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\section{Introduction}
High frequency quasi-periodic oscillations (HF QPOs) were discovered by \citet{1996ApJ...469L...1V}. They are elusive modulations hidden in the noisy X-ray flux from low mass X-ray binaries \citep[LMXBs;][]{2012MNRAS.426.1701B} and are detected as Lorentzian-like peaks in their power spectra. Both neutron star (NS) and black hole (BH) LMXBs display HF QPOs \citep[for reviews see][]{2005AN....326..798V, 2006ARA&A..44...49R}. HF QPOs often show up as couple, named \emph{twin peak} HF QPOs. Because their time scale is typical of the orbital motion within 10 $r_{g}$\footnote{$r_{g}=GM/c^{2}$ is the gravitational radius of the compact object} from the compact object (milliseconds time-scale), twin peak HF QPOs might carry the fingerprints of the general relativity in a strong field regime.

Twin HF QPOs are characterized by their central frequency, amplitude (root mean square; rms) and coherence ($Q$-factor). In NS LMXBs extensive studies of both the rms and $Q$ were pursued and revealed a systematic behavior as function of the central frequency of the peak  \citep{2006MNRAS.370.1140B}. This was interpreted as possible due to the approach of the phenomenon to the innermost stable circular orbit \citep[ISCO;][]{2005AN....326..808B}. \citet{1990ApJ...358..538K} described what type of fundamental information could be extracted from the fingerprint of the orbital motion on ISCO, such as constrains to the equation of state (EOS) of the matter at supra-nuclear density in systems with a neutron star.

Twin HF QPOs are linked to the behavior of the X-ray energy spectrum of the source \citep{2010LNP...794...53B}. It is known that the HF QPOs display correlations with the low-frequency QPOs \citep{1998ApJ...506L..39F,2002ApJ...580.1030R}.

Despite their discovery since long, the puzzling twin peak HF QPOs still lack of an accepted modeling. A first model for the twin peaks observed in NS LMXBs was proposed by \citet{1998ApJ...508..791M}, based on beat-frequency mechanisms. In the relativistic precession model \citep[RPM;][]{1999ApJ...524L..63S} the twin peaks are linked to the modulations of the X-ray flux by blobs of matter orbiting in the accretion disk. The upper peak is assumed to be the modulation at the azimuthal frequency $\nu_{\phi}$ whereas the lower one that at the periastron precession frequency $\nu_{p}=\nu_{\phi}-\nu_{r}$\footnote{$\nu_{r}$ is the oscillation frequency of the radius of the orbit: from the periastron to apoastron and back.} of the orbit of the orbiting blob.\\
An observed feature of twin peak QPOs is the 3:2 ratio at which their central frequencies cluster. \citet[][]{2001A&A...374L..19A} proposed that the twin peaks could be excited by resonance mechanisms between oscillation modes in a curved space-time. Later, the idea of the 3:2 frequency cluster caused by resonant mechanisms was reviewed by \citet{2005A&A...437..209B}, who claimed that a random-walk could reproduce the cluster at the 3:2 ratio. Subsequently the random-walk hypothesis was debated by \citet{2008AcA....58..113T}.\\
The shape of the modulations by a hot-spot orbiting in the Kerr metric was studied in detail  by \citet{2004ApJ...606.1098S} by means of ray-tracing techniques. The power spectra of the signal are characterized by peaks at the azimuthal frequency $\nu_{\phi}$, the beats $\nu_{\phi}\pm\nu_{r}$ and their Fourier harmonics.
It would be interesting to investigate whether the beats $\nu_{\phi}\pm\nu_{r}$ originate from the timing of the azimuth phase $\phi(t)$ of the orbiting object rather than from the modulations on the amplitude of the signal because of relativistic effects (Doppler/gravitational shifts).
Hence we concentrate on a frequency modulated (FM) rather than on an amplitude modulated (AM) signal \citep{taub}. This is one of the issues that has stimulated the investigation presented in this letter.

Works by \citet{2008A&A...487..527C} and \citet{2009A&A...496..307K} highlighted the role of the strong tidal force on matter orbiting close to a black hole. These works modeled the NIR/X-ray flares that are observed coming from the galactic center \citep{2003Natur.425..934G}. The numerical code on tidal disruption of small satellites
\citep{2009A&A...496..307K} was used to fit the observed light curves.\\
The simulations of the tidal stretching of a clump of matter were applied to the twin peak HF QPOs as well. It was possible to reproduce the high-frequency part of the typical power spectra observed in LMXBs. The simulated power spectra show the power law with the twin peak QPOs \citep{2009AIPC.1126..367G}.\\
It is not yet clear whether the upper/lower peak of the twin peaks corresponds to the azimuthal frequency. The results from the tidal interaction code show that the lower peak in frequency of the twin peaks corresponds to the azimuthal frequency $\nu_{\phi}$, whereas the upper one corresponds to the modulation at $\nu_{\phi}+\nu_{r}$. This is different from the RPM assumptions \citep{1999ApJ...524L..63S}, since it links the lower peak to $\nu_{p}=\nu_{\phi}-\nu_{r}$ and the upper one to $\nu_{\phi}$.

In this letter we highlight the temporal behavior of the azimuth phase $\phi(t)$ of an orbiting object and suggest it as root of the observed twin peak QPOs. Our goal is to investigate the appearance/disappearance of twin peaks in the power spectrum,
investigating as well what modulation corresponds to the upper/lower peak: $\nu_{\phi}$, $\nu_{\phi}+\nu_{r}$ or $\nu_{\phi}-\nu_{r}$?

\section{Orbital motion on non-closed orbits}
The repeating pattern in time of the azimuth phase $\phi(t)$ for orbital motion on a circular orbit can be described by a simple sinusoid
\begin{equation}\label{eq1}
A\sin\left(2\pi t\nu+\phi_{0}\right)
\end{equation}
where $A$ is the amplitude, $\phi_{0}$ the phase at $t=0$ and $\nu=1/P$ the oscillation frequency of the sinusoid of orbital period $P$. The linear term $2\pi t\nu$ draws the linear increase in time of the azimuth phase $\phi(t)$, i.e. its timing law is $\phi(t)=2\pi t\nu+\phi_{0}$ radians.\\
\begin{figure}
 \resizebox{\hsize}{!}{\includegraphics[width=0.3\textwidth]{fig1.eps}}
 \resizebox{\hsize}{!}{\includegraphics[width=0.3\textwidth]{fig2.eps}}
 \resizebox{\hsize}{!}{\includegraphics[width=0.3\textwidth]{fig3.eps}}
 \caption{\emph{Top}: Phase of the azimuth $\phi(t)$ for orbital motion on a non-closed orbit in the Schwarzschild       metric. \emph{Middle}: Phase-residuals after subtracting to $\phi(t)$ the best-fit first-order polynomial. \emph{Bottom}: Phase-residuals for an orbit at a different radius (see text).}\label{fig1}
\end{figure}
On an eccentric orbit the orbital motion is faster at the periastron than at apoastron. Thus, the phase of the azimuth on an eccentric orbit is not a linear function of time. We shall write the orbital motion on an eccentric orbit
\begin{equation}\label{eq2}
A\sin\left(2\pi t\nu_{\phi}+B\left(r_{p},e\right)\sin\left(2\pi t\nu_{r}\right)+\phi_{0}\right)
\end{equation}
where $B(r_{p},e)$ is the amplitude of the oscillating phase because of the different orbital speed of the object at periastron/apoastron passage, happening at the radial frequency $\nu_{r}$. We can write \mbox{$B(r_{p},e)\sim2\pi$(v$_{p}$-v$_{a}$)/\={v}} radians, where v$_{p}$ and v$_{a}$ are the orbital speeds at the periastron and apoastron, \={v} is the mean orbital speed on the orbit of periastron $r_{p}$ and eccentricity $e$. The exact value of $B(r_{p},e)$ is calculated numerically in Section~\ref{sec21}.

In a curved space-time the orbits are non-closed, $\nu_{r}$ is always smaller than $\nu_{\phi}$.
This leads to the periastron precession of the orbit at the frequency $\nu_{p}=\nu_{\phi}-\nu_{r}$, like in the Mercury's orbit. The power spectrum of equation (\ref{eq2}) might give peaks besides that at $\nu_{\phi}$.

The observed frequency of the twin peak QPOs are typical of the orbital motion in a region of the space-time within $r=10\ r_{g}$ from the compact object. For a Schwarzschild black hole the ratio $\nu_{r}/\nu_{\phi}$ ranges from 0 at $r=r_{ISCO}=6\ r_{g}$ (at ISCO $\nu_{r}=0$) to 1 at infinite $r$. Thus, from equation (\ref{eq2}) the phase of the azimuth is a linear function of time only at ISCO.

We write the FM signal
\begin{equation}\label{eq4}
S(t)=\mathrm{Random}\left(t\right)+A\sin\left(2\pi t\nu_{\phi}+B\left(r_{p},e\right)\sin\left(2\pi t\nu_{r}\right)+\phi_{0}\right)
\end{equation}
where the term Random($t$) is random noise, as expected in the signal from LMXBs.
The power spectrum of $S(t)$ is the squared  modulus of the Fourier transform $S'(\nu)$ calculated numerically, cross-checked with the task {\tt powspec} in the timing analysis software package Xronos\footnote{http://xronos.gsfc.nasa.gov/}.

