The incident led to him grumbling about the other person's lack of good decision making (perhaps not in so many words). I mentioned that people doing random things is one reason to build slack into any system. Tolerance for errors helps a system be flexible.
Yesterday, I was reading a friends Facebook post where she mentioned that she would be getting new prescription lenses from her eye doctor because she needed to move to progressive lenses. I wrote back that progressive eye-glass lenses were like a miracle you could wear on your face. Mine allow me to drive, or watch TV or knit, or many other things that I would not be able to do with out them.
That got me to thinking about how humans were not create perfect. We may be made in God's image but apparently perfection was not something God felt should be included. Instead God gave us brains and creativity so that we can find ways to both work around our own imperfections and help others do the same.
I've needed glasses since I was 10. Hundreds of years ago a human figured out that a transparent lens could bend and focus light. Other humans figured out that this bending property could be used to bring things into focus for people with weirdly shaped or aging eyeballs. A miracle made by humans for other humans to wear on their face.
Flexibility in the system allowing me to function without perfect sight.
This evening I was driving home from my adventures visiting parts of Puget Sound that I had never been to before, and I stopped for food before heading home.
At the restaurant I misunderstood what the cashier was asking me and got charged less than I should have for my meal. After I was done eating, I realized what happened and tried to pay the remainder. The cashier thanked me but didn't accept my money. I suspect that is in part because the accounting software isn't really set up to deal with that situation and honestly. The fact that the cashier had the flexibility to deal with the situation meant that I feel affection for the restaurant and will certainly be back (and now that I understand the system, pay full price).
All of these encounters with flexibility contrast with some of the things I have seen in the news lately about systems being allowed to run amok with no apparent flexibility built in.
It reminds me of Jesus taking the Scribes and Pharisees to task for following rules but not the spirit that may have originally engendered the rules.
When people follow rules blindly and forget about the reasoning behind the rules it can lead to terrible disasters, to injury and death, to wounds that will never heal. I think that God built imperfection into humans, animal, and (as it says in the Book of Common Prayer) the vast expanse of interstellar space, galaxies, suns, the planets in their courses, and this fragile earth, our island home.
Imperfection and flexibility go hand-in-hand. When humans begin to believe they (or their rules) are perfect then their is no room for humans left in the system and it can grind us up-- using other people as the grinders.
In order to avoid being either the grinder or the grindee, God has give us a great gift. The gift of Grace. The gift to be messy and imperfect. The gift to make space for others to be messy and imperfect.
It is out of the mess and imperfections of our lives that some of the greatest love, inventiveness, and creativity can come.
We may long for perfection-- but that is not what God gave us in our incarnation. We are born imperfect and we die imperfect and if we let that bother us we lose sight of the messy flexibility that is our birthright.
Quotations are from 2007 PDF edition of the Book of Common Prayer, page 370.
This essay was originally published at the Episcopal Cafe in May 2017.


text:
\section{Introduction}

Degenerate oxygen-neon (ONe) cores with masses near the Chandrasekhar mass
can form in the evolution of $\approx \unit[8-10]{\ensuremath{\mathrm{M}_\odot}}$ single stars
\citep[e.g.,][]{Miyaji1980, Miyaji1987}, in interacting binary systems
with varying degrees of envelope stripping
\citep[e.g.,][]{Tauris2015b, Poelarends2017}, in binary systems with
an accreting ONe white dwarf (WD) \citep[e.g.,][]{Canal1976,
  Nomoto1991}, or as the result of the merger of two WDs
\citep[e.g.,][]{Saio1985b, Brooks2017d}.
When the core reaches a central density $\approx \unit[10^{10}]{\gcc}$,
exothermic electron captures on \neon[20] occur and lead to the
initiation of a deflagration wave (``flame'') that propagates outward.
The competition between the energy release from this flame and the
electron-capture reactions on its ashes determines whether this leads
to an explosion (resulting in partial or total disruption of the star)
or implosion (resulting in the formation of a neutron star (NS)).

This situation has long been known to be finely balanced
\citep[e.g.,][]{Nomoto1991, Canal1992}, though the general conclusion
by the end of the 1990s was in favor of collapse to a NS.  Recent
multidimensional simulations have reiterated that the outcome is
sensitive to modeling choices and reopened the possibility that at
least some cases may lead to a thermonuclear explosion (possibly also leaving a low-mass bound remnant) instead of
collapse to an NS \citep{Jones2016c, Leung2019b, Jones2019a}.  One of
the key ingredients in this modeling is the speed at which the flame
propagates.

\citet{Timmes1992}, hereafter TW92, calculated the physical properties
of conductively-propagated laminar burning fronts in high-density,
degenerate carbon-oxygen (CO) and ONe mixtures.  We repeat a similar
set of calculations using Modules for Experiments in Stellar
Astrophysics \citep[{\tt MESA};][]{Paxton2011, Paxton2013, Paxton2015,
  Paxton2018, Paxton2019}, but extend these results to a wider range
of compositions motivated by expectations from detailed models of the
internal composition of ONe WDs \citep[e.g.,][]{GarciaBerro1997b, Iben1997, Siess2006}.
Section~\ref{sec:methods} describes the methods we use to calculate
the laminar flame speeds.  Section~\ref{sec:tw92} reproduces the TW92\
results in both CO and ONe mixtures.  We then focus on the laminar
flame speeds in ONe mixtures under different conditions.
In Section~\ref{sec:trace-c} we show
how the flame speeds  are only mildly affected by the presence of small amounts of
\carbon[12], but in Section~\ref{sec:low-ye} demonstrate the
significant influence of the electron fraction (\ensuremath{Y_{\rm e}}) of the material.
Section~\ref{sec:tables} provides
tabulated flame speeds and a corresponding fitting function.
Section~\ref{sec:conclusions} briefly describes the implications for models of
the collapse of ONe cores.

\section{Methods}
\label{sec:methods}

We use {\tt MESA}\ revision r12115 \citep{MESA}.  The input files necessary
to reproduce our work are publicly available\footnote{\url{https://doi.org/10.5281/zenodo.3537874}}
and an illustration of this capability has been included in the test
suite case \texttt{conductive\_flame}.

We create an initial, spatially-uniform {\tt MESA}\ model with a temperature
$\ensuremath{T_{\rm b}} = \unit[3\times10^8]{K}$, specified density
$\rho_9 = \rho / (10^9\,\gcc)$, and a specified unburned composition.
These properties characterize the cold material into which the flame
will propagate.  So long as the upstream temperature is much less than
the downstream (post-burn) temperature of $\approx \unit[10^{10}]{K}$, the
temperature jump across the flame is approximately the same and
the initial temperature does not play an important role.
The total mass $M$ defines the size of the (Lagrangian) computational
domain.  Because the flame width $\lambda$ varies substantially with
density, our domain size must as well.  We always ensure that
$M/(\rho \lambda^3) \gg 1$, but typically choose this ratio to be
$\sim 100$ to limit the computational cost.  This also implies that
$\lambda \ll r$, so the flame is effectively planar.  In practice,
$M \sim \unit[10 - 10^5]{g}$.  The small size of the domain implies
that the pressure gradient due to gravity is negligible.  The inner
boundary is at $r = 0$.  The outer boundary has a fixed temperature
$\ensuremath{T_{\rm b}}$ and a fixed pressure equal to the initial pressure of the material.

We then insert a hot spot at the center with fractional size in mass
$\ensuremath{q_{\rm s}} = 3\times10^{-4}$ at a temperature $\ensuremath{T_{\rm s}} = \unit[8\times10^9]{K}$
(for CO mixtures) or  $\ensuremath{T_{\rm s}} = \unit[10\times10^9]{K}$ (for ONe mixtures).
This hot spot should have a size of order the flame width and a
temperature of order the post-burn temperature to ensure a steady-state flame.
If the hot spot is too small the flame will die.
If the hot spot is too large the flame will exhibit a de-accelerating transient.
With a well chosen spot size much smaller than the domain, once
the flame has propagated a few flame lengths, the initial condition
will be effectively erased.

\begin{figure} [!htb]
  \includegraphics[width=\columnwidth]{f01.pdf}
  \caption{Schematic of a steady-state flame. The fuel in the upstream material
           is initially heated by conduction until the temperature becomes large
           enough to ignite nuclear reactions. At the critical temperature,
           the energy generation rate equals the energy conduction term (heating equals cooling).
           The downstream material burns to its nuclear statistical equilibrium state.
           The entire structure, approximately isobaric, propagates into the upstream fuel with a unique speed and width.}
  \label{fig:flame}
\end{figure}

We define the location of the flame to be the location of the maximal
rate of nuclear energy release in the domain (i.e., peak nuclear heating, see Figure~\ref{fig:flame}).  We evolve the model
until the flame has propagated through 90\% of the domain and then
extract the steady-state flame properties.  By repeating this process for different
initial conditions, we calculate the laminar flame speed as a function
of $\rho_9$ and composition.
In Appendix~\ref{sec:convergence}, we
demonstrate that our results are insensitive
to the details of the initial conditions
and are numerically converged.

