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

Element diffusion, sometimes named ``atomic" diffusion, is a basic
physical element transport mechanism which is driven by pressure
gradients (or gravity), temperature gradients and composition
gradients. The effects of helium diffusion on the structure of solar
models were first studied by Noerdlinger (\cite{Noerdlinger}). Later
helioseismology provided an effective method to study this physical
process (Guenther et al. \cite{Guenther93}; Guenther
\cite{Guenther94}; Bahcall \& Pinsonneault \cite{Bahcall92b};
Christensen-Dalsgaard et al. \cite{Christensen-Dalsgaard93};
Guenther \& Demarque \cite{Guenther97}). Recently, helioseismic
inferences have demonstrated that models incorporating element
diffusion are in substantially better agreement with the inferred
sound speed than the models that neglect it.

Up to date, the effect of element diffusion has been tested by
asteroseismic method in solar type stars. According to the ``second
differences", Vauclair \& Th\'{e}ado (\cite{Vauclair}), Th\'{e}ado
et al. (\cite{Theado}) and Castro \& Vauclair (\cite{Castro})
presented discussion of asteroseismic signatures of pure helium
diffusion in main-sequence stars between 1.1$M_{\odot}$ and
2.0$M_{\odot}$. In the present work, we study the effects of both
helium and metal element diffusion on the models with mass less than
1$M_{\odot}$.

Metal element could affect temperature gradient and convection in
the envelope of stars. It also leads to the variations of the
central temperature, density, pressure and radiative opacity. It is
important to consider the influence of metal element on the internal
structure of star. In this paper we mainly study the effects of
metal diffusion on the stellar structure, evolution and the
oscillation frequency for the late K-type star $\epsilon$ Eridani.

The bright K2V dwarf $\epsilon$ Eridani (HD22049, HIP16537, HR1084,
PLX742) is one of the nearest solar-like stars, with a distance of
about 3.218pc. It has a planetary companion $\epsilon$ Eridani b
(Hatzes et al. \cite{Hatzes}). Its proximity makes this planetary
system as a prime target for future extrasolar planet direct --
imaging efforts and studying the process of planetary systems
formation. The success of these efforts will depend on the mass and
the age of the system. Therefore the study of exoplanet -- host star
$\epsilon$ Eridani is a key issue.

In order to determine precise global parameters of the star
$\epsilon$ Eridani, some authors performed numerous theoretical
analysis (Guenther \& Demarque \cite{Guenther86}; Guenther
\cite{Guenther87}; Soderblom \& D\"{a}ppen \cite{Soderblom})
(hereafter GD86, G87 and SD89 respectively). Thanked for  Noyes et
al. (\cite{Noyes}), they measured the $p$-mode oscillation spectrum
of $\epsilon$ Eridani and identified three individual frequencies in
the power spectrum between 1500 $\mu$Hz and 2000 $\mu$Hz with
average large spacing of 172 $\pm$ 5 $\mu$Hz. Based on
non-asteroseismic and asteroseismic observational constrains, GD86,
G87 and SD89 constructed a series of stellar models of $\epsilon$
Eridani. However, in their works for $\epsilon$ Eridani, there is a
contradiction between the young age implied by the high
chromospheric activity, rapid rotation rate, and the old age implied
by the slightly metal-poor composition. In their works, GD86, G87
and SD89 discussed this contradiction and given the age 12 Gyr, 10
Gyr and 1 Gyr respectively.

Recently many evidences from observations seem to indicate that
$\epsilon$ Eridani is a young main-sequence star with age less than
1 Gyr. For example, using Li abundances with the star's position in
the H-R diagram and kinematics, Song et al. (\cite{Song}) derived
the age of 0.73 $\pm$ 0.2 Gyr; Measuring the radius of $\epsilon$
Eridani by long-baseline interferometry, Di Folco et al. (\cite{Di
Folco}) estimated the age at 0.85 Gyr; Saffe et al. (\cite{Saffe})
used the calibrations of Donahue (\cite{Donahue93}) and Rocha-Pinto
\& Maciel (\cite{Rocha-Pinto}) (which corrected the age with an
effect from chromospheric activity) to estimate the ages of 0.66 Gyr
and 0.82 Gyr respectively. SIMBAD database describes the age of
$\epsilon$ Eridani to be 0.66 Gyr.

The aim of present paper is to provide the basic theoretical studies
of $\epsilon$ Eridani. We will use the latest interferometric
observational radius (Di Folco et al. \cite{Di Folco}) to constraint
the stellar models and predict the frequency spacings. Then, we will
investigate the effects of helium and metal diffusion on the
internal structure, and the frequency spacings which also depend on
the internal structure of the star.

In section 2, the global parameters of the star were summarized.
The input physics, computing method and results analysis are
summarized in section 3. The helium and metal diffusion effects on
the stellar models, and the oscillation frequency are discussed in
section 4. Finally, the conclusion is presented in section 5.

\section{Observational Constraints}

Observationally it is difficult to determine accurately the mass of
star except some binary systems. $\epsilon$ Eridani is a single star
and it has various data of masses which were published in the
literatures, for example 0.85 $\pm$ 0.04$M_{\odot}$ (Santos et al.
\cite{Santos01}), 0.80$M_{\odot}$ (Minier \& Lineweaver
\cite{Minier}), 0.82$M_{\odot}$ (Takeda et al. \cite{Takeda}),
0.83$M_{\odot}$ (Fischer \& Valenti \cite{Fischer}).

For the effective temperature of $\epsilon$ Eridani, we adopt
$T_{eff}$ = 5012 $\pm $ 67 which was determined from the infrared
flux method (IRFM) (Ram\'{\i}rez \& Mel\'{e}ndez \cite{Ramirez}).

The luminosity can be calculated using the absolute visual magnitude
$M_{v}$ = 6.18 $\pm$ 0.11 (Song et al. \cite{Song}; Takeda et al.
\cite{Takeda}). Given the bolometric correction $B.C.$ = -- 0.28
(Takeda et al. \cite{Takeda}), the absolute bolometric magnitude is
therefore $M_{bol}$ = $M_{v}$ + $B.C.$ = 5.9 $\pm$ 0.11. Then the
luminosity is computed by formulae: $M_{bol}$ = --
2.5$log(L/L_{\odot})$ + $M_{bol, \odot}$. Adopting $M_{bol, \odot}$
= 4.746, we thus obtain $\log$ ($L/L_{\odot}$) = -- 0.4176 $\sim$ --
0.5056.

$\epsilon$ Eridani is slightly metal-poor compared with the Sun.
Santos et al. (\cite{Santos04}) obtained $[Fe/H]$ = -- 0.13 $\pm$
0.04 from the spectroscopic analysis basing on 39 Fe$_{\rm I}$ and
12 Fe$_{\rm II}$ lines. In order to deduce $[Z/X]$, we assume that
the logarithmic value of $[Z/X]$ is proportional to the abundance
ratio $[Fe/H]$ (Thoul et al. \cite{Thoul03}):
\begin{equation}
\log[Z/X]_{star} = [Fe/H]_{star} + \log[Z/X]_{\odot}
\end{equation}
where $[Z/X]_{\odot}$ = 0.023 (Grevesse \& Sauval \cite{Grevesse}).
Using this ratio, we obtain $[Z/X]_{surf}$ = 0.017 $\pm$ 0.0016.

A star's initial helium mass fraction $Y_{i}$ is important for
determining its structure, but $Y_{i}$ of $\epsilon$ Eridani is
unknown by observations. GD86, G87 adopted $Y_{i}$ to be 0.236 and
SD89 considered $Y_{i}$ to be from 0.24 to 0.26. In our work, we
reference the value given by GD86, G87, SD89 and adopt the initial
helium abundance $Y_{i}$ = 0.245 $\pm$ 0.015.

The frequency, especially large spacings, sensitively depend on the
radius. In order to predict the large spacings which will be
observed by MOST, we take the latest interferometric observational
radius $R/R_{\odot}$ = 0.734 $\pm$ 0.01 (Di Folco et al. \cite{Di
Folco}).

\begin{table}
 \caption{The  observational fundamental parameters of
$\epsilon$ Eridani.
            }
\label{table : 1}

 \tabcolsep0.15in
\begin{tabular}{c| c c}
\hline\hline
 parameters &$\epsilon$ Eridani & Ref \\
 \hline

 $M/M_{\odot}$&$0.85 \pm 0.04$&(1)\\
                   &$0.80$&(2)\\
                   &$0.82$&(3)\\
                   &$0.83$&(4)\\
\\

 $[F_{e}/H]_{surf}$&$-0.13 \pm 0.04$&(5)\\
\\

 $R/R_{\odot}$&$0.743 \pm 0.010$&(6)\\

 $M_{v}$&$6.18 \pm 0.11$&(7)\\
                  &$6.18$&(3)\\

 $\log(L/L_{\odot})$&$-0.4616 \pm 0.044$&(8)\\

 $T_{eff}(K)$&$5012 \pm 67 $&(9)\\

 \hline\hline

 \end{tabular}

 (1)Santos et al. (\cite{Santos01});
 (2)Minier \& Lineweaver (\cite{Minier});
 (3)Takeda et al. (\cite{Takeda});
 (4)Fischer \& Valenti (\cite{Fischer});
 (5)Santos et al. (\cite{Santos04});

 (6)Di Folco et al. (\cite{Di Folco});
 (7)Song et al. (\cite{Song});
 (8)this paper;
 (9)Ram\'{\i}rez \& Mel\'{e}ndez (\cite{Ramirez})

 \end{table}

\section{Stellar modeling}
\subsection{Input physics}

The evolutionary models are computed using the Yale stellar
evolution code version (Guenther et al. \cite{Guenther94}) which has
been modified to include the effects of element diffusion. The
initial zero-age main sequence (ZAMS) models were calculated from
pre-main sequence evolution which were assumed to have spherical
symmetry, no rotation, no magnetic field. In the computation we use
OPAL equation of state tables EOS2001 (Rogers \& Nayfonov
\cite{Rogers}), the opacities with a smooth blend of OPAL GN93
(Iglesias \& Rogers \cite{Iglesias}) and OPAL tables (Alexander \&
Ferguson \cite{Alexander}). The relevant nuclear reaction rates and
cross sections are from Bahcall \& Pinsonneault (\cite{Bahcall92a},
\cite{Bahcall92b}) and Bahcall (\cite{Bahcall89}). $\epsilon$
Eridani is a solar-like star, we choose the Krishna-Swamy
(\cite{Krishna Swamy}) atmosphere model. The diffusion of both
helium and metal element abundance was considered in the stellar
model computation, by using the coefficients of Thoul et al.
(\cite{Thoul94}). In the next section we will introduce it in
detail.

