The procedure shown here was modified by T. Armbrister, G. Grigoriev, K. Hansgen, Z. Hess, T. Ksander, X. Ma, J. Reid, A. Rini, and S. Rudisill from D. J. Campbell, K. J. Beckman, C. E. Calderon, P. W. Doolan, R. M. Ottosen, A. B. Ellis, and G. C. Lisensky, Journal of Chemical Education, 76, 537-541, (1999).
PDMS is cured by an organometallic crosslinking reaction to give an optically transparent polymer with the ability to reproduce surface features. In this experiment the polymer is cured in contact with optical transform slides or the pits on a CD or DVD. How well are the original features copied? Use diffraction of a laser beam to measure the original feature sizes and the sizes of the copied features. Since PDMS is flexible the surface features imprinted into the elastomer can be also be distorted mechanically and their changing spacings monitored by diffraction.
PDMS monomer can be messy. Cover work surfaces with foil.
Step 1. Dispensing the viscous liquid can be messy. Cover the work surface and the balance with aluminum foil. Wear gloves.
Step 2. Add 4.00 g of Sylgard polymer base to a large weighing boat using a disposable plastic spoon. Add 0.40 g of curing agent using a disposable dropper.
Thorough mixing of the PDMS components is essential for good curing. Improper mixing can result in a polymer that is a sticky mess. On the order of 100 strokes with a stir stick are needed to mix the polymer components so that they will yield an adequately cured sample.
Bubbles degrade the optical qualities of cured PDMS so bubbles should be removed before curing. Most bubbles trapped during mixing of the components will eventually rise to the top of the liquid where they may be broken by blowing across the surface. The movie shows transparent PDMS with few bubbles.
Identify the emulsion side of an optical transform film (the side containing raised arrays). The shiny side of the film will sharply reflect room lights on its smooth surface; the matte emulsion side of the film will give more diffuse reflections. Peel open the white plastic slide mount, pick up the film by its edges, and place the film in a weighing boat with the emulsion side facing upward. A transparency master with a gray scale pattern could also be used.
Slowly pour about 4 g of the uncured PDMS mix into the mold assembly. Leave any remaining PDMS sticking to the walls of the weighing boat; too many bubbles are created during attemps to remove it. Let the assembly sit at room temperature for a few minutes so that bubbles incorporated during pouring can rise out of the PDMS. Gentle blowing over the surface may also eliminate bubbles.
Place the mold into the oven at 130°C for 20 min or 90°C for 30 min.
While the mold is in the oven continue with another portion of this experiment. Eventually remove the mold from the oven and allow it to cool. Gently remove the plastic sheet and film.
Another pattern with small features is a CD-R disk. Cut out a section using scissors.
Carefully peel off the aluminum foil. You may use either the foil or the polycarbonate support as the lithography master.
Follow the procedure above, again using 4.00 g of Sylgard polymer base and 0.40 g of curing agent. You may reuse the same weighing boat for mixing. Pour the mixture into the mold and place the mold into the oven at 130°C for 20 min or 90°C for 30 min.
While the mold is in the oven continue with another portion of this experiment. Eventually remove the mold from the oven and allow it to cool. Gently remove the foil or the CD portion from the cured PDMS.
An alternative pattern with smaller features is a DVD-R disk. Cut out a section using scissors.
Carefully peel apart the two polymer layers. You may use either the foil or the polycarbonate support as the lithography master.
While the mold is in the oven continue with another portion of this experiment. Eventually remove the mold from the oven and allow it to cool. Gently remove the foil or the DVD portion from the cured PDMS.
Use the Fraunhofer equation, d sin φn = n λ, to determine the feature spacing, d, of the original transparency and its copy by passing a laser with wavelength λ through the sample and measuring the nth diffraction angle, φn. This equation assumes the incident laser beam is perpendicular to the surface and that the beam passes through the sample.
How does the feature spacing of the copy compare with that of the original? If you stretch the PDMS slab, how does the diffraction pattern change?
How well is the track spacing copied for the CD and DVD? Determine the feature spacing in the PDMS using the Fraunhoffer equation, d sin φn = n λ, as above. You may need to rotate the sample to find the diffraction beams. If the original CD or DVD is not transparent, determine the feature spacing, d, by shining a laser on the sample and measuring the nth diffraction angle, θn as shown in the figure.
What is the feature spacing for the original samples? Show your calculations. Report your values in either µm or nm.
What is the feature spacing for the PDMS copies? Show your calculations.
Are the copied features the same size as the original features?
Do the feature sizes of the media disks match the known feature sizes for such disks?
If you stretch the PDMS slab, how does the diffraction pattern change?
Optical Transform Slides, Institute for Chemical Education, Madison, WI. A lower quality alternative is to use a dithering pattern (from standard computer art programs such as Canvas, Photoshop, or from the box shading function in Microsoft Word) printed onto a transparency.


Guide to Sigtuna Parish, Sweden ancestry, family history, and genealogy: birth records, marriage records, death records, census records, family history, and military records.
Sigtuna was founded on what was then the shore of Lake Mälaren just over 1,000 years ago. It took its name from an ancient royal estate several kilometers to the west. It operated as a royal and commercial centre for some 250 years, and was one of the most important cities of Sweden.
St. Mary's Church, built in the 13th century by the Dominican order as a monastery church, still remains largely intact. The Dominican monastery played an important role in the Swedish Middle Ages and produced many important Church officials.
Sigtuna parish, Husförhörslängd, 1835-1839, Ort register.


text:
Die USS Osterhaus (DE-164) war ein Geleitzerstörer der U.S. Navy während des Zweiten Weltkrieges und das bisher einzige Schiff, das diesen Namen trug. Sie gehörte zur Cannon-Klasse und war nach Rear-Admiral Hugo Osterhaus benannt.

Taufpatin des Schiffes war Mrs. Helen Osterhaus, eine Enkelin des Namensgebers; erster Kommandant wurde Commander Rowland H. Groff (US Navy Reserve).

Bauwerft war die Federal Shipbuilding and Dry Dock Co. in Port Newark, (New Jersey)

Nach der Ausbildungsfahrt im Gebiet des Great Sound (Bermuda) lief die Osterhaus am 21. August 1943 aus New York City aus, um ihre erste Mission in den Gewässern vor Espiritu Santo (Neue Hebriden) anzutreten. Nach dem Eintreffen am 3. Oktober unternahm der Zerstörer wiederholt Geleitschutzaufgaben zwischen den vorgeschobenen Stützpunkten der Neuen Hebriden und Neu Kaledonien zu den verschiedenen Frontabschnitten im Bereich der Salomonen.

Während einer Patrouillenfahrt vor Kola Point an der Küste von Guadalcanal griffen am Morgen des 11. Oktober 1943 zwei tieffliegende japanische Torpedobomber die Frachtschiffe SS George Bliss and SS John H. Couch an. Die Couch erhielt einen Treffer und begann zu brennen. Sie wurde daraufhin von der Osterhaus und der USS Bebas (DE–10) abgesichert; von den Zerstörern wurden in den folgenden beiden Tagen Lösch- und Rettungspersonal an Bord des Handelsschiffes kommandiert. Schlussendlich konnte das Feuer gelöscht und die wertvolle Fracht aus Munition, Ausrüstung und Pioniergrät gerettet werden.

In den folgenden Monaten eskortierte der Zerstörer Truppentransporter und Versorgungsschiffe von Nachschubbasen nach Guadalcanal und Bougainville Island, unterbrochen wurden diese Geleitfahrten von Unterseeboot-Abwehrpatrouillen zwischen Guadalcanal und den Fidschi-Inseln.

Nachdem die Vorbereitungen für die amphibischen Landungen auf den Marianen abgeschlossen waren, nahm die "Osterhaus" Kurs von Guadalcanal nach Eniwetok auf den Marshallinseln, um hier Truppentransporte abzuschirmen. Nach der Ankunft am 18. Juni 1944 verließ das Schiff den Hafen am nächsten Tag wieder, um einen Versorgungstransport in das Gebiet östlich von Saipan zu eskortieren. Während dieser Fahrt kam es zu keiner Feindberührung.

Am 23. Juli 1944 begann von Eniwtok aus eine erneute Geleitfahrt, die einen Truppenkonvoi nach Guam führte, das am 29. Juli erreicht wurde. Am nächsten Tag begann die Landungsoperation in der Agat Bay. Mit der Escort Division Eleven trat die "Osterhaus" am Abend des 30. Juli die Rückfahrt nach Eniwetok an. Von dort lief sie am 20. August 1944 aus, um ihre Operationsbasis nach Seeadler Harbor auf Manus (Admiralitätsinseln) zu verlegen. Von hier aus geleitete das Flaggschiff der Escort Division Eleven am 6. September drei Geleitflugzeugträger und eine Anzahl an Flottentankern zu einem Treffpunkt mit der Fast Carrier Task Force. Nach dem Eintreffen im vorbestimmten Gebiet am 11. September wurde die Fast Carrier Task Force von diesem Konvoi mit Material und Ausrüstung beliefert, was der Vorbereitung zum Angriff auf die Westlichen Carolinen und die Philippinen diente. Am 20. November 1944 verließ die "Osterhaus" Seeadler Harbor und lief über Hawaii zurück nach San Francisco, wo sie am 13. Dezember 1944 eintraf. Dort wurde sie zur Überholung nach dem Terminal Island Shipyard in San Pedro verlegt. Danach fuhr sie nach Pearl Harbor, wo sie am 23. April 1945 eintraf. Von hier aus fuhr der Zerstörer im Geleit eines Konvois aus Transportern und Handelsschiffen über die Marshallinseln nach Ulithi auf den Karolinen, wo er am 9. Juni 1945 eintraf. Danach führte die "Osterhaus" bis zum Kriegsende Geleitschutzaufgaben zwischen den Karolinen, den Marianen und den Marshallinseln durch. Mit der Escort Division Eleven verließ sie Kwajalein Lagoon am 16. September und lief über Pearl Harbor, San Diego und den Panamakanal nach New York City, wo sie am 27. Oktober 1945 eintraf. Es erfolgte die Verlegung nach Green Cove Springs in Florida mit der Außerdienststellung am 26. Juni 1946. Die "Osterhaus" verblieb bis zum 1. November 1972 in der Reserve und wurde danach aus der Schiffliste gestrichen. Am 30. Mai 1974 wurde das Schiff auf Abbruch verkauft.