We should bear in mind that the exact shape $S(t)$ of the modulation by an orbiting object/hot-spot is obtained by performing  ray-tracing of photons in the curved space-time \citep[e.g.][]{2004ApJ...606.1098S,2009A&A...496..307K}. Here we are only attempting to study the azimuth phase temporal behavior $\phi(t)$ of the orbiting object/hot-spot, i.e. its kinematics.  This is a well known method used in pulsar timing analysis to study the neutron star and its environment. Pulsars timing is performed by studying the phase temporal behavior $\phi(t)$ of the rotating hot-spot \citep[e.g.][]{1975ApJ...195L..51H,1994Sci...264..538W,2002ApJ...581..501S,2006Sci...314...97K,
2012arXiv1210.1796G}.

\subsection{Orbital motion in the Schwarzschild metric}\label{sec21}
To justify the approach described above, we calculate the orbital motion in the Schwarzschild metric, following the parametrization in
\citet{1994PhRvD..50.3816C}\footnote{The integrals reported in \citet{1994PhRvD..50.3816C}, describing both the azimuth phase $\phi(\chi)$ and time $t(\chi)$ as function of the radial phase parameter $\chi$, were calculated in the limit of orbits of small eccentricity. The relativistic frequencies from this calculation were cross-checked with those obtained analytically (German\`a 2006, Laurea thesis).}.
Fig.~\ref{fig1} (top) shows the parametric plot between the azimuth phase $\phi(\chi)$ and the coordinate time $t(\chi)$, for an orbit of eccentricity $e=0.1$, with periastron at $r_{p}=7.5\ r_{g}$ and around a $8\ M_{\odot}$ black hole. The overall linear increase simply shows the amount of the azimuth phase in coordinate time, as function of the radial phase parameter $\chi$. The simulation lasts for 10 radial oscillations, corresponding to 20 azimuth turns ($\sim125$ rad), because for this orbit $\nu_{\phi}=2\nu_{r}$.

The overall linear behavior in Fig~\ref{fig1} (top) is simply the argument $2\pi t \nu_{\phi}$ in equation (\ref{eq4}). For a circular orbit, only the term
$2\pi t\nu_{\phi}$ describes the orbital phase $\phi(t)$. We notice that in Fig~\ref{fig1} (top) the overall linear behavior wobbles. Fig~\ref{fig1} (middle) shows the residuals of the  azimuth phase after fitting to the function $\phi(t)$ a first-order polynomial and subtracting it. There are oscillations at the relativistic radial frequency typical for this orbit, $\nu_{r}=90$ Hz. The amplitude of the oscillation is \mbox{$B(7.5\ r_{g},0.1)\sim0.3$ rad}. Fig~\ref{fig1} (bottom) shows the phase-residuals for an orbit with the same
$e$ at an inner radius, $r_{p}=6\ r_{g}$\footnote{For an orbit with $e=0.1$ the innermost stable bound orbit has the periastron at $r_{p}=5.5\ r_{g}$.}. At this radius, $\nu_{r}=70\ Hz$. In Fig~\ref{fig1} bottom the number of oscillations is smaller than in Fig~\ref{fig1} middle, because $\nu_{r}$ is smaller.

To conclude, the azimuth phase $\phi(t)$ on a slightly eccentric orbit close to a compact object ($r\sim r_{g}$) is not a linear function of time. The phase oscillates at the radial frequency $\nu_{r}$ because of the different orbital speed at periastron/apoastron passage. In a curved space-time the frequency at which an orbiting object is at the  periastron/apoastron is $\nu_{r}\neq\nu_{\phi}$. We write the timing law
\begin{equation}
\phi\left(t\right)=2\pi t\nu_{\phi}+B\left(r_{p},e\right)\sin\left(2\pi t\nu_{r}\right)+\phi_{0}.
\end{equation}
Because the first derivative of the phase $\phi(t)/(2\pi)$ is the frequency of the orbital motion as a whole, in a curved space-time the orbital motion is not periodic.

\section{Results}
The noisy function $S(t)$ (eq.~[\ref{eq4}]) is shown in Fig.~\ref{fig2} (top).
From the calculations in Section~\ref{sec21}, the radial frequency is $\nu_{r}=90$ Hz whereas the azimuthal one is $\nu_{\phi}=2\nu_{r}=180$ Hz, for an orbit with periastron $r_{p}=7.5\ r_{g}$ around
a $8\ M_{\odot}$ Schwarzschild black hole.
We are not interested in any parametrization of the amplitude of $S(t)$, so we choose to use arbitrary units to describe it.
\begin{figure}
\resizebox{\hsize}{!}{\includegraphics[width=0.3\textwidth]{fig4.eps}}
\resizebox{\hsize}{!}{\includegraphics[width=0.3\textwidth]{fig5.eps}}
\caption{\emph{Top}: The simulated FM signal $S(t)$ from a non-closed orbit described by equation (\ref{eq4}). The bin time of the temporal series is $dt=0.0001$ s. \emph{Bottom}: Power spectrum of the signal described by equation (\ref{eq4}) ($B=0.5$).}\label{fig2}
\end{figure}

\subsection{Power spectra}
Fig.~\ref{fig2} (bottom) shows the power spectrum of the FM signal $S(t)$ described  in Fig.~\ref{fig2} (top). The simulated power spectrum reproduces the twin peaks seen in observed power spectra of LMXB XTE J1550-564 containing a black hole \citep{2002ApJ...568..845O,2006ARA&A..44...49R}.
In Fig.~\ref{fig2} (bottom) the uppermost couple of peaks in frequency corresponds to $\nu_{\phi}=180$ Hz and \mbox{$\nu_{\phi}+\nu_{r}=270$ Hz}.
Because in this region of the space-time \mbox{($r_{p}=7.5\ r_{g}$)} \mbox{$\nu_{r}/\nu_{\phi}=0.5$}, $\nu_{\phi}+\nu_{r}$ and $\nu_{\phi}$ are in a 3:2 ratio. In observed power spectra the peaks are in a 3:2 ratio. This feature has led to the idea that twin peaks could be produced by resonance mechanisms \citep{2001A&A...374L..19A}. The simulation shows a third peak at the periastron precession frequency $\nu_{p}=\nu_{\phi}-\nu_{r}=90$ Hz. The three peaks display a harmonic relation in frequency, 1:2:3. Such harmonic relation was noticed by \citet{2002ApJ...580.1030R} in a set of observations of the source XTE J1550-564, with the frequency of the peaks \mbox{$\sim$ 90:180:270 Hz}.
\begin{figure}
\resizebox{\hsize}{!}{\includegraphics[width=0.3\textwidth]{fig6.eps}}
\resizebox{\hsize}{!}{\includegraphics[width=0.3\textwidth]{fig7.eps}}
\caption{Power spectra of the signal described by equation (\ref{eq4}) showing the uppermost two peaks in frequency \emph{not} in a 3:2 ratio. \emph{Top}: Power spectrum with twin peaks for an orbit with $r_{p}\sim10\ r_{g}$ and $B=0.5$. \emph{Bottom}: Power spectrum for an orbit at $r_{p}\sim6\ r_{g}$.}\label{fig3}
\end{figure}

Fig.~\ref{fig3} (top) shows the power spectrum of the signal $S(t)$ for an orbit at
$r_{p}\sim10\ r_{g}$ with the uppermost couple of peaks \emph{not} in a 3:2 ratio. The azimuthal frequency is $\nu_{\phi}=108$ Hz and the radial one $\nu_{r}=76$ Hz, such that $(\nu_{\phi}+\nu_{r})/\nu_{\phi}\sim1.7$. Fig.~\ref{fig3} (bottom) shows the power spectrum for an inner orbit, $r_{p}\sim6\ r_{g}$, with $\nu_{\phi}=238$ Hz and $\nu_{r}=70$ Hz. The ratio of the uppermost couple is $(\nu_{\phi}+\nu_{r})/\nu_{\phi}\sim1.3$.
Fig.~\ref{fig3} (top/bottom) suggests that resonance mechanisms to explain the twin peaks might not need to be invoked.