 Using the standard mixing-length theory, we
set $\alpha$ = 1.7 for all models, close to the value which is
required to reproduce the solar radius under the same physical
assumptions and stellar evolution code (Murphy \& Demarque
\cite{Murphy}). If rotation and magnetic field are neglected in the
construction of stellar model, convection is the most important
mechanism that is usually included in standard stellar models which
describes material motions within a star especially for low-mass
main sequence star. The convective overshoot is an another factor to
influence the chemical composition of the star. The change of
mixing-length parameter $\alpha$ would also influence principally
the radius of the base of the external convection zone. The presence
of core overshoot would extend the core-burning phase of evolution
and increase the estimated age of star. This important topic has
been studied separately by Bi et al. (\cite{Bi}). However, the
element diffusion could also lead to the redistribution of the
element in star and change the depth of the convective envelope
(Guenther \cite{Guenther94}). In order to test the effect of
diffusion on the chemical composition, internal structure and the
frequency of $\epsilon$ Eridani, we would not discuss the influence
of the convection and overshoot in present work.

\subsection{Element diffusion}

The element diffusion in stars is driven by gravitational setting,
temperature gradients, composition gradients and radiation pressure.
It is described by Bahcall \& Pinsonneault (\cite{Bahcall92a}) in
detail. The gravity and temperature gradients tend to concentrate
the helium and heavier elements toward the center of the star, while
the hydrogen diffuses outward. The concentration gradients oppose
the above processes.  In addition, radiation pressure can cause
partially ionized or neutral species to rise relative to species
with a small cross section. However, the radiation pressure are
efficient in the external regions of main-sequence stars with
$T_{eff}>6000K$ (Michaud \cite{Michaud}). So the radiative pressure
causes negligible diffusion in the K-type star and will be neglected
in this paper.

\subsubsection{Basic equation for element diffusion}

Most works on chemical diffusion use either the Chapman - Enskog
procedure (Chapman \& Cowling \cite{Chapman}) or the method of
Burgers (\cite{Burgers}) for deriving the transport properties from
the Boltzmann equation. In our work the element diffusion is
described using the equations of Burgers (\cite{Burgers}) with
diffusion velocity coefficients from Thoul et al (\cite{Thoul94}). A
single model includes both helium and metal element diffusion. The
change rate of the element mass fractions due to the diffusion is
now written as (Thoul et al \cite{Thoul94}; Bahcall \& Loeb
\cite{Bahcall90}):
\begin{equation}
 \frac{\partial X_{s}}{\partial t} = -
\frac{1}{\rho r^{2}} \frac{\partial
[r^{2}X_{s}T^{5/2}\xi_{s}(r)]}{\partial r}
\end{equation}
where the partial derivatives are evaluated in the local rest frame
of a mass shell in the star. $\rho$, $r$, $T$ are the local value of
density, radius, temperature and $X_{s}$ is the mass fraction of
element $s$.

The diffusion velocity for species $s$ is defined by

\begin{equation}
w_{s} = \frac{T^{5/2}\xi_{s}}{\rho}
\end{equation}
and the function $\xi_{s}(r)$ is expressed as
\begin{equation}
\xi_{s}(r) = A_{p}(s)\frac{\partial\ln p}{\partial r} +
A_{T}(s)\frac{\partial\ln T}{\partial r} + \sum\limits_{c\neq e,2}
A_{c}(s)\frac{\partial\ln C_{c}}{\partial r}
\end{equation}
In equation (4), $A_{p}$, $A_{T}$, $A_{c}$ correspond to
gravitational setting, thermal diffusion and concentration gradient
diffusion which are the functions of the mass fractions only.
Species $c$ can equal to $s$, but $c$ aren't electron and helium
element.

 \subsubsection{The treatment of diffusion in the evolutionary
code}

 The Yale stellar evolution code has been modified to include
the effects of $He$ diffusion from gravitational settling and
thermal diffusion (Bahcall \& Pinsonneault \cite{Bahcall92a}) using
the method of Bahcall \& Loeb (\cite{Bahcall90}) and added the metal
diffusion in 1994. About the method by which treatment of element
diffusion in a standard stellar evolution code, it has been
described by Bahcall \& Pinsonneault (\cite{Bahcall92a}) in detail.
In this section, we summarize it again.

In the diffusion subroutine written by Bahcall and Pinsonneault, the
main problem is to solve the diffusion equation and calculate the
change of the element abundance by diffusion. The diffusion equation
(2) can be written as following form:
\begin{equation}
\frac{dx}{dt}=\frac{1}{\rho
r^{2}}[\frac{d}{dr}(D_{1})+\frac{d}{dr}(D_{2}\frac{dx}{dr})]
\end{equation}
where $D_{1}$, $D_{2}$ is the diffusion coefficients.

For helium diffusion

\begin{equation} \label{eq:1}
\left\{ \begin{array}{l}
         D_{1}(Y)=\frac{F_{gy}\cdot r^{2}\cdot T^{5/2}}{\ln\Lambda}\cdot\frac{d\ln p}{dr}\cdot X\cdot(A_{p}^{X}+A_{T}^{X}) \\
                  D_{2}(Y)=\frac{F_{gy}\cdot r^{2}\cdot T^{5/2}}{\ln\Lambda}\cdot A_{c}^{X}
                          \end{array} \right.
                          \end{equation}

For metal diffusion
\begin{equation} \label{eq:1}
\left\{ \begin{array}{l}
         D_{1}(Z)=\frac{F_{gz}\cdot r^{2}\cdot T^{5/2}}{\ln\Lambda}\cdot\frac{d\ln p}{dr}\cdot Z\cdot(A_{p}^{Z}+A_{T}^{Z}) \\
                  D_{2}(Z)=\frac{F_{gz}\cdot r^{2}\cdot T^{5/2}}{\ln\Lambda}\cdot A_{c}^{Z}
                          \end{array} \right.
                          \end{equation}
and radius, temperature, and density are in nondimensional units
defined by $r=r'/R_{\odot}$, $T=T'/10^{7}K$, $ \rho=\rho'/100g$
$cm^{-3}$ and $t=t'/10^{13}yr$ (Bahcall \& Pinsonneault
\cite{Bahcall92a}; Chaboyer et al. \cite{Chaboyer}).

In expressions (6) and (7), $F_{gy}$ and $F_{gz}$ are the adjustment
factors by which the helium and metal diffusion coefficients are
multiplied. In our work, we set both of the two factors to 1.0.
 $A_{p}$, $A_{T}$, $A_{c}$ are the diffusion velocity coefficients as described in equation (4).
 The exact
numerical solution of these coefficients are calculated by an export
subroutine which was developed by Thoul in 1994. The computation
method is exhibited detailedly by Thoul et al. (\cite{Thoul94}).

In equation (5) the partial time derivative is evaluated at constant
mass shell of the star. The diffusion equation is solved with zero
hydrodynamic velocity of the stellar plasma. The right hand of
diffusion equation (5) has two terms: the first term depends on
first spatial derivatives of the element mass fraction and the
second term depends on second spatial derivatives of the element
abundance. The first term is solved explicitly using the two-step
Lax-Wendroff technique (Press et al. \cite{Press}) by neglecting the
second derivatives of the element abundance. We then use this trial
solution as the initial abundance to determine the second
derivatives by a fully implicit method (Bahcall \& Pinsonneault
\cite{Bahcall92a}). At last, the element abundance were updated.

For the helium diffusion, we only consider $^{4}$He diffusion and
ignore $^{3}$He diffusion (Loeb et al. \cite{Loeb}).  The time rate
of change of the $^{4}$He mass fraction $Y$ is equal in magnitude
and opposite in sign to the rate of change of the hydrogen mass
fraction.

The diffusion of all metal elements were assumed to diffuse at the
same rate as fully ionized iron. Because of the diffusion of metal
elements, the radiative opacity have to be changed at each spherical
shell in the stellar model after each time step. We calculate the
effect of metal element diffusion on the opacity by computing a
total metal element abundance at each model radius $Z(r)$, and then
interpolating for the opacity between opacity tables with different
total metal element abundances (Bahcall et al. \cite{Bahcall95}).

The diffusion subroutine carries out the diffusion calculations
using data supplied by other parts of the Yale code, in which the
thermal structure and the element abundances are calculated. It is
assumed that the amount of diffusion within a given time step was
too small to affect significantly the changes in thermal structure,
in abundances, and in nuclear reaction rates that are calculated
elsewhere. After the diffusion computation, we update the element
abundance and then calculate the thermal structure.