Für ihre Verdienste wurden der Osterhaus zuerkannt:
 drei Battle Stars
 das Combat Action Ribbon
 die American Campaign Medal
 die Arctic-Pacific Campaign Medal mit drei Sternen
 die World War II Victory Medal
 die Philippines Liberation Medal

Quellen
  DANFS
  Fotogalerie

Cannon-Klasse
Schiff im Zweiten Weltkrieg
Federal Shipbuilding and Drydock Company

redpajama_set_name: RedPajamaWikipedia


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Diploma in Elementary Education programme 2017- 2019 is designed by NIOS (National Institute of Open Schooling) on the initiative of the Ministry of Human Resource Development (MHRD), Government of India. Nios is conducting the 4th Semester examination for the Diploma In Elementary Education (D.El.Ed.) in the month of March 2018. The form fillup for the 4th semester examination is now ended. There will be a total of two subjects, i,e, 508 and 509/ 510 for all 4th sem candidates. So all the candidates who applied for the examination need to carry admit card/ Hall Ticket for attending the exam. The Nios will issue the Admit Card for 4th Sem D.El.Ed. Exam 2019 one week before the schedule of the examination. Here we are discussing "how you can download Nios Deled Admit Card 2019 or Hall Ticket".
How to Download Nios Deled Admit Card For 4th Semester Exam?
Update: The Admit Card/ Hall Ticket for the D.El.Ed. 4th Semester examination is now available on the official website of NIOS D.El.Ed. You can get the admit card by accessing the NIOS D.El.Ed. Portal using the enrolment no. OR just follow below steps.
Click on the banner (or direct link added above for your convenience).
Enter your Enrolment number and Date of birth and then Hit Submit.
You will see the hall ticket on the screen with the print option.
Now you can download the Nios Deled Admit card.
Take 2 print out of it and keep it safe for future reference.
Hope this article will help you to get your Exam Hall Ticket Online. To check the latest update go to the Teacher login page by visiting from here http://dled.nios.ac.in/teacherlogin.aspx and then enter your email and password to access the D.El.Ed system. If you have any question, then comment down below. Also, share the article with all the teachers who applied for D.El.Ed exam. Keep Visiting Us For All Nios Deled Updates.
Why u late own schedule of d.el.ed final result?
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Nios Deled Result: How to Check 4th Sem Result Online?
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•The ability to deliver constant outstanding Health and Social Care lessons that involve the pupils of all abilities.
CANDIDATE - CANDIDATE - The teacher is required to work mainly as a Health and Social Teacher, but may be required to step in and support throughout all specialisms within the Faculty if required. The department is a strong team, who believe in a strong working relationship among colleagues.


text:
\section{Introduction}

Open star clusters (OCs) are abundant in the Milky Way disc. Their number is estimated to be of order $10^5$
\citep{Piskunov2006}.
In contrast, there are approximately 150 globular clusters (GCs) known in the Milky Way \citep{Harris2010}.
While the GCs are orbiting on eccentric orbits with partly high inclinations with respect to the stellar disc
plane of the Milky Way,
most OCs reside on near-circular orbits in the disc (although they may show a vertical oscillation with an amplitude of order
$\approx 0.5$ kpc \citep{Cararro1994}. The GCs are long-lived\footnote{If one considers them as ``living''.} with a
mean age of 10 Gyr.
The OCs are short-lived with a mean lifetime of only 300 Myr \citep[][Figure 8.5, hereafter: BT2008]{Binney2008}. Moreover,
the lifetimes of OCs range from a few tens of Myr to a few Gyr. Age distributions are also given by \citet{Lamers2006}
and \citet{Bonatto2011}.

\citet{Baumgardt2010} presented a weak evidence that there are two distinct GC populations outside the solar radius, namely a population of massive compact clusters with very small half-mass radii compared to the Jacobi radius and a population of low-mass and extended clusters with  $r_h/r_J > 0.1$. They argued that King models allow only a restricted range of
$r_\mathrm{h}/ r_\mathrm{t}$ and used the half-mass radius to quantify the Roche volume filling of GCs. However, there are other dynamical models like polytropes \citep[see, e.g., ][]{Converse2010} with a much larger half mass radius compared to the tidal radius. Additionally Baumgardt et al. used the Jacobi radius of circular orbits instead of the more general definition provided by \citet{King1962} for eccentric orbits (see Appendix B4 for a more detailed comparison to the present work).
We apply a more general derivation for circular and eccentric orbits including  $r_\mathrm{h}$ and $r_\mathrm{t}$ in order to distinguish the compactness of a cluster and the Roche volume filling factor.

It has been shown by \citet{vandenBergh1994}, that the half-light radii $r_h$ of GCs are correlated with the Galactocentric radius $R$
according to the relation

\begin{equation}
r_h \propto R^{2/3} \label{eq:vdb}
\end{equation}

\noindent
This relation has never been explained in terms of a deeper physical reason, although van den Bergh suspected already in
1994 that the correlation (\ref{eq:vdb}) could be imposed by the underlying galactic tidal field.
Assuming that the GCs are moving in an isothermal halo we find from analytical calculations that the time-dependent Jacobi radius
(i.e., the distance to the Lagrange points $L_1$ and $L_2$)
for eccentric orbits in such a halo scales as

\begin{equation}
\lim_{R \gg L/V_C} r_{J, \, \rm isoth.} \propto R^{2/3} \label{eq:rjiso}
\end{equation}

\noindent
(see appendix \ref{sec:iso}).
From the assumption of an isothermal halo, Eqns. (\ref{eq:vdb}) and (\ref{eq:rjiso}) and
$\langle R \rangle \gg \langle L\rangle/V_C$, where $\langle R \rangle,  \langle L\rangle$ and $V_C$ are median Galactocentric radius, orbital angular momentum and the halo's circular velocity, respectively,
it is possible to conclude that GCs in the Milky Way are characterized by a ratio $r_h/r_J$ which is independent
of $R$. The consequence is that, within the scatter of the correlation (which may be due to the scatter in GC masses),
GCs are characterized by a common average relative size.
We note that the Jacobi radius (i.e., the distance from the cluster centre to the
Lagrange points $L_1$ and $L_2$) provides a natural scale
for star clusters in the tidal field. Other (dependent) scales are given by the positions/widths of the dominant
resonances in the star cluster.

To gain a better understanding of the difference between OCs and GCs and why they form two distinct populations,
one may ask: Which values takes ratio $r_h/r_J$ on in the case of OCs.
While for GCs on eccentric orbits we may assume that their size is enforced by quantities in the pericenter, it seems reasonable to
suspect that OCs on near-circular orbits are not strongly influenced by the orbital evolution.

In the following discussions, we denote the ratio $r_{h}/r_J$ of 3D half-mass radius and Jacobi radius
with the letter $\lambda$. We also define $\widehat{\lambda} = r_t/r_J$
using the cluster cutoff radii $r_t$ (i.e. the radii at which the density drops to zero)
instead of the projected half-mass radii $r_h$.

The 3D half-mass radius $r_h=r_{h,\rm 3D}$ of a spherically symmetric stellar system
is typically larger than the projected (2D) half-mass radius $r_{h,\rm 2D}$.
We have $r_{h,\rm 3D} \approx 1.3 \, r_{h,\rm 2D}$. For the Plummer model $r_{h, \rm 3D}/r_{h,\rm 2D} \approx 1.30$
can be obtained analytically.

This paper is organized as follows: Section 2 presents the theory, section 3 lists the current status of observations
and simulations. In Section 4 the results are calculated and Section 5 contains the discussion and conclusions.

\section{Theory}

Following the approach by \citet{King1962}, the Jacobi radius of a star cluster in the tidal field of a galaxy
(i.e. the distance from the star cluster center to the Lagrange points $L_1$ and $L_2$) can generally be written as

\begin{equation}
r_J = \left[ \frac{G M_{cl}}{\Omega^2 - \frac{d^2\Phi}{dR^2}} \right]^{1/3} \label{eq:geniso2}
\end{equation}

\noindent
where $G$, $M_{\rm cl}$, $\Omega$, $\Phi$ and $R$ are the gravitational constant, the star cluster mass,
the angular speed, the gravitational potential of the galaxy and the galactocentric radius, respectively.
The last closed (critical) equipotential surface through the Lagrange points $L_1$ and $L_2$ encloses
the Roche or Hill volume.

Furthermore we define the ``(circular) velocity radius''

\begin{equation}
r_v  = \frac{GM_{cl}}{V_{\rm C}^2} \label{eq:rv}
\end{equation}

\noindent
It is the length scale at which the Keplerian circular velocity in the cluster (assuming a point mass cluster potential)
would be equal to the circular velocity $V_{\rm C}$ in the Milky Way.

The orbital periods $t_{\rm orb}$ and $T_{\rm orb}$ of a star at the half-mass radius of the star cluster and that of
the star cluster orbit around the galaxy, respectively, are given by

\begin{eqnarray}
t_{\rm orb}&=&\pi t_{\rm cr} = \frac{2\pi r_h}{\sigma_0} \approx 2\pi \sqrt{\frac{2 r_h^3}{GM_{\rm cl}}} \label{eq:kepler}
\ \ \ \mathrm{and}  \label{eq:torb1} \\
T_{\rm orb}&=&\frac{2\pi}{\Omega_C} = \frac{2\pi R_C}{V_C},  \label{eq:torb2}
\end{eqnarray}

\noindent
where $t_{\rm cr}$ is the crossing time (i.e. the time needed for a star to cross the half-mass sphere)
and $\sigma_0^2\approx GM_{\rm cl}/(2 r_h)$ in dynamical equilibrium.

