text:
\section{INTRODUCTION}

Supernova (SN) models in spherical symmetry (1D) --- even the latest
ones with ``Boltzmann neutrino ($\nu$)
transport''~\cite{janka.ref_BTsims} --- do not explode, neither by
the prompt bounce-shock mechanism, nor by the delayed
neutrino-heating mechanism. Suggestions that neutron-finger
convection in the neutron star (NS) could enhance the $\nu$
luminosity and thus the heating behind the shock~\cite{janka.ref_wilmay}
could not be confirmed by detailed analysis~\cite{janka.ref_bru04}.
Also Ledoux convection in the nascent NS seems to be
ineffective in this respect~\cite{janka.ref_jan04a,janka.ref_buras03}.
A reduction of the $\nu$ opacity by several 10\% at densities
below $\sim\,$10$^{13}$g$\,$cm$^{-3}$ would also allow $\nu$'s
to leave the accretion layer more easily and could produce
explosions~\cite{janka.ref_froeh04}, but a physical effect
of corresponding size is not known.

Multi-dimensional simulations of core-collapse SNe
revealed that hydrodynamic overturn behind the stalled accretion
shock develops on a relevant timescale and increases the efficiency
of the $\nu$-heating mechanism, enabling explosions
even when spherical models fail~\cite{janka.ref_SN2D}.
Initially there
was hope that this new twist in the theory of SNe
was the long-sought guarantee for ``robust'' explosions.
But the first generation of multi-dimensional models employed
a simplified treatment of the $\nu$ transport --- at best
by grey flux-limited diffusion schemes --- which fell much
behind the sophistication of the transport in non-exploding
1D models. It was therefore suspected that the transport
approximations might have contributed to the success
of the multi-dimensional simulations~\cite{janka.ref_mezz98}.

Recently, two-dimensional (2D) models have become available with
a significant improvement of the $\nu$ transport by solving
the energy-dependent equations of $\nu$ number, energy, and
momentum, making use of closure relations obtained from a model
Boltzmann equation~\cite{janka.ref_jan04a,janka.ref_jan04b}.
The description of
$\nu$-matter interactions has thus reached a new level of
accuracy and refinement, although the transport
is still treated to be essentially radial (lateral flux components
are ignored in the moments equations but terms associated
with lateral velocities and lateral gradients of $\nu$
pressure are included). Simulations with thus improved
treatment of the $\nu$ physics could not find explosions
despite of convective activity in the $\nu$-heating layer
behind the SN shock~\cite{janka.ref_buras03}, confirming the
suspicion that radical transport approximations might have
favored the rapid and powerful explosions seen in other 2D
and 3D models~\cite{janka.ref_SN2D,janka.ref_SN3D}.

So what is missing in the currently most advanced SN
models which fail to produce explosions? In the following, we
shall first briefly summarize the status of core-collapse
modeling by the Garching group. In particular,
we shall discuss that any limitation of the angular wedge of 2D
simulations to less than 180 degrees (e.g. to 90 degrees as in
many previous simulations) imposes artificial constraints
to the fluid flow and suppresses large-scale modes that can
play an important role for the growth of convection. It is
further demonstrated that even a ``modest'' amount of rotation
in the SN core, in the ballpark of predictions of current
stellar evolution models~\cite{janka.ref_heger04}, may
have an important impact on the postbounce evolution. Finally,
we shall elaborate on uncertain aspects of the nuclear physics
which the SN shows sensitivity to.

\begin{figure*}[t!]
\tabcolsep=0.5mm
\begin{tabular}{lr}
$\ \ $
\epsfclipon \epsfig{file=janka_f1a.eps,width=0.425\hsize}
$\ \ $
   \raisebox{5.0cm}{
         \parbox[t]{0.45\hsize}{
\epsfclipon \epsfig{file=janka_f1b.eps,width=\hsize}
\epsfclipon \epsfig{file=janka_f1c.eps,width=\hsize}
}}
\end{tabular}
\vspace{-25pt}
\caption{\small
{\em Left:} Composition in the highly degenerate 1.38$\,M_{\odot}$
core of an 8--10$\,M_{\odot}$ progenitor~\cite{janka.ref_nom87}
with O, Ne and Mg in the central region enclosed by a C-O shell.
$\left\langle X \right\rangle$ denotes the mass fraction of a
representative neutron-rich heavy nucleus that appears in
nuclear statistical equilibrium, and $Y_e$ is the electron
fraction.
{\em Right, top:} Mass trajectories, shock position (thick solid line
that rises to the upper right corner of the plot, where it reaches
the surface of the C-O shell), neutrinospheres ($\nu_e$: solid;
$\bar\nu_e$: dash-dotted; $\nu_{\mu},\,\bar\nu_{\mu},\,\nu_{\tau},\,
\bar\nu_{\tau}$: dashed), and gain radius (dotted) for the collapsing
O-Ne-Mg core. The mass trajectories are equidistantly spaced with
intervals of 0.02$\,M_{\odot}$. The outermost line corresponds to
an enclosed mass of 1.36$\,M_{\odot}$ near the outer edge of the carbon
shell. The (blue) hatched region is
characterized by a dominant mass fraction of alpha particles.
{\em Right, bottom:} Luminosities of $\nu_e$ (solid),
$\bar\nu_e$ (dashed) and heavy-lepton $\nu$'s
(individually; dotted) as functions of time. The
sawtooth pattern during the collapse phase until about 50$\,$ms
is a numerical artifact.
(The plots were taken from Ref.~\cite{janka.ref_kit03}.)
}
\label{janka.fig1}
\end{figure*}

\begin{figure*}[t!]
\tabcolsep=0.5mm
\begin{tabular}{lcr}
\epsfclipon \epsfig{file=janka_f2a-low.eps,width=0.33\hsize} &
\epsfclipon \epsfig{file=janka_f2b-low.eps,width=0.33\hsize} &
\epsfclipon \epsfig{file=janka_f2c-low.eps,width=0.33\hsize}
\end{tabular}
\vspace{-25pt}
\caption{\small
Three stages (at postbounce times of 141.1$\,$ms,
175.2$\,$ms,
and 225.7$\,$ms from left to right)
during the evolution of a (non-rotating) 11.2$\,$M$_{\odot}$
progenitor model from Ref.~\cite{janka.ref_wooetal02}, visualized
in terms of the entropy. The scale is in km. The dense NS
is visible as low-entropy circle at the center.
The computation was performed in
spherical coordinates, assuming axial symmetry, and employing
the ``ray-by-ray plus'' variable Eddington factor
technique~\cite{janka.ref_ramjan02}
for treating $\nu$ transport in multi-dimensional
SN simulations. Equatorial
symmetry is broken on large scales soon after bounce, and
low-mode convection begins to dominate the flow between
the NS and the strongly deformed SN shock.
The model continues to develop a probably weak explosion, the
energy of which was not determined before the simulation had
to be stopped because of CPU time limitations.
}
\label{janka.fig2}
\end{figure*}

\section{EXPLOSION MODELS}

Simulations leading to explosions can be reported for stars
near the low-mass end of SN progenitors, namely for
stars in the mass range of $\sim$8--10$\,M_{\odot}$ with
O-Ne-Mg cores~\cite{janka.ref_nom87}, and for an 11.2$\,M_{\odot}$
progenitor~\cite{janka.ref_wooetal02}, both characterized
by small cores of less than $\la$1.3$\,M_{\odot}$ (O-Ne-Mg
or Fe, respectively) and a steep density decrease (entropy
increase) outside.

\subsection{Stars in the 8--10$\,M_{\odot}$ range with O-Ne-Mg cores}

The main improvement of our new simulations of O-Ne-Mg core collapse
--- which we did so far only in spherical symmetry ---
compared to previous approaches is the more accurate,
spectral treatment of $\nu$ transport and $\nu$-matter
interactions. Using the nuclear equation of state (EoS) of
Lattimer \& Swesty~\cite{janka.ref_latswe91} and more recently
also that of Hillebrandt \& Wolff~\cite{janka.ref_hiletal84}, we
could {\em not} confirm the prompt explosions found in calculations
with simpler $\nu$ treatment~\cite{janka.ref_hiletal84}.
The shock is created much deeper inside the collapsing core
than in the ``old'' models (cf.\ also
Ref.~\cite{janka.ref_baretal87}), typically at a mass coordinate
around $\sim$0.45$\,M_{\odot}$~\cite{janka.ref_kit03}
(defined by the moment when the postshock entropy first exceeds
3$\,k_{\mathrm B}$ per nucleon), and it stalls
(defined by the time when the postshock velocity becomes negative)
only 1.2$\,$ms later at $\sim$0.8$\,M_{\odot}$, still
well inside the neutrinosphere and {\em before} energy losses by
the prompt $\nu_e$ burst could have contributed to its
damping~\cite{janka.ref_kit03}.
We also do not find the powerful shock revival by $\nu$ heating
as seen in Ref.~\cite{janka.ref_maywil88} and for some choice of
the nuclear EoS by Fryer et al.~\cite{janka.ref_fry99}.
Instead, the shock
continuously expands due to the monotonically decreasing preshock
density and the steep density decline at the
interface between C-O shell and He shell (Fig.~\ref{janka.fig1}).
At the end of
our simulation the mass accretion rate by the shock has
correspondingly dropped to less than 0.03$\,M_{\odot}\,$s$^{-1}$.
Although our simulation is not yet finally conclusive in this
point, we see indications that a $\nu$-driven wind begins
to fill the volume between SN surface and shock and
will lead to mass ejection with a rather low explosion energy
(a few $10^{50}\,$erg due to the wind power and nuclear burning).
Little nickel production ($\sim$0.01$\,M_{\odot}$),
can be expected, corresponding to the wind mass loss rate that
can be estimated for an initial $\nu_e+\bar\nu_e$ luminosity of
$\sim 8\times 10^{52}\,$erg$\,$s$^{-1}$
(Fig.~\ref{janka.fig1}) using the equations in
Refs.~\cite{janka.ref_nuwind}.
The baryonic mass of the NS will be very close
to or only some 0.01$\,M_{\odot}$
less than the C+O core mass (which is 1.38$\,M_{\odot}$).
These findings are very similar to the outcome
of simulations of accretion induced white dwarf collapse to
NSs (AICs)~\cite{janka.ref_woobar92}.