In the diffusion subroutine, the element diffusion is treated only
in the radiation region. The characteristic time for element to
diffuse a solar radius under solar conditions is of the order of
$10^{13}$ yr (Bahcall et al. \cite{Bahcall95}), much larger than the
age of the sun and $\epsilon$ Eridani. However, helioseismic
inferences have demonstrated the significance of the element
diffusion (Cox et al. \cite{Cox}; Bahcall \& Loeb \cite{Bahcall90};
Bahcall \& Pinsonneault \cite{Bahcall92a}; Proffitt
\cite{Proffitt}), we would test how much effect on the internal
structure, the age and the frequency of $\epsilon$ Eridani by both
the helium and metal diffusion using the asteroseismic method.

\subsection{Computational method and results analysis }

\begin{table*}
 \caption{Model Parameters of
$\epsilon$ Eridani.
            }
\label{table : 1}

 \tabcolsep0.10in
\begin{tabular}{c| c c c|ccc|ccc}
\hline\hline

Model&A1&A2&A3&B1&B2&B3&C1&C2&C3\\
\hline

     &\multicolumn{3}{|c|}{$M/M_{\odot}=0.83$}&\multicolumn{3}{|c|}{$M/M_{\odot}=0.83$}&\multicolumn{3}{|c}{$M/M_{\odot}=0.83$}\\
     &\multicolumn{3}{|c|}{$Z_{i}=0.012$}&\multicolumn{3}{|c|}{$Z_{i}=0.013$}&\multicolumn{3}{|c}{$Z_{i}=0.014$}\\
     &\multicolumn{3}{|c|}{$Y_{i}=0.2315$}&\multicolumn{3}{|c|}{$Y_{i}=0.2365$}&\multicolumn{3}{|c}{$Y_{i}=0.2415$}\\
\hline

Dif.&None.&Y.Dif&Y\& Z.Dif&None.&Y.Dif&Y\& Z.Dif&None.&Y.Dif&Y\& Z.Dif\\
Age(Gyr)&1.151&1.089&1.0&1.206&1.138&1.0&1.264&1.191&1.0\\
$L/L_{\odot}$&0.321&0.321&0.321&0.319&0.319&0.319&0.317&0.317&0.317\\
$R/R_{\odot}$&0.749&0.750&0.744&0.750&0.751&0.743&0.751&0.753&0.741\\
$T_{eff}$&5024.9&5019.8&5039.5&5012.2&5006.7&5036.3&4999.9&4993.8&5033.5\\
&&&&&&&&&\\
$r_{cz}/R$&0.7073&0.7053&0.7048&0.7046&0.7033&0.7024&0.7024&0.7022&0.7000\\
$\tau_{cz}(s)$&1504.8&1514.1&1496.7&1514.4&1522.9&1496.7&1523.2&1529.5&1497.0\\
$\tau_{0}(s)$ &2524.5&2532.5&2502.4&2530.1&2538.8&2493.6&2535.7&2545.2&2484.5\\
$\tau_{cz}(s)/\tau_{0}(s)$&0.5961&0.5979&0.5981&0.5986&0.5999&0.6002&0.6007&0.6009&0.6025\\
$<\Delta \nu>$&192.2&191.4&193.8&191.6&191.0&194.6&191.2&190.5&195.1\\

 \hline\hline

 \end{tabular}

 \end{table*}

\subsubsection{Evolutionary tracks and candidates for pulsation}

\label{sect:intro}
 \begin{figure}
  \centering
  \includegraphics[angle=0,totalheight=5cm,width=8cm]{HRD1.eps}
  \vskip 0.15in
\includegraphics[angle=0,totalheight=5cm,width=8cm]{HRD2.eps}
\vskip 0.15in
  \caption{(a)Evolutionary tracks (12 in total) in the H-R diagram from ZAMS.
 The solid lines indicate the boxes delimited by the observed luminosity and effective temperature. The two dash dot lines denote the boxes delimited by the
 interferometric radius. (b)Enlarge the error box of Fig (a). The model A3, B3 and C3 are denoted by filled circle, triangle
 and five pointed star respectively.}%
   \end{figure}

In order to reproduce observational constraints of $\epsilon$
Eridani, we have computed a grid of evolutionary tracks for six
masses $M/M_{\odot}$: 0.80, 0.81, 0.82, 0.83, 0.84, 0.85 and the
initial metallicity $Z_{i}$: 0.011, 0.012, 0.013, 0.014.

From a series of evolutionary tracks which are computed, we select
those models that land within the observational error box (being
composed by $\log T_{eff}$, $\log L/L_{\odot}$, $\log R/R_{\odot}$)
in the theoretical H-R diagram. Then we further choose the models on
the basis of the constraint of the observational $[Z/X]$. In terms
of the computation alone, we note that the age of $\epsilon$ Eridani
is likely in the range ~ 0.1 Gyr -- 1.0 Gyr. Here we consider the
age ($\leq$ 1 Gyr) as a property of star which be same as SD89.
According to the age estimation from observation, which given in the
introduction, we constraint the age of models in the range ~ 0.60
Gyr -- 1.0 Gyr. At last, 12 tracks fall within the observational
error box and are plotted in Fig. 1 (a).

In order to deduce the set of parameters lending to the better
agreement with observations, we perform a $\chi^{2}$ minimization
method described by Eggenberger (\cite{Eggenberger}). We define the
$\chi^{2}$ function as follows:
\begin{equation}
\chi^{2}\equiv\sum\limits^{4}_{i=1}(\frac{C_{i}^{theo}-C_{i}^{obs}}{\sigma})^{2}
\end{equation}
where the vector $C_{i}^{obs}$ contains the observations:
$C_{i}^{obs}$ $\equiv$ ($L/L_{\odot}$, $T_{eff}$, $R/R_{\odot}$,
$[Z/H]_{s}$). The value $C_{i}^{obs}$ and the vector $\sigma$ which
contains the errors on the observations are given in Table 1. From
this method we obtain three models A3, B3 and C3 which are given in
Fig. 1 (b) and Table 2.

\subsubsection{Calibration of models with and without diffusion}

In order to investigate the effect of element diffusion, especially
metal diffusion, basing on the selected models A3, B3 and C3, we
calibrate three groups of models with mass $M/M_{\odot}=0.83$. There
are the different initial chemical compositions among the different
groups. The models at the same group have the same initial chemical
compositions, but they have different types of element diffusion.
The detail description of the models are given in Table 2.

We use the stellar pulsation code of Guenther (\cite{Guenther94}) to
calculate the eigenfrequencies and the large spacings of models
listed in Table 2. For solar-like stars, the eigenfrequencies
$\nu_{n,l}$ of oscillation modes, characterized by the radial order
$n$ at harmonic degree $l$, satisfy the simplified asymptotic
relation (Tassoul \cite{Tassoul}):
\begin{equation}
\nu_{n,l}=\Delta
\nu(n+\frac{l}{2}+\alpha+\frac{1}{4})+\epsilon_{n,l}
\end{equation}
The large spacings is defined by the frequencies of the same
harmonic degree $l$ and the adjacent radial order $n$:
\begin{equation}
\Delta\nu_{n,l}\equiv\nu_{n,l}-\nu_{n-1,l}
\end{equation}
We average the large spacings over the modes $l$ = 0, 1, 2, 3 and
$n$ = 10, 11, ..., 30 to obtain the average large spacings.

From the age of the star in Table 2, we can see that the diffusion
could speed up the evolution of stars. The model with both helium
and metal diffusion has the smallest age of all the models in the
same group. The average large spacings is about 194 $\pm$ 1$\mu Hz$
of models A3, B3 and C3. The pure helium diffusion hardly affect
$\nu_{n,l}$, but the effect is relatively obvious after adding the
metal diffusion. It also seems that the diffusion effect is increase
alone with the increase of the initial heavy element abundance
($Y_{i}$, $Z_{i}$). In the following section, we select models in
group (C) to discuss differences in their internal structures in
detail using the asteroseismic method.

\section{Asteroseismic test helium and metal diffusion effects}

\subsection{``Second differences" tests helium and metal gradients}
   \begin{figure}
\includegraphics[angle=0,totalheight=6.5cm,width=11cm]{YZHDR113.eps}
\vskip 0.15in
\includegraphics[angle=0,totalheight=6.5cm,width=11cm]{tdcdrHDR113.eps}
\vskip 0.15in
\includegraphics[angle=0,totalheight=6.5cm,width=11cm]{sedfHRD113.eps}
\vskip 0.15in \caption{The stellar structures of the group (C)
models in Table 2 with $Y_{i}$ = 0.2415, $Z_{i}$ = 0.014. The
detailed notes are labeled in the figure. Solid lines: standard
homogeneous model C1 without diffusion; dashed lines: model C2 with
pure helium diffusion; dash dot lines: model C3 with both helium
diffusion and metal diffusion. The panel (a) helium profiles as a
function of the acoustic depths in the models, i.e. the time for the
acoustic waves to travel from the surface down to the considered
layer; (b) the metal profiles: a clear gradient at the bottom of the
convection zone; (c) the adiabatic exponent $\Gamma_{1}$ profiles
which show a clear feature at the place of the He$_{\rm II}$
ionisation zones; (d) the sound speed gradients: the dips are
clearly visible at the place of the He$_{\rm II}$ ionisation zones
and the bottom of the convection zones; (e) the second differences
of the oscillation frequencies plotted as a function of the
frequencies; (f) the Fourier transform of graph (e).}
\end{figure}
Stellar acoustic $p$-modes with low $l$ degree can propagate deeply
inside the stars. However, as mentioned by Gough (1990), rapid
variations of the sound speed inside a star lead to partial
reflections of the sound waves. A conveniently and easily evaluated
measure of this oscillatory component is the ``second differences"
with respect to the radial order $n$ of the frequencies $\nu_{nl}$
for the same value of the harmonic degree $l$:
\begin{equation}
\Delta_{2}\nu_{nl}\equiv \nu_{n-1,l}-2\nu_{n,l}+\nu_{n+1,l}
\end{equation}
This measure is contaminated less than the first difference
$\Delta_{1}\nu_{nl}$ $\equiv$ $\nu_{n,l}$ - $\nu_{n-1,l}$ by the
smoothly varying components of $\Delta_{1}\nu_{nl}$. This modulation
in the frequency has been extensively studied in the He$_{\rm II}$
ionization zone and the edge between the convective and radiative
zones. In the He$_{\rm II}$ ionization zone there is a rapid
variation of the adiabatic exponent $\Gamma_{1}$ and in the base of
the convection zone there is essentially a discontinuity in the
sound speed gradient, i.e. $dc/dr$, produce a discontinuity in
$\nu_{nl}$. In order to identify the different components which
modulate the oscillations, we have computed the Fourier transform of
the ``second differences". The modulation period of the ``second
differences" is twice the ``acoustic depth" of the region where the
feature occurs:
\begin{equation}
\tau_{s}=\int^{R}_{r_{s}}\frac{dr}{c(r)}
\end{equation}
where $\tau_{s}$ is the time needed for the acoustic waves to travel
between the surface and the considered region (the He$_{\rm II}$
ionization zone or the base of the convection zone), $c(r)$ is the
sound speed at radius $r$, and $r_{s}$ is the radius of the
considered region.