\subsection{Microphysics}
\label{sec:micro}

As discussed in TW92, the flame will have a width such that the
diffusion timescale across it is comparable to the timescale at which
nuclear reactions heat the material.  This argument leads to an
estimate of the flame speed,
\begin{equation}
  v_{\rm flame} \approx \left(\frac{D_{\rm th}\ensuremath{\epsilon_{\mathrm{nuc}}}}{e}\right)^{1/2}~,
  \label{eq:vflame}
\end{equation}
where $D_{\rm th}$ is the thermal diffusion coefficient, $\ensuremath{\epsilon_{\mathrm{nuc}}}$ is
a characteristic specific rate of energy generation from nuclear
reactions, and $e$ is a characteristic specific energy.  Therefore,
the speed of the flame is set by the energy generation rate as
determined from the nuclear network and the assumed thermal transport
properties of the degenerate plasma.

\subsubsection{Transport properties}

\begin{figure*}
  \includegraphics[height=6.6cm]{f02a.pdf}
  \hfill
  \includegraphics[height=6.6cm]{f02b.pdf}
  \caption{Comparison of conductive opacity for pure \oxygen[16]. The square points show the values using the routines from T00, which are similar those used in TW92.  The dashed line shows the values adopted in {\tt MESA}. The right panel shows the relative difference between the two sets of values.}
  \label{fig:kap-cond}
\end{figure*}

In {\tt MESA}\, the thermal conductivity of the degenerate electrons,
accounted for via a conductive opacity
$(\ensuremath{\kappa_{\mathrm{cond}}} \propto D_{\rm th}^{-1})$, comes from tables privately
communicated by A.Y.~Potekhin \citep[see Section A.3
in][]{Paxton2013}.  TW92\ describe in detail their implementation of
the transport properties; a substantially similar approach is adopted
in \citet{Timmes2000a}, hereafter T00.  The source code for the
transport properties assumed in these works is publicly
available.%
\footnote{\url{http://cococubed.asu.edu/code_pages/kap.shtml}}

Figure~\ref{fig:kap-cond} compares the conductive opacities over the
range of temperatures and densities considered in this paper.  The
left panel shows the T00 and MESA values of $\ensuremath{\kappa_{\mathrm{cond}}}$ and the right
panel their relative difference.  Both sources show similar density
scalings, but the T00 values scale less steeply with temperature such
that while the values agree at $\unit[10^9]{K}$, $\ensuremath{\kappa_{\mathrm{cond}}}$ is
higher by a factor $\approx 2$ at $\unit[10^8]{K}$ and lower by a
factor $\approx 1.5$ at $\unit[10^{10}]{K}$.  Since these variations
are not systematically in the same direction, their effect is
difficult to estimate, but given the scaling in
Equation~(\ref{eq:vflame}), variations in $\kappa_{\rm cond}$ at this
level correspond to $\approx 30\%$ variations in the flame speed.

\subsubsection{Nuclear reaction rates}

\begin{figure}
  \fig{f03a.pdf}{\columnwidth}{(a) CO mixture with $\ensuremath{X_{\mathrm{C}}} = 0.5$ at $\rho_9 = 6$.}
  \fig{f03b.pdf}{\columnwidth}{(b) ONe mixture with $\ensuremath{X_{\mathrm{O}}} = 0.6$ at $\rho_9 = 10$.}
  \caption{Effect of nuclear network size.  For each calculation, the
    flame location is shown as a function of time.  The legend lists
    the number of isotopes (``isos'') used and the flame speed (in
    \ensuremath{\rm km\,s^{-1}}) is indicated in parenthesis.  The thin solid line underlying
    the dashed line indicates the portion of the curve used to extract
    the flame speed.
    (The ``adaptive'' and ``495 isos'' curves overlap to within the line width.)}
  \label{fig:net-size}
\end{figure}

The currently applicable default inputs for nuclear reaction rates are
described in Appendix A.2 of \citet{Paxton2019}.  Rates are taken from
a combination of NACRE \citep{angulo99} and the Joint Institute for
Nuclear Astrophysics REACLIB library (default version, dated
2017-10-20) \citep{Cyburt2010}.  The {\tt MESA}\ screening corrections are
from \citet{Chugunov2007}, which includes a physical parameterization
for the intermediate screening regime and reduces to the familiar weak
\citep{Dewitt1973, Graboske1973} and strong \citep{Alastuey1978,
  Itoh1979} limits at small and large values of the plasma coupling
parameter.

Relatively large nuclear networks are required to fully capture the
energy generation rate in neutron-rich compositions at these
thermodynamic conditions. TW92\ illustrate the increase in flame
speed with increasing network size (their Table 5) and adopt a 130
isotope network.  We perform a similar exercise, using 3 built-in
{\tt MESA}\ networks (\texttt{approx21}, \texttt{mesa\_204},
\texttt{mesa\_495}), a network constructed with the same elements as
the TW92\ 130 isotope network (see their Table 1), and also an adaptive
network that automatically adds and removes isotopes and which settles
in at around 320 isotopes.  Figure~\ref{fig:net-size} shows the flame
location as a function of time for a set of runs for a fiducial CO
mixture (panel a) and a fiducial ONe mixture (panel b).  Networks of
more than 200 isotopes appear to be required before network size no
longer makes an appreciable difference in the flame speed.  This
result is consistent with \citet{Chamulak2007}, hereafter C07, who
found that for flames in CO mixtures a 430 isotope network gave speeds
up to $\approx 25\%$ greater than a 130 isotope network.  We run with
495 isotopes unless otherwise stated.

The JINA REACLIB polynomial fits to the reaction rate data end at
$\unit[10^{10}]{K}$ as do the tabulated partition functions used to
calculate the reverse rates and ensure detailed balance.  Above
$\unit[10^{10}]{K}$, {\tt MESA}\ fixes the rates to be their
$T = \unit[10^{10}]{K}$ values.  In some cases, especially for the ONe
flames, the temperature exceeds $\unit[10^{10}]{K}$ and the peak in
$\ensuremath{\epsilon_{\mathrm{nuc}}}$ occurs near the temperature threshold.  If the {\tt MESA}\
treatment underestimates the true peak of $\ensuremath{\epsilon_{\mathrm{nuc}}}$, then this can
lead to an underestimate of the flame speed.  (For example, if we
truncate the rates at $T = \unit[8\times10^{9}]{K}$, the ONe flame
in Figure~\ref{fig:net-size} has a speed of \unit[82]{\ensuremath{\rm km\,s^{-1}}}, a
$\approx 10\%$ reduction.)  However, we have physical reasons to
expect that this effect is not particularly large.  By
$\approx \unit[1.2\times10^{10}]{K}$ photodisintegration is strong
enough to decompose nuclei into neutrons, protons, and alpha
particles.  This is an endothermic process, meaning there is an upper
limit to how much more positive $\ensuremath{\epsilon_{\mathrm{nuc}}}$ can be achieved beyond the
place where {\tt MESA}\ truncates the rates.

Our results depend slightly on our adopted rate sources.  If we use
pure JINA REACLIB defaults (eliminating NACRE), the flame speeds
increase.  For the calculation shown in Figure~\ref{fig:net-size}, the
result with the 495 isotope net and only the JINA rates is
\replaced{
\unit[94.1]{\ensuremath{\rm km\,s^{-1}}} for the CO case and \unit[207]{\ensuremath{\rm km\,s^{-1}}} for the ONe
case.}{
\unit[207]{\ensuremath{\rm km\,s^{-1}}} for the CO case and \unit[94.1]{\ensuremath{\rm km\,s^{-1}}} for the ONe
case.}
These represent an approximately 5\% speed up.

Thus there is some systematic uncertainty from nuclear reaction rates in our results which is difficult
to characterize, but seems unlikely to be smaller than $\approx 10\%$.
We note that both the above caveats result in even faster flame speeds
than the ones we will report.
The open and reproducible nature of our work allows this problem to be
  easily revisited, enabling the impact of future experimental and theoretical progress in the relevant reaction rates to be quickly assessed.

\section{Comparison with past work}
\label{sec:tw92}

First, we consider CO mixtures.  Following TW92\, we select a
\carbon[12] mass fraction and put the remainder in \oxygen[16].
Figure~\ref{fig:tw92-co} compares our results with those of TW92.
Qualitatively, the agreement is good, and we reproduce the trends with
$\rho_9$ and $\ensuremath{X_{\mathrm{C}}}$.  Quantitatively, above $\rho_9 = 4$, our results
are $\approx 5-10\%$ slower, while below $\rho_9 = 4$, our results are
faster, up to $\approx 40\%$ at $\rho_9 = 1$.