The ratio $(\nu_{\phi}+\nu_{r})/\nu_{\phi}$ ranges from $\sim$ 1.7 to 1.3 as long as the frequency $\nu_{\phi}$ ranges from 108 Hz to 238 Hz, thus with a relative increment of (238-108)/238$\sim$ 0.55. We can use this clue to further investigate whether the  couple of twin peaks in the observed power spectra is ($\nu_{\phi}$, $\nu_{\phi}+\nu_{r}$) or ($\nu_{\phi}-\nu_{r}$, $\nu_{\phi}$). If the observed couple of peaks were ($\nu_{\phi}-\nu_{r}$, $\nu_{\phi}$) they would have been in a 3:2 ratio at \mbox{$r_{p}\sim6.3\ r_{g}$}. Around such radius \mbox{($r_{p}\sim6.5$ -- $5.8\ r_{g}$)} the ratio ranges from 1.7 to 1.3 as long as $\nu_{\phi}$ relatively increases by 0.19. Fig.~3 in \citet{2006AIPC..861..786T} shows the frequency distribution of twin peaks in several sources. In NS LMXBs the distribution clusters at the 3:2 frequency ratio and mostly ranges from \mbox{$\sim$ 1.7 to 1.3} (the lower peak from 400 to 900 Hz, the upper one from 700 to 1200 Hz). If the observed couple of peaks is \mbox{($\nu_{\phi}-\nu_{r}$, $\nu_{\phi}$)} the upper peak $\nu_{\phi}$ on the y-axis of that figure relatively increases by 0.42. The typical relative error on the measured frequency of HF QPOs is $\sim1\%$ \citep{1996ApJ...469L...1V}, implying an error of $\left(\sigma_{(\nu_{2}-\nu_{1})}/(\nu_{2}-\nu_{1})+\sigma_{\nu_{2}}/\nu_{2}\right)\times0.42\sim0.02$ on the factor 0.42. Thus, the  relative increment of 0.42 from observations is statistically in disagreement with the numerical one, equal to 0.19. If instead the observed couple of peaks corresponds to ($\nu_{\phi}$, $\nu_{\phi}+\nu_{r}$) the lower peak $\nu_{\phi}$ on the x-axis of Fig.~3 in \citet{2006AIPC..861..786T} relatively increases by $\sim$0.56, in agreement with the 0.55 increment  estimated numerically. This further suggests that the observed twin peaks correspond to the couple ($\nu_{\phi}$, $\nu_{\phi}+\nu_{r}$) and they might take place over a window of radii corresponding to \mbox{$r_{p}\sim6$ -- $10\ r_{g}$} in the Schwarzschild metric.

\section{Discussion and Concluding Remarks}
The investigation reported in this letter shows that the twin peak HF QPOs observed in LMXBs might be the clue of the kinematics of orbital motion in a strongly curved space-time ($r\sim r_{g}$).
With respect to a static observer at infinity, the azimuth phase $\phi(t)$ is described by the linear function $2\pi t\nu_{\phi}$ plus a term of amplitude $B(r_{p},e)$ oscillating at the radial frequency $\nu_{r}\neq\nu_{\phi}$. The phase
$\phi(t)$ wobbles at the radial frequency $\nu_{r}$ making the whole orbital motion not being periodic. The observed width of the QPOs, therefore their quasi-periodicity, could be a consequence of the orbital phase wobbling.

The appearance/disappearance of the twin peaks depends on $B(r_{p},e)$.
The function $B(r_{p},e)$ characterizes the non-linear part of the azimuth phase $\phi(t)$.
The simulated power spectra show that the uppermost couple of peaks in frequency corresponds to $\nu_{\phi}+\nu_{r}$ and $\nu_{\phi}$. Three peaks are reproduced by these simulations and the lowest peak in frequency corresponds to the periastron precession frequency of the orbit $\nu_{p}=\nu_{\phi}-\nu_{r}$. At a given radius ($r_{p}\sim7.5\ r_{g}$) such three peaks display a 1:2:3 harmonic relation in frequency. Evidence of these peaks in a 1:2:3 harmonic relation was reported in \citet{2002ApJ...580.1030R}.

Simulations of the tidal disruption of a clump of matter by a Schwarzschild black hole \citep{2009A&A...496..307K} show that a signal with only the uppermost two peaks can be obtained, i.e. $\nu_{\phi}$ and $\nu_{\phi}+\nu_{r}$ \citep[][]{2009AIPC.1126..367G}. The tidal stretching might blur the phase temporal behavior of the signal, thus affecting the appearance of the beats $\nu_{\phi}\pm\nu_{r}$. The typical power law seen in the observed power spectra might originate from the increase of the signal because of the tidal disruption of the clump of matter \citep[e.g.][]{1990A&A...227L..33B,2009AIPC.1126..367G,2012mgm..conf..928K}.\\ Thus, tidal effects on matter orbiting a compact object might be complementary to the features of FM signals described here. Interestingly, \citet{2012Sci...337..949R} recently reported a QPO in the X-ray flux  coming from the tidal disruption of a star by a supermassive black hole.

We note that twin peaks might be produced even when their frequencies are not in a perfect 3:2 ratio. This suggests that their nature could not be a key feature of resonance mechanisms \citep{2005A&A...437..209B}, but rather their root might be inherent to a FM signal characterized by the orbital phase $\phi(t)$ on a generic eccentric relativistic orbit.

\section*{Acknowledgments}
The author acknowledge financial support from the \mbox{CNPq-Brazil}.\\
I would like to thank Massimo Calvani  and Antonio Kanaan for stimulating discussions. I also thank Andrej \v{C}ade\v{z} and Uro\v{s} Kosti{\' c} for the help with their simulations from the tidal interaction code. Thanks to Rodolfo Angeloni for fruitful discussions on interacting binaries. The author wish to acknowledge the Aqueye/Iqueye team whose work on pulsar timing analysis has contributed to stimulate this study.

\bibliographystyle{mn2e}

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UniverSelf, realizing autonomics for Future Networks
FP7 Project Contract Number: 257513
Duration: 36 months
Project Total Cost: 16.6 million euro
EC Contribution/Funding: 10.5 million euro
Project Coordinator: Laurent Ciavaglia, Alcatel - Lucent Bell Labs France
Technical Manager: Christian Destré, France Telecom SA
UniverSelf unites 17 partners with the aim of overcoming the growing management complexity of future networking systems, and to reduce the barriers that complexity and ossification pose to further growth.
While there has been undeniable progress in the field of autonomics research over the past several years across the world and especially in Europe, widespread deployments of self-management techniques are still missing. At the same time the need for techniques enabling the transformation of operational models, the evolution of networks towards a flexible playground for operators, and more generally techniques participating to the increase of the return on investment, is becoming more and more evident. Further, most efforts and initiatives have been focussed on solving manageability bottlenecks in a given technological domain, while services extend anywhere, regardless of the technological boundaries (e.g., wireline/wireless).
UniverSelf arises from this context and is thus driven by the need and objective to take self-management a leap further, and, in doing so, be both a federating and impactful project.
This translates into four major goals :
The design of a Unified Management Framework for the different existing and emerging architectures, or for architectures designed in past autonomic research. This unified and evolvable framework will constitute a cross-technology (wireless and wireline), common substrate for both systems and services.
The design of all required functions to achieve self-management and embed these features right into the systems and network equipments that constitute the infrastructure and support service delivery, paving the way to full network empowerment.
The impact on the industry and the push of European research into the direction of exploitation. This will be done by demonstrating the possibility to deploy autonomic solutions in carrier grade networks.
Finally, UniverSelf will bring confidence and trust into autonomic technologies for telecommunication networks. This will be achieved by setting a durable trend, across Europe, on the definition of labelling or "certification" techniques for autonomics empowered products.
Technical Approach
UniverSelf combines both top-down and bottom-up methodologies that shall enable to:
Build on the relevant existing know-how and technologies that have proven their value. Consolidate existing initiatives and approaches. Identify the main features of a unified framework that could host these. Identify the architectural and functional constraints. We refer to this as a "cleaned state" approach (compared to the "clean slate" term).
Identify the nature of problems appearing in different use-cases (distributed observation, optimization, control…), provide adequate formal models and algorithms, and integrate architectural and functional concerns.
Bring the results of the research and development to the products by natural phased proof of concepts, validation and benchmarking as well as bring the technologies and solutions to the market by standardisation.
UniverSelf is organized into 4 technical work-packages :
WP2 (Unified Management Framework) aims at federating self-management approaches and architectures to release a global autonomic management system for both current and future networks and services, spanning wireline and wireless technologies.
WP3 (Network Empowerment) is dedicated to the study, design and evaluation of common classes of algorithms with self-x and cognitive capabilities together with the requirements for their embodiment into network functions.
WP4 (Deployment and Impact) has the mission of: (1) producing use-case refinements (pointing out real manageability bottlenecks and the related requirements); (2) making simulations and emulations of the solutions designed by the joint work of WP2 and WP3; (3) eventually deploying them into test-beds for experimental validation; (4) analyzing the impact of above solutions; (5) making the assessments for establishing trust in autonomics.
WP5 (Trend Setting) has the mission to disseminate the research outcomes and give international visibility to the project and its corresponding findings, as well as to actively support the trust and certification/labelling initiative.
An essential structuring element of UniverSelf consists in the so called use-cases, the study of which (from identification to prototyping/validation) takes the form of a life-cycle throughout the work-packages (WP4>WP3>WP2>WP4) which in turns strongly participates to the realization of an Integrated Project and maximizes the efficiency of these work-packages.
More details about the Work Packages can be found on the "About UniverSelf/Work Packages" page of this website: http://www.univerself-project.eu/work-packages.
Key issues will of course arise from the use-cases and the complexity they impose to problem solving
approaches. Unification and so, for example, finding the correct level of abstraction and generalization across heterogeneous components, identifying com
monalities in the nature of different problems,
finding common classes of algorithms for seemingly different problems are key challenges that will need to be tackled in view of the design of the UMF and the embodiment of intelligence. Standardization and more precisely, in a context where proprietary intelligence is a differentiator, the identification of the suitable elements for standardization (architecture, protocols, data formats …) is an important challenge also.
UniverSelf plans to achieve highest impact with reference to the work-programme 2009-2010:
By providing operators flexible infrastructures for increased network demand, new business opportunities as well as efficient services integration, reinforcing European leadership.
Through self-x capabilities, enabling dynamic optimized network resource usage and allocation, resulting in reduced CapEx/OpEx and human intervention.
Through pre-standard specifications, combined with a strong large scale experimental validation phase
Through a novel unified framework easing the development and integration of end-to-end global interconnectivity, cooperation and real-time experience future internet services.