Vauclair \& Th\'{e}ado (\cite{Vauclair}), Th\'{e}ado et al.
(\cite{Theado}) and Castro \& Vauclair (\cite{Castro}) described
asteroseismic signatures of pure helium diffusion in stars between
1.1$M_{\odot}$ and 2.0$M_{\odot}$ in terms of ``second differences".
They have studied the precise signatures on the oscillation
frequencies of helium gradients inside stars. In our work we compute
stars of 0.83$M_{\odot}$ in which not only including helium
diffusion but also containing metal diffusion. The aim of the
present section is to study the precise signatures on the
oscillation frequencies of not only helium gradients but also metal
gradients inside stars and to test the effect of metal diffusion on
the internal structure.

Fig. 2(a)(b) display the helium and metal abundance profiles in the
models without element diffusion (solid line), with pure helium
diffusion (dashed line) and with both helium and metal diffusion
(dash dot line) as a function of the acoustic depth. Due to
diffusion, helium and metal drift inward and form a gradient just
below the convective zone. The acoustic depth of the bottom of the
convection zones $\tau_{cz}$ and the corresponding
$\tau_{cz}/\tau_{0}$ , where $\tau_{0}$ is the total acoustic depth
of the star, are listed in Table 2 about models with different
initial chemical composition and different types of diffusion. Fig.
2(c)(d) give the adiabatic exponent $\Gamma_{1}$ profiles and the
sound speed gradients $dc/dr$ versus the acoustic depth. From the
$dc/dr$ profiles it is clear to see that the dips around 300s and
1500s are caused by the He$_{\rm II}$ ionization zones and the
bottom of the convection zones.

Considering the asymptotic approximation validity, we select modes
of degrees $l$ = 0, 1, 2, 3 and oscillation frequencies between
1500$\mu Hz$ and 3000$\mu Hz$ to compute the ``second differences".
In Fig. 2(e)(f) we present the second differences of our models and
the Fourier transforms of these curves. We have explained that the
modulation period corresponding to the peaks in the Fourier
transforms are twice the ``acoustic depth" of the region where the
feature occurs. By comparing the dips of $dc/dr$ profiles in Fig.
2(d) with Fourier transforms in Fig. 2(f), one can easily recognize
the peaks due to the He$_{\rm II}$ ionization zones and those due to
the bottom of the convective zones in Fig. 2(f).

From the Fourier transforms in Fig. 2(f), we can see that the
amplitudes of the peaks corresponding to the modulation periods due
to the base of the convection zones of models C1, C2, C3 are
different. Mazumdar \& Antia (\cite{Mazumdar}) shown that the
amplitude of the oscillatory signal in the second differences
contains an amplification factor of
$4\sin^{2}(\pi\tau_{s}/\tau_{0})$. When $\tau_{s}/\tau_{0}
> \frac{1}{2}$, the Fourier transforms show the peak amplitudes
decrease for deeper layers (Vauclair \& Th\'{e}ado \cite{Vauclair}).
In terms of $r_{cz}/R$ and $\tau_{cz}/\tau_{0}$ in Table 2, we find
that diffusion could deepen the outer convective zone, especially
including the metal diffusion, the base of the convective zone is
deepest of all in the same group. From the Fourier transforms, we
can see that the peak amplitude at $2\tau_{cz}$ of models with pure
helium diffusion is lower than that without diffusion. In term of
amplification factor of $4\sin^{2}(\pi\tau_{s}/\tau_{0})$, the peak
amplitude of models with both helium and metal diffusion should be
lowest of all, but it is higher than that with pure helium
diffusion. So we think that the peak amplitude is mainly determined
by the depth of the base of the convection zone, meanwhile it is
also sensitive to the element gradient at the bottom of convective
zone. From Fig. 2(b), it is clear to see that the metal gradient
steepen more rapidly than helium gradient. There is a stronger
reflection of the sound waves in the region of the metal gradient,
that is why the model contain metal diffusion have a higher
amplitude of the peak of $\tau_{cz}$.

\subsection{Tests of internal structure}
\begin{figure}
\centering
\includegraphics[angle=0,totalheight=5cm,width=8cm]{113.d02.eps}
\vskip 0.30in
\includegraphics[angle=0,totalheight=5cm,width=8cm]{113.r02.eps}
\vskip 0.20in
 \caption{Upper part: small spacings $d_{02}(n)$, lower
part: frequency separation ratios $r_{02}(n)$ for the models in
group (C). The detailed notes are labeled in the figure.}
\end{figure}

\begin{figure}
\centering
\includegraphics[angle=0,totalheight=4.6cm,width=8cm]{dc.cHDR113.eps}
\vskip 0.20in
\includegraphics[angle=0,totalheight=4.6cm,width=8cm]{dT.THDR113.eps}
\vskip 0.20in
\includegraphics[angle=0,totalheight=4.6cm,width=8cm]{du.uHDR113.eps}
\vskip 0.20in
 \caption{From up to down, each panel of figure give
the relative sound-speed difference $\delta c/c$, the temperature
difference $\delta T/T$ and the mean molecular weight $\delta
\mu/\mu$ respectively for the models in group (C). All differences
are with respect to the model C1 which without any diffusion. The
dashed lines render the differences between the model with pure $He$
diffusion and the model without any diffusion (e.g.  $\delta
\mu/\mu$ = ($\mu_{Y.Dif}$ - $\mu_{None. Dif}$) / $\mu_{None. Dif}$).
The dash dot lines render the differences between the model with
$He$ \& $Z$ diffusion and the model without any diffusion (e.g.
$\delta \mu/\mu$ = ($\mu_{Y \& Z.Dif}$ - $\mu_{None. Dif}$) /
$\mu_{None. Dif}$). }
\end{figure}
In this section, we compute the so-called small frequency spacings
and frequency separation ratios of the low-$l$ $p$-modes to test the
internal structure of models in which considered different types of
diffusion. The small frequency spacings is given by the combination:
\begin{equation}
d_{ll+2}(n)=\nu_{n,l}-\nu_{n-1,l+2}
\end{equation}
Using the asymptotic theory of $p$ modes it can be shown that
(Christensen-Dalsgaard \& Berthomieu
\cite{Christensen-Dalsgaard91}; Basu et al. \cite{Basu07}):
\begin{equation}
d_{ll+2}(n)\simeq
-(4l+6)\frac{\Delta\nu_{nl}}{4\pi^{2}\nu_{n,l}}\int^{R}_{0}\frac{dc}{dr}\frac{dr}{r}
\end{equation}
where $R$ is the stellar radius and $\Delta\nu_{nl}$ is the large
spacings. In the core the gradient of the sound speed is large and
$r$ is small, the integral in equation (14) is dominated by
conditions in the core. So the small spacings usually test the
stellar core. But the small spacings are also slightly affected by
near-surface effects. In order to reduce the effect of near surface
uncertainties, the frequency separation ratios are used (Roxburgh \&
Vorontsov \cite{Roxburgh}):
\begin{equation}
r_{02}(n)=\frac{d_{02}(n)}{\Delta_{1}(n)},\hspace{0.5cm}r_{13}(n)=\frac{d_{13}(n)}{\Delta_{0}(n+1)}
\end{equation}

Each panel of Fig. 3 show small spacings $d_{02}$ and frequency
separation ratios $r_{02}$ for different models in group (C) with
different types of diffusion which are labeled in the figure. From
the small spacings and frequency separation ratios we can see that
the pure helium diffusion hardly alter the internal structure in
these young low--mass models. By comparing the models included metal
diffusion with the models no element diffusion, the differences of
their internal structures are relatively obvious.

In order to explain the changes of the internal structure from the
asteroseismic test, we compare the internal physical parameters of
models with and without diffusion. It is known that the sound speed
depends on both the mean molecular weight and the temperature (Basu
et al. \cite{Basu07}; Bi et al. \cite{Bi} )
\begin{equation}
c^{2}\simeq\frac{K_{B}T}{\mu m_{u}}\propto\frac{T}{\mu}
\end{equation}
In Fig. 4, we give the $\delta c/c$, $\delta T/T$, and $\delta
\mu/\mu$ variations as function of radius.