A weak explosion of an 8--10$\,M_{\odot}$ star has been
suggested as an explanation of the observed properties of the
Crab SN remnant~\cite{janka.ref_nom82}. The wind-driven
explosion seen in our models, however, does not provide the
conditions for the low-entropy, low-$Y_e$ r-process nucleosynthesis
discussed for prompt explosions of collapsing O-Ne-Mg cores
in previous work~\cite{janka.ref_promptrp}.
R-processing in the high-entropy environment of the
$\nu$-driven baryonic wind can also not be expected
to take place, because sufficiently high entropies,
short expansion timescales, and low proton-to-baryon ratios
require the NS to be very massive
($\sim$2$\,M_{\odot}$) and compact ($\la$10$\,$km) (e.g.,
Refs.~\cite{janka.ref_nuwind}).
It is therefore unclear how O-Ne-Mg core collapse events could
contribute to the production of high-mass r-process nuclei.

\begin{figure}[htb]
\begin{minipage}[t]{80mm}
\epsfclipon \epsfig{file=janka_f3.eps,width=\hsize}
\end{minipage}
\hspace{\fill}
\begin{minipage}[t]{75mm}
\vspace{-7.6truecm}
\caption{\small
Maximum and minimum radii of the shock (giving a rough
measure of deformation)
vs.\ time for 2D simulations with a polar coordinate grid
(models ``2D''),
compared to 1D results with the same physics, but no
convection (models ``1D'').
{\em Top:} 11.2$\,M_{\odot}$ star~\cite{janka.ref_wooetal02},
simulated with a full
180$^{\mathrm o}$ grid (Model 2D(128))
and with a 90$^{\mathrm o}$ angular wedge around the
equatorial plane (Model 2D(64)).
{\em Bottom:} 15$\,M_{\odot}$ star
(Model~s15s7b2 of Ref.~\cite{janka.ref_woowea95})
without (Model 2D(32)) and with rotation (Model 2D(rot); see
also~\cite{janka.ref_buras03,janka.ref_mueller04}).
In the former 2D simulation a
90$^{\mathrm o}$ wedge around the equator was used, in the
latter a 90$^{\mathrm o}$ grid from pole to equator.
}
\label{janka.fig3}
\end{minipage}
\end{figure}

\subsection{Massive stars with iron core}

Progenitor stars in the mass range between 11$\,M_{\odot}$
and 25$\,M_{\odot}$ were found to neither explode by the
prompt bounce-shock mechanism nor by the delayed
$\nu$-heating mechanism in spherically symmetric
simulations~\cite{janka.ref_jan04c}, in agreement with
results of other groups~\cite{janka.ref_BTsims}.
This implies that state-of-the-art SN models do not
support suggestions that r-process nucleosynthesis might
occur in prompt explosions of low-mass ($\sim$11$\,M_{\odot}$)
progenitors~\cite{janka.ref_sumi01}.

We have also started to perform core-collapse simulations
for the mentioned stellar mass range in 2D, using a polar
coordinate grid and assuming azimuthal
symmetry~\cite{janka.ref_buras03,janka.ref_jan04a}. Because of
the energy-dependent treatment of $\nu$ transport and
$\nu$-matter interactions the requirements of CPU
time are substantial, and we were so far able to perform
only a handful of such 2D calculations. To limit the need of
computer resources we initially constrained the computational
volume to a $\sim$90$^{\mathrm{o}}$ wedge (between roughly
$+$45$^{\mathrm{o}}$ and $-$45$^{\mathrm{o}}$ around the
equatorial plane and periodic boundary conditions for
nonrotating models and between 0$^{\mathrm{o}}$ and
90$^{\mathrm{o}}$ with reflecting boundaries for rotating ones),
using an angular resolution of $\sim$1.4$^{\mathrm{o}}$.
This choice was also motivated by 2D models of the
first generation which were able to obtain explosions with
a similar setup due to the help of hot-bubble
convection~\cite{janka.ref_SN2D}.

First simulations of stars of 11.2, 15, and 20$\,M_{\odot}$
with a 90$^{\mathrm{o}}$ wedge, however, did not produce
explosions~\cite{janka.ref_buras03}.
This suggests that the success of the previous calculations
with simplified transport was most probably connected with
the use of transport approximations. One of our new models,
a 15$\,M_{\odot}$ star (Model s15s7b2 of
Ref.~\cite{janka.ref_woowea95}), was also collapsed with a
modest rotation: The pre-collapse core was assumed
to rotate (essentially rigidly) with a period of 12$\,$s,
i.e. $\Omega \approx 0.5\,$rad$\,$s$^{-1}$
(see Fig.~1 in \cite{janka.ref_mueller04}), which is
significantly faster --- but not orders of magnitude
faster --- than predicted by the latest stellar evolution
models~\cite{janka.ref_heger04}. Even this
``modest'' amount of rotation turned out to make a big
difference. As visible in the lower panel of
Fig.~\ref{janka.fig3}, the shock expands to a much larger
radius than in the 2D simulation without rotation
(although both simulations did not lead to explosions
within $\sim$270$\,$ms of postbounce evolution), mostly
because of the influence of centrifugal forces and the
more violent convection in a more extended region of
$\nu$ heating~\cite{janka.ref_buras03}.

\subsection{Nonradial shock instabilities and
low-mode postshock convection}

While the 11.2$\,M_{\odot}$ simulation with 90$^{\mathrm{o}}$
wedge did not explode (see Fig.~\ref{janka.fig3}, upper panel),
the same model with a full 180$^{\mathrm{o}}$
grid developed a presumably weak explosion
(Figs.~\ref{janka.fig2} and \ref{janka.fig3}). Equatorial
symmetry is broken on large scales some 10$\,$ms after
convective activity in the
postshock region has started (at $\sim$50$\,$ms p.b.), and
low modes ($l = 1,2$) begin to dominate the flow pattern between
NS and shock after about 140$\,$ms p.b., a phenomenon which
might be linked to the observed large recoil velocities of young
pulsars~\cite{janka.ref_pulsarkicks}.
The convection becomes significantly more
violent than in the 90$^{\mathrm{o}}$ simulation where obviously
important degrees of freedom were suppressed.
This latter fact was emphasized in an interesting paper
by Blondin et al.~\cite{janka.ref_blondin04}, who found a similar
development of low-mode asymmetries in the postshock flow and
shock oscillations as a consequence of the instability
of standing accretion shocks (``SASI'') against non-radial
perturbations that are amplified in a ``vortical-acoustic
feedback cycle''~\cite{janka.ref_foglizzo02}.

Blondin et al.\ considered idealized conditions in their
numerical studies, assuming steady-state mass accretion
with a constant rate, a fixed inner boundary radius, a simple
ideal-gas EoS, and ignoring $\nu$ heating and
cooling. We decided to test the effects of $\nu$'s and of
the size of the angular wedge (and thus of the possible modes)
in a separate set of simulations with a realistic EoS
but an approximative treatment of the $\nu$
transport (as described in Refs.~\cite{janka.ref_pulsarkicks}),
which allowed us to save computer time and thus to perform faster
calculations with higher resolution, and to run more models.
The mass accretion rate was given by the collapse of a
15$\,M_{\odot}$ progenitor star and the NS was replaced
by a gravitating point mass inside
a contracting inner boundary that followed the behavior of the
shrinking NS in our full-scale SN simulations with
detailed transport physics.

With this setup we confirmed that 2D simulations with a
180$^{\mathrm o}$ grid can yield explosions even if models with
90$^{\mathrm o}$ wedge do not explode. In these
studies, with $\nu$ effects switched on or off, we found
that $\nu$ losses promote the action of the vortical-acoustic
cycle by allowing matter to settle on the proto-NS
surface.
Our results show that corresponding shock deformation produces
growing perturbations in the postshock flow which
can accelerate the onset of convective overturn even in cases where
the infall timescale is initially shorter than the growth timescale
of Ledoux convection. We also
see that dipolar shock oscillations become more violent in case
of a rapid contraction of our inner boundary (mimicing a NS
that becomes rapidly more compact due to a soft nuclear
EoS), thus releasing gravitational
binding energy which partly is converted to turbulent kinetic
energy of the postshock flow. In this case $l=1,2$ modes begin to
dominate faster and the SASI conspires with
convective instability to establish favorable conditions for
a high efficiency of $\nu$ heating behind the shock.
Both nonradial instabilities differ characteristically in the way
how anisotropies emerge: Convective overturn is driven by the
negative entropy gradient in the $\nu$-heated layer, which
becomes Rayleigh-Taylor (RT)
unstable first on small scales, while the SASI starts from
vorticity producing sound wave interactions with the shock and
induces dipolar oscillations of the postshock layer
before convective activity is initiated and the typical RT
mushrooms become visible.

\begin{figure*}[t!]
\tabcolsep=0.5mm
\begin{tabular}{lcr}
\epsfclipon \epsfig{file=janka_f4a.eps,width=0.30\hsize} &
\epsfclipon \epsfig{file=janka_f4b.eps,width=0.348\hsize} &
\epsfclipon \epsfig{file=janka_f4c.eps,width=0.352\hsize}
\end{tabular}
\vspace{-25pt}
\caption{\small
{\em Left:} Pressure (top) and adiabatic index
$\Gamma \equiv \left ({\mathrm d}\ln P/{\mathrm d}\ln\rho\right )_s$
(bottom) vs.\ mass density
for an entropy $s = 1\,k_{\mathrm B}$ per nucleon (and
$Y_e = 0.4$) for the EoSs
of Ref.~\cite{janka.ref_hiletal84} (``Wolff'', thin lines),
Ref.~\cite{janka.ref_shenetal98} (``Shen'', medium)
and Ref.~\cite{janka.ref_latswe91} (``L\&S'', thick).
{\em Middle:} Shock positions (solid lines) and
neutrinospheric radii of $\nu_e$ (dashed)
as functions of time for collapse simulations of a 15$\,M_{\odot}$
progenitor (Model~s15a28~\cite{janka.ref_wooetal02})
with the three nuclear EoSs (top) and with two
different EoSs at densities $\rho < 10^{11}\,$g$\,$cm$^{-3}$
(L\&S compared to an ideal gas EoS of $e^-$, $e^+$, $\gamma$'s,
and Boltzmann gases of $n$, $p$, $\alpha$ and a
representative heavy nucleus in NSE; bottom).
{\em Right:} Prompt $\nu_e$ burst (left panel) and postbounce
luminosities of $\nu_e$ (solid lines), $\bar\nu_e$ (dotted) and
heavy-lepton $\nu$'s and $\bar\nu$'s (dashed) for the
simulations of the 15$\,M_{\odot}$ star with the three different
nuclear EoSs (top) and the two different low-density EoSs (bottom).
(The plots were taken from Ref.~\cite{janka.ref_marek03}.)
}
\label{janka.fig4}
\end{figure*}

\subsection{Nuclear physics sets the stage}

Nuclear physics therefore governs not only the
collapse phase, where electron captures on nuclei were
recently included in a much improved way and were found to determine
the position of shock formation and the structure of the layers
the shock expands into~\cite{janka.ref_ecapture}
(also W.R.~Hix and G.~Mart\'{\i}nez-Pinedo, this conference).
Nuclear physics and in particular the properties of the nuclear
EoS also determine the contraction and size of the nascent NS
and thus may influence the growth of nonradial
instabilities and anisotropies in the postshock accretion flow
during the $\nu$-heating phase.