. And this year Santa's developer elves went a bit further. They created a Chrome extension that enables you to simultaneously browse the web on your Chrome Browser and follow Santa along his route. Simply install the Santa Tracker Chrome extension from the Chrome Web Store.
Before Santa takes off on Christmas Eve, you can also use the extension to follow the countdown to his departure, play around with his blimp, elf bus, and write messages on a frosty browser window.
While everyone in Santa's Village is busy gearing up for the big day, they always make time for visitors. You can meet some elves and ask Santa to make a personal phone call to a friend or your family.
For more ways to get holiday inspired Chrome themes, apps, and extensions, check out the holiday collection in the Chrome Web Store - including the Santa Tracker chrome theme. And, if you don't have Chrome yet, give it a spin.
Happy holidays from all of us at Google!
On Christmas Eve, as Santa makes his way across the world, you can follow his progress and keep tabs on how many presents he's delivered with the Google Maps's Santa Tracker. And this year Santa's developer elves went a bit further. They created a Chrome extension that enables you to simultaneously browse the web on your Chrome Browser and follow Santa along his route. Simply install the Santa Tracker Chrome extension from the Chrome Web Store.
we released This Exquisite Forest, a Chrome Experiment that lets you create collaborative animations using an online drawing tool. Thousands of people from all over the world have contributed to the project, creating unique animations like Looking Up / Looking Down, Wine after Coffee and Animated Typography. For any of these animations, you can click the button in the lower right to add to the story and branch it in a new direction.
A few months ago we released This Exquisite Forest, a Chrome Experiment that lets you create collaborative animations using an online drawing tool. Thousands of people from all over the world have contributed to the project, creating unique animations like Looking Up / Looking Down, Wine after Coffee and Animated Typography. For any of these animations, you can click the button in the lower right to add to the story and branch it in a new direction.


text:
B Curve Space-time from Spinning disc?
Thread starter lucas_
lucas_
No. There were non-relativistic treatments of spin before the Dirac equation was discovered.
Can you please share some peer review reference(s) about the equations for spin (0, 1/2, etc) without using relativity?
lucas_ said:
the equations for spin (0, 1/2, etc) without using relativity?
"Equations for spin" is a bit of a misnomer. In quantum mechanics, "spin" is an observable on a Hilbert space that is separate from the "configuration space" on which the position and momentum observables are defined. We can define the Hilbert spaces for a given spin (spin 1/2, spin 1, etc.) without using relativity at all. Most QM textbooks will discuss this.
In order to link the above quantum mechanical "spin" observable with the usual classical understanding of angular momentum, the standard technique is to look at representations of the group that describes the symmetries of spacetime. In relativity, this group is the Poincare group; in non-relativistic classical mechanics, it is the Galilei group. Both groups have SU(2) as the subgroup that describes rotations, and the irreducible representations of SU(2) are labeled with the standard "spin" indexes of 0, 1/2, 1, etc.
The references in the Wikipedia articles on the representation theory of the Poincare and Galilei groups are a decent starting point for digging into the gory details of all this; I have barely scratched the surface above.
Representation theory of the Poincaré group - Wikipedia
Representation theory of the Galilean group - Wikipedia
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The references in this Wikipedia article, along with the discussion in the particular section I link to, might also be useful if you want to understand the basic QM model of spin (which, as noted in my previous post, does not require relativity):
Spin (physics) - Wikipedia
I'm now convinced to stay away from pop sci. But for laymen like us. If we don't read the pop-sci. How do we know what to read or focus on in textbooks.
But pop-sci is almost akin to disinformation, isn't it. For 4 facts, 2 were already refuted.
1. Spinning disc can cause space to be curved - FALSE
2. Relativity is what cause spin - FALSE
Please address the 3rd and 4th claim of Michio which is:
3. "Moreover, since relativity governs the properties of electricity and magnetism, all modern electronics would come to a halt, including generators, computers, radios, and TV.". Relativity really governs the
properties of electricity and magnetism?
4. "Without relativity, earth would freeze solid", "The nuclear furnace that drives the sun and stars would shut down without relativity. If there were no E=mc^2, the universe would suddenly become dark and cold, making life impossible". True?
For 3 above. Relativity doesn't really govern the properties of electricity and magnetism? If not, then what governs them? And what is the relationship of relativity to electricity and magnetism (all I know is they are part of symmetry when using special relativity, maybe this is the context that without relativity, there is no electricity and magnetism?)
For 4 above. At least this may be true that without relativity, there would be no E=mc^2 or sun, right?
I'd not ask other items. I'm now convinced why only peer reviewed references were allowed in PF. Without, we would spend so much time just sorting through the disinformation in the sources.
How do we know what to read or focus on in textbooks.
In general, unless you already have a good background in the subject of a textbook, you should not try to pick and choose; you should just read the textbook and work the problems.
Relativity doesn't really govern the properties of electricity and magnetism?
I would say this is backwards; the fact that the properties of electricity and magnetism (and, as we now know, the properties of all fundamental interactions) are Lorentz invariant, rather than Galilei invariant, is what makes relativity the correct theory, rather than non-relativistic mechanics.
without relativity, there would be no E=mc^2
It depends on how you interpret that equation. The best current interpretation is that it is simply an expression of a unit conversion: the conventional units of energy are the conventional units of mass, times ##c^2##. In itself this equation says nothing about whether rest mass and other forms of energy can be inter-converted.
It is true that no one has ever developed a non-relativistic theory in which rest mass and other forms of energy can be inter-converted, for example by a particle and antiparticle annihilating each other and producing radiation. However, that could just be due to historical accident--that by the time experiments showed that such reactions were possible, relativity had already been developed and shown to give more accurate predictions in many other experiments, so there was no incentive to try to develop a non-relativistic theory of such reactions. In itself this does not prove that a non-relativistic theory of such things is impossible, or that they would be impossible in a hypothetical alternate universe where relativity was not true.
More generally, claims of the sort Kaku is making are not claims about physics anyway. They are just sensationalistic claims made to sell books, articles, and TV shows. Neither Kaku nor anyone else can do experiments in some alternate universe in which relativity is not true, so nobody knows for sure what would or would not be possible in such a universe.
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I heard about E=mc^2 since grader. Do you have any peer reviewed reference(s) exactly how they are derived? Or is it ad-hoc only? About Michio statement "If space and time become distorted, then everything you measure with meters and clocks also becomes distorted, including all forms of mass and energy", it may have a iota of truth in it? I want to see the exact derivations or proof of it. I heard about E=mc^2 since a grader and now need to see it in detail and in full glory. Thank you.
This is a good example of why it's not a good idea to learn science from pop science articles. The article's description is highly misleading. See below.
It's possible that it played a role, but I don't think the connection the article is claiming is valid.
First, a key distinction: the article discusses curved space, but space is not the same as spacetime, and the curvature of the "space" of a spinning disk has nothing whatever to do with spacetime curvature. Spacetime in the case of the spinning disk is flat.
Second, the "space" of the spinning disk isn't even a 3-dimensional spatial "slice" cut out of 4-dimensional spacetime. It's an abstract "space" that you get by performing a particular mathematical operation (the technical term is "quotient space"), and doesn't correspond to any actual 3-dimensional space at all.
Wait. First I know LET discussion is banned (although historical discussion of it not banned). But we are not discussing the details but historical context. I'm just pointing out that Michio Kaku may have it in mind in the analogy of the spinning disc. For if the material physically contract, then in the spinning disc, the inner part contracts more than outside so curvature is actually initiated so here we have LET GR in its full glory? Just state if it is possible. Because Michio Kaku article in Einstein 100 year anniversary is one of the most powerful pop-sci articles about relativity written so it's justified to at least tell the truth whether Michio spinning disc is an example of actual LET GR. If it works, just say yes or no to not violate that details of LET would not be discussed. We are not discussing details of it but I was just asking if Michio example of it can work and historical context.
Remember also when Einstein fist cooking up general relativity. He wasn't using the Minkowski interpretation of space-time. So with regards to Michio statement "One key to Einstein's thinking is to analyze a spinning disk. Since the rim of the disk travels faster than the cetner of the disk, the theory of relativity states that the rim is compressed more than the center. If so, the disk must be distorted" Just see the illustration in the OP. Maybe Einstein really thought of it and it was LET GR in its full glory? Note historical discussion of LET is allowed according to Forum rules. Only details of LET not allowed. So the historical discussion is justified.
Third, the "rubber sheet" model that the article describes is not an analogue of the curved "space" of the spinning disk. Why? Because the curved "rubber sheet" space is an actual 3-dimensional spatial "slice" cut out of the 4-dimensional spacetime of a static gravitating mass. However, this "space" is curved because of the particular way it is cut from the spacetime; there are other ways of cutting such slices that make the spatial slices flat. So once again, the curvature of the "rubber sheet" space is not the same as the curvature of the spacetime; the latter is there no matter how we cut spatial slices out of the spacetime.
Nugatory
Do you have any peer reviewed reference(s) exactly how they are derived? Or is it ad-hoc only?
Googling for "E=mc^2 derivation" will find some good derivations, and any first-year textbook (such as Kleppner and Kolenkow) will cover this.
Be aware that ##E=mc^2## is a special case (the mass is at rest so the momentum ##p## is zero) of the more general ##E^2=(m_0c^2)^2+(pc)^2##. A pretty good rule of thumb is that if whatever you're reading doesn't eventually get around to that more general relationship... it's not giving you the whole story.
phinds
@lucas_ as others have already pointed out (a point you seem to have taken to heart) your faith in pop-science is very seriously misplaced. I would add to that that your belief in Kaku is even MORE misplaced. He is one of the worst popularizes in terms of reliability and accuracy.
You can find numerous threads here on this site pointing out his flaws. Here are a couple from off-site
http://rationalwiki.org/wiki/Michio_Kaku
http://scienceblogs.com/pharyngula/2011/02/16/why-do-physicists-think-they-a/
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For if the material physically contract, then in the spinning disc, the inner part contracts more than outside so curvature is actually initiated so here we have LET GR in full glory?
No, the spacetime is still flat. The disk is experiencing internal stresses because different parts of it want to move in different directions; either these stresses distort it (as Kaku describes) or it breaks.
Because Michio Kaku article in Einstein 100 year anniversary is one of the most powerful articles about relativity written....
In the 24 hours that this thread about Kaku has been running, you could have worked your way well into the first chapter of "Spacetime Physics" by Taylor and Wheeler. It's the difference between looking at a photograph of a delicious meal in a cooking magazine and experiencing the real thing by sitting down and eating it.
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About Michio statement "If space and time become distorted, then everything you measure with meters and clocks also becomes distorted, including all forms of mass and energy", it may have a iota of truth in it?
Not really. Consider the current SI definitions of the meter and second: the second is defined in terms of a particular hyperfine transition in cesium, and the meter is defined in order to make the speed of light exactly 299,792,458 meters per second. So meters and seconds are defined in terms of a physical process that can be measured anywhere. Since that process defines what meters and seconds are, it doesn't even make sense to ask whether meters and seconds can become distorted.
More generally, suppose you are on Earth and I am in some galaxy a billion light-years away. How could we possibly compare our meters and seconds to see whether they were the same? There is no invariant way of doing that. The only thing we can do is to define our meters and seconds in terms of the same physical process, as SI units do.
LET GR
There is no such thing. LET was never extended to cover curved spacetime the way standard Special Relativity was extended to General Relativity.
Going to your statement: "
First, a key distinction: the article discusses curved space, but space is not the same as spacetime, and the curvature of the "space" of a spinning disk has nothing whatever to do with spacetime curvature. Spacetime in the case of the spinning disk is flat."
But what would happen if the spinning disc is rotating near the speed of light (in convensional SR). Won't the inner rim be more length contracted? What would happen to the spinning wheel when seen at its plane. Won't it create folds in the wheel?
what would happen if the spinning disc is rotating near the speed of light.
It wouldn't change anything I said.
But is not a muon is length contracted and time dilated or any object is length contracted or time dilated when moving near the speed of light. So just want to analyze it in terms of spinning disc at speed of light. Nothing would be length contracted or time dilated? why doesnt it apply to spinning wheel rotating near the speed of light?
is not a muon is length contracted and time dilated or any object is length contracted or time dilated when moving near the speed of light. So just want to analyze it in terms of spinning disc at speed of light. Nothing would be length contracted or time dilated? why doesnt it apply to spinning wheel rotating near the speed of light?
I didn't say anything about any of this being wrong. All I said was that spacetime is flat for the spinning disc. That's true regardless of how fast it is spinning. The disc itself being length contracted does not mean spacetime isn't flat; length contraction and time dilation occur in SR, i.e., in flat spacetime.
Adding to the above. Remember in LHC, the particle has time dilation when it spins around the accelerator.. so imagine million of particles (different accelerators) with different radius of particle accelerator superimposed.. each particle would encounter different time dilation and length contraction?
Oh. Ok. I'd give it a thought experiment.
Btw. Einstein first thought experiment was racing to go head to head with light. And he couldn't imagine a frozen wave. What principle violated a frozen wave in the first place? Why didn't he just adjust the concept like how Planck had to invent quanta to solve the ultraviolet catastrophe?
@lucas_ if you want to go into how the spinning disc is actually analyzed in relativity, I suggest looking up the Ehrenfest paradox and Born coordinates. The Wikipedia articles on these topics give a reasonable starting point:
Ehrenfest paradox - Wikipedia
Born coordinates - Wikipedia
There are a lot of complexities lurking here, which require more than a "B" level background. So if you want to discuss this after taking some time to read up, you should start a new thread at the "I" level, not the "B" level. Such discussion is off topic for this thread since we're only talking about the fact that spacetime is flat for this scenario.
What principle violated a frozen wave in the first place?
The fact that there is no solution of Maxwell's Equations that describes an electromagnetic wave in free space that varies only in space, not time.
The "quotient space" corresponds to the non-Euclidean geometry that one would actually measure by placing rulers on the disc or walking along it with an odometer. So it's not that abstract, but raher quite practical.
A.T. said:
The "quotient space" corresponds to the non-Euclidean geometry that one would actually measure by placing rulers on the disc or walking along it with an odometer.
More precisely, it's the non-Euclidean geometry you get if you make local distance measurements and then put them together into a global 3-dimensional space. But as I said before, this space does not correspond to any actual 3-dimensional spacelike slice of the 4-dimensional Minkowski spacetime.
The complexities lurking here were discussed in detail in this previous thread from 2014:
The rotating disk of Albert Einstein
Hello To demonstrate that we can deduce from special relativity the existence of an observer who finds that his three-dimensional space is not euclidean (a conclusion that is false in my opinion), in subsection "Behaviour of Clocks and Measuring Rods on a Rotating Body of Reference" of his...
www.physicsforums.com
Here is another relevant thread from 2013:
Ehrenfest's paradox
I'm reading about Ehrenfest's paradox where one considers a rotating disk. If one let r' be the radius of the disc in an inertial frame and r be the radius of the disc when it is at rest. Then the periphery must be Lorentz' contracted such that ##2\pi r' < 2\pi r##, but since the radial line is...
None of the particles encounter any time dilation or length contraction; as far as each particle is concerned, time passes at one second per second.
An observer at rest relative to any one of these particles (and therefore moving rapidly relative to the surface of the earth) will find that clocks on the surface of the earth are running slow relative to their own clock, just as an observer on the surface of the earth will find that a clock at rest relative to the particle is running slow.
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text:
A Continental Airlines foi uma companhia aérea dos Estados Unidos. Era a quinta maior companhia aérea dos Estados Unidos e uma das maiores do mundo até sua fusão com a United Airlines, criando a terceira maior companhia aérea do mundo. A Continental começou a atividade com o nome de Varney Speed Lines. A empresa inaugurou voos de passageiros e transporte postal em 15 de julho de 1934, entre as cidades de El Paso e Pueblo, com uma pequena frota de Lockheed Vegas.