From Fig. 4, it is clear to see that the effect of the pure helium
diffusion on the sound speed $c$, temperature $T$ and the mean
molecular weight $\mu$ is small. The helium diffusion hardly alter
the $c$, $T$ and $\mu$ in the radiation interior and the effect
mainly concentrate on the convection zone. Due to diffusion, helium
drift inward just below the convection zone. It induce $\mu$ is
smaller than that without diffusion in the envelope. On the other
hand, the increase of the opacity in the envelope due to the
settling of $He$ leads to the lower temperature than that without
diffusion. However, the helium diffusion decrease both the $T$ and
$\mu$, the sound speed $c$ slightly in the convective envelope. So
the small spacings and separation ratios are similar with and
without helium diffusion.

In Fig. 4 the dash dot lines describe the differences of $c$, $T$
and $\mu$ between the model with both helium and metal diffusion and
the model without any diffusion. From Fig. 4, we can see that the
effect of metal diffusion on the $c$, $T$ and $\mu$ not only in the
convective envelope but also in the radiation interior. Due to
diffusion, helium and metal drift inward just below the convection
zone and decrease $\mu$ in the outer envelope. At the same time, the
depletion of $Z$ increase the opacity in the envelope, otherwise the
concentration decrease the opacity in the radiation interior. It
leads to lower temperature in the envelope and higher value in the
interior. From Fig. 4, we can see that the temperature is more
sensitive to the metal diffusion than other physical parameters. The
$\delta c/c$ is mainly dependent on the variation of $\delta T/T$.
Except the convective envelope, the sound speed $c$ is much larger
in the interior of the model. From  the expression of the sound
speed gradient in terms of the equation (16):
\begin{equation
\frac{dc}{dr} \propto  \frac{d(\frac{T}{\mu})^{1/2}}{dr}\\
=-\frac{1}{2}(\frac{T}{\mu^{3}})^{\frac{1}{2}}\frac{d\mu}{dr}+\frac{1}{2}\frac{1}{(T
\mu)^{\frac{1}{2}}}\frac{dT}{dr}
\end{equation}
 we find that the temperature $T$ is the dominate factor in the
 sound speed gradient in causing the differences between the models
 with and without metal diffusion. Due to $dT/dr$ is negative,
 $|dc/dr|$ is larger than that of model without metal
 diffusion in the radiation interior. So from equation (14), the
 small spacings are larger than other models. That are explained the
 variation of
 the internal structure including metal diffusion.

\section{Conclusions}

Taking into account the effects of helium and metal diffusion on
stellar evolution, we have presented a detailed modeling of the MOST
target: the star $\epsilon$ Eridani by fitting the available
observational constraints: effective temperature, luminosity, high
precision interferometric observational radius and metallicity. We
also consider the age ($\leq$ 1 Gyr) as a property of star to
constraint the models, which are the same as SD89.

According to our results, the location in the H-R diagram indicates
that the star $\epsilon$ Eridani has evolved little since its
arrival on the zero-age main sequence. Taking into account the
helium and metal diffusion, we find that the mean large spacings
$<\Delta\nu>$, which are averaged over $l$ = 0, 1, 2, 3 and $n$ =
10, 11, 12, ..., 30, is about 194 $\pm$ 1 $\mu Hz$.

In order to test the effect of helium and metal diffusion, we
construct three groups of models with the same mass but different
$Y_{i}$ and $Z_{i}$. Then, for the given chemical composition we
calibrate three models with the different types of diffusion which
are listed in Table 2. In our work we fixed the mixing length
parameter $\alpha$ = 1.70 and neglected convective overshoot. The
results show that the age of diffused models is about 1 Gyr, and be
younger than that determined by the models without diffusion.

Due to the effect of diffusion, helium and metal fall below the
outer convective zone and form a gradient. We use the ``second
differences" to test the depth of the convective zones. When metal
diffusion is considered, the convective zone deepens more quickly
and the metal gradient steepens more rapidly than the helium
gradient. That induce a stronger reflection of the sound waves
just below the convection zone, which explains the higher
amplitude of the peak related to the base of the convective zone
than that of pure helium diffusion.

The small spacings and frequency separation ratios have been used to
test the differences of internal structure in models with and
without diffusion. According to our results, the pure helium
diffusion hardly alter the internal structure in the young low-mass
models. Taking into account the metal diffusion, it mainly induce a
much higher temperature in the radiation interior, thereby the
higher sound speed in the interior of the model. Correspondingly,
the frequencies and large spacings are larger obviously than that of
models without metal diffusion. The variation of internal structures
between models with and without metal diffusion is increase
obviously alone with the increase of initial metallicity. So we
conclude that it is necessary to consider the metal diffusion in the
young main-sequence low-mass star.

\begin{acknowledgements}
 We are grateful to anonymous referee for his/her constructive
suggestions and valuable remarks to improve the manuscript. This
work was supported by The Ministry of Science and Technology
 of the People's republic of China through grant 2007CB815406,
 and by NSFC grants 10173021, 10433030, 10773003, and 10778601.
\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


All the little children know this story.
The voice is an arrow, felt in the body.
Such a long ear! Of course she heard them.
She heard, she heard them, three daughters, no sons, what's the use, what's a womb if it yields no name, the name, the womb is a means to a name, to a history, she heard them say history is dying, history is darkening, names are dissolving, all the stars falling she heard them say it, this body making only nameless vessels is cursed, this body is cancerous, see where she walks, watch for her shadow, don't touch her hand, if you're pregnant don't look at her, yes, she heard them, her ear growing longer, more sensitive, delicate, quivering, bleeding, an ear like a quiver, she heard them, those arrows, she heard them, she felt them, she heard them. She overheard.
Dhegdheer's story is the longest one.
It lasts all night, it keeps the watchman awake.
We too, who watch, are waiting for dawn.
I remember, the oldest daughter says, when my youngest sister was born. Another girl. My father walked out, silent, he went to the café. My grandmother, my father's mother, was so angry she locked herself in her room. She wouldn't bring my mother anything to eat. My mother lay in bed with the baby and cried. She called my name. I remember her face, her arm, a faint glimmer in the darkness of the room. Bread, she said. Take the money out of my purse. Outside the sun was a glare, the streets loud, my shadow stark and black, cut out with a pair of scissors.
Years later I learned that, during pregnancy, some of the baby's cells enter the mother's body. So the mother feeds the child, and she also eats the child, she takes in cells that remain in her body for decades. And when she is injured or ill, the cells of the child rush to the site of the damage.
All of me rushing to my mother then. My cells in her body rushing, I believe, to heal her. My cells on the street rushing to buy her bread. In the kitchen I made her a sandwich of white cheese. When I carried it to her, it glowed.
I knelt in that radiance. Eat, Mama. Eat.
Cannibal/ cannonball/ laughable/ animal/ fanciful/ fallible/ flammable/ radical/ natural/ lavender/ tamarind/ tarragon/ mandarin/ cardamom/ calamus/ cannibal.
Photography: adapted from Whenever You Need Me, I Will Be There, by Lotus Carroll.


text:
ONLINE - DREAM - Temporalities of Revolts. Hopes, projection and visions
23. Januar | 13:00
We are pleased to announce the 3rd cycle of the DREAM Seminar which will start on 23 January 2023. This new series is dedicated to the Temporalities of Revolts. Hopes, Projection and Visions.
Over the course of seven sessions to be held online between 23 January and 5 June 2023 we propose to explore the presence of the past and future in the present of the uprising. We will be listening to research on the projection patterns - heroes and heroines, icons and images to be confronted with; on the places of projection, which are places to be reached or conquered. Hopes may also be inscribed in the space in the form of the dreamed, possible or unattainable conquest of a "Winter Palace", a symbol for a popular victory and the installation of revolutionaries in the places of power. These figures of projection can also be declined in the form of an eschatology that allows the sacrifice or renders it acceptable. This will also be an opportunity to reflect on the notion of defeat, which is present in the shape of the echo of past defeats (linked in particular to Palestine). The people in revolt draw from these imaginaries possible futures and present battles. Finally, we will consider the question of archives as a place of activation of the past in the present.
To discuss all these issues, we will be pleased to welcome and hear from invited researchers and members of the DREAM team: Nayera Abdelrahman Soliman, Hashem Abushama, Charlotte Al-Khalili, Emma Aubin, Fadi A. Bardawil, Kmar Bendana, Kinda Chaib, Nibras Chehayed, Leyla Dakhli, Youssef El Chazli, Giulia Fabbiano, Fouad Halbouni, Mélanie Henry, Dina Heshmat, Alia Mossallam, Michèle Riot-Sarcey, Birgitte Stampe Holst, Maria-Nicola Stragapede, Josepha Wessels.
Please find attached the full programme of the seminar. Detailed information on the different sessions will be published on our Blog Hypotheses and on our social networks Facebook and Twitter.
Finally, we would like to wish you a happy new year 2023 and we hope to see many of you in our virtual conference room.
Dorothee Mertz
mertz ( at ) cmb.hu-berlin.de
16.01.23 DREAM_Seminar_Progra ... (pdf 1.22 MB)

redpajama_set_name: RedPajamaCommonCrawl


Calcium D-Glucarate enhances Phase II detoxification by inhibiting beta-glucuronidase. Calcium D-Glucarate also supports immune function and promotes healthy estrogen metabolism.
Take one capsule per day or as directed by your healthcare practitioner.


text:
Q: Database Design for a Questionnaire I have a database of 100-200 topics with 20 questions in each topic. Each question can have multiple parameters (max 7) and can go into multiple sets (max 20). The division of questions into sets is done manually. I have to store this into the database. I am thinking on following lines:
Make a table for storing the questions having the schema as:
topic_id, question_id,question,sets,parameters,correct_answer
sets column will store like 1,2,3,4..
parameters column will store like a,b,c,d..
I have not worked with multiple value fields before and I don't know if it will be feasible as I will have more than 4000 rows at some point.