In fact, differences in the nuclear EoS have interesting
consequences for core collapse, bounce conditions, shock formation,
and postshock evolution
in 1D simulations~\cite{janka.ref_marek03}
(for a brief summary, see~\cite{janka.ref_jan04c}).
Figure~\ref{janka.fig4} shows selected results for three
different EoSs (Lattimer \& Swesty~\cite{janka.ref_latswe91},
Shen et al.~\cite{janka.ref_shenetal98}, and Wolff \&
Hillebrandt~\cite{janka.ref_hiletal84}). The softest of them
(L\&S) leads to the highest densities at bounce and the smallest
enclosed mass of the shock formation position. Lateron the
nascent NS contracts most rapidly, forcing the shock
to retreat much more quickly than in case of, in particular, the
stiff Wolff EoS (Fig.~\ref{janka.fig4}, upper middle panel).
These differences
affect the $\nu$ luminosities during the $\nu_e$ burst and
the postbounce accretion phase (Fig.~\ref{janka.fig4},
upper right panel). While for the Wolff EoS the $\nu_e$
release in the burst is highest,
a more compact NS and thus hotter neutrinosphere
causes higher post-burst $\nu$ luminosities and mean energies.
In the lower middle and right panels we show the result of a
test which we performed with a four-nuclei NSE-EoS replacing
the low-density ($\rho < 10^{11}\,$g$\,$cm$^{-3}$) part of the
L\&S EoS (where an error in the treatment of $\alpha$-particles
has recently been discovered; C.\ Fryer, J.\ Lattimer, personal
communication). The conditions in the postshock
layer were hardly affected because the gas is disintegrated into
free nucleons at the high
entropies encountered in simulations with relativistic gravity.
Minor differences in the evolution of the
shock radius (Fig.~\ref{janka.fig4}, lower middle panel) and
$\nu$ luminosities (Fig.~\ref{janka.fig4}, lower right panel)
were caused by differences in the mass accretion rate associated
with the EoS treatment in the infall region ahead of
the shock.

\section{SUMMARY}

Non-radial instability of the accretion shock can amplify vorticity
in the postshock flow and thus can support the growth of convection
in the $\nu$-heated layer. It may be an important ingredient
for eventually robust explosions by the $\nu$-driven mechanism.
Low modes in the flow can develop when the explosion sets in slowly.
The relative importance of the different instabilities seems to
depend on $\nu$ cooling and heating on the one hand and the
high-density EoS, which controls the contraction of the nascent
NS, on the other. Simulations require the use of a
full 180$^{\mathrm{o}}$ grid and ultimately may have to be done
in 3D.

{\small
\medskip\noindent
{\bf Acknowledgements.}
We are grateful to K.~Nomoto, A.~Heger, S.~Woosley, and
M.~Limongi for providing us with their progenitor data.
Supercomputer time at the John von Neumann Institute for
Computing in J\"ulich and the Rechenzentrum Garching is
acknowledged.
}

{\small

redpajama_set_name: RedPajamaArXiv


text:
Creating Brass For Rare And Obsolete Cartridges
Philip Massaro
Creating brass for rare and obsolete cartridges is easier than you think. Here's what you need to know to create your own at home.
What You Need To Know About Making Brass:
Opens door to obscure and rare calibers.
The Handloader's Manual of Cartridge Conversions is an indispensable tool.
Can be as complex as removing a belt from a magnum.
Can be as simple as resizing a cartridge's neck.
There are times when certain cartridge cases are just unavailable, if not simply unaffordable. I ran into just this situation while I was looking for ammunition for a new rifle I'm having built. I've had a desire to own and hunt with a .318 Westley Richards since I first began to read the classic African stories of W.D.M. 'Karamoja' Bell and John 'Pondoro' Taylor (there's something cool about earning an African nickname, eh?) as they recounted their tales and experiences with the classic cartridges.
Left: 250-gr. Woodleigh RN. Right: 200-gr. Hawk RN
In all honesty, there's really nothing revolutionary about the classic .318 Westley Richards; it shoots a .330-inch diameter bullet, with the choices being between 180-, 200- and 250-grains, depending on the manufacturer, the classic load being a 250-grain round nose at 2,400 fps muzzle velocity. The .318 WR is the older cousin to the .338-06, with the latter having a much wider selection of bullets, but the former making you want to lift your pinky in the air when you sit down to afternoon tea. At any rate, I think it's a cool cartridge, and I am an aficionado of the classics. My rifle is still in the construction phase, going through its metamorphosis at Hillbilly Custom Rifles, and I needed some dummy ammunition to test the magazine length and the new chamber. This posed a bit of a problem: There are very few sources for .318 Westley Richards brass. The dies were no problem—RCBS makes a great set of full-length dies—and there are some good bullets on the market. I've chosen the Woodleigh 250-grain round nose Weldcore as an all-purpose bullet, as well as a nice 200-grain round nose from Hawk Bullets in New Jersey, which would work perfectly for deer and lighter game. But the brass…
There are a couple boutique brass producers that will make a run of properly headstamped .318 WR brass, but those runs are few and far between, not to mention expensive. There is a British company still making loaded ammunition, but at almost $10 per cartridge, that wasn't exactly the route I wanted to take either. So, I dug out my well-thumbed-through copy of John J. Donnelly's The Handloader's Manual Of Cartridge Conversions a fantastic reference book that every handloader should own, and read about the process of making .318 Westley Richards brass out of good ole plentiful .30-06 Springfield brass. It wasn't difficult at all.
More Reloading Info:
The Flexible And Forgiving .30-06 Springfield
The .45 Colt: A Wheelgun Classic
.300 Win. Mag.: The Answer To Most Hunting Questions
Tips For Reloading the .223 Remington
First, let me explain the differences between the two. The .30-06 shares a case head diameter with the 7×57 and 8×57 Mauser (0.473 inches), while the .318 WR uses a slightly smaller rim dimension of 0.464 inches, though in the past the Mauser-sized rim has worked fine in a .318 rifle's bolt face. Since my new rifle is using the action from a 1916 Hamburg Arsenal 98 Mauser originally chambered in 8×57 Mauser, using the larger rim diameter will not pose an issue at all. The '06 is definitely a longer case at 2.494 inches, so it would eventually need to be trimmed down to the WR's length of 2.400 inches. I grabbed a bunch of RP .30-06 cases, used the RCBS Universal Case Prep Station to trim the brass down 0.094 inches—the micrometer adjustment worked perfectly for this—and gave the case mouths a good chamfer and deburring. Other than that, the dies would do the bulk of the work.
My RCBS resizing die has a tapered expander ball, which will work the smaller diameter neck of the '06 brass slowly, for a smooth and consistent expansion. I used Imperial powdered neck lubricant and ran them through the RCBS .318 WR resizing die to open the necks to proper diameter, and to move the shoulder to the proper positioning. Viola! Though the headstamp read RP .30-06 Sprg., I had in my hands the first of the .318 Westley Richards cartridges that I plan to take on many adventures.
A must-have for any making your own brass, John J. Donnelly's The Handloader's Manual Of Cartridge Conversions.
I compared them to the two example .318 WR cases I had from Quality Cartridge, and they showed to be dimensionally identical. I loaded some bullets into unprimed and uncharged cases, and sent them off to Hillbilly Rifles to make sure everything was going well with the new barreled action, and they worked just perfect.
Making brass for rare or obsolete calibers certainly isn't something new; handloaders have been doing this for decades, and it can turn a wall-hanger rifle into a field champion once again. Sometimes the conversion is easy and only requires a single pass through a resizing die. The .318 WR above is an example, but just as easy would be making .257 Roberts brass from a 7×57 Mauser or a 6mm Remington case, or .338-06 and .35 Whelen from .30-06 brass. I've made ammunition for an older .30/.338 Magnum by obtaining a good set of dies with a tapered expander ball and using 7mm Remington Magnum brass. Other times a set of forming dies, which will reduce or expand the brass in smaller steps, will be required to best achieve the goal. Cases for the old .33 Winchester can be made from .45-70 Government brass, but in several steps, as the reduction from .458-inch diameter to .338-inch diameter is too radical to be accomplished in a single pass.
Some of the more advanced and radical transformations may require some advanced tools, as there are instances where a rim may need to be turned down to a different diameter, or a belt taken off in order to make something that will work. A good dial or digital caliper is a must, and like any handloading setup, the better your trimmer is, the more uniform your product will turn out. One last note: When you make brass for one cartridge from another, with a different headstamp, please be sure and keep that new ammo in a clearly marked box, with detailed notes. While I don't think my .318 WR ammo would chamber in a .30-06 rifle, if it did and were fired, the results would be tragic, if not fatal.
I strongly suggest you grab a copy of Mr. Donnelly's book, as it contains the formulae for making all sorts of wildcats in addition to the SAAMI accepted cartridges, as well as many of the older black powder cartridges. You never know when you may find a treasure in the form of a rare rifle in the dusty corner of your favorite gun shop, and you'll be happy to have the ability to make your own brass.
Editor's Note: This article originally appeared in the July 2016 issue of Gun Digest the Magazine.
Categories: Ammunition, Gear & Ammo, Reloading
Tags: ammo, Reloading

redpajama_set_name: RedPajamaCommonCrawl


Linear dampers provide resistive forces to provide improved feel for aircraft control surfaces or to dissipate energy from aerodynamic or mechanical loads. Arkwin dampers endure millions of cycles undergoing high side loads in dither conditions in the most demanding environments. Designs can be self-contained with integral reservoir or can be connected to the hydraulic system. Stepped damping curves can be developed to suit the application's need.


The Battle Save feature is an option present in certain games throughout the Fire Emblem series. It is a feature that allows the player to save the game in the middle of a chapter. It is different from the Bookmark feature in that Battle Saves are a permanent save file, while Bookmarks are merely a temporary save file that is erased upon loading.
The feature debuted in Genealogy of the Holy War, where the player is allowed to make Battle Saves at the beginning of a new turn. As chapters in this game are quite long, this is a helpful and sometimes necessary feature to make use of.
Following Genealogy, Battle Saves did not return until Radiant Dawn, where they then became a regular feature of the series from that point on. In Radiant Dawn, Battle Saves can now be made at any point during the Player Phase, except in Hard Mode, where they are disabled and replaced by the "Bookmark" feature (also known as "Suspend"). The Battle Save feature was also completely absent from the original Japanese release of Radiant Dawn.
In Shadow Dragon and New Mystery of the Emblem, Battle Saves are present in a much more limited form. Here, Battle Saves can only be made at "save points", glowing circles that are present on the map. You must move a unit onto a save point and use the "save" command, which allows you to make a single Battle Save and concludes the unit's turn. Save points disappear after a single use, and cannot be used again unless you restart the chapter, so they must be used wisely. Some chapters feature multiple save points.
In Awakening and Fates, Battle Saves return to functioning as they did in Radiant Dawn, but they can only be used in Casual Mode. In Classic Mode, Battle Saves are replaced by the "Bookmark" feature.
Battle Saves are very useful in the event that the player loses a unit, since they can reload the Battle Save until the outcome becomes positive, rather than restart from the beginning of the chapter. Some players would also make a Battle Save right before a level up occurred, and then reload the Battle Save if the level up does not produce good stat increases, and try again in hopes of better stats. This can happen because the Battle Save does not reuse the same random numbers but generates new ones with each reloaded save. These manipulations made it much easier for characters to cap their stats, or just generally get decent level ups. However, this cannot be done in Fates, as the game will remember the last few random numbers that were generated, so you must do things differently if you wish to change the outcome of a battle or a level up.