Em julho de 1937 adotou o nome de Continental Airlines e no final de 1954 adquiriu a Pioneer Airlines, passando a usufruir da extensa malha desta empresa nos estados do Texas e Novo México.

Suas origens regionais começaram a mudar em 1957, quando inaugurou voos entre Los Angeles e Chicago, com escalas em Denver e Kansas City. A realização destes voos só foi possível graças ao recebimento dos primeiros Douglas DC-7B, suplementados no ano seguinte pelos Vickers Viscount 800. Pela terceira vez consecutiva em apenas dois anos, uma nova substituição de equipamento ocorreu em 1959, com a entrada em serviços dos primeiros Boeing 707-120. Com estes quadrimotores a Continental deu seus primeiros passos na era da aviação a jato.

Já nos anos 80, a Texas Air Corp., controladora da Texas International Airlines, tornou-se sócia majoritária da Continental e fundiu as duas empresas em outubro de 1982, mantendo-se o nome Continental. A fusão em nada ajudou a já debilitada saúde financeira da empresa: em 1983 solicitou pela primeira vez sua concordata preventiva, o famoso "Chapter 11".

Em 1986, após sua reestruturação, dispensou a concordata. Em 1987 as empresas New York Air e People Express foram compradas e novos problemas começaram a surgir, levando-a a solicitar novamente concordata.

A situação só melhorou no início da administração Gordon Bethune, que conseguiu, a partir da segunda metade da década de 90, reorganizar a empresa e torná-la competitiva.

A frota passou por um processo de racionalização, aeronaves mais antigas e onerosas foram aposentadas, os funcionários ganharam nova moral e começaram a receber participações em dinheiro nos resultados do grupo. Novas rotas internacionais foram sendo conquistadas: hoje a Continental voa para quase toda a Europa, e também para o Oriente Médio, Ásia, América Latina e Caribe, desde seus dois principais hubs, Newark e Houston.

Hoje em dia, operado uma das frotas mais modernas dos Estados Unidos, a Continental foi a quinta maior empresa aérea de seu país e uma das melhores na qualidade de serviços. Prova disso é que já ganhou duas vezes o cobiçado prêmio de "Airline of The Year" da revista Air Transport World.