A: Comma-separated value fields are difficult to use in selections and to maintain.  Instead it is better to use multiple tables.  Specifically, you would have a QuestionSets table (sets that questions belong to) and QuestionParameter table.
Questions would have

*

*question_id

*topic_id,

*question

*answer (is it multiple choice?)

Then you would have Sets/Parameters with ID and other values.  The mapping tables would reference both IDs
QuestionSets
question_id | set_id

redpajama_set_name: RedPajamaStackExchange


text:
What It's like to be a half-caste German Jew in Occupied Austria
There are lots of things I notice this Christmas that I've never noticed before. When my mother takes me shopping, for instance, which is only between the hours of three and five, there are certain village stores she will go into and certain stores she won't. And the stores she will not enter are usually the smarter ones, the fish shop and the cooperative, for instance, which are near the best inns like Franzi Wimmer's and have glossy portraits of the Führer prominently on show inside, while the shops she does enter are the cheaper ones, even the dirtier ones, like the baker whose bread is often stale and the dairy where the milk is often sour. They have pictures of the Führer on their walls too, of course, but smaller ones and not so often dusted. Some of them even have little specks of fly-shit on his face.
I'm puzzled by my mother's shopping choices. I take it that as we are from Berlin, we must be a cut above the rest, so we should be going to the best shops, not the worst. And why do we go only in the late afternoon? I know that other people like Jägerlein go at any time of the day. My mother doesn't explain these anomalies, and I sense I'm not supposed to know the real reason, although I'm still convinced it has to do with our being proper Germans, while the villagers are not. Nobody tells me where I've gone wrong. Nobody explains that my mother is a vicious and degenerate Jewess, that the best shops won't serve her, that in any case she's allowed to shop only between the hours of three and five so that decent Aryans shoppers can arrange to avoid the disgusting sight of her altogether.
My parents have always been bickering and crying (I think that's normal—what else do I know?), but they never openly mention this source of their troubles. Imagine, I can't recall ever being called a half-Jew yet, let alone a Yid, and perhaps I never have been. I don't even know what a Yid or half-Jew is. Sara does, of course; she knows all right. And so do the others. But not me. Why should I? I'm never allowed out to play with the village children, so they aren't going to tell me. And neither Jägerlein nor my mother is going to either. As for my brother and sisters—they're certainly not going to tell me what it's like to be called a half-Jew or a dirty Yid. Like rape victims, they never tell because they feel they're guilty.
Filed Under: General Tagged With: Austria, Christmas, Fuhrer, Germany, half-Jew, Nazi, Yid
Frau Kaminsky, a Habsburg, agrees to educate half-Jewish Children
Scouring the Vienna papers, my mother has learnt that a lady with the highest references is prepared to offer coaching in various subjects to private pupils of good family. Correspondence has revealed that this lady is Fraülein Hertha von Kaminsky, a former governess to some family of a distant branch of the Habsburgs, and Gabi has gone to Vienna (staying illegally with Helena before her marriage) to supplicate her help.
Acutely conscious that hers is not what a von Kaminsky might consider a good family, Gabi has abandoned subterfuge this time. Hoping that this dependent of the royal family will be no friend of the upstart Nazis, she has laid her petition frankly and humbly before Fraülein von Kaminsky, who is about as broad as she is tall, in her comfortable apartment on the Ring.She has ended with the words "I feel so guilty. It's all my fault that my children are being treated like this." Yes, Gabi like Ilse feels guilty. Guilty for being the victim that makes her children victims, while the Führer and his cronies who have brought her to this pass are proudly pinning medals on each other's chests and dreaming of a new Berlin—Germania, the Jew-free capital of their Jew-free Reich. (Most of them are also kind to dogs.)
Fraülein von Kaminsky is not a connection of the Habsburgs for nothing. She possesses a sense of noblesse oblige as well as that aristocratic disdain of the Nazis which Gabi had hoped for. So in the New Year she will be coming to teach the older children.
Filed Under: General Tagged With: Austria, Berlin, Frau Kaminsky, Fuhrer, Germania, governess, Jewish, Nazis, private education, Reich, Vienna, World War II
The Kaminsky Cure
The village we live in, Heimstatt, is lodged deep in the Alps, squeezed between the cliff-like mountains and a black and glacial lake that holds many bodies and many secrets, with more of both to come. For five months of the year the winter sun never makes it above the surrounding mountain tops, and when the merest sliver of it makes its first brief gleaming reappearance each spring, the villagers all come out of their houses to watch and celebrate. The chief business of this ancient place is its ancient quarry, the chief characteristics of its inhabitants inbreeding and goiters. People were living here in the Stone Age, and some of them still are.
I'm told it was snowing when I was born, and I believe it, because it's always snowing here in Heimstatt in February. Thick silent wodges of it, filling the somber daylight with their muffling presence. The mountains that stand like grim gravediggers round the coffin-shaped valley become invisible, and you can hardly even see the lake, which is frozen solid except for the swath the ferry crunches through the ice as it grinds its way across to the railway station on the other side. Gloomy and cold—it's not an auspicious way to start your life.
Filed Under: General Tagged With: Alps, Austria, Heimstatt, Nazis, wartime, World War II
Well here I am at five and three-quarters
It's Christmas 1939 in a little Austrian village that's now part of Hitler's Third Reich and I'm just beginning to notice things. Like what my brother and sisters are about and why my parents are often crying and my father usually shouting when he isn't crying. I think it has something to do with the war we're fighting, which according to the wireless is due to The International Jewish Conspiracy, whatever that is. But that's not all. I don't know it yet, but I was born at the wrong time and in the wrong place. [Read more…]
Filed Under: General Tagged With: Austria, fiction, half-Aryan, holocaust, Luthern, Nazis, Third Reich, war fiction, World War II
On the Line Between Memory and Invention Lies the Story by Kimberly Olson Fakih December 11, 2022
Six Thoughts on Historical Fiction by Don Zancanella, author of A Storm in the Stars August 8, 2022
Seeing Red – an essay by Margaret Hermes, author of The Opposite of Chance (available in paperback March 2022) April 20, 2022
In the Shadows of The Unknown Woman by Brooks Hansen October 18, 2021
Thoughts On Writing IN THE FIELD By Rachel Pastan August 3, 2021
Old Enough to Have Succeeded, but Also to Have Failed: on writing the short stories You Would Have Told Me Not To by Chris Coake available in paperback July 27, 2021 July 26, 2021
Delphinium Authors
1954 acceptance speech artists Austria autobiographical Books Booz Allen Hamilton bottoming out celebrity demotic Dostoyevsky dysfunctional Edward Snowden fame fiction fiction-writing Fitgerald Fuhrer George Elliot Germany Hemingway Historical Fiction holocaust imagination James Frey Jewish Karen Silkwood literature Memoir memoirist Middlemarch Nabokov Nazi Nazis Nobel Prize novelist novelists NSA Reading redemption Sobibor style World War II writers writing


text:
Construction of Hilton Praia is expected to begin in Cabo Verde in 2018
| Cabo Verde
The construction of the Hilton Praia hotel may begin in 2018, three years after the first stone of the first five-star hotel in the capital was laid, following an agreement signed on Wednesday between the Cape Verdean government and TRG Praia, of The Resort Group PLC, which is promoting the project.
The Resort Group's consultant, Victor Fidalgo, said that it was a "long and complex" process that began in 2013, with the acquisition of the site and licensing of the work by the Praia Municipal Council. The document that sets out the obligations and incentives negotiated between the Cape Verdean State and the company, he said.
Fidalgo said that there are procedures that must comply with the standards of the Hilton Worldwide chain, but added that the process will be concluded this year "so that Hilton can authorise the beginning of the work," according to the Inforpress news agency.
The Minister of Tourism and Transport and Minister of the Maritime Economy, José Gonçalves, said that signing the document allows Praia to become a "tourism, conference and business point" because, despite being the capital of the country, there is a lack of accommodation.
Hilton Praia is expected to create around 150 direct jobs and will have 201 rooms, as well as restaurants, bars, leisure and entertainment areas, common and private pools, a SPA, health club, convention centre and meeting rooms. (macauhub)
Kimberley Process Certification System comes into force on 1 October in Macau
Macao holdings of securities in lusophone world US$55.1 mln
Brazilian power infrastructure deal signed at Macao forum
Portugal's financial regulator lists Macao as relevant jurisdiction for local banks
Gaming and gambling employs over 58,000 people in Macau in 2019


To ensure fair competition in New Jersey's natural gas and electric markets, the New Jersey Board of Public Utilities (BPU) has established rules governing transactions by and between regulated utilities, such as New Jersey Natural Gas (NJNG) and their unregulated retail and energy affiliates, such as NJR Home Services and NJR Energy Services. Company Affiliate Relations, Fair Competition and Accounting Standards and Related Reporting Requirements (Affiliate Rules) require specific information be made publicly available.
This area of our Web site exists to comply with specific Affiliate Rules that require a means by which to notify interested parties of a transaction occurrence by, and between, NJNG and its retail and energy affiliates.
A complete copy of the Affiliate Rules along with additional information on energy competition in New Jersey can be found at the BPU Web site, http://www.bpu.state.nj.us/.
A current listing of New Jersey licensed energy providers can be found on the NJNG Web site.
Below is a list of NJNG transactions that will be posted to this site.
If shown in the listing below, NJNG has offered access to utility information, services and/or unused supply or capacity to one or more of its affiliates, and notice to non-affiliated market participants is made by way of this public posting.
If shown below, NJNG has offered access to surplus energy to one or more of its affiliates and notice to non-affiliated market participants is made by way of this public posting.
If noted below, NJNG has offered a discount, rebate or waiver of a charge, penalty or fee to one or more of its affiliates and notice to non-affiliated market participants is made by way of this public posting.
There are no offerings at this time.
If NJNG has offered non-customer, non-specific information to one or more of its affiliates, notice to non-affiliated market participants is made by way of this public posting.
Below is a listing of NJNG-transferred employees to one or more of its affiliates. This information is being provided publicly by way of this posting. Any changes will be posted to this site.
Below is a listing of NJNG affiliate companies, which is being provided publicly by way of this posting. Any changes will be posted to this site.
New Jersey Natural Gas Company Charity, Inc.
NJNG provides advertising, billing and collection services to its retail affiliate and that service may be provided to non-affiliated companies in the same line of business, subject to NJNG's determination that the necessary financial, operational and technical requirements have been met. Please contact the Senior Vice-President of Regulatory and External Affairs for NJNG at 732-938-1214 for additional information.