\subsection{Circular orbits}

For an OC on a circular orbit with radius $R_{\rm C}$ and velocity $V_C$ in a tidal field the Jacobi radius from
Eqn. (\ref{eq:geniso2})
can be written as \citep{King1962, Kuepper2008, Just2009}

\begin{equation}
r_J = \left[\frac{GM_{\rm cl}}{(4-\beta_C^2)\Omega_C^2}\right]^{1/3}
= \left(4-\beta_C^2\right)^{-1/3} r_v^{1/3} R_{\rm C}^{2/3}  \label{eq:rj1}
\end{equation}

\noindent
with $\beta_C=\kappa_C/\Omega_C$ (see appendix \ref{sec:betac}), where $G$, $M_{\rm cl}$,  $\kappa_C$, $\Omega_C$ and $R_C$ are the gravitational constant, the total mass of the star cluster, the epicyclic and the circular frequency and the obital radius,
respectively, and $r_v$ is given by Eqn. (\ref{eq:rv}).

\noindent
Inserting (\ref{eq:torb1}) and (\ref{eq:torb2}) into (\ref{eq:rj1}) yields

\begin{equation}
\lambda_{\rm OC}=\left(\frac{r_{h}}{r_J} \right)_{\rm OC} =  \left(\frac{4-\beta_C^2}{2}\right)^{1/3} \left(\frac{t_{\rm orb}}{T_{\rm orb}}\right)_{\rm OC}^{2/3} \label{eq:ratio1}
\end{equation}

\noindent
for star clusters on circular orbits.

While $r_J$ determines the geometry of equipotential
surfaces and cannot be observed, $r_h$, $t_{\rm cr} \propto r_h/\sigma_0$ and $T_{\rm orb}$ can be determined by observations and simulations.
For realistic Milky Way models, the ratio $\beta_C$ is approximately
 constant as a function of Galactocentric radius and the dependency on it is so weak (see Figure \ref{fig:betaall} and appendix \ref{sec:betac})
 that we can safely neglect its variation beyond $2-3$ kpc of the center of the Milky Way.

\bigskip\bigskip
\subsection{Eccentric orbits}

For GCs on eccentric orbits in an isothermal halo ($V_C=\mathrm{const}$) we must extend the theory (see appendix \ref{sec:iso}).
Following the approach by \citet{King1962} the Jacobi radius from Eqn. (\ref{eq:geniso2}) can be written as

\begin{equation}
r_J = r_v^{1/3} \left(\frac{R^4}{R_g^2 + R^2} \right)^{1/3}
\end{equation}

\noindent
where $R=R(t)$ is time-dependent, $r_v$ is given by Eqn. (\ref{eq:rv}), $V_C$ is the rotation speed of the isothermal sphere, $R_g=L/V_C$ is a guiding radius and the angular momentum $L=L(V_C,R_P,R_A)$
is a constant of motion given by Eqn. (\ref{eq:angmom}).
From Eqns. (\ref{eq:geniso2}) and (\ref{eq:kepler}) we also find

\begin{eqnarray}
\lambda_{\rm GC} &=& \left( \frac{r_{h}}{r_J} \right)_{\rm GC} = \left(\frac{t_{\rm orb}}{2\pi}\right)^{2/3} \left[\frac{L^2}{R(t)^4} + \frac{V_C^2}{R(t)^2} \right]^{1/3}  \label{eq:ratio2} \\
&=& \left(\frac{t_{\rm orb}}{2\pi}\right)^{2/3}\left(\frac{V_C^2}{2}\right)^{1/3} \left(\frac{R_g^2 + R(t)^2}{R(t)^4}\right)^{1/3}.
\end{eqnarray}

We distinguish between two cases:

\begin{enumerate}
\item With the van-den-Bergh correlation (\ref{eq:vdb}) we obtain from Eqn. (\ref{eq:kepler})
along one orbit

\begin{equation}
t_{\rm orb} \propto R \label{eq:vdbprop}
\end{equation}

\noindent
and

\begin{equation}
\frac{t_{\rm orb}(t)}{R(t)} = \frac{t_{\rm orb,P}}{R_P} = \frac{t_{\rm orb, A}}{R_A}, \ \ \ \ \ \frac{t_{\rm orb}}{T_{\rm orb}} = \mathrm{const}
\end{equation}

\noindent
where the subscripts ``P'' and ``A'' stand for peri- and apocenter. From Eqn. (\ref{eq:ratio2}) we obtain with (\ref{eq:vdbprop})

\begin{equation}
\lambda_{\rm GC}^3
\propto \frac{A}{R^2} + B
\end{equation}

\noindent
where $A$ and $B$ are two constants.
It follows that

\begin{equation}
\lim_{R\gg R_g}\lambda_{\rm GC} = \mathrm{const}, \ \ \ \ \ \lim_{R \ll R_g}\lambda_{\rm GC} \propto R^{-2}
\end{equation}

\noindent
where $R_g$ is given by Eqn. (\ref{eq:guiding}).

\item Contrariwise, direct $N$-body simulations suggest that for a bound GC the half-mass radius changes more slowly than the time scale $T_{\rm orb}$ while the Jacobi radius oscillates on that time scale according to Eqn. (\ref{eq:gen}) (see Figure \ref{fig:radii}).
This would mean that, if $M_{cl}\approx \mathrm{const}$,

\begin{equation}
t_{\rm orb} \approx \mathrm{const} \label{eq:constprop}
\end{equation}

\noindent
in difference to Eqn. (\ref{eq:vdbprop}).
 From Eqn. (\ref{eq:ratio2}) we obtain with (\ref{eq:constprop})

\begin{equation}
\lambda_{\rm GC}^3
 \propto \frac{C}{R^4} + \frac{D}{R^2}
\end{equation}

\noindent
where $C$ and $D$ are two constants.
\end{enumerate}

\begin{figure}
\includegraphics[angle=90,width=0.5\textwidth]{betaall2.pdf}
\caption{The ratio $\beta_C$ at $z=0$ for the JSH95 and P90 models of \citet{Dinescu1999} and the
three-component Plummer-Kuzmin (3PLK) model used in \citet{Kharchenko2009} and \citet{Just2009}.}
\label{fig:betaall}
\end{figure}

\begin{figure}
\includegraphics[width=0.5\textwidth]{radii.pdf}
\caption{Time evolution of half-mass and Jacobi radii for a direct $N$-body simulation of a
star cluster with $N=50000$ particles on an eccentric orbit within the disc plane. The cluster has a
standard double-segment
\citet{Kroupa2001} IMF and is initially Roche volume filling, i.e. the cutoff radius equals the Jacobi radius.
The half-mass radius is calculated with respect to the current mass within the initial Jacobi radius.
Both radii are scaled with the initial half-mass radius
$r_{h,i}\approx 9$ pc.}
\label{fig:radii}
\end{figure}

\section{Observations and simulations}

\label{sec:simobs}

\subsection{Samples and medians for OCs and GCs}

\begin{table}
\caption{Values for OCs and GCs. The values are medians if not denoted otherwise.
The errors are standard errors of the median, i.e. divided by $\sqrt{N}$
of the sample size except for the error  $\Delta T_{\rm orb,OC}$. The data for OCs are derived
from \citet{Piskunov2007}
and BT2008. The data for GCs are derived
from \citet{Harris2010} and \citet{Dinescu1999}.}
\label{tab:clust-par}
\begin{center}
\begin{tabular}{ll}
\hline
OC parameter & Value \\
\hline
Sample size $N_{\rm OCs}$ & 236 \\
Median projected half-mass radius $r_{h, \rm 2D}$ [pc] &  $1.94 \pm 0.15$ \\
Median tidal radius $r_t$ [pc] &  $7.90 \pm 0.51$ \\
Velocity dispersion $\sigma_0$ [pc Myr$^{-1}$] & $0.31$ \\
Median crossing time $t_{\rm cr, OC} = 2 r_{h, \rm 2D}/\sigma_0$ [Myr] & $12.52 \pm 0.96$ \\
Average orbital period $T_{\rm orb, OC}$  [Myr] & $220 \pm 30$ \\
Average eccentricity $e_{\rm OC}$ & $0.127 \pm 0.003$ \\
\hline
GC parameter & Value \\
\hline
Sample size $N_{\rm GCs}$ & 34 (38) \\
Median half-light radius $r_{h,\rm 2D}$ [pc] & $3.13\pm 0.51$ \\
Median tidal radius $r_t$ [pc] & $33.02 \pm 4.83$ \\
Median velocity disp. $\sigma_0$ [pc Myr$^{-1}$] & $5.11 \pm 0.64$ \\
Median crossing time $t_{\rm cr, GC} =  2 r_{h, \rm 2D}/\sigma_0$ [Myr] & $1.175 \pm 0.726$ \\
Median Galactocentric radius $R_{\rm orb, GC}$ [kpc] & $ 7.75 \pm 0.84$ \\
Median height above the disc plane $z_{\rm GC}$ [kpc] & $4.00$ \\
Median velocity $V_{\rm GC}$ [pc Myr$^{-1}$] & $175 \pm 16$ \\
Median orbital period $T_{\rm orb, GC}$ [Myr] & $207 \pm 54$ \\
Median eccentricity $e_{\rm GC}$ & $0.622 \pm 0.044$ \\
\hline
\end{tabular}
\end{center}
\end{table}

 For OCs we use the sample of 236 OCs of \citet{Piskunov2007}. We obtain
 the values given in the upper part of Table \ref{tab:clust-par}.
 The projected half-mass radii of the 236 OCs have been obtained by solving 236 transcendental  equations
 with the Newton-Raphson method using the table of core and tidal radii provided by \citet{Piskunov2007} at the CDS.
The transcendental equation is given by

 \begin{equation}
 \ln X_h + \frac{X_h}{C} - 4\sqrt{\frac{X_h}{C}} -\frac{\ln C}{2} - \frac{1}{2C}  - \frac{2}{\sqrt{C}} + \frac{3}{2} = 0 \label{eq:transz}
 \end{equation}

 \noindent
 with

 \begin{equation}
 X_h = 1 + (r_h/r_c)^2 \ \ \ \mathrm{and} \ \ \ C = 1 + (r_t/r_c)^2
 \end{equation}

 \noindent
where $r_c, r_h$ and $r_t$ are the core, half-mass and tidal cutoff radii, respectively \citep[cf.][Section 3]{Ernst2010}.
Eqn. (\ref{eq:transz}) is solved for $r_h$.