Frota

Ver também
 Vôo Air France 4590
 United Airlines

Empresas aéreas extintas dos Estados Unidos
Empresas aéreas fundadas em 1934
Empresas aéreas extintas em 2012

redpajama_set_name: RedPajamaWikipedia


text:
Health is an area, which presents enormous challenges for the region and where targeted, joint action can produce tangible results.
PA Health focusses on the following actions:
Promoting active and healthy ageing to address the challenges of demographic change;
Engaging and better utilizing stakeholders from other sectors to promote a Health in All Policies approach with focus on the impact of environmental factors, and especially climate change on human health;
Increasing stakeholder and institutional capacity to tackle regional health challenges.
The above health-related actions correlate with the goals and operational targets included in the NDPHS Strategy and its Action Plan, the 2030 Agenda for Sustainable Development Goals, the principle of universal health coverage (UHC), the WHO Decade of Healthy Ageing 2020-2030 and other global and regional strategic frameworks.
PA Health contributes to several Sustainable Development Goals (SDG): most directly to SDG 3 "Good health and well-being" with the ongoing work against HIV, TB and associated infections, the reduction of non-communicable diseases (with an approximate 30% reduction of premature avoidable deaths on average in the BSR already achieved), the prevention of harmful use of alcohol, tobacco and other substances as well as strengthening Primary Health Care, which is of utmost importance for a sustainable healthcare system and access to care for the most vulnerable people.
The secondary effects of good health are far-reaching. A healthy population is a more productive population, which contributes to the SDG 8 "Decent work and economic growth" and a population given the opportunity to be productive is less affected by poverty, contributing to SDG 1 "Zero poverty".
Other concrete examples include the PA Health work on occupational health and safety (SDG 8 "Decent work and economic growth"), tackling the threat of antimicrobial resistance improving both human health and also livestock health and farm waste management (SDG 2 "Zero hunger" and SDG 6 "Clean water and sanitation") as well as focus on the health of vulnerable groups, in particular prisoners, contributes SDG 10 "Reduce inequalities".
PA Health will focus increasingly on healthy and active ageing, to address the demographic change in the region. Optimizing opportunities for good health at all stages of life will ensure that older people can maintain independence and increase their social and economic participation in society, while reducing healthcare costs. This work will contribute to several SDGs, among which are SDG 4 "Ensure inclusive and quality education for all and promote life-long learning", SDG 5 "Achieve gender equality and empower all women and girls", SDG 10 "Reduced inequality within and among the countries" and SDG 11 "Make cities and human settlements inclusive, safe, resilient and sustainable".


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text:
Selena: Her Life Story
Latin music sensation Selena was tagged as the unrivalled Queen of Tejano Music. But her blossoming career and well-meaning life were cut short with her untimely death in 1995 – and sadly, it happened in the hands of somebody who was once her good friend.Named Selena Quintanilla in real life, she was born in Lake Jackson, Texas and was a real performer even in her early age. At six, she was already a budding star in her own right and at the moment she turned nine, she is singing in her own band named Selena y Los Dinos that her father founded. Her band sings regularly at a family owned restaurant and even if the bistro eventually failed, Selena and her band successfully recorded two songs under their name.Selena officially recorded her first album in 1984 for a local record company. Her second was in 1986 and just year after that, she was named the Best Female Vocalist and Performer of the Year in the Tejano Music Awards. She then went on and held that recognition for at least seven years (Behnke, 2005).Selena met her husband Chris Perez in 1988. Perez is also a musician and he too owns a band. Perez was hired by her father to play in their band. But when he discovered that the two fell in love, Selena's father disapproved of it. He tried to fire Chris but eventually, he gave in and asked them to get married. They did get married in Nueces County, Texas on April 2, 1992.Selena's fame continued to rise as she successfully held concerts in places like New York, Houston, Central America, Argentina, and Puerto Rico. She had been chosen as an official endorser by different commercial companies including beverage giant Coca-cola. She was even given cameo roles for Hispanic films like Don Juan DeMarco, which starred Marlon Brando and Johnny Depp.Everything is rosy for Selena until she discovered an anomaly happening in her business she personally owned. Selena owned a chain of boutiques and the president of her fan club, Yolanda Saldivar, managed it. Selena found out that there was a lot of money disappearing from her business and she decided to confront Yolanda about it. They met at Days Inn and there, Selena requested the paperwork of the business for tax filing. Saldivar purposely delayed handing over the papers saying that she was under stress herself because she was raped. To prove that, Selena drove Saldivar to a hospital but doctors found no evidence for such. When they returned to the hotel Selena asked for the papers again and that's when a heated argument between them arose. Saldivar is carrying a gun then and she shot Selena in the back as she was going out of the room to leave. Selena reached the front desk half-bleeding to death but she was able to name her assailant and where she was shot. Selena eventually died in the hospital from blood loss (Valdez, 2005).Selena's death had caused distraught and grief to both to Latin and non-Latin music fans alike. The loss of a great Mexican singer hand created a big impact throughout the American community that a lot of activities were made in her honor, including memorials and vigils conducted all over the nation. After her death, Selena's two hits "Dreaming of You" and "I Could Fall In Love" had made it in Billboard's Hot 100.Selena's assailant was convicted and is sentenced to life imprisonment in 1995. Two years hence, Selena's life story was made into a film entitled "Selena." Jennifer Lopez played the main role, and it actually became her own stepping-stone to stardom. This film written and directed by Gregory Nava was the biggest tribute given to Selena and the life that she had lived.
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In any household trying to negotiate the economic minefield, the main navigator is likely to be the woman of the house.
Kathy Peel, author of 18 books to help families, says in her latest, The Busy Mom's Guide to a Happy, Organized Home that every family needs a family manager. In most families, even if she has a full or part-time job, that manager is mom.
Because running a family is a lot like operating a small business, Peel said certain "standard operating procedures" need to be in place.
"Good business principals and strategies help run your home well," said Peel, who lives in Dallas, Texas.
Home and property. How do you take care of all your stuff?
Food. Who makes sure there are 1,095 meals on the table each year?
Family and friends. Who manages relationships?
Finances. How do you pay bills, stretch dollars and save?
Special events. Busy calendars include holiday seasons and birthdays and vacations.
Time and scheduling. Transportation and distribution is getting the right people to the right place at the right time with the right equipment.
Self management. You must take care of the mind, body and spirit that God has given uniquely to you.
Peel even goes so far as to say an organized household saves not only money, but marriages. When couples sit down and decide who is responsible for "the small routines of life," little aggravations don't have time to build up.
Peel, who describes herself as "domestically challenged" when she married Bill 37 years ago, said "God doesn't waste experiences." She grew up in a home where everything was done for her. Then she married a minister and her resource level changed.
No one is good at all seven of the management roles, she said. Find a friend who can help in one of your weak areas and barter services. If you are a great shopper but can't organize a closet, take your friend's shopping list to the grocery and turn her loose with your shelves, hooks and hangers.
Join someone at work and each cook a double portion two nights a week, and share your extra portion giving you each two nights off from cooking.
Host a swap party in your neighborhood or with friends from church around a certain theme, like baby equipment or children's clothing. "Everyone goes home with treasures without spending a cent," she said. Rather than selling those pieces at a yard sale for pennies on the dollar, get dollar for dollar value in a swap.
Split the cost of a carpet shampoo with a neighbor and do it yourself.
Set up a babysitting co-op and car pooling to save time and money.
Be creative with your entertainment instead of paying for someone or something to entertain you. Stay home and play board games or make up a family trivia game.
"Attitude is everything," Peel said. She said the two greatest tests in life are: what we do with success and how we respond to adversity.
With money problems the No. 1 reason for divorce, Peel said coming to grips with what is important in life, and finding creative ways to stretch a dollar will save marriages.
Additionally, she said the financial difficulty of the day may prompt "the revival that we've been praying for so long" if people see Christians reacting positively to adversity.


We Welcome you to Hudson County NJ Limo Service Rental and Party Buses. We have a complete line of Hudson County NJ Limo Service Rentals and NJ Party Buses for Hudson County New Jersey. We possess an extensive Limousine fleet of Stretch Limos and New Jersey Party Buses. View our NJ Party Bus and NJ Limo Fleet on-line or in person. We offer several Hudson County NJ Wedding Limos that have packages which can be customized to accommodate any budget. We also offer special pricing and rates for our Hudson County NJ Prom Limos Rental Service. If you are in search for NJ Limo Rental Service in Hudson County NJ, you have come to the right place! At TRU Limousine, we have Hudson County NJ Limo Service! Our NJ Limousines are out 24 hours a day, 7 days a week. Before you look at other limo company, give us a call to compare our Hudson County NJ Limo Service rates and our limo service quality standards. Our New Jersey Limo Rental Rate may be comparable, however our NJ Limo Rental Service isn't! Our New Jersey Limousine Service in Hudson County NJ is best in class!
Everyone is welcome to visit our showroom to view our extensive Hudson County NJ Limo Service and New Jersey Party Bus Fleet in person. Allow yourself a large window of time since our fleet consists of over 25 NJ Party Buses and NJ Limos. You can always contact us and we would be happy to send you brochure information on our Hudson County NJ Limo Service fleet. We are happy to accommodate you for your special occasion and event. Whether you need Hudson County NJ Limo Service for a Wedding, Prom, Bachelor Party, NJ Bachelorette Party Limos, Birthday Party, Quinceanera, Sweet Sixteen, Wine Tour, Casino, Atlantic City Limo, Concert, NJ Airport Limo Transfer, Cruise Ship Transfer, Corporate Function or simply as directed. We have you covered for Hudson County NJ Limo Service! Check out our complete line of Hudson County NJ Party Bus page and Fleet information. We also offer Limousine Service in the following Townships of New Jersey.
Our Hudson County NJ Limo fleet is prepared and ready for your memorable occasion. We offer several limousine packages and amenities.