If you've got a question about your order, delivery or any other aspect of our service, you should be able to find the answer below. Simply click on the relevant question to reveal the answer. If you have a question about any of our products, visit our Product FAQs page. If you need any further help, then please get in touch with our Amazing Customer Care team and they will do their very best to help.
1. How do I place my AmazingCosmetics® order?
Find the AmazingCosmetics® item you wish to order using the search box or browsing the AmazingCosmetics® Shop. Where applicable, choose your perfect AmazingCosmetics® shade (find out how here) and click 'Add to basket'. Your browser will refresh and your basket at the top right of the page will show your items.
Either click 'Go to basket' or continue shopping to add more Amazing items to your basket. Add any further items in the same way and when you've finished shopping, click on the basket summary at the top right of the page.
2. Can I change my AmazingCosmetics® order?
You can ask, and we'll do our best, but please be aware that AmazingCosmetics® orders placed before 2pm are usually dispatched the same working day and so it may not always be possible.
Sorry, but we cannot add an item to your AmazingCosmetics® order. Once your payment has been processed, we are unable to make changes to it and you will need to place a new order. As standard delivery to the UK and Ireland is FREE, it will not cost you any more to place a second order for the item you forgot. If you place a second order and let us know quickly here, we'll do our best to ensure they are sent together so that you only receive one delivery.
4. Can I cancel my AmazingCosmetics® order?
You can, but please be quick. We aim to dispatch all AmazingCosmetics® orders placed before 2pm the same working day and so we may be unable to stop it from being dispatched to you.
However, you still have a legal right to cancel your contract with us at any time within 14 days without giving reason. The cancellation period expires 14 days from the day after you receive the products. To cancel your order, you must inform us in writing at: AmazingCosmetics® Unit A1, Lingard Court, Lingard Lane, Bredbury, Stockport. SK6 2QU. UK. Alternatively you can call our Amazing Customer Care Team on 0844 800 7661. You must also return the products to us as soon as reasonably practicable and at your own cost. You will receive a full refund of the price paid for the products.
5. Can I only order AmazingCosmetics® online?
You can order online in the AmazingCosmetics® Shop or if you prefer, you can visit one of our high street stockists such as Marks and Spencer. For further details, please view our stockists.
6. I forgot to use my promotion code, can I add it now?
Sorry, but you must enter a promotion code at the point you place your AmazingCosmetics® order.
7. What payment methods do you accept online?
Yes, we accept payments by PayPal on the AmazingCosmetics® website.
9. When will the payment go out of my account?
10. What is 'Verified by Visa' and MasterCard 'SecureCode'?
Verified by Visa and MasterCard SecureCode are services to help protect your card details when shopping online. They allow you to create your own password which only you know and you will be asked to use this every time you shop online with one of these cards. For more information about these services, visit Verified by Visa or MasterCard SecureCode.
11. Do your prices include VAT?
Yes unless stated otherwise. Any items purchased from the AmazingCosmetics® website are inclusive of VAT. This is a UK registered website and we have no legal obligation to offer VAT free shopping to customers shopping in the Channel Islands.
If you register and shop online as a professional Make-Up Artist or Salon/Spa, then prices will be quoted excluding VAT.
12. How much is delivery?
Standard delivery to the UK and Ireland is absolutely FREE. We also offer Next Day delivery (on orders placed before 2pm) for just £4.95.
13. Do you deliver AmazingCosmetics® to the Channel Islands?
Yes, we deliver AmazingCosmetics® to the Channel Islands.
14. Do you deliver AmazingCosmetics® to the Republic of Ireland?
Yes, we deliver AmazingCosmetics® to the Republic of Ireland.
15. Do you deliver AmazingCosmetics® overseas?
No, we are only able to deliver AmazingCosmetics® to the UK and Ireland. Please visit amazingcosmetics.com to find details of how to purchase from other countries.
16. How long will delivery take?
17. Can I get my AmazingCosmetics® order any quicker?
18. Can I select the day I want my AmazingCosmetics® order delivered?
19. Can I get my AmazingCosmetics® order delivered on a Saturday?
Sorry, whilst Royal Mail may deliver your AmazingCosmetics® order on a Saturday, we cannot guarantee delivery on a Saturday. Our Next Day delivery service does not include Saturdays and so an order placed before 2pm on a Friday with Next Day delivery would be delivered on Monday.
20. When will my AmazingCosmetics® order be dispatched?
21. Which courier do you use?
If you have selected Next Day Delivery, your AmazingCosmetics® order will be sent with DPD. All other orders will be sent via Royal Mail.
22. Can I track my AmazingCosmetics® order?
If you would like to track your order, please get in touch with our Amazing Customer Care team.
23. I still haven't received my AmazingCosmetics® order, where is it?
If your estimated delivery date has passed and you still haven't received your AmazingCosmetics® order, please get in touch with our Amazing Customer Care team and they will look in to it for you.
24. I've tracked my AmazingCosmetics® order online and it says 'delivered', but I haven't received it, what should I do?
Please get in touch with our Amazing Customer Care team and they will look in to it for you.
25. I missed my AmazingCosmetics® delivery, what should I do now?
26. Can I change my delivery address?
Please get in touch with our Amazing Customer Care team here explaining the reason you wish to return the product and they will let you know what to do next.
We will refund you within 14 days of your receiving your returned order and we will email you when your refund has been processed. The money may take 3-6 working days to show in your account. Unfortunately these timescales are dependent on your card issuing bank and are completely out of our control. Once we have issued the refund, there is nothing we can do to make this go back in to your account any quicker.
30. Have you got any Amazing offers?
To receive the latest Amazing offers and promotions, please sign up to receive our newsletter at the footer of this website.
31. Why hasn't the promotion code I used been applied to my AmazingCosmetics® order?
This could be because your order does not meet the Terms and Conditions with the code you are trying to use. Unless otherwise stated, the following Terms and Conditions apply to all promotion codes.
If you think your order meets our Terms and Conditions and the code still hasn't worked, please check that the code used has not expired. If you are still unsure, please get in touch with our Amazing Customer Care team.
32. What should I do if the item I receive is faulty?
If you think your AmazingCosmetics® order is faulty, please get in touch with our Amazing Customer Care team.
33. Part of my order is missing, will it get sent separately?
We're sorry you haven't received all of your order, please get in touch with our Amazing Customer Care team and they will look in to it for you.
34. You've sent me the wrong item, what should I do now?
We're sorry, mistakes do sometimes happen. If you've received the wrong item, please get in touch with our Amazing Customer Care Team and they will resolve it as quickly as possible for you.


Author of historical fiction: Sarah's Valley, Return to Sarah's Valley, The Widow's Walk. Two mystery series: Beryl Swallows, and The Mabel Wickles series.
Thanks for featuring Mabel, Murder, and Muffins! I almost didn't scroll to the end. Found your blog so interesting. I was an only child too!
#FF @JulieSeedorf @BarbaraJCoast @timhallbooks @abwrites @Sharonmierke @par2323 @NanciRathbun @PCSilvestri @aliceboatwright @NellMusolf @CozyCatPress #Write On!


Pictures of Dining room hutch with glass and carafe also decorative plant is created to be the inspiration of for you. This image was published on April 15, 2017 and published by this is fall into the category Interiors Design, the size of image is 1931 x 2997 and this post has 17 related images. If you have any questions please Contact Us. Hope it could inspire you, our beloved reader in nashuahistory.com, back to article please click Beautiful and Luxurious Dining Room Hutch.


text:
Upskill
Drive change
Menu Open menu Close menu
2021-2030 Strategy
Globally responsible programme
From 2002 to 2019, we provided over 205,400 hours of pro-bono engineering to our partners' projects around the world. Together we achieved a lot – increasing access to clean water, improved sanitation facilities, reliable energy resources and resilient built environments. You can find out more about some of these projects below.
We are proud of the impact our international placements had and they remain an important part of our history and the journey we went on to evolve into the movement we are today. But the number of people they've helped either directly, or indirectly, is relatively small compared to the size of the global challenges we face. We took time to assess our work and realised that we can positively affect many more lives by using our influence and educational programmes to encourage change on a much larger and strategic scale. As such our focus has moved from running individual pro-bono projects to creating systemic change. Learn more about our 2021-2030 strategy to put global responsibility at the heart of engineering, ensuring a safe and just future for all.
Better connected in Nepal
Many people in Nepal lack access to the internet. This means that they miss out on global knowledge, education, healthcare, communications and e-commerce.
Dry toilets in Peru
Two related problems were stopping Lobitos being a great place to live and a bigger draw for tourists: inadequate water supplies and poor sanitation.
Reinforced plaster in Bangladesh
Low-lying, Bangladesh is susceptible to flooding, cyclones and tidal surges. Battered by torrential rain and strong winds during the monsoon season, it is frequently hit by flash floods and landslides.
Off-grid renewables in Kenya
In east Africa, the electricity gap is being filled by small off-grid renewable-energy businesses who are providing power to rural communities.
Re-engineering urban spaces in Kenya
Kibera doesn't have enough toilets or adequate flood defences. When it rains heavily, homes are damaged and raw sewage mixes with drinking water supplies, spreading disease.
Clean water in Mexico
When the groundwater supply of Mexico's rural Guanajuato region was contaminated, it exposed 200,000 people to life-threatening pathogens.
Disaster resistant building in Rwanda
Rwanda sits on the East African Rift fault line. It suffers frequent, often deadly, earthquakes.
Pollution revolution in India
Every day 3 billion people cook over open fires or inefficient stoves. Breathing in the air they produce is equivalent to smoking two packets of cigarettes a day.
Diversity, equity and inclusion statement
Follow the Movement
We're a member association of
Engineers Without Borders UK is a registered charity in England & Wales (No. 1101849) and Scotland (No. SC043537) and is a company limited by guarantee (No. 04856607).