The error of the median value of the projected half-mass radius $r_{h,\rm 2D}$ is defined as

 \begin{equation}
 \Delta r_{h, \rm 2D} = \sqrt{\frac{\sum_{i=1}^{N_{\rm OCs}} \left[r_{h,i, \rm 2D} - \mathrm{Median}(r_{h,i, \rm 2D})\right]^2}{N_{\rm OCs}(N_{\rm OCs}-1)}} \label{eq:errmed}
 \end{equation}

\noindent
We do not have an error on the velocity dispersion $\sigma_0$ of OCs.
Thus we have set $\Delta\sigma_0 = 0$ for OCs.
Note also that in a
bound system $r_h$ and $\sigma_0$ are related through the virial theorem, i.e. we have
$\Delta\sigma_0/\sigma_0=(1/2) \Delta r_h/r_h$ in virial equilibrium. We neglect this correlation since the virial theorem is not generally valid for star clusters in a tidal field. Namely, it is not valid for Roche volume overfilling star clusters.
The derived crossing time and its relative error are given by
\begin{equation}
t_{\rm cr} = 2 r_{h,\rm 2D}/\sigma_0, \ \ \ \Delta t_{\rm cr}/t_{\rm cr} = \sqrt{\left(\Delta r_h/r_h\right)^2 + \left(\Delta \sigma_0/\sigma_0\right)^2} \label{eq:errder}
\end{equation}

\noindent
The OCs in the sample by \citet{Piskunov2007} have approximately the orbital period of the Local
Standard of Rest (LSR) taken from BT2008, table 1.2.

For GCs we use the median values from 34 out of a sample of 38 Milky Way globular clusters from
\citet{Dinescu1999}.  The
data compilation of 157 Milky Way GCs by Harris
(\citet{Harris2010}) was also used.
The median values are obtained from the equivalents of Eqns. (\ref{eq:errmed}) and (\ref{eq:errder})
for the observed/simulated and the derived quantities.
We obtained the values given in the bottom part of Table \ref{tab:clust-par}. Only for 97 out of 157 GCs from the Harris catalogue
$\sigma_0$ is given. For 5 of these 97 GCs $r_h$ is not given as well.
From the GC sample in \citet{Dinescu1999} with 38 GCs we further find a median value
of the orbital period of GCs. Only for 34 out of 38 GCs in the Dinescu et al. sample $\sigma_0$ is given in the Harris catalogue.
The minimum Galactocentric radius is $R = 2.7$ kpc for NGC 6144 such that we can neglect the dependency on $\beta_C$
according to Figure \ref{fig:betaall}.  We further remark that a few recently discovered GCs have been added to
Harris' compilation by \citet{Ortolani2012}.

\section{Results}

\subsection{OCs}

\label{sec:ocs}

\begin{figure}
\includegraphics[width=0.5\textwidth]{histsocs3.pdf}
\caption{The ratios $r_{h,\rm  3D}/r_J$ (top panel) and $r_t/r_J$ (bottom panel) for OCs calculated from Eqn. (\ref{eq:ratio1})
for the sample of \citet{Piskunov2007}. The histograms for a canonical $\pm 20$\% error on $\sigma_0$
and for the substitution $\sigma_0\rightarrow2\sigma_0$ in Eqn.
(\ref{eq:ratio1}) are also shown. The vertical lines denote the medians. Note that $r_{h, \rm 2D}$ of the data set
is corrected with a factor
1.3 to obtain $r_{h, \rm 3D}$.}
\label{fig:histmain}
\end{figure}

\begin{table}
\caption{Quantiles for OCs.}
\label{tab:OC-par}
\begin{center}
\begin{tabular}{llll}
\hline
Parameter & $10^{Q_{10}}$ & $10^{Q_{50}}$ & $10^{Q_{90}}$ \\
\hline
$\lambda_{\rm OC}$, Table \ref{tab:clust-par} &  0.239  &    0.379   &    0.675    \\
$\lambda_{\rm OC}$, $\sigma_0\rightarrow 2\sigma_0$ & 0.151 &    0.239 &     0.425   \\
$\widehat{\lambda}_{\rm OC}$, Table \ref{tab:clust-par} &  0.506 &     0.812 &      1.35 \\
$\widehat{\lambda}_{\rm OC}$, $\sigma_0\rightarrow 2\sigma_0$ &   0.319 &   0.511  &    0.852 \\
\hline
\end{tabular}
\end{center}
\end{table}

Figure \ref{fig:histmain} shows the distributions of $\log_{10}\lambda_{\rm OC}$ (top panel) and $\log_{10}\widehat{\lambda}_{\rm OC}$ (bottom panel) for OCs according to Eqn. (\ref{eq:ratio1}). We used the isothermal approximation $\beta_C=\sqrt{2}$.
There is a large scatter of the sizes around the medians. We find also Roche volume overfilling
OCs.

$\widehat{\lambda}_{\rm OC}$ was found from Eq. (\ref{eq:ratio1}) with the values of Table \ref{tab:clust-par} using the tidal radii instead of
the half-mass radii in the definitions of crossing time (i.e, $t'_{\rm cr} = 2 r_t/\sigma_0$ instead of
$t_{\rm cr} = 2 r_h/\sigma_0$).

Figure \ref{fig:histmain} shows also the distributions of $\log_{10}\lambda_{\rm OC}$ with the substitution
$\sigma_0\rightarrow2\sigma_0$ which leads to $t_{\rm cr, OCs}\rightarrow t_{\rm cr, OCs}/2$
in Eqn. (\ref{eq:ratio2}).

We find the medians $Q_{50}$ given in Table \ref{tab:OC-par}.
The quantiles $Q_{10}, Q_{50}$ and $Q_{90}$ have been calculated with an {\sc idl} routine by Hong \citep{Hong2004}.

\subsection{GCs}

\label{sec:gcs}

\begin{figure}
\includegraphics[width=0.5\textwidth]{histsgcs5.pdf}
\caption{Top panel: The ratio $r_{h, \rm 3D}/r_J$ of GCs today and in the peri- and apocenter  calculated from Eqn. (\ref{eq:ratio2})
 for 34 GCs out of the sample by \citet{Dinescu1999}
under the assumption that the GCs are moving in an isothermal halo with $V_C\approx 228.5$ km/s and that the van-den-Bergh correlation holds. Middle panel: The same as in the top panel assuming that instead of the van-den-Bergh correlation
$r_h$ is independent of Galactocentric radius.
Bottom panel: The ratio $r_t/r_J$ for GCs today calculated from Eqn. (\ref{eq:gen}). The vertical lines denote the medians.
Note that $r_{h, \rm 2D}$ of the data set is corrected with a factor 1.3 to obtain $r_{h, \rm 3D}$.}
\label{fig:histsgcs3}
\end{figure}

\begin{table}
\caption{Quantiles for GCs. The subscript ``0'' denotes present-day values.}
\label{tab:GC-par}
\begin{center}
\begin{tabular}{lclll}
\hline
Parameter & & $10^{Q_{10}}$ & $10^{Q_{50}}$ & $10^{Q_{90}}$ \\
\hline
$\lambda_{\rm GC,0}$ &  & 0.0318 &   0.0701 &     0.239  \\
$\widehat{\lambda}_{\rm GC,0}$ &  & 0.286   &  0.469 &   0.742  \\
\hline
$\lambda_{\rm GC,P}$ & ($r_h\propto R^{2/3}$) &   0.0427 &    0.0928  &    0.178 \\
$\lambda_{\rm GC,A}$ & " &  0.0297 &    0.0593 &    0.125  \\
\hline
$\lambda_{\rm GC,P}$ &($r_h\propto R^{0}$) &  0.0785   &     0.161  &    0.455 \\
$\lambda_{\rm GC,A}$ & " &  0.0174   &    0.0313   &    0.0847  \\
\hline
\end{tabular}
\end{center}
\end{table}

The top and middle panels of Figure \ref{fig:histsgcs3} show the distributions of $\log_{10}\lambda_{\rm GC}$ today and in the peri- and apocenter  calculated from Eqn. (\ref{eq:ratio2})  for 34 GCs of the sample by \citet{Dinescu1999}
under the assumptions that the GCs are moving in an isothermal halo with $V_C\approx 228.5$ km/s. In the top panel, we
assumed that the van-den-Bergh correlation is valid, and for the middle panel we assumed that $r_h\propto R^0$, i.e.
that it is independent of $R$.

The bottom panel of Figure \ref{fig:histsgcs3} shows the distribution of $\log_{10}\widehat{\lambda}_{\rm GC}$ today calculated from Eqn. (\ref{eq:gen})  for the same sample using the $r_t$'s given in the Harris catalogue.
It seems as if the GCs are today Roche volume underfillling and, moreover, at most Roche volume filling with
$\widehat{\lambda}_{\rm GC} = 0.3 - 1.0$.