text:
IBA sets up large working group for sustainable finance
Representatives of key banks including SBI, HDFC Bank, PNB, Canara and Axis are part of the group that will help in formulating recommendations on green finance.
ETBFSI
The Indian Banks' Association (IBA) has set up a working group, comprising representatives of key banks, including State Bank of India, Punjab National Bank, HDFC Bank and Bank of Baroda to focus on green financing.
This working group will help in recommendations on sustainability finance ahead of India's G20 presidency in December, where environmental, social and governance (ESG) issues will be in focus, according to reports.
The other members of the working group include representatives of Canara Bank, Union Bank of India, ICICI Bank, Axis Bank, Yes Bank, IndusInd Bank and Kotak Mahindra Bank and four foreign banks -- Standard Chartered Bank, Bank of America NA, Qatar National Bank QPSC and Mashreq Bank PSC. The two other members are Exim Bank and SIDBI.
Banks are also seeking priority sector status to sustainable finance to increase funding to projects mitigating climate risks.
A PSL status will lead to improved credit flow to sectors that cater to green environment needs.
Banks, under the aegis of the IBA, may soon approach the Reserve Bank of India with the demand.
India's needs
While there is significant green finance available globally, there is a paucity of such capital in India and hence there is a need for a mechanism for Indian companies to tap into the global capital.
Green investments of $200 billion are needed annually to meet India's net-zero target. Of that, the country is managing just about $20 billion currently. Even there, a large part comes from traditional public and domestic sources.
There is a need for heavily polluting industries to transition to green processes, for instance, the steel industry replacing coking coal with green hydrogen, for which green bank can help.
RBI paper on sustainable finance
The RBI has taken steps for furthering green finance. In 2021, it joined the Network for Greening Financial System, a voluntary group of 116 central banks that promotes the exchange of best practices on green finance.
In July this year, the RBI released a discussion paper on climate risk and sustainable finance to help regulated entities deal with the issues arising from a warming planet.
The guidelines revolve around appropriate governance, strategy to address climate change risks and risk-management structure to manage them from a micro-prudential perspective, the paper said.
Regulated entities may explore aligning their climate-related financial disclosures on the lines of the Financial Stability Board's Task Force on Climate-related Financial Disclosures' framework.
This framework is increasingly being recognised as a suitable basis for climate-related financial disclosures, the paper said. Adapting the same would also help improve the consistency and comparability of the climate-related financial disclosures of regulated entities with their counterparts globally, the paper said.
These entities may make such disclosures annually, to begin with and may use their sustainability reports, annual reports, website, or a combination of them to facilitate public access, the paper said.
Growth-oriented, progressive Budget aimed to boost consumption and inclusion, says Bankers
Budget 2023: Banks surge on pro-growth measures, support for digital payments
RBI relax restrictions on SBM Bank (India) till March 15
Budget 2023 I Life insurance policies' income with an aggregate premium over Rs 5 lakh to be taxed
Budget 2023 I FM announces savings scheme for women with 7.5% interest rate, deposit sops for seniors


In May, an eight-member California federal jury awarded Apple a staggering $500+ million verdict as a result of a patent litigation lawsuit that has been ongoing for at least 7 years. The verdict has proved to be particularly puzzling for patent law professors and other patent advocates that disagree over whether an article of manufacture in relation to a patented design can cover a product encompassing many distinct technical inventions and improvements, such as a cell phone; or whether the article of manufacture should be considered to be the components within the product. Still further, there appears to be some significant disagreement over whether the four-factor test put forth by the Solicitor General and adopted by the Court is even appropriate or straightforward enough to be applied consistently across a wide variety of patent disputes moving forward.
The verdict provided no information about how jurors calculated the amount of damages they ordered Samsung Electronics Co. Ltd. to pay Apple Inc. for infringing smartphone patents, or how they applied the 2016 Supreme Court ruling in the case that was widely viewed as limiting the damages available for design patents. However, it has been reported that the article of manufacture considered for infringing Apple's D'305 patent was the entire cell phone and the article of manufacture considered for infringing the D'677 patent was only certain parts of the phone.
Those that have been following this case may ask how the amount in damages could rise to over $500 million. As it turns out, after Samsung was determined to be a willful infringer and made representations to the Court that it would stop selling infringing products, Judge Lucy Koh determined in January during a hearing that such a representation was "just not accurate". Perhaps these ongoing sales account for a portion of the difference between the $400 million verdict and the $500 million verdict.
sandbagging Apple with new demonstratives in the form of slides that the attorneys were making on the fly.
Gregory "Lars" Gunnerson is a Patent Attorney in the Mechanical and Electrical Patent Practice Group at McKee, Voorhees & Sease, PLC. For additional information please visit www.ipmvs.com or contact Lars directly via email at gregory.gunnerson@ipmvs.com.


text:
package com.haulmont.cuba.core.app.filestorage.amazon.auth;

import com.haulmont.cuba.core.app.filestorage.amazon.util.BinaryUtils;
import org.slf4j.Logger;
import org.slf4j.LoggerFactory;

import java.net.URL;
import java.nio.charset.StandardCharsets;
import java.util.Date;
import java.util.Map;

/**
 * Sample AWS4 signer demonstrating how to sign 'chunked' uploads
 */
public class AWS4SignerForChunkedUpload extends AWS4SignerBase {

    private static final Logger log = LoggerFactory.getLogger(AWS4SignerForChunkedUpload.class);

    /**
     * SHA256 substitute marker used in place of x-amz-content-sha256 when
     * employing chunked uploads
     */
    public static final String STREAMING_BODY_SHA256 = "STREAMING-AWS4-HMAC-SHA256-PAYLOAD";

    private static final String CLRF = "\r\n";
    private static final String CHUNK_STRING_TO_SIGN_PREFIX = "AWS4-HMAC-SHA256-PAYLOAD";
    private static final String CHUNK_SIGNATURE_HEADER = ";chunk-signature=";
    private static final int SIGNATURE_LENGTH = 64;
    private static final byte[] FINAL_CHUNK = new byte[0];

    /**
     * Tracks the previously computed signature value; for chunk 0 this will
     * contain the signature included in the Authorization header. For
     * subsequent chunks it contains the computed signature of the prior chunk.
     */
    private String lastComputedSignature;

    /**
     * Date and time of the original signing computation, in ISO 8601 basic
     * format, reused for each chunk
     */
    private String dateTimeStamp;

    /**
     * The scope value of the original signing computation, reused for each chunk
     */
    private String scope;

    /**
     * The derived signing key used in the original signature computation and
     * re-used for each chunk
     */
    private byte[] signingKey;

    public AWS4SignerForChunkedUpload(URL endpointUrl, String httpMethod,
                                      String serviceName, String regionName) {
        super(endpointUrl, httpMethod, serviceName, regionName);
    }

    /**
     * Computes an AWS4 signature for a request, ready for inclusion as an
     * 'Authorization' header.
     *
     * @param headers         The request headers; 'Host' and 'X-Amz-Date' will be added to
     *                        this set.
     * @param queryParameters Any query parameters that will be added to the endpoint. The
     *                        parameters should be specified in canonical format.
     * @param bodyHash        Precomputed SHA256 hash of the request body content; this
     *                        value should also be set as the header 'X-Amz-Content-SHA256'
     *                        for non-streaming uploads.
     * @param awsAccessKey    The user's AWS Access Key.
     * @param awsSecretKey    The user's AWS Secret Key.
     * @return The computed authorization string for the request. This value
     * needs to be set as the header 'Authorization' on the subsequent
     * HTTP request.
     */
    public String computeSignature(Map<String, String> headers,
                                   Map<String, String> queryParameters,
                                   String bodyHash,
                                   String awsAccessKey,
                                   String awsSecretKey) {
        // first get the date and time for the subsequent request, and convert
        // to ISO 8601 format for use in signature generation
        Date now = new Date();
        this.dateTimeStamp = dateTimeFormat.format(now);

        // update the headers with required 'x-amz-date' and 'host' values
        headers.put("x-amz-date", dateTimeStamp);

        String hostHeader = endpointUrl.getHost();
        int port = endpointUrl.getPort();
        if (port > -1) {
            hostHeader = hostHeader.concat(":" + Integer.toString(port));
        }
        headers.put("Host", hostHeader);

        // canonicalize the headers; we need the set of header names as well as the
        // names and values to go into the signature process
        String canonicalizedHeaderNames = getCanonicalizeHeaderNames(headers);
        String canonicalizedHeaders = getCanonicalizedHeaderString(headers);

        // if any query string parameters have been supplied, canonicalize them
        String canonicalizedQueryParameters = getCanonicalizedQueryString(queryParameters);

        // canonicalize the various components of the request
        String canonicalRequest = getCanonicalRequest(endpointUrl, httpMethod,
                canonicalizedQueryParameters, canonicalizedHeaderNames,
                canonicalizedHeaders, bodyHash);
        log.debug("Canonical request: {}", canonicalRequest);

        // construct the string to be signed
        String dateStamp = dateStampFormat.format(now);
        this.scope = dateStamp + "/" + regionName + "/" + serviceName + "/" + TERMINATOR;
        String stringToSign = getStringToSign(SCHEME, ALGORITHM, dateTimeStamp, scope, canonicalRequest);
        log.debug("String to sign: {}", stringToSign);

        // compute the signing key
        byte[] kSecret = (SCHEME + awsSecretKey).getBytes(StandardCharsets.UTF_8);
        byte[] kDate = sign(dateStamp, kSecret, "HmacSHA256");
        byte[] kRegion = sign(regionName, kDate, "HmacSHA256");
        byte[] kService = sign(serviceName, kRegion, "HmacSHA256");
        this.signingKey = sign(TERMINATOR, kService, "HmacSHA256");
        byte[] signature = sign(stringToSign, signingKey, "HmacSHA256");

        // cache the computed signature ready for chunk 0 upload
        lastComputedSignature = BinaryUtils.toHex(signature);

        String credentialsAuthorizationHeader =
                "Credential=" + awsAccessKey + "/" + scope;
        String signedHeadersAuthorizationHeader =
                "SignedHeaders=" + canonicalizedHeaderNames;
        String signatureAuthorizationHeader =
                "Signature=" + lastComputedSignature;

        return String.format("%s-%s %s, %s, %s",
                SCHEME, ALGORITHM, credentialsAuthorizationHeader, signedHeadersAuthorizationHeader, signatureAuthorizationHeader);
    }

    /**
     * Calculates the expanded payload size of our data when it is chunked
     *
     * @param originalLength The true size of the data payload to be uploaded
     * @param chunkSize      The size of each chunk we intend to send; each chunk will be
     *                       prefixed with signed header data, expanding the overall size
     *                       by a determinable amount
     * @return The overall payload size to use as content-length on a chunked
     * upload
     */
    public static long calculateChunkedContentLength(long originalLength, long chunkSize) {
        if (originalLength <= 0) {
            throw new IllegalArgumentException("Nonnegative content length expected.");
        }

        long maxSizeChunks = originalLength / chunkSize;
        long remainingBytes = originalLength % chunkSize;
        return maxSizeChunks * calculateChunkHeaderLength(chunkSize)
                + (remainingBytes > 0 ? calculateChunkHeaderLength(remainingBytes) : 0)
                + calculateChunkHeaderLength(0);
    }