← Get Into the Spooky Spirit!
The hottest most anticipated show of the fall is back! With new arrivals and even more surprises introduced this season, The Walking Dead continues to amaze us. The core group has now split up, giving us multiple plots and new characters to obsess about, including a lion! We can count on one thing never changing, ZOMBIES! They will always find themselves playing survival of the fittest. Which makes us wonder, would we make in a world like The Walking Dead? Zombies aren't exactly an issue in our world now, but just to cover all the bases try practicing your survival skills at Dark Escape 4D. Remember, only the strong survive.


Nicolas Batum had 21 points and eight assists and Marvin Williams had 14 points and 12 rebounds for the Hornets, who wrapped up a seven-game road trip with an impressive victory with the help of O'Bryant.
Johnny O'Bryant was great. ... He gave us a big lift.
O'Bryant was signed Feb. 24 after playing on two 10-day contracts with Denver in January and February. He had seven points in the fourth quarter when the Hornets held off a late rally to win for just the fourth time in the last 14 games.
O'Bryant had a little inside knowledge after spending 20 days with the Nuggets, and it helped him Saturday with Kaminsky sidelined with a sprained left shoulder suffered Thursday in Phoenix.
Charlotte finished its longest road trip of the season with a 3-4 record.
The Nuggets came out flat after two impressive road wins in the middle of the week. Nikola Jokic led them with 31 points and 14 rebounds, while Danilo Gallinari scored 22 points.
Charlotte took the lead for good with a 17-0 run late in the first quarter and then scored the first 10 points of the third to go up 71-52.
The Hornets led by as many as 20 in the third before Denver made a run to get it under 10 on Mason Plumlee's three-point play with 7:13 left. Marco Belinelli answered with a corner 3-pointer - his only points of the game - to push the lead to 100-89.
Denver got within four with 4:33 left, but Charlotte scored nine straight, including a big 3-pointer by Walker, to go back up by 13 and closed it out at the line.
Hornets: Charlotte finished its longest road trip of the season with a 3-4 record. ... The Hornets held Denver to 45 percent shooting after Phoenix hit nearly 60 percent of its shots Thursday. ... Walker and Batum have combined to score at least 20 points in eight games this season.
Nuggets: G Gary Harris, the team's fourth-leading scorer, went without a point and missed the only shot he took. ... F Kenneth Faried missed his fourth straight game with low back soreness. He first hurt it against Brooklyn on Feb. 24 and hasn't played since. ... G Emmanuel Mudiay was back to third string after playing 18 minutes in Milwaukee on Wednesday.
Kaminsky, Charlotte's 7-foot center, is expected to miss several games. Kaminsky, who averaged 17.9 points a game since Feb. 1, was hurt in the fourth quarter of Thursday's loss to the Suns.
He will get an MRI done on the shoulder once the Hornets return home.
Hornets: Host the Indiana Pacers on Monday night.
Nuggets: Host the Sacramento Kings in a battle of playoff hopefuls on Monday night.


text:
Meeting With the Goddess: Notes from the First Symposium on Venus Science Enabled by Human Proximity
Izenberg, Noam and Lefland, Mallory and MacDonald, Alexander and Beauchamp, Patricia and Chai, Patrick and Cummings, Nick and Esty, Clark and Daniels, Matt and Duggan, Matt and Goods, Dan and Grinspoon, David and Landers, Jamie and Runyon, Kirby and Shelhamer, Mark and Tymofyeyeva, Ekaterina and Wallace, Mark and Worden, Pete and Yant, Marcella (2022) Meeting With the Goddess: Notes from the First Symposium on Venus Science Enabled by Human Proximity. California Institute of Technology , Pasadena, CA. (Unpublished) https://resolver.caltech.edu/CaltechAUTHORS:20220920-221751543
In July of 2022, the Keck Institute for Space Studies (KISS) hosted a symposium entitled "Science Enabled by Human Proximity to Venus." Convened to explore the potential science that could be enabled by human mission fly-bys of Venus while en route to Mars, the symposium conversation expanded to encompass the policy and social rationales for a dedicated human mission to Venus, as well as a new concept for a potential human mission to Venus—The Venus Back-Flip. This symposium summary, compiled by contributions from symposium participants listed at the beginning of this report, is the start of a broader discussion that is likely to become more and more relevant in the coming years as the multiple human space exploration capabilities under development provide potential opportunities to execute a human mission to Venus—whether en route to Mars or as a dedicated mission. This summary will outline some of the relevant options for Venus human fly-by and orbital missions, some of the new or enhanced science investigations that could be achieved in tandem with human fly-by or orbital missions, why integrating Venus into the overall Moon-to-Mars strategy may be valuable, how social and cultural activities might advance human missions to Venus, and why Venus may deserve its own journey of exploration independent of other destinations. This report is a summary of the discussions, observations, and ideas that were generated at the symposium. The summary is written primarily for three types of audiences: human spaceflight mission and campaign planners, Venus scientists and technical innovators, and individuals interested in the social aspects of organizing to promote the human exploration of Venus. The symposium revealed that Venus is a desirable human spaceflight destination in its own right. The compelling narrative of exploration combines planetary science at Venus, the search for life in its clouds, and an encounter with our sister planet that may shed light on our future climate.
Report or Paper (Report)
https://www.kiss.caltech.edu/symposia/2022_venus_science/index.html Related Item Symposium website
Izenberg, Noam 0000-0003-1629-6478
Beauchamp, Patricia 0000-0002-7859-1432
Grinspoon, David 0000-0002-2265-7551
Runyon, Kirby 0000-0001-6361-6548
Shelhamer, Mark 0000-0002-5040-6573
Tymofyeyeva, Ekaterina 0000-0001-5638-366X
Yant, Marcella 0000-0002-1499-8735
© September 2022. Study Report prepared for the W. M. Keck Institute for Space Studies (KISS). Team Leads: Noam Izenberg, Mallory Lefland, Alexander MacDonald With thanks to the support of the Keck Institute for Space Studies, including Tom Prince, Michele Judd, Janet Seid, Iryna Chatila, and Antonio Soriano. Additional thanks to Keith Miller, Robert Hurt, and Gordon Squires at Caltech/IPAC for the cover art, Bobak Ferdowsi and Maggie Handler for organizing support, and to Meg Rosenburg for copy editing. Presentations from the Symposium can be found at the Keck Institute for Space Studies: https://www.kiss.caltech.edu/symposia/2022_venus_science/index.html
Keck Institute for Space Studies
10.7907/68mv-np46
Iryna Chatila


"For Baby E and me, breastfeeding got off to a nightmarish start. Despite having taken classes and feeling confident in my role, still I struggled daily to get through his feeding times without melting into tears. It didn't take long for me to resort to pumping 8-10 times a day, bottle-feeding him so I could keep my sanity.
I took E to doctors and midwives, explained and re-explained our difficulties to professional breastfeeding counselors, read numerous articles, and ran in circles until I was ready to give up on the supposed "blessedness" of breastfeeding for good. After having endured nine weeks, I finally called La Leche League. Hearing my description of the pain, the lady soon exclaimed, "You need to see Meredith Wentzel! She'll help you solve this." I'd heard that line about several other "help routes" in the past and was not very hopeful. Giving Meredith a call, however, I felt immediately encouraged. Finally, someone didn't blame me for doing it wrong! She listened compassionately and soon came to my house for an observation.


Cross Match Technologies Inc., a global provider of biometric identity solutions, announced that David Ellison will lead product management and Shawn Mokhtari will be in charge of international integration.
Ellison has been named vice president, global product management. A former vice president of programs and product management for Vectronix Inc., an electro-optics supplier to the defense and homeland security markets, he brings diverse knowledge and expertise to this new position.
Ellison is responsible for the product planning and execution throughout the product lifecycle, including: gathering and prioritizing product and customer requirements, defining the product vision, and working closely with engineering, sales and marketing to ensure successful launch of new products.
Ellison graduated with a Bachelor of Science degree from the United States Naval Academy with concentrations in science, mathematics and engineering.
Mokhtari has been named vice president, international integration. In his most recent position, Mokhtari was operations program manager for Hewlett Packard's Global Business Unit. He worked closely with contract manufacturing and engineering teams in the U.S. and China and was responsible for the HP Touchpad product ramp-up and launch.
Mokhtari has extensive knowledge and experience in manufacturing and supply chain operations. For the past several years he has focused on international operations where he was responsible for several large-scale merger and post-merger factory and product launches with large global companies including Solectron and Flextronics.
Mokhtari is a member of Tau Beta Pi Engineering Honorary Society and has a Master's degree in engineering management and operations research from University of Missouri – Rolla.
"With Dave and Shawn's extensive knowledge, experience and leadership capabilities, Cross Match is well positioned to continue expansion of its worldwide relationships and implement the strategies necessary to meet both customer's needs and Cross Match business targets," said Fred Baradari, president, Americas and APAC at Cross Match Technologies.