\documentclass[landscape, 25pt]{foils}
\usepackage{amsmath,amssymb}
\usepackage[pdftex]{color}
\usepackage{graphicx}

% Movie related stuff:
\usepackage{hyperref}
\usepackage{geometry}
\geometry{verbose,letterpaper}
\usepackage{movie15}

% Margins, schmargins!
\setlength{\hoffset}{-0.75in}
\setlength{\topmargin}{0in}
\setlength{\oddsidemargin}{0in}
\setlength{\evensidemargin}{0in}
\setlength{\voffset}{-0.75in}
\setlength{\textheight}{7.5in}
\setlength{\textwidth}{10.5in}
\setlength{\footskip}{0in}
\setlength{\headsep}{-0.5in}
\setlength{\headheight}{1.0in}
\setlength{\baselineskip}{0in}
\setlength{\foilheadskip}{-0.6in}


\usepackage[display,
   darkbackground]{texpower}

\title{The Sun's Atmosphere and its Magnetic Field}
\author{Charles Kankelborg}


\begin{document}

\MyLogo{} % Sorry foilTeX, that's no place for a logo!
\leftheader{\includegraphics[totalheight=1.0in]{images/msuvertreverse07.pdf}}
\rightheader{\includegraphics[totalheight=1.2in]{images/color_solar_physics_logo.jpg}} 

\maketitle

\foilhead[0.25in]{Photosphere}
\begin{center}
   \begin{tabular}{cc}
      \begin{minipage}{0.4\textwidth}
         The photosphere is what you see through your sunglasses. It's the top of the
         solar convection zone. Things to notice:
         \begin{itemize}
            \item Yellowish-white color
            \item Sharp edge, $R_{\odot} = 6.96\times 10^{10}$\,cm
            \item Limb darkening
         \end{itemize}
      \end{minipage}
      &
      \begin{minipage}{0.55\textwidth}
         \includegraphics[width=0.95\textwidth]{images/Sun201010261258-Continuum.jpg}
         \\ {\tiny ESAC Astronomy Club}
      \end{minipage}
   \end{tabular}
\end{center}

\foilhead[0.25in]{Effective Temperature}
\noindent The solar luminosity $L_{\odot} = 3.84 \times 10^{33}$\,erg/s is due almost entirely to continuum radiation from the photosphere. This isn't quite a blackbody spectrum, but we can derive some of the basic properties by treating it as such:
\[
   L_{\odot} = 4\pi R_{\odot}^2 \, \sigma T^4.
\]
Stefan's constant is $\sigma = 5.67 \times 10^{-5}$\,erg\,cm$^{-2}$\,s$^{-1}$\,K$^{-1}$. This results in an effective temperature 
\[
   T_{\mathrm{eff}}=5775\,\mathrm{K}. 
\]
Wien's law puts the maximum of the Planck function at
\[
   \lambda_{\mathrm{max}} = \frac{ 2.90\times 10^6\,\mathrm{nm\,K} }{ T_{\mathrm{eff}} } 
      = 502\,\mathrm{nm}.
\]
We shouldn't take this number too seriously, but it is consistent with a spectrum peaked in the visible.



\foilhead[0.25in]{Solar Spectrum}
\noindent \begin{center}
   \begin{tabular}{cc}
      \begin{minipage}{0.49\textwidth}
         \includegraphics[width=0.9\textwidth]{images/Solar_Spectrum.png}
         \\ {\tiny Wikipedia}
      \end{minipage}
      &
      \begin{minipage}{0.49\textwidth}
         \includegraphics[width=0.9\textwidth]{images/SolarCCD.jpg}
         \\ {\tiny R. Kurucz, CfA}
      \end{minipage}
   \end{tabular}
\end{center}
This is what the solar spectrum really looks like.


\foilhead[0.25in]{Back up the train!}
\noindent Q: What is the Sun made of?

\noindent You know about atoms. Hydrogen for example:
\begin{center}
   \includegraphics[height=0.5\textheight]{images/hydrogen_spectrum.png}
   \\ {\tiny Encyclopedia of Science}
\end{center}


\foilhead[0.25in]{Atoms}
\noindent Perhaps you've seen an experiment like this in class:
\begin{center}
   \includegraphics[width=0.49\textwidth]{images/HydrogenDischarge.jpg}
   \includegraphics[width=0.49\textwidth]{images/HydrogenSpectrum.jpg}
   \\ {\tiny Brian K. Niece, Assumption College}
\end{center}
Why doesn't the solar spectrum look like this?

\foilhead[0.5in]{Radiative Transfer}
\noindent \begin{itemize}\zerolistvertdimens
   \item Astrophysical objects like the Sun are large. There's a lot more hydrogen
   there than in your discharge tube in the lab.
   \item The mean free path of the light is \emph{much} smaller than the Sun. 
   \item Light is scattered countless times before it escapes the photosphere.
   \item Each scattering event shifts the wavelength (why?)
   \item The outcome is a continuous spectrum. If the gas were all one temperature,
   we'd see a blackbody spectrum.
\end{itemize}

\foilhead[0.25in]{Appearance of the Limb}
\noindent\begin{itemize} \zerolistvertdimens
   \item We are looking into an opaque ball of gas. 
   \item Our line of sight takes in a range of temperatures.
   \item What does that imply as we observe from center to limb?
\end{itemize}
\begin{center}
   \includegraphics[height=0.5\textheight]{images/limbdarkening.pdf}
\end{center}
But why does the limb appear so \emph{sharp}?