    /**
     * Returns the size of a chunk header, which only varies depending on the
     * selected chunk size
     *
     * @param chunkDataSize The intended size of each chunk; this is placed into the chunk
     *                      header
     * @return The overall size of the header that will prefix the user data in
     * each chunk
     */
    private static long calculateChunkHeaderLength(long chunkDataSize) {
        return Long.toHexString(chunkDataSize).length()
                + CHUNK_SIGNATURE_HEADER.length()
                + SIGNATURE_LENGTH
                + CLRF.length()
                + chunkDataSize
                + CLRF.length();
    }

    /**
     * Returns a chunk for upload consisting of the signed 'header' or chunk
     * prefix plus the user data. The signature of the chunk incorporates the
     * signature of the previous chunk (or, if the first chunk, the signature of
     * the headers portion of the request).
     *
     * @param userDataLen The length of the user data contained in userData
     * @param userData    Contains the user data to be sent in the upload chunk
     * @return A new buffer of data for upload containing the chunk header plus
     * user data
     */
    public byte[] constructSignedChunk(int userDataLen, byte[] userData) {
        // to keep our computation routine signatures simple, if the userData
        // buffer contains less data than it could, shrink it. Note the special case
        // to handle the requirement that we send an empty chunk to complete
        // our chunked upload.
        byte[] dataToChunk;
        if (userDataLen == 0) {
            dataToChunk = FINAL_CHUNK;
        } else {
            if (userDataLen < userData.length) {
                // shrink the chunk data to fit
                dataToChunk = new byte[userDataLen];
                System.arraycopy(userData, 0, dataToChunk, 0, userDataLen);
            } else {
                dataToChunk = userData;
            }
        }

        StringBuilder chunkHeader = new StringBuilder();

        // start with size of user data
        chunkHeader.append(Integer.toHexString(dataToChunk.length));

        // nonsig-extension; we have none in these samples
        String nonsigExtension = "";

        // if this is the first chunk, we package it with the signing result
        // of the request headers, otherwise we use the cached signature
        // of the previous chunk

        // sig-extension
        String chunkStringToSign =
                CHUNK_STRING_TO_SIGN_PREFIX + "\n" +
                        dateTimeStamp + "\n" +
                        scope + "\n" +
                        lastComputedSignature + "\n" +
                        BinaryUtils.toHex(AWS4SignerBase.hash(nonsigExtension)) + "\n" +
                        BinaryUtils.toHex(AWS4SignerBase.hash(dataToChunk));

        // compute the V4 signature for the chunk
        String chunkSignature = BinaryUtils.toHex(AWS4SignerBase.sign(chunkStringToSign, signingKey, "HmacSHA256"));

        // cache the signature to include with the next chunk's signature computation
        lastComputedSignature = chunkSignature;

        // construct the actual chunk, comprised of the non-signed extensions, the
        // 'headers' we just signed and their signature, plus a newline then copy
        // that plus the user's data to a payload to be written to the request stream
        chunkHeader.append(nonsigExtension).append(CHUNK_SIGNATURE_HEADER).append(chunkSignature);
        chunkHeader.append(CLRF);

        try {
            byte[] header = chunkHeader.toString().getBytes("UTF-8");
            byte[] trailer = CLRF.getBytes("UTF-8");
            byte[] signedChunk = new byte[header.length + dataToChunk.length + trailer.length];
            System.arraycopy(header, 0, signedChunk, 0, header.length);
            System.arraycopy(dataToChunk, 0, signedChunk, header.length, dataToChunk.length);
            System.arraycopy(trailer, 0,
                    signedChunk, header.length + dataToChunk.length,
                    trailer.length);

            // this is the total data for the chunk that will be sent to the request stream
            return signedChunk;
        } catch (Exception e) {
            throw new RuntimeException("Unable to sign the chunked data. " + e.getMessage(), e);
        }
    }
}

redpajama_set_name: RedPajamaGithub


This is a placeholder page for Corey Bell, which means this person is not currently on this site. We do suggest using the tools below to find Corey Bell.
You are visiting the placeholder page for Corey Bell. This page is here because someone used our placeholder utility to look for Corey Bell. We created this page automatically in hopes Corey Bell would find it. If you are not Corey Bell, but are an alumni of East Prairie High School, register on this site for free now.


text:
use DBI;
use List::Util 'shuffle';

$result_dir = $ARGV[0];
$start_value = $ARGV[1];
$stop_value = $ARGV[2];

#
# Set up DB connections
#
	my $dbh = DBI->connect("DBI:mysql:nfp:sloth:3306", "nfp", "secret");
	my $get_rating = $dbh->prepare('select rating from movie_rating where `movie_id` = ? and `user_id` = ? limit 1');

open(PROBE, "< /home/simon/np/probe.txt") || die "can't read: $!\n";
while (<PROBE>){
	chomp;
	if(/.*\:$/){
		($movie_id) = (split /:/, $_);
		$movie_number++;
		$percdone = $numValues/1425333;
		if ($movie_id == $start_value){
			$status = "go";
		}
		if ($movie_id == $stop_value){
                        $status = "stop";
                }
	}
	else{
		if ($status eq "go"){
			$user_id =  $_;

			$get_rating->execute("$movie_id", "$user_id");
			@get_rating_response = $get_rating->fetchrow;
			$rating = $get_rating_response[0];

			($prediction,$user_avstddev_ratings,$user_av_ratings, $seer_rating_average, $std_status) = &predict_rating($movie_id, $user_id);
			open(RESULTS,">>/home/simon/np/good/dist/linux/$result_dir/results.txt");
			# MovieID, rating, prediction, std, user average, seer average, whether std was used in prediction
			#print RESULTS "$prediction, $rating\n";
			my $delta = $rating - $prediction;
			$delta = abs($delta);
			print RESULTS "$movie_id,$rating,$prediction,$delta,$user_avstddev_ratings,$user_av_ratings,$std_status\n";
			close(RESULTS);
			$numValues++;
			$sumSquaredValues += $delta*$delta;
		}

	}
}
close(PROBE);

sub predict_rating {
	my $movie =  $_[0];
	my $user = $_[1];

	my $get_user_movies = $dbh->prepare('select movie_id,rating from movie_rating where user_id = ?');
	$get_user_movies->execute("$user");

	my @user_movies;
	my @row0;
	my %target_user_ratings;
	my $movie_count;
	my $total_seers;
        my $seer_user_id;
        my %seer_user_ratings;
        my %seer_user_hit_count;
        my $total_seer_rating_delta;

        my $seer_rating_average_calc;
        my $seer_rating;

        my %predictor_value_hash;

        my $count;
	my $first_movie;
	my $seer_movie;
	my $get_seer_moviesq;
	my $secount = 0;

	while ( @row0 = $get_user_movies->fetchrow_array ) {
		# These are all the movies that user has seen
		push @user_movies, $row0[0];

		# This is target user's ratings
		#$target_ratings{$movie} = $row[1];
		$target_user_ratings{$row0[0]} = $row0[1];
  	}

	my $get_user_stats = $dbh->prepare('select avg(rating), stddev(rating) from movie_rating where user_id =  ?');
	$get_user_stats->execute("$user");
	my $user_av_ratings;
	my $user_avstddev_ratings ;
	while ( @stats = $get_user_stats->fetchrow_array ) {

                # This is target user's avg ratings
                $user_av_ratings = $stats[0];
                $user_avstddev_ratings = $stats[1];
        }

	$movie_count = @user_movies;
	print "\nCurrent user [$user] has seen $movie_count movies, beginning to cross reference...";

	my $sample;
	if ($movie_count > 500){
		$sample = "limit 700000";
	}elsif(($movie_count < 500) and ($movie_count > 400)){
		$sample = "limit 800000";
	}elsif(($movie_count < 400) and ($movie_count > 300)){
                $sample = "limit 900000";
	}elsif(($movie_count < 300) and ($movie_count > 200)){
                $sample = "limit 1000000";
	}elsif(($movie_count < 200) and ($movie_count > 100)){
                $sample = "limit 1100000";
	}
	# Else no limit...

	#print "Sample is $sample\n";

	# Randomize sample
	@user_movies = shuffle(@user_movies);
	$first_movie = $user_movies[0];
	$get_seer_moviesq = "select user_id, rating, movie_id from movie_rating where user_id != $user and (movie_id = $first_movie";
	foreach $seer_movie (@user_movies) {
                if ($seer_movie != $movie){
                        $get_seer_moviesq = "$get_seer_moviesq or movie_id = $seer_movie";
                }
        }
        $get_seer_moviesq = "$get_seer_moviesq ) $sample";

	$get_seer_movies = $dbh->prepare("$get_seer_moviesq");
	$total_seers = $get_seer_movies->execute();

	while ( @row1 = $get_seer_movies->fetchrow_array ) {

                # This is seer's ratings
		$seer_user_id = $row1[0];
                $seer_user_ratings{$seer_user_id} = $row1[1];

		$seer_rating = $row1[1];
                $seer_movie = $row1[2];

		# Going through list of all movies seen by both seer and user
		$count = 0;
               	$count++;

		# Get the delta
		$user_rating = $target_user_ratings{$seer_movie};
		$seer_rating_delta = abs($user_rating - $seer_rating);
		$total_seer_rating_delta{$seer_user_id} = $total_seer_rating_delta{$seer_user_id} + $seer_rating_delta;

        	$seer_user_hit_count{$seer_user_id} = $seer_user_hit_count{$seer_user_id} + 1;

	}

	for my $seer (keys %seer_user_hit_count){
		my $percentage_hit =  $seer_user_hit_count{$seer}/$movie_count;
		my $predictor_value = $total_seer_rating_delta{$seer} / $percentage_hit;

		if (($predictor_value == 0) and ($percentage_hit < .05)){
			delete $seer_user_hit_count{$seer};
			delete $total_seer_rating_delta{$seer};
		}
		else{
			$predictor_value_hash{$seer} = $predictor_value;
		}
	}
        # Calculating the top percentage of seers to use
        my $number_of_valued_predictors;
        $number_of_valued_predictors = keys (%predictor_value_hash) * .00001 ;
	# Round the number
	$number_of_valued_predictors = int($number_of_valued_predictors + 5);

	my @sorted_predictor_value_keys_by_value;
        @sorted_predictor_value_keys_by_value = sort { $predictor_value_hash{$a} <=> $predictor_value_hash{$b} } keys %predictor_value_hash;

        # Shorten the array by the number that we are interested in
        $#sorted_predictor_value_keys_by_value = $number_of_valued_predictors;

	$predictor_numbers = @sorted_predictor_value_keys_by_value;

	my $weight_count;
	my $weight;
	my $value;
	my $total_value_calc;
	my $total_weight_calc;
	foreach my $seer_uid (@sorted_predictor_value_keys_by_value){

		$weight_count++;
                $seer_rating = $seer_user_ratings{$seer_uid};
		$weight = $predictor_numbers / $predictor_numbers + $weight_count;
		$total_weight_calc = $total_weight_calc + $weight;
		$value = $weight * $seer_rating;
                $total_value_calc = $total_value_calc + $value;
        }

        $seer_rating_average = $total_value_calc/$total_weight_calc ;

	my $uar_weight;
	if ($user_avstddev_ratings != 0){
		$uar_weight = 1 / $user_avstddev_ratings;
	}
	else{
		$uar_weight = 1000000;
	}
	my $uar_value ;
	$uar_value = $uar_weight * $user_av_ratings;

	my $std_dev_weighted_average ;
	$std_dev_weighted_average = ($seer_rating_average + $uar_value) / (1 + $uar_weight);