World of Tanks is getting it's own Comic. Firs issue will be out August 31, both in comic book retailers and digitally at darkhorse.com. This hard-hitting story, written by Garth Ennis (Preacher, War Stories, The Punisher), is a historically-based war tale, skilfully illustrated by the renowned Carlos Ezquerra (Judge Dredd, Strontium Dog, War Stories Vol. 2). Each issue is wrapped in the epic cover art of Isaac Hannaford (Halo: Reach, The Punisher) and is bursting to the seams with explosive action.
don't forget that console world of tanks also is able to buy the tank from sept 1st till sept 15th. and it comes with a special skill snakebite Improves your gunner's accuracy by reducing dispersion by 5% when fully trained. (Skill more effective when combined with Vertical Stabilizer, Snap Shot, Smooth Ride).


Startlingly light weight at 7.9oz (224 grams) for women's size 10.
We use USPS priority mail for all shipments. Orders are shipped within 3-5 business days. While we offer free shipping on exchanges and returns, it's non-refundable.
Check our exchanges and refund policy for more.
Exchanges: If your product is not a good fit, please don't take them out for a trial run, just put them back in their original bag and reach out at hello@endarunning.com. We'll send you a return label for the shoes.
Given limited stock, we may be out of supply for your requested size or color, and thank you for your patience if this means we aren't able to get you your desired exchange product immediately.
"I love your shoes! I have ran a 50-mile race in them, and ran the Grand Canyon rim-to-rim-to-rim with them"
We brought the toe box down so when you flex your toes, the Iten will move with your foot. We also made the Iten just slightly wider than other speed work shoes, giving your toes just a bit more room to splay.
At a mere 7.9 oz (224 grams) for a men's US size 9 (UK 8), the Iten will never be a drag when you pick up the pace.
Your foot is a powerful set of muscles and tendons. When training, you want a shoe that gives your foot a full range of motion so your arch, ankle, and toes can build the strength and endurance you need. The Iten does just that.
If you run barefoot, you'll find yourself landing on your midfoot or forefoot. Having a big cushioned heel on your shoe can throw off this natural gait. So the Iten has only 4mm more cushioning in the heel than the forefoot to help you land naturally.
Whenever you take a turn or run across an uneven surface (like the crown of a road), your foot wants to move laterally. Since the Iten's midsole cups the foot, it keeps you locked into the shoe even on the sharpest of turns.
We named our first shoe 'Iten' after a small town on the edge of the Rift Valley that produces an exceptional number of the world's best athletes. We cut a rift into the heel in homage Rift Valley, where you'll find this Home of Champions.
Along the side of the Iten, you'll find 12 lines. Two shoes makes it 12/12 - or 12 December. Jamhuri day. That great day in 1963 when Kenya finally gained independence from the United Kingdom and exactly one year later when it became a republic.e.
Under the sole, you'll find the word "Harambee". In Swahili it means "all pull together", and is used to refer to moments where communities come together to accomplish something individuals couldn't do alone.
Whether Maasai and Samburu beading or Swahili lesos and kangas, you'll see consistent repetition of triangle patterns in Kenyan design. We brought those same triangles to several different places on the Iten.
A traditional symbol of Kenya found on the flag, national crest, and given as one of the highest honors - similar to a presidential commendation or knighthood. We made our own running spear and proudly emblazon it on all Enda gear.


text:
History's Greatest
History's Greatest People, Places and Events.
History Greatest People
Manuel Mora y Araujo, Argentine sociologist and political analyst, Died at 79
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Manuel Mora y Araujo was born on September 30, 1937, and died on May 26, 2017.
He was an Argentine sociologist and political analyst.
He was an expert in market research and analysis and the founder of the consulting firms Mora y Araujo and Comunicación Institucional.
He was also an author of a number of books and other published work in the fields of politics and sociology and he also as a dean, Torcuato di Tella University in Buenos Aires.
Manuel Mora y Araujo passed away at 79 years old.
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text:
Sturm, Korbel schools collaborate to help immigrant workers
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Katie Brown, right, stands with her clients after their victory in Arapahoe County court. The four immigrant day laborers pictured won $15,000 in stolen wages and damages.
Students, Community Impact •
The happiest moment of Katie Brown's life came in an Arapahoe County courtroom in March.
A judge had just validated that her 100 hours of work and tedious, intensive preparation were worthwhile.
The third-year student in the Sturm College of Law had just scored the first major victory of her legal career.
"There was a lot of energy and heart that was put into the case," said Brown, who will graduate in May. "We were learning as we went and teaching ourselves, so there was a lot of pressure on me personally as well as pressure to get it done for my clients."
Thanks to Brown, the University's Civil Litigation Clinic and a host of other programs across campus, four immigrant day laborers won $15,000 in damages and wages an employer had stolen from them. Since November, Brown has been on the case, working for class credit under the supervision of Denver Law professor Tamara Kuennen.
In the Civil Litigation Clinic, students working with Kuennen take on relatively expeditious cases that require fewer documents filed in court but entail more outside-the-courthouse research. Often, they are less-lucrative cases that other attorneys tend to decline. And that students tend to win.
"Usually our students are able to out-prepare the other side," Kuennen said, noting students are expected to put in 25–30 hours of work per week to earn nine University credits. "Even when experienced attorneys get involved [on the other side, the students are] just able to devote a lot of time to their cases. They draft and redraft and practice every single word they would utter in court with me many times before we actually have a hearing."
While Brown was the face of the case in the courtroom, the win would not have been possible without cross-disciplinary collaboration among the law school, the Josef Korbel School of International Studies and a multitude of community partners.
Brown got to know her clients after she visited El Centro Humanitario and met Diego Bleifuss-Prados and the other Korbel students staffing its Direct Action Team. The community organization works to promote the rights of day laborers and domestic workers. For years now, Korbel students have been researching wage theft and interviewing workers, employers and lawyers about their experiences. They often help workers recoup wages outside the often costly and time-consuming legal process.
Learn more about wage theft problems and solutions at DU's upcoming Wage Justice Day
"It's a great example of how community members and groups can come together and each contribute their own skills, knowledge, and time to righting injustices and reclaiming unpaid wages," Bleifuss-Prados said.
In this case, legal help represented the last available option. The Korbel students connected with Brown who, working pro-bono, saw a chance to tap into her passion.
"I saw a great opportunity to work with people and help them in the most important aspect of their life," she said. "It's not just about money. It's about earning a livelihood and feeling proud of yourself and supporting yourself."
It's not just about the money for Brown either. Although unpaid, she feels as though she has gained an immeasurable wealth of practical experience.
The Korbel students also acquire skills that launch them into a variety of jobs in immigrant and labor rights.
"They're getting really tangible work experience, as well as knowledge of the issues and the ability to work with stakeholders," said Rebecca Galemba, an assistant professor at the Korbel School. "They learn how to take a lot of initiative and creatively address an issue. For me as a researcher who is also now expanded into outreach, it's part of our commitment to the community. You not only want to research what is happening to workers, but also share what you have learned and help contribute to real change."
Katie Brown plans to continue the community work she took on in the Civil Litigation Clinic. She can't imagine doing anything else now that she has experienced how satisfying litigation can be.
"If I hadn't done this and I'd left law school just taking classes, I would have been so far behind entering the working world," she said. "There are so many ways you can use the law to help people earn their livelihood and be successful and contribute to society."
NewsAnnouncement
Sturm College of Law Announces Grants to Launch Immigration Justice Project
Denver Law recognized by preLaw Magazine for excellence in public service work
Law Students Spend Spring Break Providing Aid to the Borderlands Region


Southampton officials have agreed to build a new tentlike pavillion at the old Parrish Art Museum space. The pavilion will serve as a location for outdoor concerts and events.
The new structure will also show outdoor movies and there is also a possibility that there will be an ice skating rink. A design firm in Manhattan known as the Rockwell Group designed the structure. The cost of the building is estimated to be $650,000 to $975,000 and the seating capacity is expected to be 300 people.


There is now substantial evidence that associative processes contribute to the development and expression of narcotic tolerance. Like other conditioned responses, the compensatory response (CR) thought to mediate tolerance can be extinguished by repeatedly presenting the conditioned stimulus (CS, drug-paired contextual cues) alone. In the present experiments, rats were used to determine if conditioned tolerance to the analgesic effect of morphine would spontaneously recover following a sufficient delay between the last extinction trial and reexposure to the CS. It was found that tolerance spontaneously recovered 72, but not 24 h following the last of nine extinction trials. As well as providing support for a Pavlovian model of narcotic tolerance, this finding has important clinical implications for cue-exposure drug and alcohol rehabilitation strategies.