Figure~\ref{fig:tw92-co} also compares the subset of our results that
overlap with C07. We agree well at $\ensuremath{X_{\mathrm{C}}} = 0.5$.  (It
is difficult to see the symbols as they overlap.)
We note, as do C07, that their
fitting function does not appear to do a good job of matching their
tabulated results.  Our results are slower at $\ensuremath{X_{\mathrm{C}}} = 1$,
though we note the C07 values also disagree with TW92\ and that
the primary focus of C07 was on $\ensuremath{X_{\mathrm{C}}} = 0.3 - 0.7$.

\begin{figure}
  \includegraphics[width=\columnwidth]{f04.pdf}
  \caption{Comparison with TW92\ for CO mixtures.  We compare our
    results (solid circles) to both their tabulated speeds (lighter, outlined symbols) and provided fitting function (line).  We do the same for
    the subset of conditions that have data from C07
    \citep{Chamulak2007}.  This is tabulated points and a fit for
    $\ensuremath{X_{\mathrm{C}}} = 0.5$, $\rho_9 \le 6$ and points for
    $\ensuremath{X_{\mathrm{C}}} = 1.0$, $\rho_9 \le 4$.}
  \label{fig:tw92-co}
\end{figure}

Next, we consider ONe mixtures.  Following TW92, we first select a
mass fraction \ensuremath{X_{\mathrm{O}}}\ of \oxygen[16].  When the mixture is not pure \oxygen[16], we
also choose a mass fraction 0.1 of \magnesium[24].  The remainder is
\neon[20].  Figure~\ref{fig:tw92-one} compares our results with those
of TW92.
There is qualitative agreement, with a trend (as in the CO case) that
our flame speeds are faster than TW92\ below $\rho_9 = 4$, up to
$\approx 50\%$ at $\rho_9 = 1$.  Above $\rho_9 = 4$ and for
$\ensuremath{X_{\mathrm{O}}} = 0.6$ and $\ensuremath{X_{\mathrm{O}}} = 1.0$, the agreement is within $\approx 10\%$ of
TW92.  For $\ensuremath{X_{\mathrm{O}}} = 0.8$, the agreement is somewhat worse and the speeds
are systematically $\approx 15\%$ lower above $\rho_9 = 6$.

This section demonstrates that our speeds are generally in good
agreement ($\approx 10\%$) with the results of past work.  Relative to
TW92, our calculations adopt a larger nuclear network (leading to
faster flames), but have slightly higher conductive opacities (leading
to slower flames).  In the end, these effects may offset somewhat.  We
have no reason to expect exact agreement with TW92\ as this is not an
identical calculation.

\begin{figure}
  \includegraphics[width=\columnwidth]{f05.pdf}
  \caption{Comparison with TW92\ for O/Ne/Mg mixtures.  We compare our
    results (solid circles) to both their tabulated speeds (lighter,
    outlined symbols) and provided fitting function (line).
    Composition labels appear in the same vertical order as their
    corresponding lines.}
  \label{fig:tw92-one}
\end{figure}

\section{Influence of trace carbon}
\label{sec:trace-c}

\begin{figure}
  \includegraphics[width=\columnwidth]{f06.pdf}
  \caption{Effect on flame speed of trace carbon in an ONe mixture.  Each point shows
    the ratio of $v_{\rm flame}$ with the indicated mass fraction of
    \carbon[12] to an equivalent calculation with no \carbon[12].}
  \label{fig:trace_C}
\end{figure}

ONe cores are formed after off-center carbon ignition occurs
and a convectively-bounded carbon deflagration propagates to the
center \citep[e.g.,][]{Farmer2015}.  Incomplete carbon burning that
occurs as the flame approaches the center can leave residual carbon
mass fractions of up to a few percent.  \citet{Schwab2019} performed
calculations of accreting ONe WDs including the presence of this
carbon and concluded that models are unlikely to reach carbon
ignition (and subsequently oxygen ignition and the formation of the
deflagration) below the threshold density for \magnesium[24] electron
captures.  Here we explore whether, once the deflagration is ignited,
the carbon affects the flame speed.

We select the $X_{\rm O} = 0.6$, $X_{\rm Ne} = 0.3$,
$X_{\rm Mg} = 0.1$, composition used by TW92\ and add a small amount of
\carbon[12], reducing the \oxygen[16] mass fraction accordingly.
Figure~\ref{fig:trace_C} shows the ratio of this flame speed to the
carbon-free speed shown in Figure~\ref{fig:tw92-one}.  The flame speed
increases, reflecting the additional energy release from fusion of
\carbon[12] (relative to the \oxygen[16] that it replaced).  However,
for carbon mass fractions of a few percent, the flame speed increases
only by $\approx 10\%$.  Therefore, we conclude that the presence of
small amounts of carbon is unlikely to have a significant effect on
the laminar flame speeds.

\section{Influence of lower electron fraction}
\label{sec:low-ye}

\begin{figure}
  \includegraphics[width=\columnwidth]{f07.pdf}
  \caption{Effect of lower \ensuremath{Y_{\rm e}}\ on flame speed in a primarily
    \oxygen[16]/\neon[20] mixture at $\rho_9 = 10$.  The different
    sequences of points achieve the $\ensuremath{Y_{\rm e}}$ values by varying the mass
    fractions of the indicated Ne isotope.}
  \label{fig:lowye-ne}
\end{figure}

\begin{figure}
  \includegraphics[width=\columnwidth]{f08.pdf}
  \caption{Effect of the density-dependent \ensuremath{Y_{\rm e}}\ on flame speed.  The
    composition is $\ensuremath{X_{\mathrm{O}}} = 0.6$ and $\ensuremath{X_{\mathrm{Ne}}} = 0.3$ (\neon[20]) with 0.05
    each of the $A =23$ and $A=24$ isotopes.  The upper panel shows
    the ratio of the flame speed in a calculation where these were
    transformed based on density to the neutron-rich isotopes
    \neon[23] and \neon[24] to one where they remained \sodium[23] and \magnesium[24].  The dashed
    lines show the locations of these composition shifts.  The electron fraction of
    the material is indicated in the lower panel.}
  \label{fig:lowye}
\end{figure}

Detailed models of ONe WDs do not give compositions that are only
\oxygen[16], \neon[20], and \magnesium[24].  Several neutron-rich
isotopes are typically present at mass fractions of a percent or more,
meaning that material is expected to have $\ensuremath{Y_{\rm e}}$ significantly below
the $\ensuremath{Y_{\rm e}} = 0.5$ value of a \oxygen[16]/\neon[20]/\magnesium[24]
mixture.  Table~\ref{tab:siessx} summarizes the abundances in the ONe
core of a representative stellar model from \citet{Siess2006}.  This
mixture has $\ensuremath{Y_{\rm e}} \approx 0.49$. See their Section 5 for an explanation
of this core nucleosynthesis.

\begin{deluxetable}{lR}
  \tablenum{1}
  \tablecolumns{2}

  \tablecaption{Approximate core composition for the $Z = 0.02$ $\unit[9.5]{\ensuremath{\mathrm{M}_\odot}}$ model of \citet{Siess2006}.
    \label{tab:siessx}}
  \tablehead{
    \colhead{Isotope} & \colhead{Mass Fraction (\%)}}
  \startdata
  \carbon[12]    & \approx 1.0 \\
  \oxygen[16]    & \approx 55 \\
  \neon[20]      & \approx 30 \\
  \neon[21]\tablenotemark{a}  & \approx 0.8 \\
  \neon[22]      & \approx 0.7 \\
  \sodium[23]\tablenotemark{a}    & \approx 5.5 \\
  \magnesium[24]\tablenotemark{a} & \approx 3.3 \\
  \magnesium[25]\tablenotemark{a} & \approx 1.5 \\
  \magnesium[26] & \approx 0.9 \\
  \aluminum[27]\tablenotemark{a} & \approx 0.7
  \enddata
  \tablenotetext{a}{This model has a central density $\approx 7 \times \unit[10^7]{\gcc}$.  Indicated isotopes can undergo additional electron captures as the density increases towards $\approx \unit[10^{10}]{\gcc}$, the density at which the oxygen deflagration is expected to form.}
\end{deluxetable}

As the core slowly grows and its density increases
further, the Fermi energy of the
degenerate electrons rises.  Electron-capture reactions on a given
isotope become energetically favored when material exceeds its
threshold density.%
\footnote{The energetics of these weak reactions are critical for
  understanding the thermal evolution of SAGB cores and accreting ONe
  WDs \citep[e.g.,][]{Jones2013, Schwab2015,Schwab2017a}.}
In Table 1, we indicate isotopes where these electron captures are
likely to occur before the formation of the oxygen deflagration
(meaning that their threshold densities are below the threshold
density of \neon[20], which is $\approx\unit[10^{10}]{\gcc}$).  In
what follows, we focus on the most abundant of these isotopes,
\sodium[23] and \magnesium[24].  The effective threshold density for
\sodium[23] is $\approx \unit[1.6\times10^9]{\gcc}$ and for
\magnesium[24] is $\approx \unit[4\times10^9]{\gcc}$.  The timescales
for the electron capture reactions are typically shorter that the
evolutionary timescale of the object, so they are expected to
completely convert the parent isotope to its daughter.

The electron captures imply that \ensuremath{Y_{\rm e}}\ spatially varies through the
core, with \ensuremath{Y_{\rm e}}\ becoming lower at higher density.  By time the
deflagration forms and begins to propagate, electron captures have
already completely converted the \sodium[23] to \neon[23] and the
\magnesium[24] to \neon[24] over the inner $\approx \unit[0.2]{\ensuremath{\mathrm{M}_\odot}}$
of the star.\footnote{A representative \ensuremath{Y_{\rm e}}\ profile as a function of
  mass is shown in Figure~11 of \citet{Schwab2017a}.  One caveat is
  that if a large core convection zone were to develop, as happens in
  models adopting the Schwarzschild criterion for convection
  \citep[e.g.,][]{Miyaji1980}, the central region would likely be
  homogenized.}  For the mixture in Table~\ref{tab:siessx}, this
further reduces $\ensuremath{Y_{\rm e}}$ to $\approx 0.485$.