#	print "Using the top $predictor_numbers similar users to compare against\n";
#	print "User's standard deviation is $user_avstddev_ratings, user's average rating is $user_av_ratings";
#	print "Seer Average calculation is ($total_value_calc/$total_weight_calc)\n";
#	print "SD Weighted average calculation is ($seer_rating_average + $uar_value) / (1 + $uar_weight)\n" ;
#	print "Average seer rating: $seer_rating_average \n";
#	print "Weighted average seer rating: $std_dev_weighted_average  \n";

	if ($user_avstddev_ratings < .5){
		$std_dev_weighted_average = int($std_dev_weighted_average + .5);
#		print "Returned user standard deviation included value\n";
		# Prediction, std, user average, seer average, whether std was used in prediction
		return($std_dev_weighted_average,$user_avstddev_ratings,$user_av_ratings, $seer_rating_average, STD);
	}

    	$seer_rating_average = int($seer_rating_average + .5);
	return($seer_rating_average,$user_avstddev_ratings,$user_av_ratings,$seer_rating_average,NSTD);
}


Consortium is a great place to work!
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text:
Q: Include admins in author drop-down on edit post screen In the back-end when editing a post there is a dropdown to select post author which is populated by registered usernames.
But, users with an admin role do not appear in the list, there is an "Admin" which appears top of the list.
That means the only way to assign a post to a particular user with role = admin is to go into phpMyAdmin and manually update the entry in the wp_post table.
Anyone know how to override the behaviour that removes admins from the dropdown?
[EDIT]
I inherited my theme files from someone else and now see that they had added a function in functions.php to manipulate the dropdown (I have CPTs which can be posted via forms on the front-end. All my users are subscribers, and so to be able to reassign posts in the back-end, that dropdown box is rebuilt to include users with role = subscriber. The admins hadn't been properly added back in.)
For the record, anyone looking to manipulate that dropdown for whatever reason, you can hook into the filter wp_dropdown_users )
[/EDIT]

redpajama_set_name: RedPajamaStackExchange


text:
Update on Jenny
Updated on February 26, 2021 in General Stuff
Piecesofmalarkey 7 0 on December 21, 2020
The last week and a half has been, understandably, a bit sketchy with information coming from Detroit about my wife's niece, Jenny, but tonight we deciphered some news. Looks like Jenny has Stage 4 cancer. Still not sure of the exact prognosis, but I'm guessing it ain't good. After a few days in the U. of M. hospital, she's now gone home to Penny's and her husband Dan's house. Some good news is that if anybody can bear that burden financially and materially, it's those two.
Christmas will go on since there's really no choice but to move forward bravely.
As always, thanks for letting me vent.
Please select General Stuff
The last week and a half has been, understandably, a bit sketchy with information coming from Detroit about my wife's niece, Jenny, but tonight we deciphered some news. Looks like Jenny has Stage 4 cancer. Still not sure of the exact prognosis, but I'm guessing it ain't good. After a few days in the U. of M. hospital, she's now gone home to Penny's and her husband Dan's house. Some good news is that if anybody can bear that burden financially and materially, it's those two. Christmas will go on since there's really no choice but to move forward bravely. As always, thanks for letting me vent.
Fauxmaha 0 0 on December 21, 2020
Just awful stuff.
robjh22 1 0 on December 21, 2020
She's so young to have to endure this!
To the extent it helps and isn't trite, tell her your friends are wishing her well.
Piecesofmalarkey 0 on December 21, 2020
I will. Thank you.
She's so young to have to endure this!
To the extent it helps and isn't trite, tell her your friends are wishing her well.
Sidhedude 1 0 on December 21, 2020
That sucks, P. Let me know if there's anything I can do.
Thank you, sir. But there's really nothing anyone can do. This is as real as it gets and in the end, we're just bit players all trying to struggle through.
Thank you, sir. But there's really nothing anyone can do. This is as real as it gets and in the end, we're just bit players all trying to struggle through.
Piecesofmalarkey 1 2 on February 26, 2021
So about 3 weeks ago Jenny bugged out of Michigan, along with sister Penny, to Florida for some warm weather and walks on the beach. Penny shared pictures on FB that showed Jenny and her legitimately enjoying the break. Turns out Penny went back to Michigan last weekend- without Jenny. She's loving the walks on the beach and the non-Rona panic life (no masks and big smiles in the pictures) that she's just staying there. Penny says the plan at the moment are that Jenny will only return to Michigan for treatment. And then go back. That also takes a huge load off sis.
God, that's good news.
robjh22 0 on February 26, 2021
Glad to hear it. Sounds like your family was due for some good news!
So about 3 weeks ago Jenny bugged out of Michigan, along with sister Penny, to Florida for some warm weather and walks on the beach. Penny shared pictures on FB that showed Jenny and her legitimately enjoying the break. Turns out Penny went back to Michigan last weekend- without Jenny. She's loving the walks on the beach and the non-Rona panic life (no masks and big smiles in the pictures) that she's just staying there. Penny says the plan at the moment are that Jenny will only return to Michigan for treatment. And then go back. That also takes a huge load off sis.
God, that's good news.
Click here to start your discussion


text:
HomeFeaturesChampions League flops are no laughing matter
Champions League flops are no laughing matter
There was plenty for West Ham fans to laugh about as Arsenal and Chelsea continued to flounder in the Champions League.
October 9, 2015 Blowing Bubbles Features 0
Yet while the results will have given one or two people some fun at work there could be an unexpected consequence for the Hammers. If English teams continue to struggle there is a real chance Uefa will cut the number of spots available to Premier League teams – with the number being cut back to three from the current four.
That would be a real kick in the teeth for the Premier League – which prides itself as being 'the best league in the world'. It's strange the results have gone the way they have as you don't need to look too far back to when the English clubs were dominating and had teams in the semi-finals and final every year in the mid-2000s. If the place is lost – and the success of the Italian clubs means this could well happen – it will hit the big clubs hardest because they won't have the luxury of having a bad season and scraping into the Champions League in fourth.
For the rest of the league though it'll make the challenge of getting into Europe even harder. It's very tough already and one less place will make it more difficult to compete with the likes of Arsenal, Manchester United, City and Chelsea
Keeping what we've got is as good as a brand new signing
Blowing Bubbles' top writers settle down to put the world to rights…


Average: 4.5 / 5 stars, based on 3 reviews.
= PERFECT coffee experience… Thank you she said…. You're very welcome, he said….we are all about you wanting to come back again… And again…..
Excellent coffee- could this be the best in Canning Vale?
Only open Friday, Saturday and Sunday Mornings. Quirky and cool.


Impara, J. C., Wolkowitz, A.A., & Buckendahl, C. W. (2015). Closing the loop: Providing test developers with performance level descriptors so standard setters can do their job. Presented at the 2015 Standard-setting: International state of research and practices in the Nordic countries conference, Centre for Educational Measurement in Oslo, Norway.