Escape to a place where lush tropical foliage provides a charming canopy from an unrelenting sun, as you meander amidst ambitious paintings, sculptures, and photographs from the masters of contemporary arts. Discover the Brickell, part of our luxurious Professionals collection inspired by the unique heritage of historical art neighborhoods in Miami.
Drawing on the famed Art Deco pastel buildings from the 1930s, this dress shirt features a handsome pink and white stripe pattern that will set your mind at ease as soon as you slip into it. Settled in the mid-1800s by early pioneers, Brickell quickly grew to become Miami's "Millionaire's Row," before establishing itself as one of the largest financial districts in the US. Crafted to embody all the wonder and prestige of its namesake, our Brickell showcases our cutaway collar, and a dobby fabric.
A pink dress shirt is a staple in a modern man's wardrobe, and a must-have during summer months. Great for softening the dark hues of navy, charcoal, and black, a pink shirt can easily bring balance to your outfit, and provide a slimming shape. Furthermore, our Brickell's thin stripes pattern provides a stylistically modern and masculine look simultaneously.
Pinks pairs well with just about every color — from khaki to cream, and black. Though it looks particularly sophisticated with our navy or charcoal Seneca. Pink is also good for wearing with traditionally masculine accessories including suspenders, a vest, or a medium gray tie.
Don't be afraid of wearing bright colors this summer. You'll find this shirt provides the perfect pop of color to accompany navy slacks during the work week, as well as to wear with dark denim for weekend brewery tours, antiquing, and more.
Explore our limited run Brickell, and set aside moments for discovery every day. Or get started by finding your custom fit.


This is my first time trying Kama Ayurveda product.
And i'm having mixed emotions about it.
It comes is a simple tinted plastic bottle.
Not very user friendly as i have to literally hit the bottle against my palm to take out the product.
I wish it came with a pump dispenser.
That would've made it so much easier.
It has a stopper but it becomes tedious removing and putting it back everytime i use the moisturiser.
So ,i would suggest them to improve on the packing a little bit.
It has a very creamy texture.
Makes application really easy,spreads evenly .
Gets readily absorbed and it does an amazing job of moisturising my dry skin.
It is supposed to be made of Rose and Jasmine ingredients.
But the Jasmine smell completely over powers the rose .
I'm not a big fan of Jasmine .
It is overwhelming and the smell persists for a long duration.
i tend to avoid applying it only because of the smell.
However , some people might love it.
As for me, this smell is just OTT.
I apply the moisturiser after taking shower .
It removes any dry patches and makes the skin soft and radiant.
I would suggest this for those with moderately dry skin.
It might not work for Ultra dry skin.
The effect lasts for 4-5 hours .
1.Instant moisturising of the skin.
2.Brightens the complexion and makes skin soft.
3.No artificial preservatives,colorants,petrochemicals and fragrance.
2.Overwhelming Jasmine fragrance is a turn off for me.
3.Available only in Kama Ayurveda Outlets.
I would've loved it if it came in other fragrances.
im usually not that into herbal products.


It is getting to that time of year again, when we are beginning to organise the 2010 Stonestead Annual Outdoor Quilt Festival, so to begin with we are having a Challenge in conjunction with Sawmillers Quiltery, so if you would like all the details go through to the Sawmillers Blog/Newsletter and read them there.
We shall be having regular updates, so keep coming back to see where we are with the planning and registration details.
Previous More Quilt Festival Pictures Next Registration Form for 2010 Stonestead Outdoor Quilt Festival.


Your primary care physician has referred you to Southern Oregon Neurosurgical & Spine Associates, PC. In preparation for your first visit to we ask that you download and complete our patient registration form before you arrive for your appointment. Reviewing them in the comfort of your own home is more convenient for you and allows sufficient time to complete some of the more detailed sections. Should you have any questions about the forms our staff is happy to help you when you arrive for your first appointment or you call during business hours.
In addition to completing the medical forms before your appointment, please be sure that all current medical reports, X-rays, CT and/or MRI scans and myelograms are at our office prior to your appointment. If you are having difficulty in obtaining them, please call our scheduling department at (541) 779-1672.
Please also bring all available information about your insurance coverage, including claim number if applicable. It is always advisable to contact your insurance company regarding any specific preauthorization requirements they have. It is the patient's responsibility to ensure that any referrals or authorizations required by insurance plans have been issued and are current. If this information is not available, your appointment may need to be rescheduled.
With thousands of insurance and pharmacy plans available, and identity theft a potential risk, we need to confirm your identity and insurance coverage every time we see you.
Please bring a photo ID, and your insurance card with you to your appointments atSONSA. If you have a prescription card, please bring this to your appointment as well.
Our contracts with the insurance companies require us to collect your co-payment, patient percentage and/or deductible or your portion of the cost at the time of your visit. Please be prepared to pay this when you arrive for your appointment. For your convenience, we do accept payments by MasterCard and Visa.
If you are being seen for a motor vehicle accident, a personal injury or any other third party insurance coverage, these visits are considered private pay. Payment at time of service is required.
All Worker's Compensation claims must be preauthorized by the insurance carrier prior to appointment.
Please visit SONSA's insurance and financial policies for more information.
We do our best to see patients promptly. However, occasionally emergencies cause unavoidable delays in the doctor's schedule. Should your appointment be delayed, we will strive to keep you informed and will try to make your wait as short as possible.
If you are unable to keep your appointment, please give us at least 24 hours notice, which will enable us to offer that time to another patient.
We will first obtain a detailed medical history by asking you questions concerning your general health, your current medications, past illnesses and surgeries. Your physician will then perform a physical examination. Further diagnostic studies may be needed. Detailed information describing these studies will be discussed with you. These studies will need to be scheduled at other facilities. A full written report will be sent to your referring physician, after all studies have been completed and reviewed.
If surgery is required, detailed information concerning the procedure will be discussed with you. Our staff will make the arrangements for your admission to the hospital. Prior authorization and/or second opinion may be required by your insurance company. Our staff will also facilitate this process for you, but it is your responsibility to be aware of the requirements in your insurance policy prior to any procedure or surgery being performed.
Your surgery require the services of an anesthesiologist and/or a surgical assistant. These charges are billed separately from the physician charges.
PLEASE NOTE: If you are scheduled for surgery, you should avoid aspirin or blood thinning products, such as Coumadin, Plavix, Aggrenox, or Omega-3 fatty acids for seven days prior to your surgery. Speak with your referring provider regarding any medications you are taking.


Volleyball serving drills help players become more consistent and accurate with serving. Simulating game-like pressure in practice is important for developing great serving skills for winning volleyball at a high level.
Warm up your arms and work on serving the ball flat. After you serve a ball in, serve the next ball harder. As long as you serve the ball in, keep serving the ball harder. Keep serving the ball harder than the previous one before. Eventually you get to the point to where you are serving the ball so hard, it won't land in. You're working on discovering where your limit is.
How hard are you hitting it? What's your limit to how hard you can serve without serving the ball out? When you go back and serve an ace, that serve is good enough. Stay with the serve that you were able to ace your opponent with. There's no point in serving harder if your serve is so tough your opponent can't pass it.
This is a wash drill where you have to win both rallies to win the point. Serves that are below 32 miles an hour is one point. 33 to 36 miles per hour is 2 points. 37 to 40 miles per hour is 3 points. Above 40 is 4 points.
You can choose your own unique scale points for your team. That's what the serving team is playing for. The receiving team gets a point when they win the rally. The drill starts with a serve. After the first rally is finished, the free ball will go to the serving team and the rally is played out.
Also, to add more to this drill, you can create point values for the passes of the receiving team. For example, if it's a 3 pass and they win both rallies, they could win 3 points. So, both teams have the chance to win equal points. This becomes a server vs passer game.
So in the beginning, the serving team has the advantage because if they serve a 40 mile per hour ball, they are playing for 4 points while the receiving team is playing for only 1 point.
Passers are competing against each other. If you win, you move up. If you lose, you move down. The best passers have to fight to stay up at the top court or they will get knocked down the ladder.
If you get knocked down, you have to work your way back up there. Have 2 people serving, 2 people passing, and 1 target on each court. Each server serves 5 balls. Passers count how many out of 10 are good passes (good passes are passes that end up within 8 feet of the net). After 5 serves, the passers and servers rotate. After rotating 5 times, everyone on the court as served, passed, and been the target. Compare scores.
Top 2 players move up, middle person stays, bottom 2 players moves down.
Volleyball serving drills need to be good at creating competition for serving and passing under pressure. And you have the players at the top of the ladder fighting to stay at the top. Spend 15 or 20 minutes once a week to do a passing ladder.
Six balls "in" the court in a row (players serving one after the other). This is a team serving drill.
Next, every serve to zone 1 and 2 for 6 in a row.
Next, every serve to zone 4 and 5 for 6 in a row.
Next, make it tougher by focusing a one zone.
Another thing to do is require every serve to float. Or require every serve to be over 30 miles per hour.
In a row is game-like pressure.
You could also do 6 vs 6 competition of how many in a row can you get.
The receiving team is trying to sideout 3 times in a row. The serving team is trying to win 2 rallies in a row. So, the serving team wants 2 in a row while the receiving team is trying to get 3 in a row. The same server keeps serving until one of those 2 things happens (3 sideouts in a row or 2 serving rallies won). When "rallies won in a row" is achieve, a point is awarded and the other team gets to serve. Teams don't rotate. Set a timer for 3 minutes. When time is up, players then rotate positions.


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ACCEPTED

#### According to
International Plant Names Index

#### Published in
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#### Original name
Scutellaria lorinjensis Rech.f. & Fitz

### Remarks
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redpajama_set_name: RedPajamaGithub