In a concluding comment, TW92\ note that $\ensuremath{Y_{\rm e}} < 0.5$ is expected and
mention two calculations including reduced $\ensuremath{Y_{\rm e}}$ in the form of
\neon[22].  They report that for a flame in CO with $\ensuremath{Y_{\rm e}} \approx 0.498$ the speed
decreased by $\approx 5\%$ and for a flame in ONe with $\ensuremath{Y_{\rm e}} = 0.48$ the
speed decreased by $\approx 30\%$.  For CO flames, the effect of
\neon[22] was studied by C07. They found the
opposite sign of the effect, with a \neon[22] mass fraction of 0.06
leading to a $\approx 30\%$ increase in the flame speed.

To quantify the effect of lower \ensuremath{Y_{\rm e}}, we calculated flame speeds at
$\rho_9 = 10$ with a variable amount of neutron-rich material.  We
performed a set of calculations using each of \neon[22], \neon[23],
and \neon[24].  In all cases, the mixture had a mass fraction 0.6 of
\oxygen[16] with the remaining material being \neon[20].
Figure~\ref{fig:lowye-ne} shows the significant impact of the neutron
richness, with the flame speed relative to that at $\ensuremath{Y_{\rm e}} = 0.5$
doubling by $\ensuremath{Y_{\rm e}} \approx 0.488$.  The sequences with the different
isotopes overlap, indicating the speedup is largely independent of the
neutron source.

The small change in $\ensuremath{Y_{\rm e}}$ does not significantly affect the internal
energy or thermal conductivity, but does lead to a significant change
in \ensuremath{\epsilon_{\mathrm{nuc}}}\ as the initial source of extra neutrons opens additional
energy producing reaction channels.  We examined the peak values of
$\ensuremath{\epsilon_{\mathrm{nuc}}}$ in the calculations shown in Figure~\ref{fig:lowye-ne} and
confirmed that the increasing flame speed is due to an increasing
\ensuremath{\epsilon_{\mathrm{nuc}}}\ at lower \ensuremath{Y_{\rm e}}\ and that it quantitatively follows the
expectation from Equation~\eqref{eq:vflame}.

To illustrate that this implies a density-dependent enhancement of the
flame speed over the TW92\ result, we construct two sets of models that
initially have a mass fraction $X_{23} = 0.05$ of $A = 23$ elements
and $X_{24} = 0.05$ of $A = 24$ elements.  In one, the $A=23$ material
is always \sodium[23] and the $A=24$ material is always
\magnesium[24].  In the other, the spatially-uniform composition is
selected differently depending on the chosen $\rho_9$.  The $A=23$
material is \sodium[23] if the density is below its threshold density
and \neon[23] if it is above it, while the $A=24$ material is
\magnesium[24] if the density is below its threshold density and
\neon[24] if it is above it.  We then run these models
and extract their flame speeds.

Figure~\ref{fig:lowye} compares these two sets of calculations by
showing the ratio of the flame speed in the case where the initial
material has electron captured to the case where it has not.  Above
both threshold densities, where $\ensuremath{Y_{\rm e}}$ has fallen to $\approx 0.49$,
the flame is $\approx 80\%$ faster.

\section{Fitting Formula}
\label{sec:tables}

To allow this important effect to be incorporated in hydrodynamics
calculations, we provide a simple fitting function like that of TW92,
but including $\ensuremath{Y_{\rm e}}$ as an additional parameter.  As shown in
Figure~\ref{fig:lowye-ne}, the flame speed varies with $\ensuremath{Y_{\rm e}}$
approximately independently of the neutron source.  Therefore, we run
a set of calculations for \oxygen[16] / \neon[20] / \neon[23]
mixtures.  We use densities $\rho_9 = \{1,2,4,6,8,10,12,14\}$,
\oxygen[16] mass fractions $\ensuremath{X_{\mathrm{O}}} = \{0.5, 0.6, 0.75\}$, and select
\neon[23] mass fractions such that
$\ensuremath{Y_{\rm e}} = \{0.485, 0.490, 0.495, 0.500\}$.  Figure~\ref{fig:final-v}
plots the results.

\begin{figure}
  \includegraphics[width=\columnwidth]{f09.pdf}
  \caption{Flame speeds used to generate the fit given by
    Equation~\eqref{eq:fit}.  Point shape indicates $\ensuremath{Y_{\rm e}}$ and point
    color indicates \ensuremath{X_{\mathrm{O}}}.  The dashed black curves show the fitting
    function.}
  \label{fig:final-v}
\end{figure}

\begin{figure}
  \includegraphics[width=\columnwidth]{f10.pdf}
  \caption{Relative error between calculated points and the fit.
    Point symbols are the same as in Figure~\ref{fig:final-v}. }
  \label{fig:final-err}
\end{figure}

At $\ensuremath{Y_{\rm e}} = 0.5$, the flame speed always increases with increasing
oxygen abundance (as found in TW92).  However, in our results at lower
\ensuremath{Y_{\rm e}}, this is no longer true.  Incorporating the effect of $\ensuremath{X_{\mathrm{O}}}$ in the
fit would require something beyond the power-law scaling used in the
fit of TW92. Given the relatively weak dependence on \ensuremath{X_{\mathrm{O}}}, we circumvent
this complication and propose the following simple fitting function
that includes only $\rho_9$ and \ensuremath{Y_{\rm e}}:
\begin{equation}
  \label{eq:fit}
  v_{\rm flame}  = 16.0 \,\rho_9^{0.813} \left[1 + 96.8 \,(0.5 - \ensuremath{Y_{\rm e}})\right]\;{\rm km\,s^{-1}} ~.
\end{equation}
As shown in Figure~\ref{fig:final-err}, the fit agrees with the
calculated points within 10\% relative error at $\rho_9 > 4$, with the
maximum error growing to a 30\% underestimate at $\rho_9 = 1$.  This
fitting function will also do a worse job in pure oxygen mixtures (a
relative error $\approx 30\%$ for the $\ensuremath{X_{\mathrm{O}}} = 1$ points shown in
Figure~\ref{fig:tw92-one}), but such pure mixtures are unlikely to
arise in astrophysical contexts.  If a more precise reproduction of
our results is desired, the flame speed values are provided in Table~\ref{tab:final-grid},
allowing direct interpolation in our results.

\begin{deluxetable*}{llllllllll}
  \tablenum{2}
  \tablecolumns{10}

  \tablecaption{Flame speed (in \ensuremath{\rm km\,s^{-1}}) for models described in Section~\ref{sec:tables} and shown in Figure~\ref{fig:final-v}.
    \label{tab:final-grid}}
  \tablehead{
         \colhead{\ensuremath{X_{\mathrm{O}}}} & \colhead{\ensuremath{Y_{\rm e}}} & \multicolumn{8}{c}{$\rho_9$} \\
& & \colhead{1}  & \colhead{2} & \colhead{4} & \colhead{6} & \colhead{8} & \colhead{10} & \colhead{12} & \colhead{14}}
  \startdata
0.50 & 0.485 & 53.8 & 83.5 & 128 & 167 & 212 & 256 & 296 & 333 \\
0.50 & 0.490 & 40.1 & 65.8 & 104 & 137 & 170 & 206 & 241 & 273 \\
0.50 & 0.495 & 27.2 & 46.1 & 75.6 & 102 & 126 & 150 & 178 & 205 \\
0.50 & 0.500 & 15.9 & 26.3 & 45.0 & 62.6 & 79.8 & 96.4 & 113 & 132 \\
0.60 & 0.485 & 50.7 & 77.7 & 121 & 160 & 208 & 254 & 295 & 334 \\
0.60 & 0.490 & 36.2 & 60.3 & 98.9 & 133 & 167 & 206 & 242 & 277 \\
0.60 & 0.495 & 25.4 & 43.6 & 73.5 & 100 & 126 & 153 & 182 & 211 \\
0.60 & 0.500 & 15.7 & 26.1 & 45.3 & 63.6 & 81.8 & 99.6 & 117 & 138 \\
0.75 & 0.485 & 51.2 & 75.1 & 115 & 154 & 204 & 251 & 294 & 334 \\
0.75 & 0.490 & 35.0 & 56.2 & 93.1 & 127 & 165 & 206 & 245 & 282 \\
0.75 & 0.495 & 23.9 & 40.7 & 70.6 & 99.0 & 127 & 157 & 190 & 221 \\
0.75 & 0.500 & 15.6 & 26.1 & 45.9 & 65.8 & 86.0 & 106 & 126 & 150 \\
\enddata
\tablecomments{A machine readable version of this data is provided.}
\end{deluxetable*}

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

Using {\tt MESA}\ calculations that resolve the structure of
conductively-propagating deflagrations, we calculated laminar flame
speeds in oxygen-neon mixtures.  These speeds are a necessary
ingredient in simulations of the final stages of electron-capture
supernovae and accretion-induced collapse.