We find the medians $Q_{50}$ given in Table \ref{tab:GC-par}.

\subsection{Comparison of OCs and GCs}

\begin{figure}
\includegraphics[width=0.5\textwidth]{histrtrh2.pdf}
\caption{Top panel: The ratio $r_{h, \rm 2D}/r_t$ for OCs and GCs today
 for the 236 OCs of the sample by \citet{Piskunov2007}, the 34 GCs of the sample by \citet{Dinescu1999}
 and 156 GCs of the Harris catalogue \citep{Harris2010}.
Note that $r_h=r_{\rm h, 2D}$ is in this Figure the projected half-mass radius (OCs) or the half-light radius (GCs) given in the
Harris catalogue, respectively. The vertical lines denote the medians.}
\label{fig:histrtrh}
\end{figure}

Figure \ref{fig:histrtrh} shows the ratio $r_{h, \rm 2D}/r_t$ for OCs and GCs today
 for the 236 OCs of the sample by \citet{Piskunov2007}, the 34 GCs of the sample by \citet{Dinescu1999}
 and 156 GCs of the Harris catalogue \citep{Harris2010}.
Note that $r_h=r_{\rm h, 2D}$ is the projected half-mass radius (OCs) or the half-light radius (GCs) given in the
Harris catalogue \citep{Harris2010}, respectively. The vertical lines denote the medians.

We find the medians $\langle r_t/r_h\rangle = \langle\widehat{\lambda}/\lambda \rangle\approx 3.9$ (OCs),
$\langle r_t/r_h\rangle \approx 11.0$ (Dinescu GCs), $\langle r_t/r_h\rangle \approx 8.7$ (Harris GCs).
Therefore, with respect to this ratio, the average OC corresponds to
a King model with low $W_0$ while the average GC corresponds to a King model with high $W_0$
according to Table 1 in \citet{Guerkan2004}.
We remark that the projected (2D) half-mass radius $r_h=r_{\rm h, 2D}$  is larger than the
3D half-mass radius $r_{\rm h, 3D}$.
For the Plummer model $r_{\rm h, 3D}/r_{\rm h, 2D} \approx 1.30$ can be obtained analytically.

Applying Eqns. (\ref{eq:ratio1}) and (\ref{eq:ratio2}) to the data
we find that

\begin{equation}
\lambda_{\rm GC} < \lambda_{\rm OC}, \ \ \ \widehat{\lambda}_{\rm GC} < \widehat{\lambda}_{\rm OC}. \label{eq:tend}
\end{equation}

\noindent
for an ``average''\footnote{``Average'' means here that its parameters are identical with the parameter
median values of the whole sample.}
GC and an ``average'' OC, with proportionality factors

\begin{equation}
\mu = \frac{\lambda_{\rm OC}}{\lambda_{\rm GC}}, \ \ \ \widehat{\mu} = \frac{\widehat{\lambda}_{\rm OC}}{\widehat{\lambda}_{\rm GC}}
\end{equation}

\noindent
with $\mu \approx 5.4$ today and $\widehat{\mu}\approx 1.7$ today
from the median values of crossing and orbital times given in Tables \ref{tab:clust-par}, \ref{tab:OC-par}
and \ref{tab:GC-par}.
The isothermal approximation $\beta_C=\sqrt{2}$ was used.

The relative error in $\mu$ is given by

\begin{eqnarray}
\frac{\Delta\mu}{\mu}&=&
\sqrt{\left(\frac{\Delta\lambda_{\rm OC}}{\lambda_{\rm OC}}\right)^2 + \left(\frac{\Delta\lambda_{\rm GC}}{\lambda_{\rm GC} }\right)^2}  \\
&=& \ln(10)\sqrt{ \left[\frac{  \Delta\log_{10}\lambda_{\rm OC}  }{\sqrt{N_{\rm OCs}}} \right]^2 +  \left[\frac{  \Delta\log_{10}\lambda_{\rm GC}   }{\sqrt{N_{\rm GCs}}} \right]^2 } \nonumber \\
&\lesssim& \ln(10)\sqrt{ \left[\frac{ (Q_{90} - Q_{10})_{\rm OCs}  }{\sqrt{N_{\rm OCs}}} \right]^2 +  \left[\frac{ (Q_{90} - Q_{10})_{\rm GCs}   }{\sqrt{N_{\rm GCs}}} \right]^2 } \nonumber
\end{eqnarray}

\noindent
The last line containing the 10 and 90 percent quantiles of the $\log_{10}\lambda$-distributions serves as an upper limit to the error.
We obtain $\Delta\mu/\mu\lesssim 0.23$ for the upper limit.

We further remark that taking $t_{\rm cr, OC}/2$ instead of $t_{\rm cr, OC}$ in Eqn. (\ref{eq:ratio1}) with all other quantities kept the same
leads to $\mu\approx 3.4$ implying at least a $3\sigma$ confidence provided that there is no bias due to systematic
errors (see discussion).

\section{Discussion and conclusions}

The results of the present study are as follows:

\begin{enumerate}
\item We found under the assumptions stated below that GCs are
generally Roche volume underfilling in terms of $\widehat{\lambda}=r_\mathrm{t}/r_\mathrm{J}$.
In the pericenters of their orbits a significant fraction might be Roche volume
overfilling dependent on the dynamical compression of the outer
shells compared to the smaller Jacobi radius.
\item We found under the assumptions stated below
with at least $3\sigma$ confidence that the ratio $\lambda=r_h/r_J$ of half-mass and Jacobi radius
is tendentially larger for an average open cluster within the nearest kpc of the Sun
than for an average globular cluster and quantified the
proportionality factor

\begin{equation}
\mu=\left(\frac{r_h}{r_J}\right)_{\rm OCs}\Big{/}\left(\frac{r_h}{r_J}\right)_{\rm GCs} \approx 3-5.
\end{equation}

\item The difference between OCs and GCs seems to be that, with respect to the concentration, the
average OC has low concentration
while the average GC has a high concentration.
\item  A fraction of OCs may be Roche volume overfilling. However, the simple assumption of virial equilibrium
breaks down for Roche volume overfilling clusters.
\item A closer inspection of \citet{Baumgardt2010} suggests that there is a physically extended subsample
of low mass GCs with $r_\mathrm{h} > 10$\,pc, which may represent the post core collapse sequence of
dissolving clusters. Our sample of GCs with known orbits is too small to confirm this scenario.
\end{enumerate}

We make the following remarks:

\begin{enumerate}
\item The fact that $\lambda_{\rm GC}\ll 1$ explains (i)
why GCs are spherically shaped as compared to the often irregularly shaped OCs, (ii) why
GCs are stable against dissolution over a Hubble time and (iii) why
not many GC tidal tails have been found observationally.
\item A fraction of OCs may be Roche volume overfilling ($\lambda_{\rm OC}>1$) at the time of their formation,
but the shear forces of the tidal field will rapidly remove the material outside the Jacobi radius.
\item Only if the star cluster is in virial equilibrium Eqn. (\ref{eq:kepler}) is valid. Therefore the correlation found by
\citet{vandenBergh1994} suggests that an average GC is in virial
equilibrium if we postulate that a constant ratio $\lambda_{\rm GC}$
is reasonable with respect to the general structure of GCs. We emphasize that the virial theorem cannot be
valid for Roche volume overfilling clusters.
\end{enumerate}

We rely on the following assumptions, stated in order of importance according to our view:

\begin{enumerate}
\item That the orbits of GCs in the sample of \citet{Dinescu1999} can be approximated by
orbits in a purely isothermal halo for which the total angular momentum is conserved.
\item That the orbits of OCs can be approximated by circular orbits \citep[for orbit calculations of OCs
see, e.g.,][]{Cararro1994}.
\item That there are no selection effects concerning the GC sample, i.e. the sample of GCs in \citet{Dinescu1999} is
representative for the GC population of the Milky Way.
\item That the half-light and projected half-mass radii coincide.
\item That the velocity dispersion of OCs is not too much biased due to the presence of binaries.
\end{enumerate}

It is crucial to this investigation whether the approximations (i) and (ii) are justified.
In the future, our results may be falsified or improved towards
higher confidence levels when more and better data are available.

Our investiation suggests that most GCs were formed deep in their potential well, i.e. Roche volume
underfilling in contrast to OCs, which can be even Roche volume overfilling after gas expulsion.
In future work we plan to investigate the dynamical reasoning for
these intrinsic differences and to quantify the impact on the
dissolution process of the star clusters.