text:
Audible Empire: Music, Global Politics, Critique
Review of Ronald Radano and Tejumola Olaniyan (eds), Audible Empire: Music, Global Politics, Critique (Duke University Press, 2016). Written in 2016 and published as 'The Endless Circuits of Global Music' in Reviews in Cultural Theory 8/1 (2019): 17-22.
The possibilities for connecting the musics of the world to assumptions about cultural identity were amplified significantly with the advent of recorded sound in the late nineteenth century, a period contemporaneous with extensive imperialist projects undertaken by Euro-American powers. The ensuing phonographic era provided an increasingly accessible soundtrack to the shift from colonialism and empire to a period of more general globalisation.
The role of global musics in constituting regional, national, racial, sexual and other identities in the phonographic era has become an area of growing scholarly interest, with important recent books including Michael Denning's study of the global recording boom of the 1920s and 1930s, Roshanak Kheshti's analysis of race and gender in the world music industry and the innovative collection of texts on 'seismographic sounds' published by the Norient network. Audible Empire, a collection of sixteen wide-ranging essays combining 'music, global politics [and] critique', adds to this literature through engaging studies of Mexican sonideros, Cuban hip hop, field recordings from Mozambique, jazz in interwar Shanghai, tango in contemporary Buenos Aires and much more. The essays are written from a variety of intersectional perspectives that emphasise historicity, hybridity, flows, channels, interstices and unexpected details: the role of cigarettes in the Chinese jazz scene of the 1930s; the use of dub poetry in 1990s to narrate the end of the cold war; the recasting of music-making as 'exemplary labour' in South Africa; the politics of protecting music as 'intangible heritage' in Argentina.
As described in an informative introduction by editors Ronald Radano and Tejumola Olaniyan (both professors at the University of Wisconsin, Madison), the imposition of Euro-western tonality played a vital role in the project of colonialism. Sound which fell outside the melodic, harmonic and rhythmic norms of the colonisers was typically cast as noise or sonic barbarity, further proof of the need for civilising force. This historical notion can be (and is, in this book) traced though to our present society, for sound, as an excessive and ultimately uncontainable force, has the ability to continually fill, create or otherwise colonise new spaces. Audible empires of various sizes and structures surround us on a daily basis and we are made regularly aware of the ways in which noise can disrupt, disturb or comfort. By bringing together insights from ethnomusicology and contemporary sound studies, while keeping an ear open to history, Audible Empire mixes nation-defining colonial projects with an understanding of sound as a border-crossing entity caught up in, and sometimes foretelling, processes of everyday globalisation.
There is much to savour at length in this collection; here I focus on the essays that I found particularly engaging. Following Michael Denning's essay on the decolonisation of the ear through recorded music (an argument with which I felt familiar through its more extensive discussion in the author's Noise Uprising), I was drawn to Nan Enstad's fascinating text on jazz and cigarette smoking in interwar Shanghai. By bringing these aspects together in her essay, Enstad is able to succinctly unpack the relationship between multinational corporations (the tobacco and culture industries), the semiotics of popular culture (cigarettes, sartorial style, jazz music) and the processes by which music creates spaces for illicit pleasures; dancing and sharing cigarettes, in this case, allowing for moments of imperial intimacy.
Andrew Jones's essay on 'circuit listening', which unfolds around a case study of 1960s Hong Kong pop diva Grace Chang, makes a strong case for music scenes as both historically specific and overlapping. Discussing the ways in which Chang was able to appropriate foreign musical styles, Jones writes, 'Globally circulating genres such as mambo and calypso … are musical vernaculars, emerging from particular (and often marginalized) cultural circuits, and they serve as a common language between an imperial dominant and local particulars.' (78) What I found revelatory in this essay was the sense of the circuit covering so many different places, with no clear origin or destination, just the seemingly endless circuitry of music genres and global flows. To be cosmopolitan, then as now, was to be aware of these flows and to find ways to join and extend the circuit, through cultural appropriation if need be.
Elsewhere the circuits being emphasised are those which produce an international network of resistance. Marc Perry writes of 'circuits of solidarity' that have long connected African American and Cuban revolutionary campaigns (217), as personified in figures such as Assata Shakur, a Black Panther wanted by the authorities in the US and granted asylum in Cuba (and given hip hop credence as godmother to Tupac Shakur). The need for solidarity in the face of discrimination comes to the fore in Nitasha Sharma's essay on what she terms 'post-9/11 Brown', a lumping-together of culturally diverse groups in the wake of kneejerk reactions to Middle Eastern, West Asian and South Asian foreignness in twenty-first century America. The gradual conflation of these groups has led to a situation in which post-9/11 Brown subjects cross-identify and, in the musical field, often do so via the longstanding tools and techniques of hip hop's Black American grammar. The cultural, ethnic and religious conflation of these subjects serves as both an object of critique and a platform of strategic (self-)essentialism among the performers Sharma discusses. So too are US-based media platforms such as Google, Facebook, YouTube and Twitter seen by younger musicians and activists as simultaneously objects of imperialism and platforms for self-expression and communal mobilisation. Facebook, in the words of rapper Chee Malabar, 'has more information about people than the FBI or CIA' (307), but it has also worked to bring otherwise isolated groups into conversation with each other.
Such observations tally with those made by Michael Hardt and Antonio Negri when they discuss globalisation as both threat and opportunity, and I was often surprised, when reading Audible Empire, not to find more reference to Hardt and Negri's work; only Gavin Steingo makes explicit use of their book Empire in his discussion of South African kwaito. While it's by no means compulsory to subscribe to Hardt and Negri's take on Empire (which they capitalise in order to demarcate it as a newly understood concept based on a 'monarchical' order of dominant international organisations), it has shaped a substantial amount of debate on the subject in the new millennium and might have warranted more discussion than it receives here. Radano and Olaniyan do state early on, however, that they wish to move away from what they interpret (unconvincingly, in my view) as a 'neoliberal turn' in contemporary sound studies and to do so via a return to the historicity of local, material examples with seemingly clear root and branch manifestations. Perhaps the notion of Empire as a more rhizomatic, placeless entity conflicts too much with these aims. This would be fair enough except that the editors also claim the same aims and objectives for the other contributors to the volume and I'm not so sure that all the essayists here are so antithetical to the notion of a post-material Empire.
As is perhaps inevitable with a set of texts so caught up in notions of flow, migration and hybridity, there is space for the deployment of many provocative metaphors. Josh Kun, who explores the migrational aspects of music cultures via the example of Mexican sonideros, uses the crossfade as a metaphor for border crossing: 'The art of the crossfader is not only moving between two worlds but also moving between them seamlessly and strategically, finding common beats, tempos, melodic moments – points of convergence that allow new mixes to be born. Crossfading mixes while preserving difference, and it slides between worlds without fully erasing one in the pursuit of another' (102). Meanwhile Micol Seigel, reflecting on the unfortunate career of Brazilian musician Elsie Houston, writes that 'Music from somewhere else offers a Rorschach blot of the highest order' (120). Her point is about interpretation, and she notes that music can be used as evidence for more or less anything one might wish to argue. Against such tendencies, Seigel places the necessity to consider historical and social contexts and the fields of possibility that mark the hard lines of difference between music and musicians and their places and times. Brent Hayes Edwards sounds a relative note when discussing the African fieldwork undertaken by Hugh Tracey in the 1940s. Citing the critique of Tracey produced by Leroy Vail and Landeg White four decades later, Hayes Edwards writes of a 'counterarchival' approach that can be launched against the cultural misunderstandings of the past, based as they inevitably were on particular historical, imperial and prejudicial (or at least essentialist) positions. But the intent here is not just to blast the blunders and shortcomings of past perspectives but 'to ask whether an archive devoted to the sedimentation of the "traditional" can be used or abused to trace a history of transformation' (272). Is it possible, Hayes Edwards wonders, 'to excavate from Tracey's archive of African music a counterarchive of anticolonialism in sound?' (272). More than a Rorschach blot, then, the trace left by the music from spatial and temporal elsewheres may continue to inform as much as reflect.
Missing from some of the essays is an extensive discussion of sound itself, with the audibility of Empire sometimes being left as an implicit rather than explicit presence in the narratives. I found myself thirsting, for example, for knowledge of how the sonic textures of Chee Malabar's music might underline, extend or even contradict his powerful lyrics. The Internet can, of course, help to quench this thirst but it would still be useful to hear how these essayists hear the sound of Empire in the music they discuss. It is perhaps fitting, then, that the collection concludes with Kofi Agawu's description of the 'musical violence' done to African subjects during the colonial era through the imposition of Western European tonality by missionaries and other 'educators'. Protestant hymns, Agawu argues, would 'keep Africans trapped in a prisonhouse of diatonic tonality' from which the sonic language of the continent has struggled to escape (337-8). Agawu locates the traces of this tonality in a series of examples drawn from popular and art music, searching for moments where an active rather than passive hybridity can be discerned; not in South Africa's Ladysmith Black Mambazo or Ghana's Peace Brass Band, apparently, but perhaps in Nigerian composer Joshua Uzoigwe and Ga highlife band Wulomei. That Agawu's analysis draws on a musical grammar developed to accommodate European art music is an issue that is not discussed, however.
At any given point in the phonographic era, we can find configurations of musical style, lyric, language, performance technique or dissemination method that will tell us something about the nature of contemporary Empire. This is a story which emerges again and again from these essays, but that doesn't make the story repetitive, tiring or boring; rather, the enjoyment is in the detail, the variation, the subtle shading of the standard experience. Reading about tango's journey towards UNESCO recognition as intangible heritage, I was struck by many parallels with Portuguese fado, a musical world and cultural context with which I have more familiarity. This in turn recalled for me the studies of fado I discovered in Buenos Aires book shops (including at least one comparative study of fado and tango) and how that discovery once again challenged the way I've tended to consider global cultural networks from a UK perspective.
What becomes evident from Audible Empire is the extent to which any group of people can be any other group of people's exotic and/or feared others. This may recall Arjun Appadurai's call to resituate globalisation theory away from still dominant 'West and the Rest' perspectives, an ambition which seems central to many of the contributors to this collection. If it remains questionable to what extent such a goal can be achieved when we are only provided, as in this book, with narratives emanating from U.S. academic institutes, at least those narratives invite us to consider numerous intersectional perspectives. At its best, Audible Empire helps to displace common tropes of imperialist debate and encourages its readers to listen to the soundtrack of Empire's past and present with refreshed ears.
Appadurai, Arjun. Modernity at Large: Cultural Dimensions of Globalization. Minneapolis: U. of Minnesota Press, 1996.
Beyer, Theresa, Thomas Burkhalter and Hannes Liechti, eds. Seismographic Sounds: Visions of a New World. Bern: Norient, 2015.
Denning, Michael. Noise Uprising: The Audiopolitics of a World Musical Revolution. London: Verso, 2015.
Hardt, Michael and Antonio Negri. Empire. Cambridge, MA: Harvard UP, 2000.
Kheshti, Roashanak. Modernity's Ear: Listening to Race and Gender in World Music. New York: New York University Press, 2015.


text:
New advanced stereo videoprobe added to rental fleet
Ashtead Technology has added the Olympus IPLEX RX to its rental fleet of remote visual inspection equipment. "We have been very impressed with the functionality of this new videoprobe, and we believe that it will be particularly popular with our customers; as a high-value instrument it is ideal for rental," said Branch Manager Alan Hasson. "The main advantages are an advanced imaging capability and a screen-switching system that enables users to employ in-built stereo measurement technology to easily measure defects from a variety of different angles.
"The stereo measurement facility provides users with enormous capability to accurately characterise defects; a 'distance' mode enables the measurement of defect length by clicking the cursor at both ends of the defect. In the 'point-to-line' mode, it is possible to create a reference line and then measure a distance from that line. Similarly, a 'depth' mode enables the measurement of depth or height from a specified reference surface to any point, and an 'area/lines' mode can be employed to measure the circumference or area between marker points.
"Users are able to quickly switch between normal observation mode to the stereo modes, and measurements are quick and easy to undertake."
The IPLEX RX produces the best video and still image quality of any Olympus videoscope thanks to a unique PulsarPic™ image processor, which reduces noise and sharpens images, resulting in an exceptionally high-resolution image. This is complemented by a new LED illumination system that is approximately twice as bright as conventional videoscopes, and dynamically adjusts light output to reduce halation when metal or reflective surfaces are inspected. The image processor interacts intelligently with the illumination system to deliver an optimised amount of light and gain enhancement to provide images that are very clear and sharply defined.
Weighing just 2.9 kg, the IPLEX RX is battery powered, running for up to two hours on a single charge. It also features a 6.6" monitor and has been designed to military specifications, passing a range of severe environmental tests, such as blowing rain/dust, high humidity and icing rain. In addition, the low-reflection daylight view monitor displays clear images, even under bright sunlight. The insertion tube is covered with a tough, processed tungsten braid and is high-temperature resistant, crush and abrasion proof.
Summarising, Alan Hasson said: "The advanced capability of this new instrument will make it popular in inspection applications within industries such as aerospace, oil & gas, power generation, renewable energy, processing and manufacturing, and the availability of rental systems will mean that stereo measurement technology is now available to everyone, without the burden of capital cost."
www.ashtead-technology.com


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Ground Corn, Soybean Meal, Wheat Bran, Calcium Carbonate, Cane Molasses, Canola Oil, Oyster Shell Flour, Suncured Alfalfa Meal, Mono Dicalcium Phosphate, Flax Seed, Salt (Sodium Chloride), Choline Chloride, Marigold Extract, Red Pepper Extract, Propionic Acid (a preservative), Zinc Oxide, Manganous Oxide, Ferrous Sulfate, Vitamin A Acetate, Vitamin E (Alpha Tocopherol), Vitamin D3 Supplement, DL-Calcium Pantothenic Acid, Riboflavin Supplement, Niacin Supplement, Vitamin K (Menadione Sodium Bisulfite Complex), Thiamine Mononitrate Pyridoxine Hydrochloride, Copper Sulfate, Ethylenediamine Dihydriodide, Vitamin B12 Supplement, Folic Acid, Sodium Selenite (Selenium).