We demonstrated that the values of $\ensuremath{Y_{\rm e}} \approx 0.48-0.49$ expected in
these objects lead to an increase in the flame speed by a factor of
$\approx 2$ over that at $\ensuremath{Y_{\rm e}} = 0.5$, the value assumed in
the widely-used prescription of \citet{Timmes1992}.
The low $\ensuremath{Y_{\rm e}}$ is due to the nucleosynthesis during the helium and carbon
burning phases that preceded the formation of the ONe core and to
subsequent electron captures on isotopes initially present in the ONe
core (most importantly \sodium[23] and \magnesium[24]) that occur as
the core grows.  As shown in Figure~\ref{fig:lowye}, this implies that
the realized enhancement is density-dependent and most significant
for $\rho \gtrsim \unit[4\times10^9]{\gcc}$ (i.e., above the
\magnesium[24] threshold density).

Full star hydrodynamics simulations that follow the propagation of the
deflagration through the ONe core do so by including a sub-grid model
for the flame.  These models enhance the laminar speed by including a
sub-grid model of the flame-turbulence interaction (which allows for a
larger, non-planar area to undergo burning), such that the laminar
speed is only a lower limit. Eventually, this speed becomes irrelevant
once the turbulence is fully developed, as a turbulent deflagration no longer
depends on the laminar speed.  In Section~\ref{sec:tables}, we
provide a tabulated set of laminar flame speeds as well as a
convenient fitting function.  These are suitable for incorporation
into sub-grid flame models.

Figures 4 and 5 in \citet{Jones2016c} show the laminar and turbulent
flame velocities in their 3D hydrodynamic simulations.  Typically,
these flames remain laminar for $\approx \unit[0.4]{s}$, corresponding
to $\approx \unit[100]{km}$ of flame propagation.  Typically, the inner
$\approx \unit[200]{km}$ is above the \magnesium[24] threshold density
and thus at the lowest \ensuremath{Y_{\rm e}}.  Therefore, we believe the factor of 2
speedup is representative of what will be realized in practice.  The
more rapid release of energy associated with a faster flame pushes
models in the direction of being more likely to explode (meaning less
likely to form a neutron star).  The full implications of our results
await the incorporation of this updated prescription in
multidimensional models.

\acknowledgments

We thank Sam Jones, Pablo Marchant, Bill Paxton, and Fritz R\"{o}pke for helpful conversations.
We thank the referee for a useful report.
This work benefited from the May 2019 Lorentz Center program
Electron-Capture-Initiated Stellar Collapse.  We are grateful to Zo\"{e}
Weber-Porter for performing some exploratory calculations of this
problem as part of her UC Santa Cruz undergraduate thesis.
We acknowledge use of the lux supercomputer at UC Santa Cruz, funded by NSF MRI grant AST 1828315.
We thank Brant Robertson for the rapid and friendly technical support that enabled us to make use of this machine.
This research  was supported by the National Science Foundation (NSF) under the Software Infrastructure
for Sustained Innovation program grants (ACI-1663684, ACI-1663688, ACI-1663696).
JS is supported by the A.F. Morrison Fellowship in Lick Observatory.
RF is supported by the Netherlands Organization for Scientific Research (NWO)
through a top module 2 grant with project number 614.001.501 (PI de Mink).
This research was also supported at ASU by the NSF under grant PHY-1430152 for the
Physics Frontier Center "Joint Institute for Nuclear Astrophysics—Center for the Evolution of the Elements" (JINA-CEE).
This research made extensive use of the SAO/NASA Astrophysics Data System (ADS).

\software{
{\tt MESA} \citep{Paxton2011, Paxton2013, Paxton2015, Paxton2018, Paxton2019},
\texttt{MESASDK} 20190830 \citep{mesasdk},
\texttt{sig99} \ \url{http://cococubed.asu.edu/code_pages/kap.shtml},
\texttt{matplotlib} \citep{hunter2007},
\texttt{NumPy} \citep{walt2011},
\texttt{py\_mesa\_reader} \citep{pmr},
\texttt{MesaScript} \citep{MesaScript}
}

redpajama_set_name: RedPajamaArXiv


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redpajama_set_name: RedPajamaCommonCrawl


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text:
Скво-Лейк () — город в округе Айтаска в штате Миннесота (США).

Географическое положение
По данным Бюро переписи населения США город имеет общую площадь в 2,15 км² (2,07 км² — суша, 0,08 км² — вода). Он расположен между двумя озёрами — Раунд-Лейк и Нэйчерс-Лейк.

Через город проходит  .

Население

В 2010 году на территории города проживало 107 человек (из них 50,5 % мужчин и 49,5 % женщин), насчитывалось 39 домашних хозяйств и 26 семей. На территории города было расположено 63 постройки со средней плотностью 28,6 построек на один квадратный километр суши. Расовый состав: белые — 46,7 %, коренные американцы — 51,4 %.

Население города по возрастному диапазону по данным переписи 2010 года распределилось следующим образом: 33,6 % — жители младше 21 года, 51,5 % — от 21 до 65 лет и 15,9 % — в возрасте 65 лет и старше. Средний возраст населения — 35,9 лет. На каждые 100 женщин в Скво-Лейк приходилось 101,9 мужчин, при этом на 100 совершеннолетних женщин приходилось уже 87,5 мужчин сопоставимого возраста.

Из 39 домашних хозяйств 66,7 % представляли собой семьи: 36,9 % совместно проживающих супружеских пар (12,8 % с детьми младше 18 лет); 28,2 % — женщины, проживающие без мужей, 2,6 % — мужчины, проживающие без жён. 33,3 % не имели семьи. В среднем домашнее хозяйство ведут 2,74 человека, а средний размер семьи — 3,23 человека. В одиночестве проживали 23,1 % населения, 7,7 % составляли одинокие пожилые люди (старше 65 лет).

В 2015 году из 75 человек старше 16 лет имели работу 43. В 2014 году средний доход на семью оценивался в  $, на домашнее хозяйство — в  $. Доход на душу населения —  $ в год.