\section{Acknowledgements}

AE is grateful for support by grant JU 404/3-1 of the German Research Foundation (DFG)
and thanks Prof. Dr. Eva Grebel for a comment made during a talk which directed his interest
to the van-den-Bergh correlation.
Discussions with Prof. Dr. Rainer Spurzem are gratefully acknowledged and the fact, that
the idea to Eqn. (\ref{eq:ratio1}) was first written down on a notepad of him.
Both authors thank the referee for the thoughtful comments.

redpajama_set_name: RedPajamaArXiv


text:
Complete Analysis of Strikeforce: Overeem vs. Werdum
Opposing Views Staff
Saturday, June 18th, Strikeforce invades the American Airlines Center in Dallas, Texas. Strikeforce: Overeem vs. Werdum (aka Strikeforce: Dallas) features the final two bouts of the Heavyweight Grand Prix Quarterfinals, with the winners moving on to the Semis to face either Antonio Silva or Sergei Kharitonov. After many scheduled bouts had to be taken off the card and fighters shuffled around, the final fight card is set.
Let's take a look at the Main Card, being broadcasted on Showtime, and see how each fight breaks down.
The first bout of the broadcast is a Heavyweight Grand Prix Alternates bout between Valentijn "The Python" Overeem (29-25) and Chad "The Grave Digger" Griggs (10-1). Both fighters last fought in February on the Strikeforce: Fedor vs. Silva card, in which they each won their HWGP alternate bout in the first round. These two men both have a grappling and striking background, so this fight could end up being contested in every inch of the cage. With twenty knockouts and eighteen submissions between the pair, this fight could be over at any second.
In the next bout, rising Heavyweight prospect Daniel Cormier (7-0) faces his toughest test to date as Jeff "The Snowman" Monson (42-11) makes his return to the mainstream audience. While Monson has faced just about every big-name Heavyweight fighter under the sun, he may have not faced anybody like Daniel Cormier in the past two years. Consequently, Cormier has also never fought anybody like Monson. Cormier's wrestling pedigree is a laundry list of accolades, and he has heavy hands to sweeten the deal. Monson on the other hand isn't known for his power, but is considered to be one of the top submission grapplers in the world, earning twenty-six of his victories by way of submission. Cormier is used to dominating his opponents in all aspects of the fight, but if he may want to think twice before he goes to the ground with The Snowman.
The third bout of the Showtime broadcast, and the only non-Heavyweight bout, is between KJ Noons (10-3) and Jorge "Gamebred" Masvidal (21-6) in the Lightweight Division. Before losing to Nick Diaz in his last fight, Noons was on a six-fight win streak that included four KO/TKO victories. Masvidal is a perfect fight for Noons to bounce back with because he is predominantly a boxer and Noons loves to strike. He better not take him lightly, however, as Masvidal has picked up ten of his wins by way of KO/TKO. If things go the way they look on paper, we are in for a standup battle that will not only test the cardio of these fighters, but also their chins.
The Co-Main Event of the evening, and the first of two HWGP Quarterfinal bouts, between Josh "The Baby Faced Assassin" Barnett (29-5) and Brett "The Grim" Rogers (11-2). Barnett is currently riding a six-fight win streak spanning just over three years, while Rogers is trying to build his momentum back up after winning his first ten fights and then losing back-to-back. This fight is going to be a battle of styles as Barnett puts his catch wrestling up against Rogers' boxing. Barnett has only been knocked out once and Rogers has never been submitted. If Barnett can get this fight to the ground, Rogers could really be in trouble and face his third Strikeforce loss in a row. However, Barnett hasn't had his chin tested in a few years and Rogers could definitely hurt him if he catches him with a big right hand.
Overeem will look to avange his loss to Werdum
The Main Event, and second HWGP Quarterfinal bout, of the evening is possibly one of the most highly anticipated fights of the year as Alistair "Demolition Man" Overeem (34-11-1) takes on Fabricio "Vai Cavalo" Werdum (14-4-1). This fight is also a battle of styles as Overeem looks to use his powerful kickboxing to defeat Werdum's deadly Brazilian Jiu-Jitsu. In their last fight, they each used their strengths to defeat their opponent: Overeem KO victory over Todd Duffee, Werdum submission victory over Fedor Emelianenko. The last time these two-faced each other, back in 2006 in the Pride Open Weight Grand Prix, Werdum was victorious in defeating the smaller Overeem via submission due to a kimura. Just over five years later they cross paths again as two completely different fighters. Overeem has put on a lot more muscle and settled into his Heavyweight frame, and Werdum has greatly improved his striking abilities. Both men are riding huge waves of momentum coming into this fight and it could literally end at any given time. When an unstoppable force meets an immovable object, an explosion is bound to happen.
Look for the Strikeforce: Overeem vs. Werdum predictions on the site as well as the betting corner to help you make some solid plays.
Daniel Cormier faces MMA Legend Jeff Monson
The Betting Corner – Strikeforce: Overeem vs. Werdum
Strikeforce Heavyweight Grand Prix Bracket Contest
Strikeforce Heavyweight Grand Prix Finally Returns on June 18
Strikeforce: Fedor vs. Silva Predictions
Get more great MMA news, recaps and analysis over at MMAValor.com
MMA Analysis, Odds: Strikeforce's Overeem vs. Werdum
Final Look Back at Strikeforce: Overeem vs. Werdum
Strikeforce Preview, Predictions: Overeem vs. Werdum
Strikeforce: Overeem v. Werdum Preview, Predictions
MMA Analysis: Lessons Learned From Overeem vs. Werdum
Strikeforce Grand Prix Preview: Alistair Overeem vs. Fabricio Werdum
Strikeforce Werdum vs. Overeem Prelim Results
MMA Analysis: Can Fabricio Werdum Really Beat Overeem?

redpajama_set_name: RedPajamaCommonCrawl


What's the time after the items are purged when using Tiny Tiny RSS at online.tt-rss.org? Are the unread items also purged?
These options seem to have been disabled for obvious reasons, but it might be a good idea to still have these options in the preferences page even if the user couldn't change the values. This way the user could at least see which values these options have.
edit: Wow, that was quick. Thanks for the answer.
Last edited by matti1234 on 10 Nov 2011, 16:25, edited 1 time in total.
30 days. I suppose it's not a bad idea to show the time in the UI.


