.hasPopin()) {
			this.$Popin().toggleClass("sapMLIBActive", bSwitch);
		}
	};

	return ColumnListItem;

});

redpajama_set_name: RedPajamaGithub


By checking this box you acknowledge that this piece of equipment must be connected with an Ethernet cable to the local area network.
The Star Micronics TSP654K Ethernet LAN thermal receipt printer is designed for applications that require liner free labels. Features include a fast, efficient, and reliable receipt printer that connects via your local area network (LAN) to an Apple iPad running Square Register. This printer is perfect for those with an existing local area network (LAN) or are able to run an Ethernet connection from the router to the location of each printer. Hard wiring printers provides a time tested solution that eliminates the nuances of wireless connectivity. As a rule of thumb if you can wire, wire!!
The TSP654K Ethernet prints at 300mm per second, fast enough to make a regular receipt in less than one second. Thermal receipt printers use heat to print receipts on special heat-sensitive paper. This printer is unique in that it utilizes liner free rolls of restick paper. They are fast, quiet, and clean to operate. TSP654K Ethernet has an auto-cutter that severs receipts so they are easy to grab and is compatible with 80 mm (3 inch) liner free maxstick thermal receipt paper. Connect TSP654K Ethernet to a compatible cash drawer to open the drawer straight from the Square Register app.
Accessories include splash proof covers, vertical stands, wall mount brackets and extendable warranties like the Swap-a-Star or Extend-a-Star warranty.


text:
Realism & Restraint
Economic Concentration
Home/Austin At Large
Austin At Large
J. Arthur Bloom
Jordan was TAC's associate editor. He also reviews music for Tiny Mix Tapes, is a contributor at The Umlaut. His work has appeared elsewhere at the Washington Post, Washington Times, The Daily Caller, and Doublethink magazine, among others. He is a graduate of the College of William & Mary and lives in Washington DC. Follow him on Twitter
Media Skewers 'Sexist' Sanders for Refusing to Bend the Knee
By desperately wielding the sword of victimhood, Elizabeth Warren insults, not empowers her sex.
Barbara Boland January 17, 2020
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text:
Diane Lynn Pierce Warren
Bradley's Funeral Home
Diane Lynn Pierce Warren, age 67, passed away on Monday, January 10, 2022, at the Johnson City Medical Center. Diane was born in Monrovia, CA to the late Lawrence and Lorraine Pierce. She is also preceded in death by her husband, Kent Warren.
Diane was a pioneer for women in the electric power industry, and described herself as someone "interested in the mechanics of how things work." She founded two businesses during her career, Arroyo Company, and INNOVAT Corporation, for which she served as president and CEO. She also served as president of WW Components for many years. Diane was a member of WINUP, the Women's International Network of Utility Professionals, and the National Association of Women Business Owners. Diane was a member of the Marion Noon Rotary Club, was one of the first female Rotarians in the area, and was the recipient of the Paul Harris Fellow award. She particularly enjoyed the many years she spent hosting the Rotary Interact after-prom party for Marion Senior High School students.
In addition to devotion to her profession, and advocacy for the advancement of women in business, Diane was passionate about her family history and genealogy. She loved to travel, especially to Ireland and Germany, and research her ancestors. She dedicated her time to the Anderson Hill Cemetery Board of Directors.
Diane was a good friend and advocate, to her humans and her animals. She loved nature and rescuing and fostering animals. She also enjoyed riding in hotrods, and was a member of the Vintiques Car Club in Watertown, SD and the former Carnuts Club in Chilhowie.
Survivors include her fiancé, Brad Rorvick, Troutdale; son, Mastin Eli Warren and wife, Kayla, Marion; daughters, Rhonda Warren, Marion, and Heather Rorvick and Tom Barrella, Watertown, SD; brothers: Lawrence Pierce, Marion, Richard Pierce, Troutdale, and Gary Pierce and wife Penny, Troutdale; grandchildren: Markas Warren, Makenna Warren, Lucas Barnes, Will Barnes, Hannah Barnes, and Aaron Paschal; her African Gray Parrot, Edgar, and loving cats Yoda and Luna; nieces and many loving cousins and friends throughout the country also survive.
The family will receive friends from 5:00 pm-7:00 pm, on Friday, January 14, 2022 at the Bradley's Funeral Home in Marion. Private graveside services will be on Saturday, January 15, 2022 at the Anderson Hill Cemetery in Troutdale, with Rev. Kayla Keilholtz officiating. In lieu of flowers, donations can be made to the Marion Noon Rotary Club, P.O. Box 254, Marion, VA 24354. Expressions of sympathy may be forwarded to the family at www.bradleysfh.com. Bradley's Funeral Home, Marion is serving the family of Diane Warren.


text:
Barbara Hillary may refer to:

 Barbara Hillary (model) (born 1949), Playboy magazine's Playmate of the Month, April 1970
 Barbara Hillary (adventurer) (1931–2019), first known African-American woman to reach the North Pole

redpajama_set_name: RedPajamaWikipedia


text:
package com.bt.pi.core.messaging;

import javax.annotation.Resource;

import rice.Continuation;

import com.bt.pi.core.continuation.GenericContinuation;
import com.bt.pi.core.entity.EntityResponseCode;
import com.bt.pi.core.entity.PiEntity;
import com.bt.pi.core.message.ApplicationMessage;
import com.bt.pi.core.message.KoalaMessage;
import com.bt.pi.core.parser.KoalaPiEntityFactory;

public class KoalaMessageContinuation<T extends PiEntity> extends GenericContinuation<KoalaMessage> {

    private Continuation<T, Exception> continuation;
    private KoalaPiEntityFactory koalaPiEntityFactory;

    public KoalaMessageContinuation() {
        this(null, null);
    }

    public KoalaMessageContinuation(Continuation<T, Exception> piEntityContinuation, KoalaPiEntityFactory aKoalaPiEntityFactory) {
        super();
        continuation = piEntityContinuation;
        koalaPiEntityFactory = aKoalaPiEntityFactory;
    }

    @Resource
    public void setKoalaPiEntityFactory(KoalaPiEntityFactory aKoalaPiEntityFactory) {
        this.koalaPiEntityFactory = aKoalaPiEntityFactory;
    }

    @Override
    public void handleException(Exception arg0) {
        continuation.receiveException(arg0);
    }

    @SuppressWarnings("unchecked")
    @Override
    public void handleResult(KoalaMessage arg0) {
        if (arg0 instanceof ApplicationMessage) {
            ApplicationMessage appMessage = (ApplicationMessage) arg0;
            T payload = (T) koalaPiEntityFactory.getPiEntity(appMessage.getJson());

            if (EntityResponseCode.OK.equals(appMessage.getResponseCode()))
                continuation.receiveResult(payload);
            else
                continuation.receiveException(new KoalaMessageContinuationException(appMessage.getResponseCode(), payload));
        } else {
            continuation.receiveException(new RuntimeException("Unable to transform KoalaMessage into PiEntity" + arg0));
        }
    }

}


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