Примечания

Ссылки

Города округа Айтаска
Города Миннесоты

redpajama_set_name: RedPajamaWikipedia


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text:
About 8,000 CT exchange customers didn't pay first bill
by Arielle Levin Becker February 22, 2016 @ 4:00 pm Updated March 4, 2022 @ 10:50 pm
The Access Health CT storefront in New Britain. (File photo) Arielle Levin Becker / CTMirror.org
About 8,000 people who signed up for coverage through the Connecticut's health insurance exchange missed the deadline for their first payment and lost coverage, exchange CEO Jim Wadleigh said Monday.
"This number is bigger than we were anticipating," Wadleigh said. Just over 116,000 people signed up for private insurance through Access Health CT, the state's exchange, during the open enrollment period that ended Jan. 31. "The fact that all these customers have not made their first payment was kind of a shock to even us."
People generally must make their first payment within 30 days of getting the bill.
Wadleigh said it's possible that a similar number of people failed to make their first payment last year, but the exchange didn't have the data to know.
The consequences could be steeper this year: While the exchange last year allowed people to sign up for coverage outside the open enrollment period without checking whether they had a reason that would have qualified them to do so, Access Health is following tighter rules for off-season signups this year. That means that people who didn't pay their first bill won't be eligible to sign up again, unless they go through a change in circumstances that affects their coverage, such as getting divorced or losing a job.
Still, Wadleigh said some people could potentially gain coverage if they didn't pay because of problems with their bill, such as if it didn't include financial assistance they were entitled to receive, or if they didn't receive a bill.
Separately, about 17,000 customers must still verify information reported on their applications to maintain their coverage or federal financial assistance. Customers have 90 days to provide information on their income, citizenship or other qualifications in cases in which the information they reported did not match information available through federal sources. It's not clear how much overlap there is between the approximately 8,000 who didn't make their first payment and the 17,000 who haven't yet verified needed information.
Because the deadline for signing up for coverage was Jan. 31, some customers are still within the window to pay their first bill.
"We're trying to quickly course-correct and make sure everybody understands that there's a little bit more to do to finish the enrollment," Wadleigh said.
While people have 30 days to make their first payment, those who do get a longer grace period – 90 days – to make subsequent monthly payments before their coverage can be cut off.
Tagged: Access Health CT, Affordable Care Act, insurance
Arielle Levin Becker
alevinbecker@ctmirror.org
Arielle Levin Becker covered health care for The Connecticut Mirror. She previously worked for The Hartford Courant, most recently as its health reporter, and has also covered small towns, courts and education in Connecticut and New Jersey. She was a finalist in 2009 for the prestigious Livingston Award for Young Journalists, a recipient of a Knight Science Journalism Fellowship and the third-place winner in 2013 for an in-depth piece on caregivers from the National Association of Health Journalists. She is a 2004 graduate of Yale University.
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The Fluffy Unicorns believe they're like Rosa Parks
Posted on January 6, 2016 by ann summers
By ann summers
The Oregon Bird Sanctuary Siege continues and Fluffy Unicorn remains in charge despite being surrounded by Federal minions. The question the militant group now asks is whether they should be treated like Rosa Parks even though they are armed with assault rifles and snacks. Liberating public land for private ownership and exploitation is a recurring Western theme with some interesting questions related to the 19th Century demography of the United States. Counterfactual history will be taking a beating over the coming week(s).
There is no truth to the rumor that the Unicornists will demand that they be designated a tribally based self-governing homeland called bantustan, although it now seems possible that for the Department of Homeland Security the Bush 43 administration had the South African definition of homeland in mind.
On a related development there is no truth to the rumor that the occupiers will be submitting to DNA testing or subscribing to Ancestry to determine their eligibility for oppressed status. Apparently, essentialist philosophies will also be taking a beating in the coming weeks.
And despite the presence of many F-150 pickups, the Rolls Royce of American trucks, there are less than 93, quashing any rumors of the occupiers' fealty to the Rancho Rajneesh
The occupation reached a fifth day Wednesday with no end in sight to the conflict that started as a peaceful protest in support of two local ranchers sent to prison for setting fires on federal land. Bundy, (son of ) a Nevada rancher, and more than a dozen supporters took over a bunkhouse and say they won't leave until Dwight and Steven Hammond are freed from federal prison.
Bundy also wants federally owned land in Harney County returned to the people who live there, saying his group was sifting through property records to find instances of federal officials seizing land from private owners.
Earlier Wednesday, Bundy compared the ranchers' occupation of the refuge to the civil rights battle waged by Rosa Parks.
"We are doing the same thing as Rosa Parks did," Bundy tweeted. "We are standing up against bad laws which dehumanize us and destroy our freedom."
My open letter to @Ammon_Bundy. I think you accidentally sleep tweeted that you are like Rosa Parks. https://t.co/Ix7EEnjM0l
— Shaun King (@ShaunKing) January 6, 2016
The term "eminent domain" was taken from the legal treatise De Jure Belli et Pacis, written by the Dutch jurist Hugo Grotius in 1625, which used the term dominium eminens (Latin for supreme lordship) and described the power as follows:
"… The property of subjects is under the eminent domain of the state, so that the state or he who acts for it may use and even alienate and destroy such property, not only in the case of extreme necessity, in which even private persons have a right over the property of others, but for ends of public utility, to which ends those who founded civil society must be supposed to have intended that private ends should give way. But it is to be added that when this is done the state is bound to make good the loss to those who lose their property."
Some U.S. states use the term appropriation (New York) or "expropriation" (Louisiana) as synonyms for the exercise of eminent domain powers.
This entry was posted in American History, Breaking News, Celebrity, Civil Liberties, Crime, DHS, Fascists/Corporatists, FBI, Free Speech, Green, History, Humor, Jurisprudence, Justice, Law Enforcement, Libertarians, Media, Nazis/Nazism, Neoconservatives, Oregon, Philosophy, Political Science, Politics, Racism, Tea Party, Terrorism, Terrorists, Uncategorized, United States and tagged Cliven Bundy, Law Enforcement, Republicans, Terrorism. Bookmark the permalink.
7 Responses to The Fluffy Unicorns believe they're like Rosa Parks
Chuck Stanley says:
It seems to me that this crowd's actions came under the Hobbs Act (18 U.S.C. § 1951) the moment they issued their demands to the government at gunpoint. They demanded that Federal prisoners be set free, and that a government game preserve be turned over to "the people." They seemed to neglect the fact that in law, the government IS the people. I get the idea that by "the people," they must have meant themselves. That is extortion.
A Federal felony conviction means they will no longer be allowed to own firearms, or have firearms in their homes. That will cool their jets considerably. I guess they will have to make do with slingshots or bows and arrows.
ann summers says:
Hunger Gamez!
bigfatmike says:
Hmmm…. Rosa Parks with an assault rifle. That's interesting. I don't think we can just dismiss that out of hand.
But back to my main point. Sure, you can make the argument they are fluffy unicorns. But I think careful scrutiny will demonstrate that are each and everyone unique snow flakes.
shortfinals says:
Sometimes the actions of some of the denizens of my adopted land truly alarm me. I am trying to estimate just how long the British Government would have allowed this to state of armed rebellion to continue anywhere on its territory. It is a complex calculation involving the cruising speed Augusta-Bell A109 helicopters carrying SAS troopers…..but measure it in hours!
rafflaw says:
These crooks should be joining their arsonist friends in prison.
shortfinals,
That would make martyrs out of them, as happened at Ruby Ridge and Waco. The Feds learned from that, and are playing a more subtle game. Call them what they are. They are not protesters, but domestic terrorists. They will tire of playing the victim game eventually if there is no reward. Combine that with a high plains winter, and they will go home soon enough. Pick them up at the barber shop, the feed store, or at The IHOP. One at a time, with no cameras nearby for them to play to with the drama queen bit.
I see that one of their number took some the funds raised for them by donations, is staying at a motel in town, and went on a drinking binge. That is sure to win him the Miss Popularity contest with the group. Not!
raff,
Take it to the bank. Do you think my idea of a Hobbs Act violation will fly, or should it be some other charge(s)?
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Home Breaking The Russian Kettlebell has four wins at the start of the world...
The Russian Kettlebell has four wins at the start of the world championship in rapid chess
the world championship In rapid chess among women which passes in Moscow, ended the first day of the tournament. After four rounds the leaders are from three women. Among them, the Russian Olga Girya, who won four wins out of four.
the same result was shown by representative of Georgian Meri Arabidze and Irina bulmaga from Romania. Russians Daria Charochkina and Alina Kashlinskaya scored 3.5 points.
on December 27 at the world championship in rapid chess will be played another four rounds.
In the male part of the tournament after five rounds, the leader of the Chinese Wang Hao, who scored 4.5 points. The Russians Daniil Dubov and Alexander Motylev are in the active 4 points.
sports news chess world championship Kettlebell Moscow
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Modbury Chinese Takeaway specialises in Chinese takeaway, serving a large selection of dishes.
Please check with Modbury Chinese Takeaway for their exact delivery area and any delivery charges.
So, welcome to Modbury Chinese Takeaway now serving Chinese and other takeaway meal combinations. At Modbury Chinese Takeaway you are certain to find the perfect dish for not only yourself but for your family and friends.
Golden Bridge specialises in Chinese takeaway meals, serving a variety of dishes.
So, welcome to Golden Bridge now serving Chinese and other takeaway meal combinations. At Golden Bridge you are certain to find the perfect dish for not only yourself but for your family and friends.
Note: Please check with Golden Bridge for their exact home delivery area and any delivery costs.
"Chinese Takeaways in Ivybridge Takeaway The Easy Way"


These MINI gable boxes are so cute and would great for your next party or event. They come in tons of colors to match you party. Great for fill with candys or treats. These mini treat boxes are 3" x 2" and require Simple assembly.


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Peter Kertes, Thomas G Sheidow, Geoff Williams, Mark Greve, Ivan Galic, Emmanouil Rampakakis, Joanne Gavalakis, Andrea Scarino; Canadian Treat and Extend Analysis Trial with Ranibizumab in Patients with Neovascular AMD: Interim Analysis of the CANTREAT Study. Invest. Ophthalmol. Vis. Sci. 2017;58(8):1200.
Purpose : Age-related macular degeneration (AMD) is the leading cause of severe, irreversible vision loss in developed countries. To date, no large prospective randomized clinical studies have assessed the efficacy of a treat-and-extend (T&E) regimen compared with monthly dosing for the treatment of neovascular AMD. The purpose of this analysis was to compare the effectiveness of ranibizumab using a T&E regimen to once-monthly (OM) dosing in treatment-naïve neovascular AMD patients.
Methods : This is a 24-month, prospective, randomized (1:1), open-label, multicenter, post-authorization study. In this interim analysis, baseline characteristics, visual acuity, and injection frequency were evaluated. Summary statistics including the mean and standard deviation for continuous variables and counts and percentages for categorical variables were produced.
Results : As of November 10th, 2016, 580 patients (T&E=287; OM=293) were recruited; 404 patients (T&E=209; OM=195) and 201 patients (T&E=102; OM=99) had 12-month and 24-month follow-up, respectively. Mean (SD) age was 79.3 (7.9) years, 60.3% were females, 94.3% were Caucasian, and 22.5% had a family history of AMD. No significant between-group differences were observed. Mean (SD) baseline BCVA was 58.7 (14.2) and 59.4 (13.5) for T&E and OM, respectively, and was comparable for both groups. At Month 12, after an average of 9.2 (T&E) and 11.8 (OM) injections, mean (SD) BCVA improvement was 8.0 (12.6) and 6.2 (12.6) letters, respectively. At Month 24, after an average of 18.2 (T&E) and 23.6 (OM) injections, mean (SD) BCVA improvement was comparable between groups with 6.5 (15.3) and 6.0 (13.0) letters, respectively.
Conclusions : The results of this interim analysis show that comparable improvement in BCVA can be achieved in a real-world setting with fewer injections using a T&E compared to a monthly dosing regimen.


The Dolphins said in a statement: "The NFL required each team to submit their rules regarding the anthem before their players reported to training camp. We will address this issue once the season starts. All options are still open"
The Miami Dolphins imposed new rules this week related to its policy over anthem protesters. NBC 6's Johnny Archer reports.


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Monika/Moma is our Editor in Chief at Allt om Scrap. Besides beeing a great scrapbooker she is really good at drawing. Her flowers are just amazing. A couple a months ago she descided to start her own line of stamps, and I was happy to be one of the first to use her stamps.
I have used the "Liten pense" stamp for this card. The small size makes it really versatile.
And for this Autumn card I ´ve used the stamp "Äppelblom". I´ve painted both images with Twinkling H2O´s.
Want to pay Moma´s Lil´shop of stamps a visit? You find it here.