text:
Cloud Reliance
The 2021 Digital Readiness Survey
A global survey of executives and technology professionals on the impact of remote work on cloud adoption, IT security strategies, and the usage of analytics and AI-based technologies.
Download our infographic curated with the most insightful global findings from the survey.
The soaring importance of IT
Not only has the COVID-19 pandemic profoundly impacted all of us across the globe, it also completely transformed the way organizations function. As the pandemic forced people indoors, companies rushed to facilitate remote work and maintain business continuity. This is where IT departments stepped in. By deploying new technologies, upgrading existing solutions, and keeping a distributed workforce secure, IT teams did it all.
In order to understand more about this paradigm shift, ManageEngine conducted a global research survey focusing on remote work's effects on cloud usage and organizational security.
We also investigated trends related to AI, business analytics, and technology adoption.
The survey was completed by 1,210 qualified executives and technology professionals from India, the United States, Canada, Singapore, the United Kingdom, Australia, and New Zealand. All participants were directly responsible for IT and procuring business technologies.
8 out of 10 IT professionals report that the pandemic has led to an increase in cloud usage.
83% of respondents revealed that remote workers increase security risks.
Only 56% of companies have changed their security strategy—despite remote employees being directly targeted more often.
The popularity of AI continues to flourish with 81% of organizations reporting that their confidence in AI has grown over the last two years.
(1/4) Autoplay
We find ourselves in a new world where remote work is encouraged, and the onus lies on organizations to foster a truly hybrid workplace. This research finds that IT is now seen as a critical business enabler that plays a key role in optimizing operations and addressing the demands of a transformed workplace.
Remote work will have a lasting impact with 96% of organizations stating that they will be supporting remote workers for at the least the next two years. Unsurprisingly, cloud solutions have emerged as a forerunner in technologies that can facilitate remote work. However, companies want more from cloud offerings, specifically in terms of performance, reliability, and security.
In order to support a distributed workforce, organizations are more willing than ever to invest in new technology. Security, reliability, and cost reduction were found to be the top three drivers behind organizational decisions to adopt new technology.
The survey also finds that organizations are increasingly relying on AI and business analytics to fuel data-driven decision-making and maintain their competitive edge. 89% of the companies surveyed indicated increased usage of business analytics; interestingly, this was primarily led by IT teams. Confidence in artificial intelligence has increased as well, as organizations look to AI for improvements in operational efficiency and improved customer experiences.
The results below have been organized into three sections
(Remote work driving increased cloud reliance)
Due to the pandemic, technology professionals are increasingly prioritizing cloud security,
VPN usage, and remote worker support.
Global Trends North America	United Kingdom India Singapore Australia and New Zealand
Cloud customers are looking for improved security, performance, and reliability from cloud solutions.
96% of companies will be operating with remote workers for at least the next two years.
83% are increasing their reliance on the cloud.
42% of respondents stated that 'improved compliance' will increase their organizations' confidence in cloud-based solutions.
When asked about the new tech-related skills learned due to the pandemic situation, only 22% of respondents chose compliance.
India is the only region where public and private cloud usage were among the top three skills acquired during the pandemic.
97% of organizations reported that their reliance on cloud had increased, compared to the global figure of 83%.
Improved security, reliability, and performance would boost confidence in cloud-based solutions.
Remote worker support, security, and VPN usage were the top three related skills acquired during the pandemic.
74% of respondents increased their cloud usage; this is 9% below the global average.
Private cloud was the top-learned skill in Singapore, with 50% of respondents equipping themselves with knowledge about private cloud.
86% of respondents say their organization's reliance on cloud has increased, compared to the global figure of 83%.
Cloud usage has increased in 84% of U.K. businesses, with IT operations increasing their usage the most (57%).
51% of respondents said that use of cloud solutions has increased for data-related purposes, such as storage and backup.
47% of organizations increased their use of cloud solutions to implement services to support remote workers.
(Security attacks targeting remote workers; companies responding slowly)
Security threats have increased, making it difficult for many organizations to handle phishing,
malware, and other network endpoint attacks.
Global Trends North America United Kingdom India Singapore Australia and New Zealand
83% reveal remote workers increase security risk.
78% of companies fail to control applications and services employees use.
Only 56% of companies have adapted a security strategy for employees working from home.
52% of organizations report that phishing attacks have increased due to the pandemic.
Security is the top driver behind organizational decisions to adopt new technology.
Roughly 48% of respondents believe that social media-based attacks were the most common security threat during the pandemic.
Only 37% of respondents stated that implementing a Zero Trust network model was a key security action adopted by their company.
Only 30% had to learn about VPN in India; this is well below the global average of 35%.
48% companies have implemented zero trust networks, as opposed to the global figure of 31%.
With online meeting tools and mobile apps often purchased without IT team approval, the threat of shadow IT looms large.
81% reveal that remote workers increase security risk.
The top security threats are phishing, endpoint network attacks, and malware.
Only 57% of companies adapted their security strategy.
Only 19% of North American companies adopted a zero trust network. This is the lowest in the world, 12% below global average.
Security and remote worker support were among the top three acquired skills in Singapore.
The threat of shadow IT looms large in Singapore, as online meeting tools and mobile apps are particularly likely to be purchased without IT team approval.
83% of organizations have seen security threats increase as a result of the pandemic.
45% of U.K.-based companies have seen phishing threats increase, followed by account hijacking (38%), and social media-based attacks (36%)
In order to combat the growing security threats due to the pandemic, 65% of organizations raised employee awareness around threats, and 65% provided employee cybersecurity training.
Only 26% of organizations have opted for Zero Trust network implementation.
51% of organizations reported that improving security was the top reason behind the adoption of new technologies.
76% of companies' IT teams aren't always consulted before employees purchase new software solutions. 37% of respondents said employees had purchased online meeting tools without direct approval from IT, followed by mobile-specific apps (33%), and productivity apps (27%).
(AI and business analytics growing rapidly to support data-driven decision-making)
More than ever before, IT personnel are relying on AI-based tools and analytics software to
inform their business decisions.
89% report increased use of business analytics.
64% of organizations have reported using business analytics to improve decision-making.
86% of organizations increased their usage of AI over the last 2 years.
81% report their confidence in AI solutions has grown.
AI drives improvements in business insights, operations, and customer satisfaction.
63% of respondents are using AI to make the most of their available data.
89% of the respondents believe that the use of business analytics in their companies increased over the last two years.
93% of Indian respondents say AI has delivered measurable business results—compared to 71% globally.
91% say confidence in AI has increased over the last two years.
Respondents in India resoundingly think AI will meet business expectations.
Reasons for use include improved customer experience, operational efficiency, and business analytics.
Competition and profitability are driving the usage of business analytics in India, something not seen as much in other regions.
85% organizations reported an increase in usage of business analytics.
67% of North American executives increased their usage of business analytics, which is 20% more than global average.
77% of people in North America are using analytics for improved decision-making — nearly 13% more than the global average.
76% report their confidence in AI has grown – 5% below global average.
80% have increased use of AI in past 2 years – 6% below global average.
70% are using AI to improve business analytics – 7% above global average.
72% of North Americans are using AI for operational efficiency - 10% more than the global average.
Increased competitiveness, reliability, and security contributed to companies' adoption of new technologies, with Singapore citing "increased competitiveness" and "reliability" more than respondents from any other region.
In Singapore, the desire to improve decision-making, use available data (69% vs 61% globally), and make decisions faster were the top reasons behind their increased usage of analytics.
Nearly 80% of respondents say their confidence in AI has increased over the last two years.
85% of companies have increased their use of AI over the last two years.
59% of respondents said improving business analytics was the main driver behind employing AI tools, followed by the need to improve customer experience (53%), and increase operational efficiency (50%).
93% of respondents said they believe AI will meet business expectations.
89% of organizations have increased the use of business analytics over the last two years.
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New Denver Broncos Head Coach Vic Fangio will have say in defensive personnel.
KUSA – Defensive know-how was a big reason why Vic Fangio was hired by John Elway to become the Broncos' new head coach.
As the team's general manager, Elway is expected to follow up by allowing Fangio to have considerable influence on the Broncos' defensive personnel. It's Fangio's 3-4 system. He knows the kind of players who would fit his system.
Elway and his top personnel assistant Matt Russell held a couple weeks of meetings with their coaches on expected free agents before taking a break last week. In two more weeks, all Broncos' football operations employees will descend on Indianapolis for the NFL Combine, which will work out and provide interview access to 338 of the best incoming rookies.
After the Broncos posted 5-11 and 6-10 records the past two years, upgrades are needed on both sides of the ball. We start today with defense. After ranking No. 1 in the NFL with 283.1 yards allowed in the Broncos' Super Bowl 50 season of 2015, the Denver D fell to No. 22 in 2018 by allowing 82 more yards a game.
Fangio and his longtime assistant Ed Donatell have been brought in to help stop the slide.
Easily, the biggest area of concern as there could be two starters to replace.
One cornerback starter, Chris Harris Jr., is back for a team-friendly $8.9 million on the final year of his contract (counting a $1 million bonus that counts against 2018 cap, but must be exercised by March 12). One safety starter, Justin Simmons, is back for an even friendlier estimate of $2.005 million (after performance pay bump from his intial $720,000 fourth-year minimum).
Otherwise, there are question marks. Veteran Tramaine Brock, who played for Vic Fangio and Ed Donatell in San Francisco from 2011-14, is an unrestricted free agent who may have a better chance of returning than Bradley Roby, another free agent who could command a fairly lucrative contract.
Second-year cornerback Isaac Yiadom and safeties Will Parks, Dymonte Thomas and Jamal Carter should return for depth.
But there is no more guarantee left on starting safety Darian Stewart's contract that is otherwise scheduled to pay him $5 million in 2019. Stewart, who turns 31 in August, was a solid four-year starter for the Broncos but any veteran making decent, non-guaranteed money is vulnerable.
There's a decent chance the Broncos will have to replace veteran Domata Peko in the middle as the likeable, 34-year-old will be a free agent.
Adam Gotsis, who emerged as the Broncos' best defensive lineman in the second half of the 2018 season, returns for his fourth season.
Derek Wolfe only had 2.0 and 1.5 sacks in the past two seasons, but is still a good value at $9.55 million in the final year of his contract. However, if Elway decides to shift considerably more financial resources to the offensive side of the ball, there's a slight chance Wolfe could be vulnerable. We'll find out his fate on the five days before the league season, or March 8, when his $1 million option bonus is due. (The option would count back against the 2018 cap).
Shelby Harris is expected to return as a restricted free agent and perhaps the new coaching staff can get something out of 2017 second-round draft pick DeMarcus Walker.
Zach Kerr is an unrestricted free agent who averaged less than $1.6 million the previous two years. He gave the Broncos good on-field value and he's a good locker-room guy, so it would be a surprise if the Broncos didn't try to re-sign him.
The good news is Todd Davis, Josey Jewell, Brandon Marshall, Keishawn Bierria and A.J. Johnson are all under contract in 2019. But how many fit Fangio's system that operates best with inside linebackers who can run?
Davis and Jewell are terrific in-box linebackers, but they are vulnerable in space.
Marshall can run, but it would be a surprise if the Broncos pay his $6.5 million, non-guaranteed salary for 2019. We'll probably find out by the morning of March 13 when $1 million of his $6.5 million salary becomes guaranteed.
It wouldn't be a surprise if the Broncos select an inside linebacker within the first three rounds of the draft – something the team hasn't done since Nate Irving in 2011. And the Broncos haven't taken a non-rushing linebacker within the first two rounds since D.J. Williams was a first-round pick in 2004.
Although Von Miller and Bradley Chubb are the strength of the team, the Broncos will be needing depth as their top two backup edge rushers, Shaq Barrett and Shane Ray, are about to hit unrestricted free agency.
The Broncos would like Barrett back, but he may look for a better opportunity to start. Jeff Holland was an undrafted rookie last year who showed promise in the final three regular-season games.


The early adopter is the aspirational demographic sought out by marketers across the land. Get traction among these consumers, and all your go-to-market strategy will take care of itself.
Your new brand/product will rise to the much-lauded status of a 'household name' by the time the slack (uninformed) late majority arrive.
The early adopter effect is generally seen as a make-or-break stage in many product development and brand marketing strategies, particularly for the consumer tech and entertainment industries.
According to the classic Rogers' bell curve, the early adopter segment represents a little over 10% of a typical consumer market. But, in a consumer landscape where truly innovative products are becoming increasingly scarce, in spite of the ever-changing nature of available technology, I often question whether the 'early adopter effect' is still as relevant is it was 10 or 20 years ago.
Firstly I feel that brands should start the product cycle by reviewing whether the traditional view of early adopters is still relevant, or indeed pertinent to their particular concept. Early adopters are generally perceived by marketers to be an urban, 18-24 year old, tech-savvy demographic; they're often portrayed as capricious snobs, only engaging with cutting-edge brands considered 'cool'.
It has long been assumed that this group is inherently attracted towards digital brands and technology categories, as a natural outcome of their behaviours. However, some of our recent research into post-demographic consumers suggests that those in the traditional early adopter category, rather than being selective and fickle, advocate and use a significantly wide range of brands in varied categories, including some more traditional service-led brands such as British Airways.
In addition to this, the internet has created a global method for 'Chinese whispers' to proliferate; meaning that consumers who don't look like the traditional view of early adopters (non-urban, emerging markets, older) can now access and influence (via direct brand engagement) the development of new products and concepts.
On the other side of the coin, this has caught out a number of brands who have found themselves overwhelmed by the sheer volume of early-stage demand.
Our own research demonstrates unequivocally that the much-lauded early adopter demographic is no longer the 18-24 bracket and no longer essentially urban. Yet this understanding is not often applied in product development, particularly for brands looking to harness technology in innovation.
The early adopter of 20 years ago has become today's early majority, while retaining their interest in the democratisation of technology. As a result, the real innovators and early adopters (a potential barometer for early beta testing etc.) are now pushed further towards the thin end of the bell curve wedge, making them even less representative of the mass market, and thus less likely to impact product success/failure.
Brands must ask themselves whether they are over-complicating product development and marketing processes by focusing on this niche audience. If we're talking about developing/launching something truly ground-breaking, such as VR or 3D printing, gaining traction and advocacy among this audience is an important hurdle in reaching mass market.
However, in many instances, particularly in the areas of customer and product propositions, new ideas are seldom truly 'new news'. In these cases is it valid to be placing so much emphasis on a group of consumers who so poorly reflect the mass market? Should we, in fact, be focusing our attentions more closely on the early majority – a larger audience, and hugely receptive to new ideas.
The fact is that most brands, when targeting what they perceive as early adopters are really targeting a very narrow band of the early majority and really missing out on a much broader and richer target market to help co-author their product development story.


text:
Q: Prestashop: Disable contact form I would like to disable the contact form in my prestashop installation but there is no plugin to do so. Any suggestions how to do that?