text:
800 consensus group
Guitar Army Manifesto
GuitarArmy.net
Music universal language
How to join the Guitar
Lineup Thursday
army structure
Thursday Coming
fostering world peace
City Weely
Consensus group
Merry Christmas, looking for a consensus group.
What is the consensus group? I'm looking for 800 people who would like to weigh in on any given issue. The premise here is that 800 opinions are generally, when averaged, the right answer.
The idea. Get 800 people to guess on the close of the Dow Jones Average tomorrow, and the average guess will be very close to where the Dow will close.
If you fill a quart jar with beans, and get 800 people to guess on how many beans are in the jar. The average will be the number of beans in the jar.
DailyThis is where it begins, the online writing.
The door to this website now open. And then to begin to peek inside.
Dying is the spirit leaving the body. Spirit is consciousness. You can put it back. Start with the toes.
So this day, this day to come, comes at me at a speed. And wraps around my world as I adapt. Adapt to each and every change, by harmonizing with the now. And flow from moment to moment - the mind, logic has lost its grip or ratchets up a little.
A higher vibration, the angelic realm in sight. A higher state, one that starts out where/as we are, then follows the path to the higher realm, the higher vibration. One can be told but it won't take. The path is walked alone. And on it there are guides to help you along the way. You are never alone, we are always one.
Quickened, how is one quickened?
Prayer perhaps.
By focusing one's attention on that high source within us, that action changes our vibration to a higher frequency.
We are quickened, so to speak.
To bring the world out of the state of discord, into a state of harmony.
Guitar Amy Purpose
The Guitar Army aspires to include all the individual members of humanity, that they may join together through the universal language of music and come to celebrate Joy as their intent rather than strife.
Marching on the world
Guitar Army
Musicians around the world unite.
Come join the Guitar Army.
Drown out the drums of war with your music of joy.
Call them to put down their guns and pick up a guitar.
The Guitar Army is a thing of contagion where those who are exposed to it want to join in the drowning out the noise of dissension we hear now.
Make music not war
The Guitar Army seeks the foot soldiers. The private. The man in the trenches, your sisters, your brothers, your children, your parents and grandparents, the kid next-door., All over the world.
The Guitar Army invites you to form a band - your family.
Play music with them and come join our forces. Add your voices with those who would build a new dream of a harmonious world.
Express your desire to join this movement. To add your voice to the chorus of those who seek a harmonious world.
You'll be given a number from anyone you ask in the Guitar Army. It will be the next number of the people who have joined that line.
Then, you'll be that number in their line/army, and number 1 in your own line/army/Band. So when someone asks you to join the Guitar Army, they'll be the next available number in your line/army and number one in their own Band ... and so on!
Example: Jake is number 33 in my army/line/Band. Number 1 in his own band. His son is number 2 in Jakes band/line and so on.
Your Band
This is your choosen family.
Hopefully it will include your blood, but the Guitar Army assumes we are all of the same blood,
In music we join together
in song we raise our voices and take the world to a new dream, a dream of harmony
Schiller/Beethoven
Joy, beautiful spark of the gods,
Daughter from Elysium,
We enter, drunk with fire,
Heavenly One, thy sanctuary!
Your magic binds again
What convention strictly divides;*
All people become brothers,*
Where your gentle wing abides.
Who has succeeded in the great attempt,
To be a friend's friend,
Whoever has won a lovely woman,
Add his to the jubilation!
Indeed, who calls even one soul
Theirs upon this world!
And whoever never managed, shall steal himself
Weeping away from this union!
All creatures drink of joy
At nature's breast.
Just and unjust
Alike taste of her gift;
She gave us kisses and the fruit of the vine,
A tried friend to the end.
[Even] the worm has been granted sensuality,
And the cherub stands before God!
Gladly, as His heavenly bodies fly
On their courses through the heavens,
Thus, brothers, you should run your race,
Joyful, like a hero going to conquest.
You millions, I embrace you.
This kiss is for all the world!
Brothers, above the starry canopy
There must dwell a loving Father.
Do you fall in worship, you millions?
World, do you know your creator?
Seek him in the heavens
Above the stars must He dwell.
THIS IS ABOUT THE WAVE
You've seen them at basket ball and foot ball games.
When the fans look in the TV monitors and do a stand up then sit down in a sequence that makes a visual wave that travels all around the arena.
The Wave we're putting toether is a sound wave that travels around the world.
It goes like this:
Every Thursday at 7pm local time, where ever you are,
sing/play on your phone/join with those around you,
The Od to Joy.
the sound will move througn each time zone and tavel all around the world.
The guitar army is about you, the individual. It's purpose is to liberate the individual from the shackles of the lower mind/the voice of the internal dialogue/– by redirecting one's attention Into music as it is a conduit to Joy in the individual.
The guitararmy.net should be an organism of consensus, that is it should be a way to establish consensus.
We're all to join together in the cause of joy, to take humanity to a state of joy, to use Music, a known conduit to Joy. That communication chain could be used as a means of organizing consensus. The collective will of those on the path to Joy.
The language spoken all over the world by every civilization. Everyone knows a musician. Everyone is a musician. Everyone is a singer. If we link together with a common voice if we share with our fellow musicians the dream of peace we can bring the world to peace A new Harmony. Do your part. ask five of your fellow musicians to join the Guitar Army and from each of the five ask them to bring five more. Soon we will sing as a single voice the single Corus around the world and pursue the dream of a new Harmony
What is the length of day at the equator? I recently told a friend with great certainty that at the equator the sun rose and set at exactly 12 hour intervals at roughly 6 a.m. and 6 p.m. (depending on the time zone) every day of the year. Now I'm not so sure.
You're right. It is always exactly 12 hours. There are a couple of different ways you can convince yourself that this is so, but I think the easiest one is this symmetry argument:
In the Northern Hemisphere, the length of the day is longer during the months when the North Pole is tilted towards the Sun and shorter during the months when it's tilted away from the Sun. The reverse is true for the Southern Hemisphere. The Equator is exactly halfway in between the poles. So it wouldn't make any sense for a day on the equator to be longer when one of the poles is tilted towards the Sun, and shorter when the other one is.
How to join the Guitar Army
Anyone can join,
everyone is the singer.
All you have to do is
text your name
With a picture of your shield perhaps and phone number
Or website
Would love your help. If you could stream some version of Ode to Joy, Thursday Evenings Around Sundown, preferably you playing or singing it hopefully with at least one friend and perhaps a whole band.
Stream it live on Facebook., And get everyone you know to do the same, who knows, It could be pretty fun.
The Wave of Joy will originate during sunset at the International Date Line.
It will travel West around the world, with the setting sun.
If you will Share this Post you will have pushed the world closer to world peace
Because everyone who embraces and communicates this idea adds their voice to those who would stand up for, vote for, request from their leaders, world peace. That we all, the world over, put down our guns and pick up a guitar.
When everyone shares this document, and embraces the cause of the guitarArmy.net World Peace, the sound of singing for joy will roll around the world every Thursday night at 7 PM local time
The central GuitarArmy.net theme is this: that music is the Universal Language. It is at the core of all of us. In each of us it is the conduit to joy. If we the people of the world link together under the banner of music and the joy it brings, we may redirect the focus of the world away from strife and towards creating joy
The interview with Kate MacLeod will be a discussion of what musicians as a world presence can do in guiding the world dream.
and, if they spoke/sang with a single or unified voice, could they improve the direction of the current dream we're in.
This Thursday Nights Lineup
This weeks
Joy Riders
Dave Buranak
Kelly Dobitz
And the mystery guests
The GuitarArmy
4 PM on till close
kokopelli's koffee House
3955 S Highland Dr
Holladay, Utah 84124
acoustic jam
Bring a song if you've got one
we'll back you up
bring a song.
If everyone celebrated Joy on Thursday Evening at sunset where ever You/they are,
then a wave of joy would travel around the world every Thursday at sunset
Photos & videos from our travels.
Thursday night review
Heather was manning the boat at Kokapelli's last night for the Joy Jam.
JoAva,/manager/the daughter of the owner, the one we arranged the jam with, spent the evening with her granddaughter, and left the establishment in the good hands of Heather. She was expecting The jam.
I was detained, called Heather, she said she'd call me when someone got their . Lin Ostler came around 515 or so. Sat and enjoyed the place, but no musicians were about, and Heather didn't know she was there for the jam, or she would have put her on the phone to me.
Lauren Nebeker came around six, Lynn had already left.
Dave Branick had committed to come over and lead the jam. I told him I'd set it up with JoAva for, from 4 PM to 8 PM, the idea being that we'd then be able to catch the sunset through the fine west windows at Kokopelli's.
Dave pointed out, that he thought jam should go from 630 till 930 or 10, because then people could come home from work, then come over.
The problem has been that the proprietors want to close early, 830 at Feldman's, and that that is about the time things really get started. Kokopelli's was open to staying open later, if the business was there, if the folks were there jamming.
Kokopelli's is a terrific place for an acoustic jam.
Dave Buranak a.k.a. the Reverend, has a regular Sunday at three jam. Very cool, a lot of great players come.
The hope was another jam, could be generated on Thursday sunset for the GuitarArmy.net for those who love to play, they could come and participate. A place to have a congenial celebration of joy every Thursday evening, that could last as long as it wanted and accommodate whoever would like to come and share their music acoustically. No stage. No performance. Participatory music. The purpose of the guitarArmy.net, to get folks doing the music.
So Dave shows up around 615, meantime JoAva has text me, says no one's come, guess I'll have Heather close at the regular time. 6 PM.
Dave's now arrives Kokopelli's, I'm talking to him on the phone, tells me there's no one there, and he's going to take off. And there were going to close. Dave leaves. Heather closes.
I get a call from Christy Stolworthy, she's there outside the closed Kokopelli's. She suggests that we do a group thing on Facebook to streamline communications, great idea, will do it.
630 Michael Feldman texts me. Says, I'm here at Kokopelli's, the place is shut down nothing is happening.
Mia Kulpa. Would love to See Kokopelli's accommodate the sun set jam on Thursday evenings. It would be good for Kokopelli's and good for those who come to play. I cannot always be there, but if we can get it going, someone would always be there.
My apologies to those of you who came for the jam, and were disappointed. I hope you'll give it another try, I'll try harder to set it up so that it's more inviting.
https://www.meetup.com/Salt-Lake-City-Music-Meetup/events/246983714/comments/488552389/
"The Army of Two article was awesome. Now i understand what you are doing and will try to record something.
Damn hippies. If anyone sings Kumbayah i'm out of here."
We got this review from Long Island Dave though he currently resides in Washington.
Well the truth of it for me is, that it was a struggle.
Wrestling match, but of course, that's why we do it!
The difficulty I believe, boils down to amplification. The futile and every difficult task of trying to bring the volume dynamic into some reasonable focus.
The answer I think, maybe the cell phone. Where we somehow are all in Stream live mode, then each could play along with what they are hearing on their phone, and balance their personal volume in accordance with the volume at which they've set their phone.
I believe I will try performing with my phone on live streaming, facing The phone outward looking at the world as it appears to me.
Ann Kelly Wright started the show singing love brother Diana. It was really quite beautiful, as is she, and is quite sufficient Unto herself.
Dave Buranak was a massive help,He sang some great songs while we did the PA wrangle.
Kim brought her Drum and a big powered PA speaker. A lot of work, she set it up, and did some great drummer.
Bob Dentilman, Bobby D charmed us as always.
What we learned.!
With the gravitational axis, we have imaginary line that runs through the center of the earth, and through the center of you.
Kelly Dobitz was fantastic, but he always is, what a great energy to be around. Thanks for coming Kelly and sharing yourself with us.
John England played some originals songs about how we could do better, build a better dream. Very nice.
Bob Bland was delightful with his Trump parody,, can't wait to hear it again..
Hod, that's me, I started a couple of songs, but they didn't come to much. I was too distracted running around trying to figure out how to stream on Facebook
John Russel really got it right with early morning rain. great Sound filled the place his acoustic guitar is matchless.
Ann Kelly Wright charmed us with an original about sugarhouse, the old days the way used to be, before they turned it into a strip mall. Hope we get to see more of her.
Marv Hamelton shared a song from his second album, Stop making veterans. Great song, great point. Thank you Marv, you made the evening for me.
Mike Feldman started the evening with blues, and his featured new song, down the barrel of a gun. Great host great evening, thank you Michael you get the best of show award.
https://www.cityweekly.net/utah/army-of-two/Content?oid=7503172
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