In a recent Deloitte Global Human Capital Trends survey, 37 percent of HR leaders rated rewards as very important, with only 9 percent admitting that they are "very ready" to implement those rewards programs.
Rewards have always been a leading method of engaging and motivating employees, but many managers and HR leaders are currently struggling to create effective rewards programs as employee preferences and expectations have markedly shifted over the last decade.
Companies that used to deliver standardized rewards are moving towards more personalized systems that are highly aligned with individual preferences. Here is why you should consider personalizing employee rewards within your organization.
To put it simply, nearly every company's employee base is highly individualized, and what motivates one person won't necessarily motivate another. So, it is better to tailor-fit an incentive program to individual wants and desires. How will you know what your employees desire? Ask them! Distribute surveys, collect data, and then consider a system that can provide multiple reward options to choose from.
One example of a successfully integrated personalized employee rewards program is by the public relations company N6A. Employees can earn points to spend on a variety of rewards on different redemption levels, ranging from cash, to extra PTO, to an employee's "dream pick"–an incentive reward of their own creation. In an interview with Forbes, N6A CEO Matt Rizzetta stated that the company has seen an incredibly positive response to the new program.
Not every company needs to take personalization to this extent, but it goes to show how an organization can provide a rewards system where all employees can find value.
A more personalized employee rewards system provides the perfect opportunity to learn more about your workforce. Companies can determine if different positions or roles at distinct levels within the organization value different rewards. Personalization efforts can even provide valuable insight into a company's hourly or contingent workforce. Using this knowledge to provide a greater variety of more meaningful rewards will help attract and retain a more diverse workforce, while encouraging desired outputs.
Personalized rewards are inclusive rewards, and diversity means new perspectives, new ideas and innovation. Developing a personalized rewards program has the potential to provide value far beyond the expected bump in the engagement of current employees.
Having separate rewards for different strategic goals gives employees the opportunity to develop specific, relevant skills in order to achieve a desired business goal. To put it into perspective, a salesperson could achieve separate rewards for productivity goals—for example, after a specified number of new leads are contacted—or revenue generation goals, after a specified value of deals is achieved.
Relevant skills like time-management, deeper product knowledge, increased productivity and presentation skills can all result from these specified rewards, making for more highly skilled, well-rounded employees. Their time and effort to improve would be met with tangible rewards, and as a result, the company's bottom line would improve. A win-win for everyone!
ESG Incentives takes a strategic approach to creating successful rewards programs that achieve profitable results. Contact us for more information on our process, and for best practices in creating more personalized employee rewards.


This one-day seminar is an introduction to Graphic Design. The course encompasses creating designs for primarily for print but rules apply to screen and web designs. Learn how to create effective designs combining images/objects and typography following basic rules for designers. Learn the basic rules of design and how to creatively break the rules.
We live in in a world where visuals are constantly viewed by everyone and the palette of the audience has become much more sophisticated in recent years. Learn what makes a layout a poor layout and learn how to create empowering and dynamic designs that communicate clear messages.
Recommended participants include graphic designers, illustrators, art directors, corporate communicators, advertising executives, web designers, and multimedia artists who want to understand how to effectively create design projects for print, screen, or web. This is a must for those who want to improve skills in graphic arts, multimedia, and web design.
This is an entry level course and students do not need experience using any professional layout program. Students should have some basic computer skills and know how to use Windows or Mac operating system.


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Three Ways Baltimore City, Maryland Suffers from Parking Woes
In France, Discovery of 13th Century Mur...
Red Line Light Rail Plans Spark Needed Discussion Across Baltimore
"Autogeddon:" Is The Automobile Killing San Francisco's Infrastructure?
Transportation Options Underserving Residents in Towson, Maryland
Baltimore, Maryland's Transportation Options Minimizes School Choice Opportunities
New Zoning Bill Aims to Decrease Number of Cars in Downtown São Paulo, Brazil
by Anna Petrone
Red Line Light Rail Plans Spark Needed Discussion Across...
"Autogeddon:" Is The Automobile Killing San Francisco's ...
Transportation Options Underserving Residents in Towson,...
Good urban planning requires forward thinking as well as learning from past successes and failures. Urban planning ideals are steadily evolving, and past practices have created dicey results that today's planners are still grappling with. In particular, decades of parking policy are increasingly being questioned in many cities, including Baltimore, Maryland. Baltimore's zoning code, including requirements for off-street parking, went
by Jade Clayton @RaDaDaJade June 3, 2015 No comments
Good urban planning requires forward thinking as well as learning from past successes and failures. Urban planning ideals are steadily evolving, and past practices have created dicey results that today's planners are still grappling with. In particular, decades of parking policy are increasingly being questioned in many cities, including Baltimore, Maryland. Baltimore's zoning code, including requirements for off-street parking, went largely unchanged since 1971. In 2008, parking and other requirements were reworked as part of a comprehensive zoning code rewrite. In 2015, Baltimore still suffers from plenty of parking-related issues, including the following three examples:
1) Traffic Congestion
In popular neighborhoods like Fells Point, Federal Hill, and Hampden, where residents and businesses share limited on-street parking, congestion is noticeable. Drivers get caught in congestion caused by many factors, including drivers circling a block several times looking for parking. Drivers sometimes also park in lanes that would otherwise be open to traffic. Such a problem exists on Aliceanna Street in Fells Point, and the City's proposed solution is to restrict on-street parking to keep multiple lanes open during rush hour. However, it's possible that these restrictions will not benefit drivers, because further limiting desirable parking may result in drivers circling the block a few more times. Commuters who previously took alternate routes may also converge on Aliceanna. In these cases, the plan would fail to improve congestion, and could even leave the area worse off than before. As the plan offers little, if any, improvement to drivers at the expense of cyclists and pedestrians, bike advocates and complete streets fans are not pleased.
2) Aversion to Transit
An article from The Journal of the American Planning Association entitled "Does TOD really need the T?" included findings that the presence of transit alone doesn't make people ride transit as much as a lack of parking makes people ride transit. In Baltimore, there is not only just enough parking, in number of spaces and affordability, to discourage alternative modes, but undesirable enough transit, bike infrastructure, and pedestrian safety to encourage driving. The Shops at Canton Crossing is a good case study for this concept. The area is a would-be Red Line station, but the shops are separated from Boston Street and bus stops for two lengthy bus routes by a sea of free parking and disconnected sidewalks.
3) Unsafe School Children
While often reported as a driving issue rather than a parking issue, Baltimore is unfortunately known for being unsafe for school-aged pedestrians. In a five-year period, over 1,000 school-aged children were hit by cars in Baltimore City. That's more than one kid hit per school day based on Maryland's required 180 school days per year. The observation of one principal seems to be that dodging double-parked cars is adding to the danger. He hopes to fine parents who double-park in school zones, saying the act "leads to traffic jams and jeopardizes student safety."
These three examples are just the tip of the iceberg. From a community standpoint, parking can be incredibly divisive and is the cause of countless disputes. Add snow to on-street parking in Baltimore, and you get an entertaining, though often disturbing, string of stories detailing arguments about who has the right to park in a shoveled spot. The true costs of bad parking policy and poor parking etiquette are still not fully understood and definitely not agreed upon within planning, engineering, or other disciplines.
What are your thoughts on the impacts of parking policy in Baltimore and in other cities? How does your city deal with its lack or excess of parking? Is your city designing for vehicles or people? Share your city's stories in the comments area below.
In France, Discovery of 13th Century Murals Spur Poitiers Cathedral's Restoration
Policy Setback: New Ruling in Favour of Suburbs in Waterloo Region, Canada


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Siku is an artist, designer, writer and theologian. Considered one of the most innovative artists in the comic book field, he is the author and creator of the bestselling The Manga Bible. Siku is one of the illustrators behind The Lin Comic Book Hero Bible. He has worked for 2000AD, producing titles such as Judge Dredd, and for Marvel UK and COM X. Siku has produced an anime series on the life of Christ and a visual art/commentary project and solo music album on Psalm 27. He was also consultant on BBC's ground breaking doc-drama, Atlantis, and a finalist in the Sermon of the Year 2016 competition run by London School of Theology and Preach magazine.
Titles by the Author:
The Lion Comic Book Hero Bible


