Changeset 564 in ETALON for papers

Timestamp:

Apr 27, 2016, 6:32:09 PM (8 years ago)

Author:

hodnevuc

Message:

 

Location:

papers/2016_IPAC/IPAC16_SP_CTR/poster

Files:

• conference_poster_3.aux (modified) (2 diffs)
• conference_poster_3.log (modified) (11 diffs)
• conference_poster_3.pdf (modified) (previous)
• conference_poster_3.synctex.gz (modified) (previous)
• conference_poster_3.tex (modified) (7 diffs)

papers/2016_IPAC/IPAC16_SP_CTR/poster/conference_poster_3.aux

@@ -1 +1 @@
 \relax 
 \catcode `"\active 
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@@ -8 +6 @@
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 \pgfsyspdfmark {pgfid1}{1724248}{741207}
-\newlabel{eq:eq1}{{1}{2}}
-\newlabel{eq:lmab}{{2}{2}}
+\newlabel{eq:lmab}{{1}{2}}
+\newlabel{eq:eq1}{{2}{2}}
 \newlabel{eq:pitch_pulselength}{{}{2}}

papers/2016_IPAC/IPAC16_SP_CTR/poster/conference_poster_3.log

@@ -1 @@
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papers/2016_IPAC/IPAC16_SP_CTR/poster/conference_poster_3.tex

@@ -30 +30 @@
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+
 \begin{document}
 
@@ -73 +63 @@
 boxshade=plain,
 headerheight=0.17\textheight,
-%postertitlecolor=titlecolor
+postertitlecolor=titlecolor
 }
 {}
@@ -107 +97 @@
 
 \headerbox{Intro}{name=introduction,column=0,row=0}{
-Smith-Purcell radiation and Transition Radiation are two radiative phenomenon that occur in charged particles accelerators. For both the emission can be significantly enhanced with sufficiently short pulses and both can be used to measure the form factor of the pulse. We compare the yield of these phenomenon in different configurations and look at their application as bunch length monitors, including background filtering and rejection. We apply these calculations to the specific case of the CLIO Free Electron laser\par
+Smith-Purcell radiation and Transition Radiation are two radiative phenomenon that occur in charged particles accelerators. \par
+\begin{center}
 \textbf{Coherent Transition Radiation (CTR)}
-When a relativistic charged particle crosses the interface between two media of different dielectric properties, transition radiation (TR) is emitted. This process was calculated analytically by Ginzburg and Frank.% \cite{GF}.
+\end{center}
+When a relativistic charged particle crosses the interface between two media of different dielectric properties, transition radiation (TR) is emitted.% This process was calculated analytically by Ginzburg and Frank.% \cite{GF}.
 %\begin{equation}
 %\frac{d^2I_{GF}}{d\omega d\Theta}=\frac{q_0^2}{4\pi^3\epsilon_0c}\frac{\beta^2sin^2\Theta}{(1-\beta^2cos^2\Theta)^2},
@@ -116 +108 @@
 %where $q_0$ is electron charge, $\epsilon_0$ -- vacuum permittivity, c is the speed of light, $\beta$  is relativistic velocity and $\Theta$ is the observation angle.
 