A: If You want to block just contact form but You want to display contact page You can put in override\controllers\front\ContactController.php:

<?php
class ContactController extends ContactControllerCore
{
 public function postProcess()
 {
  if (Tools::isSubmit('submitMessage'))
   {die('Form disabled');}
  else
   parent::postProcess();
  //return null;

 }

}

This will disable ability to send mails.

Then You can cut contact form from theme: /themes/YOUR-THEME/contact-form.tpl
to not display contact form at all
After this You have to delete file /cache/class_index.php to refresh classes in prestashop.

A: Depends what you mean by disabling contact form but here are few possibilities.

*

*Modifying core contact controller (not recommended since you will lose custom code when updating Prestashop)

Open file controllers/front/ContactController.php and add this code inside the ContactControllerCode class.
public function init()
{
    Tools::redirect('pagenotfound'); // redirect contact page to 404 page
}

*Overriding contact controller

Create a new file ContactController.php and place it in folder overrides/controllers/front/ and add the following code
class ContactController extends ContactControllerCore {
    public function init()
    {
        Tools::redirect('pagenotfound'); // redirect contact page to 404 page
    }
}

*Create a small module

Create a new directory contactpagedisabler in folder modules and inside create a file contactpagedisabler.php and put this code in
class ContactPageDisabler extends Module
{
    public function __construct()
    {
        $this->name = 'contactpagedisabler';
        $this->tab = 'front_office_features';
        $this->version = '1.0';
        $this->author = 'whatever';

        parent::__construct();

        $this->displayName = $this->l('Contact page disabler');
        $this->description = $this->l('Disables contact page.');
    }

    public function install()
    {
        return parent::install() && $this->registerHook('actionDispatcher');
    }

    // hook runs just after controller has been instantiated
    public function hookActionDispatcher($params)
    {
        if ($params['controller_type'] === 1 && $params['controller_class'] === 'ContactController') {
            Tools::redirect('pagenotfound'); // redirect contact page to 404 page
        }
    }
}

And then install this module from backoffice.
2nd option is simplest and it doesn't interfere with core files.
3rd option is probably overkill for such a small thing however it doesn't require overriding and if you or store manager ever needs the contact page back he can just disable the module from backoffice.
The module could also be expanded/modified with configuration page where you could for example get a list of all pages in store and let user decide which ones to enable/disable etc.
Update April 2018
Forget first two options and use third. Always use a module (if possible) when modifying your shop.

A: Barto's solution can also be achieved without an override.
Create another module contactformdisabler
class ContactFormDisabler extends Module
{
    public function __construct()
    {
        $this->name = 'contactformdisabler';
        $this->tab = 'front_office_features';
        $this->version = '1.0';
        $this->author = 'whatever';

        parent::__construct();

        $this->displayName = $this->l('Contact form disabler');
        $this->description = $this->l('Disables contact form submission.');
    }

    public function install()
    {
        return parent::install() && $this->registerHook('actionDispatcher');
    }

    public function hookActionDispatcher($params)
    {
        if ($params['controller_type'] === 1
            && $params['controller_class'] === 'ContactController'
            && Tools::isSubmit('submitMessage')) {
               die('Contact form submission disabled');
        }
    }
}

redpajama_set_name: RedPajamaStackExchange


This has been a strong showing for Sunrise this season, with series like Phi Brain with it's complex and engaging puzzle concept to Horizon on the Middle of Nowhere with it's bizaare nonsensical sense of humour and now Gundam AGE. Now it is worth noting that I am somewhat of a newbie to the Gundam franchise, having only watched an episode of Gundam Seed and about 3 episodes of Gundam 00. So needless to say, I am not going into Gundam AGE with a wealth of knowledge on the franchise's history.
Despite going in without any prior experience with the franchise, I found myself highly engrossed in this first episode. I was hooked in with the emotional cold-open of Fleet's past and continued to be glued until it's final moments. It is not everyday an episode opens and ends in all out war and actually pulls it off with ease.
But that is exactly what Gundam AGE has done. Everything felt so grand in scale and as a whole bigger than nearly all of the new series this Fall season (you could make a case for Hunter x Hunter). Which I attribute to both the excellent pacing and execution as well as the well composed characters that held it all together.
The entire episode really set the bar for what is to come with this series, not only that but the overall production quality of the episode was phenomenal. The animation on show here was awe-inspiring, in particular the fight scene at the end between Fleet's Gundam and one of UE Mobile Suits.
Fans of the Gundam franchise have been quite vocal regarding the new art-style of this new series with some going as far as to call it "kiddy". I assure you the artwork here is not what I would classify as kiddy. If anything I'd say it is quite reminiscent of the Mega Man franchise. With a lot of the character designs reminding me of that style. Regardless, it does the job and looks great while doing so.
As for the music, well I am not entirely sold. I personally would have chosen something with a little more punch, instead of the ballad's that were used. But that is just me. For a series with giant mech fights and as much action as this, I think a much faster paced opening and ending was warranted. Thankfully, the soundtrack shines through with the background music which perfectly captured the mood and atmosphere of what was occuring on screen providing a great companion to the events of the episode.
This first episode of Gundam AGE really set the tone for things to come and if what was on show here is anything to go by we have some really huge things ahead of us with this series. The preview for next episode promises the continued struggle with the UE, which is sure to be enthralling. All-in-all I was completely blown away and eagerly anticipate the next episode to see where this series will take us.


You may have only had a couple of drinks and thought you were fine to drive, but you were pulled over and the officer felt differently. Unfortunately, that means you're arrested and charged with a DUI. While it can be devastating to consider the impact the charge can have on you and your future, you don't just have to plea guilty and hope the judge gives you a lenient sentence. Instead, you can contact a Birmingham DUI defense attorney for help.
Your defense attorney will begin by reviewing your case carefully. In most cases, you won't realize that there could be issues with your arrest. Your attorney may be able to prove that you were unlawfully stopped, for example. Or, they may be able to prove the breathalizer tests were administered incorrectly, and therefor your charges may be dropped. These are things the average person won't be able to notice or prove, but your DUI defense attorney will. They have years of experience working with cases just like yours, and they can easily spot potential issues with the case against you.
If your charges can't be dropped, your DUI attorney will still be able to help. They may be able to convince the judge to lower your charges to a charge that doesn't come with the same harsh penalties. If that doesn't work, they may still be able to help you receive the smallest sentence possible if you are found guilty. They can also help you apply for and receive a hardship license. Your driving will be restricted, but you will still be able to drive to work and back until you can regain your license again. This can be extremely helpful in ensuring you can continue working so you have the money to pay your typical bills along with the fines you may receive for the DUI.
A DUI charge is not automatically a guilty verdict. There are ways to have the charges dropped or lowered, and it is possible for you to keep your license. Contact a DUI defense attorney as soon as possible after your arrest to ensure your rights are upheld and that you receive a better outcome for your case.


Oberlin College is a small, private, four-year university enrolling 2,929 students and offering 52 degrees in Oberlin, OH.
Check out the most popular majors and specific degrees students have earned at Oberlin College.
Good alimni network. Good reputation that opens doors.
We have a career center where you can make an appointment with someone for advice on resumes, cover letters, and job applications in general. We are also a part of the Selective Liberal Arts Consortium, which offers students a better chance of interviewing with certain companies.
All classes were conducted with a view towards critical thinking. This is a great way to prepare students for any "real world" situation or career.
I don't know what they do now, it was over 20 years ago.
It's the kids in high school who are a bit different who are usually attracted to this school. The culture is extremely liberal with a healthy dose of idealism.
"People who were weird in high school fit right in at Oberlin."
The dorms are adequate, but nothing special. However, the school has started updating the dorms and making them nicer. The dining halls and classrooms are perfectly fine, though the art facilities are particularly nice. To me, the star is the library. It has four floors of a variety of study environments.
A little less than perfectly maintained.
We have these classes called excos, which are taught by students. They can range from conversational Lebanese Arabic, to frisbee golf, to cocktail mixing.
Do you have questions about furthering your education with Oberlin College? People are listening and are ready to help. Plus, we're pretty sure others have the same question you do!


text:
Eilema fraterna är en fjärilsart som beskrevs av Butler 1887. Eilema fraterna ingår i släktet Eilema och familjen björnspinnare. Inga underarter finns listade i Catalogue of Life.

Källor

Externa länkar

Björnspinnare
fraterna


Koalakrane uses its own distinctive claw machines. Our claw machine for sale around Australia has been tested and developed into what they are now over many years of research and development.
All claw machines for sale are available in not one but four different sizes. From small plush toys and rugby balls through to giant toys, we have a claw vending machine to suit every prize.
One-year warranty on PCBs and motors.
Our smallest claw machines are transportable on a trailer or in a van and can be moved by one or two people. Not only are the machines attractive but they are durable. Solid yet lightweight materials are used, and the paint goes through a process to protect it from UV. Koalakrane machines will stay looking new for many years.
Great technical support – can even be scheduled after hours!
Full membership on Koalakrane Franchisee Facebook Group. Best source of personal sales and marketing experience.
Customer service – customer support including holidays and weekend.
When you purchase new machines from Melbourne, Sydney, Canberra or anywhere from our offices, you have a one year warranty on all major parts except for normal wear and tear such as lights. The warranty does not include malicious damage.