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TPJ RACING CONTEST
TPJ RACING
PROFESSIONAL MOTOCROSS TEAM
Posted May 29, 2017 by tpjracing	Uncategorized
Glen Helen 2017
The TPJ Fly Racing team travelled to San Bernardino, CA to compete in the second round of the Lucas Oil Pro Motocross championship at Glen Helen raceway.
This week we welcomed the return of Nick Schmidt and Dylan Merriam, who were both taking time off to recover from injuries sustained during the Monster Energy Supercross season.
We also welcomed back TPJ Fly Racing rider Chad Gores, who made his return to racing this weekend.
Schmidt and Merriam both had the opportunity to ride for press and various media outlets on Thursday and Friday leading up to the races. They were able to get an early look at the track and conditions for racing on Saturday. We are very grateful to the Lucas Oil Pro Motocross team for giving our riders this opportunity.
On race day, the TPJ Fly Racing crew came out in full force with our massive pit set up, and our Karcher pressure wash station. We are very fortunate to have the support of a long list of sponsors that helps us get to the races each week.
As racing kicked off, it was clear that the track would take no prisoners. Even some of the top riders struggled during qualifying. Dylan Merriam made his debut to the 450 class at Glen Helen and qualified 20th overall. Schmidt qualified not far behind in 25th. Chad Gores made an attempt to qualify through the consolation race, but opted to pull off early and preserve himself for the next round.
As the gate dropped for the first moto, Merriam got a great start and was holding on to 15th position. While charging down a wet and rutted straightaway, he tried to cross over from inside to outside; as he cut across, his front wheel dipped into a mud hole and he tucked the front end of his bike. When he was able to recover and get his bike started again, he was 20 seconds behind last place. Merriam got up and charged all the way from 40th to 23rd, another hiccup in the sand dropped him to 30th for moto one. Later, Merriam had his foot checked due to pain, and discovered he rode the first moto with three broken toes. Due to his injury, he could not race the second moto. However, we were very impressed by his determination in his debut, and look forward to seeing him healed and back on the track.
Schmidt has been nursing a wrist injury for several weeks, and this week it continued to bother him. He made an attempt to race moto one but pulled off early and chose not to race the second moto. We hope that in the next few rounds Schmidt will be back at 100%.
We understand that injuries are a part of racing, and we are very impressed by the will power and strength of these up and coming athletes. We are very thankful to the sponsors who continue to support them through the highs and lows of race season, and we look forward to seeing what these athletes can do on a good day.
We want to extend a special thank you to Karcher pressure washers for the great power washing station, it keeps our bikes clean despite the grime of outdoors, and lets us give back to the racing community by sharing it with other teams. We also want to thank DSC Construction and Dunlop tires for their contribution to our main event qualifiers. DSC Construction pays back their fuel and entry fees, and Dunlop tires supplies them with a fresh set of tires.
It is thanks to the support of our sponsors that we are able to travel the country and help these young athletes work toward their dreams.
We are headed east and looking forward to our next round of racing in Lakewood, Colorado at Thunder Valley. We hope to see some of you there!
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Dutch Police Arrest Suspect In Hague Stabbing
Sergei Klebnikov Forbes Staff
I cover breaking news, with a focus on money and markets.
Rachel Sandler Forbes Staff
I cover breaking news.
Police arrive at the Grote Marktstraat, the site of the stabbing attack.
Sem Van Der Wal/ANP/AFP via Getty Images
(Updated: 10:24 p.m. PST, 12/1/2019)
Topline: Dutch Police arrested a 35-year-old homeless man on suspicion of stabbing three teenagers at The Hague on Saturday as authorities say there is no evidence terrorism played a role in the attack.
The Friday evening attack in the Dutch city occurred in the proximity of a Hudson's Bay department store on a busy shopping street near the main market square, police reported around 2:30 p.m. EST.
Three people were injured in the stabbing—two 15-year-old girls and one 13-year-old boy, authorities confirmed.
All three victims were later released from the hospital, according to a police statement.
Authorities said in a statement that they still don't know yet the motive for the stabbing.
Key background: This is the second major stabbing in a European city on Black Friday, following what police described as a "terrorist incident" on the London Bridge earlier today. While the London Bridge attacker was shot dead by police, two people have been confirmed dead in that stabbing, with three more wounded, according to London's Metropolitan Police Commissioner Cressida Dick.
Sergei Klebnikov
I am a New York—based reporter for Forbes, covering breaking news—with a focus on financial topics. Previously, I've reported at Money Magazine, The Villager NYC, and T
Rachel Sandler
I'm a San Francisco-based reporter covering breaking news at Forbes. Previously, I've reported for USA Today, Business Insider, The San Francisco Business Times and San


What seems bigger: the moon, or the sun?
Viewed from the earth, the sun and the moon appear to have pretty much the same size. The apparent size (radius) is defined as arcsin(R/h) where R is the true radius of the celestial body, and h is the distance to the celestial body.
For the sun, R=695,000 km and h=150,000,000 km.
For the moon, R=1,700 km and h=300,000 km.
You would need to put 200 suns (or moons) next to each other, to create a ring of suns (or moons) stretching in the sky, from North to South, with no gap.
By contrast, you would need 300,000 times more of our closest star (outside the solar system) to create the same continuous ring of stars.
It would be interesting to compute how many suns you would need to cover the entire sky, assuming the suns were cubes rather than spheres. Other than cubes, what other shapes would create a full coverage, with no empty space?
...which is the reason we can experience a total eclipse with virtually perfect coverage of the sun by the moon (except when the moon is at its most distant from the Earth, resulting in an annular eclipse).
If you really want a challenge try to work out the probability of occurrence of this coincidence in apparent size for a planet with a single moon - conditional on there being intelligent life present on the planet to appreciate it!
- the probability of the existence of proteins is about 1/3 - it follows from Bolzmann formula (distribution) and ergotic theorem.
Actually I was asking about the probability of the coincidence in apparent sun/moon size GIVEN THAT life could exist on the planet to observe it. This narrows the possibilities somewhat to just those planets of a certain size and distance from a sun (of a certain class) that would be capable of sustaining life.
Within these constraints, how likely is it that the sun and (for simplicity) a single moon would have approximately the same observed size.
Put another way, what proportion of planets capable of sustaining intelligent life could experience both total and annular eclipses, as ours does.
I think that the moon "seems'' bigger unless there is a lot of humidity in the air that acts as a magnifying. You would have to calculate air humidity as a factor of magnification.
which will be a hunter moon. And you're right, sometimes depending on how close the moon is to the horizen in transit it can appear HUGE so I would not keep the apparent size of the moon fixed. I've seen summer moons that look like you could walk onto them from earth. Magical!
When the moon appears to be huge, it's usually due to atmospheric conditions (e.g. high humidity). The same conditions would make the sun appear equally huge: in other words, whenever a full eclipse moon/sun takes place, the moon and sun will occupy exactly the same apparent spot in the sky, regarless as to whether the moon looks normal or big.
I might be wrong, especially if space clouds between the moon and the earth magnify the moon's appearance, but not the sun. But I don't think space clouds exist in our solar system. Maybe other phenomena could cause a similar sun/moon distorsion though.
I'm sure you've also seen a huge sun at sunset, when the sun is about to vanish over the Pacific ocean, and the atmospheric conditions are right.


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Search Results for : "ANTONIO GUTERRES"
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CABO VERDE / GUTERRES CLIMATE ADAPTATION
Secretary-General António Guterres spent Sunday in the island of Santo Antão, where, after five years of intense drought, a group of projects supported by the United Nations hopes to transform the agricultural sector of these Atlantic islands. UNIFEED
Production Date: 22-Jan-2023
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CABO VERDE / GUTERRES VISIT
Secretary-General António Guterres today arrived in Cabo Verde for the Ocean Race Summit – and to take a close look at some of the answers and innovative solutions under way in this 10-island archipelago off the coast of Africa. UNIFEED
UN / G77 HANDOVER
Pakistan passed the chairmanship of the Group of 77 and China to Cuba, in a ceremony in New York where the UN Secretary-General said "we can draw a straight line between the hardships suffered by your people, and the continued failure of developed countries and global institutions to support developing countries on multiple fronts." UNIFEED
GENEVA / PAKISTAN FLOODS BROLL
Since June 2022, a combination of heavy rains and riverine, urban, and flash flooding has led to an unprecedented natural disaster in Pakistan. Floods have affected 33 million people, with more than 1,730 lives lost as well as 2 million housing units impacted, and several thousands of schools and hospitals damaged or destroyed. FILE
GENEVA / PAKISTAN CLIMATE RESILIENT PRESSER
At the International Conference on Climate-Resilient Pakistan, co-hosted by the Government of Pakistan and the United Nations, which took place today at the UN Office in Geneva, UN Secretary-General Antonio Guterres called for support to help Pakistan with a 16 billion US dollars rebuilding effort following devastating floods. UNTV CH
UN / UKRAINE FACT-FINDING MISSION
The Secretary-General has decided to disband his Fact-Finding Mission (FFM) regarding the 29 July 2022 Incident at Olenivka in Ukraine "in the absence of conditions required for the deployment of the Mission to the site," a UN Spokesperson said. UNIFEED
UN / 2022 TOP STORIES
From the war in Ukraine to the response in health crisis and providing life-saving humanitarian aid, the work of the United Nations remained vital in a year marked by multiple overlapping crises. UNIFEED
Production Date: 30-Dec-2022
UN / GUTERRES NEW YEAR MESSAGE – SPANISH
En su mensaje de Año Nuevo, el Secretario General de la ONU, António Guterres, dijo, "Juntos, hagamos que 2023 sea un año en el que la paz vuelva a nuestras vidas, nuestros hogares y nuestro mundo." UNIFEED
UN / GUTERRES NEW YEAR MESSAGE – FRENCH
Dans son message pour le nouvel an, le Secrétaire général de l'ONU, António Guterres, a dit, «Ensemble, faisons de 2023 une année de paix, dans nos vies, dans nos foyers, dans notre monde.» UNIFEED
UN / GUTERRES NEW YEAR MESSAGE – PORTUGUESE
Em sua mensagem de ano novo, o secretário-geral da ONU, António Guterres, disse, "Juntos, vamos fazer de 2023 um ano em que a Paz seja restaurada nas nossas vidas, nos nossos lares e no nosso mundo." UNIFEED
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