- We use their formula with virtual-quanta method to compute the backward TR from a finite screen.%\cite{GFa} 
+ %We use their formula with virtual-quanta method to compute the backward TR from a finite screen.%\cite{GFa} 
 % \begin{equation}
 %\frac{d^2I_{disk}}{d\omega d\Theta}=\frac{d^2I_{GF}}{d\omega d\Theta}[1-T(\gamma,\omega a,\Theta)]^2
@@ -122 +114 @@
 %\end{equation}
 %where T is correction tern to finite size of the screen. 
-This gives the single electron yield (SEY) $\frac{d^2I_1}{d\omega d\Theta}$. From the SEY the  whole spectrum can be derived using the following formula:
+%This gives the single electron yield (SEY) .
+
+\begin{center}
+\textbf{Coherent Smith-Purcell Radiation (CSPR)}
+\end{center}
+%The same formula, but with a different SEY is used for calculation of the Smith-Purcell radiation (SP) spectrum. 
+SP radiation occurs when a charged particle move above a metallic periodic structure.
+% Unlike TR, SP has the advantage  that the emitted radiation is not concentrated in a small observation angle ($\Theta_{max}   \simeq1/\gamma$), but spread in angle. 
+The wavelength of the radiation for SP depends on the observing angle according to the following: 
+\begin{equation}
+\lambda=\frac{l}{n}(\frac{1}{\beta}-cos\Theta)
+\label{eq:lmab}
+\end{equation}
+where l is the grating period, n is the order of radiation, $\Theta$ is the observation angle and $\beta$ is the relativistic velocity. Spectrum calculation is based on the surface current model.\par
+From the SEY $\frac{d^2I_1}{d\omega d\Theta}$ the  whole spectrum can be derived using the following formula:
 \begin{equation}
 \frac{d^2I}{d\omega d\Theta}=\frac{d^2I_1}{d\omega d\Theta}[N+N(N-1)F(\omega)]
 \label{eq:eq1}
 \end{equation}
-Where N is the number of electrons in the bunch and $F(\omega)$ is the form factor of the time profile of the bunch. Using phase recovery methods, such as Kramers-Kronig or Hilbert~\cite{IPAC14}, it is possible to recover  the phase and then the time profile of the bunch.\par
-
-\textbf{Coherent Smith-Purcell Radiation (CSPR)}
-The same formula, but with a different SEY is used for calculation of the Smith-Purcell radiation (SP) spectrum. SP radiation occurs when a charged particle move above a metallic periodic structure. Unlike TR, SP has the advantage  that the emitted radiation is not concentrated in a small observation angle ($\Theta_{max}      \simeq1/\gamma$), but spread in angle. The wavelength of the radiation for SP depends on the observing angle according to the following: 
-\begin{equation}
-\lambda=\frac{l}{n}(\frac{1}{\beta}-cos\Theta)
-\label{eq:lmab}
-\end{equation}
-where l is the grating period, n is the order of radiation, $\Theta$ is the observation angle and $\beta$ is the relativistic velocity.\par
-To calculate the SEY and the total spectrum for SP effect, the gfw code was used~\cite{GD}. The calculation is based on the surface current model. %Taking into account the fact that the grating have a finite width, the energy per solid angle for a single electron can be written as:
+Where N is the number of electrons in the bunch and $F(\omega)$ is the form factor of the time profile of the bunch. %Using phase recovery methods, such as Kramers-Kronig or Hilbert, it is possible to recover  the phase and then the time profile of the bunch.\par
+ %Taking into account the fact that the grating have a finite width, the energy per solid angle for a single electron can be written as:
 %\begin{equation}
 %\frac{dI}{d\Omega}=2\pi e^2\frac{Z}{l^2}\frac{n^2\beta^3}{(1-\beta cos\Theta)^3}R^2
@@ -143 +141 @@
 }
 
+
+\headerbox{Conclusion}{name=conclusion,column=0,row=0,below=introduction}{
+ To choose the most appropriate grating pitch, one should use Smith-Purcell condition given in equation~\ref{eq:lmab}.  For maximum emission at 90 deg. formula \label{eq:pitch_pulselength} is applicable: $$l\approx 8\times10^{8}p_{t},$$ where l is grating pitch in meters and $p_{t}$ is bunch width (fwhm) in seconds.\par
+Using the CLIO parameters we expect a signal (in the range 0.03-3 THz [ 0.1 - 10 mm]) of {8.37e-7}{J} for CSPR and {7.35e-08}{J} for CTR.
+}
 %----------------------------------------------------------------------------------------
 %       RESULTS 1
@@ -155 +158 @@
   \end{center}
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-    \includegraphics[width=0.4\linewidth]{../MOPMB003f3.pdf}\\
+  \includegraphics[width=0.48\linewidth]{../MOPMB003f2.pdf}
+    \includegraphics[width=0.48\linewidth]{../MOPMB003f3.pdf}\\
  \smaller \textit{ Angular distribution of SEY for SP effect (left) and TR (right). The grating have 8 mm pitch.  Screen for TR is turned at $45^o$ to beam propagation direction.}
   \end{center}
-  To choose the most appropriate grating pitch, one should use Smith-Purcell condition given in equation~\ref{eq:lmab}.  For maximum emission at 90 deg. formula \label{eq:pitch_pulselength} is applicable: $l\approx 8\times10^{8}p_{t}$, where l is grating pitch in meters and $p_{t}$ -- bunch fwhm in seconds.
+ 
   \begin{center}
-  \includegraphics[width=0.4\linewidth]{../MOPMB003f4.pdf}
-    \includegraphics[width=0.4\linewidth]{../MOPMB003f5.pdf}\\
+  \includegraphics[width=0.48\linewidth]{../MOPMB003f4.pdf}
+    \includegraphics[width=0.48\linewidth]{../MOPMB003f5.pdf}\\
  \smaller \textit{ Maximum angle of emission for SP effect as function of pulsewidth and grating pitch.  The beam-grating separation is 3~mm. Total energy for SP effect presented as function of pulsewidth and grating pitch. }
   \end{center}
   \begin{center}
-  \includegraphics[width=0.4\linewidth]{../MOPMB003f6.pdf}
-    \includegraphics[width=0.4\linewidth]{../MOPMB003f7.pdf}\\
+  \includegraphics[width=0.48\linewidth]{../MOPMB003f6.pdf}
+    \includegraphics[width=0.48\linewidth]{../MOPMB003f7.pdf}\\
 \smaller \textit{ Evolution of  the CSPR spectrum with a constant grating pitch and changing bunch width (left).  The grating have 8 mm pitch.  Evolution of CTR spectrum with  changing bunch width (right). }
   \end{center}
-Using the CLIO parameters we expect a signal (in the range 0.03-3 THz [ 0.1 - 10 mm]) of {8.37e-7}{J} for CSPR and {7.35e-08}{J} for CTR.
+
 }