\foilhead[0.25in]{Scale Height}
\noindent Force balance on a volume element of gas:
\begin{center}
   \resizebox{0.9\textwidth}{!}{\input{scaleheight.pdf_t}}
\end{center}
\[
   g_{\odot} = \frac{ G M_{\odot} }{ R_{\odot}^2 } 
      = 2.74 \times 10^4\,\mathrm{cm\,s}^{-2} = 28\,g_{\oplus}.
\]
If we let $m = m_p$ (mainly hydrogen) and $T=T_{\mathrm{eff}}$, then 
\[
   L = 1.8 \times 10^7 \,\mathrm{cm} = 2.5 \times 10^{-4}\,R_{\odot}.
\]



\foilhead[0.25in]{Solar Convection (Granulation)}
\begin{center}
\includemovie[
  autoplay,
  poster,
  controls,
  % autoclose,
  % text=()
  % repeat,
  % palindrome
]{0.8 \textheight}{0.8 \textheight}{images/27May2003_15min.mpg}\\
\tiny{University of Freiburg}
\end{center}






\foilhead[0.25in]{Solar Spectrum}
\noindent \begin{center}
   \begin{tabular}{cc}
      \begin{minipage}{0.49\textwidth}
         \includegraphics[width=0.9\textwidth]{images/Solar_Spectrum.png}
         \\ {\tiny Wikipedia}
      \end{minipage}
      &
      \begin{minipage}{0.49\textwidth}
         \includegraphics[width=0.9\textwidth]{images/SolarCCD.jpg}
         \\ {\tiny R. Kurucz, CfA}
      \end{minipage}
   \end{tabular}
\end{center}
The Fraunhofer absorption lines (right) indicate that there is something in the foreground. What is it?

\noindent $\rightarrow$ Form an image in one of the more prominent absorption lines...


\foilhead[0.25in]{Chromosphere (H Balmer $\alpha$)}
\begin{center}
\includemovie[
  autoplay,
  poster,
  controls,
  % autoclose,
  % text=()
  % repeat,
  % palindrome
]{1.0 \textheight}{0.75 \textheight}{images/BBSO-H-alpha-Xflare-02july22.mpg}\\
\end{center}


\foilhead[0.25in]{Chromosphere (Ca II H)}
\begin{center}
\includemovie[
  autoplay,
  poster,
  controls,
  % autoclose,
  % text=()
  % repeat,
  % palindrome
]{1.2 \textheight}{0.6 \textheight}{images/SOT_ca_061120_0715.mpg}\\
\tiny{Hinode / Solar Optical Telescope, 2006-11-20 07:15 UT}
\end{center}
\begin{itemize}\zerolistvertdimens
   \item IRIS mission: \url{http://iris.lmsal.com}
\end{itemize}

% ********************** Magnetic Fields *************************

\foilhead[0.25in]{Hale's Discovery (1908)}
\begin{center}
    \begin{tabular}{c c}
        \begin{minipage}{0.3\textwidth}
            \begin{center}
                \includegraphics[height=0.5\textheight]
                {images/Hale-Mt-Wilson-spectrograph.jpg}
            \end{center}
            \noindent George Ellery Hale at the
            \href{https://www.mtwilson.edu/george-ellery-hale/}
            {Mount Wilson Obervatory}. 
        \end{minipage}
        &
        \begin{minipage}{0.65\textwidth}
            \begin{center}
                \includegraphics[height=0.5\textheight]
                    {images/zeeman-sunspot.png}
            \end{center}     
            \noindent Zeeman splitting in a sunspot 
            reveals its magnetic nature.
        \end{minipage}
    \end{tabular}
\end{center}


\foilhead[0.25in]{Solar Magnetism}
\begin{center}
\includemovie[
  autoplay,
  poster,
  controls,
  repeat=3
]{0.9 \textheight}{0.9 \textheight}{images/JHV-magnetograms.mp4}
\end{center}
% **********************  A I A   MOVIES  *************************


\foilhead[0.25in]{Beyond the Chromosphere...}
\begin{center}
\includemovie[
  autoplay,
  poster,
  controls,
  % autoclose,
  % text=()
  repeat,
  palindrome
]{0.6 \textheight}{0.6 \textheight}{images/wave_fade.mpg}\\
The \textbf{corona} is a million degree ionized plasma sitting
on top of the chromosphere, glowing in X-rays!!
\end{center}

\foilhead[0.25in]{Atmospheric Profile}
\begin{center}
   \includegraphics[height=0.75\textheight]
         {images/TR.jpg} 
\end{center}


\foilhead[0.25in]{Solar Atmosphere Tour: SDO/AIA}
\begin{center}
   \includegraphics[totalheight=0.7\textheight]{images/SDO_badge.png}
   \\ We'll proceed through the channels on the Atmospheric Imaging Assembly
   (AIA) in order of increasing temperature...
\end{center}


\foilhead[0.25in]{450\,nm, Continuum; $5000$\,K}
\begin{center}
\includemovie[
  autoplay,
  poster,
  controls,
  % autoclose,
  % text=()
  repeat,
  %palindrome
]{0.8 \textheight}{0.8 \textheight}{images/JHV_4500.mp4}\\
\tiny{NASA Solar Dynamics Observatory / Atmospheric Imaging Assembly}
\end{center}

\foilhead[0.25in]{170\,nm, UV Continuum; $10^4 +$\,K?}
\begin{center}
\includemovie[
  autoplay,
  poster,
  controls,
  % autoclose,
  % text=()
  repeat,
  %palindrome
]{0.8 \textheight}{0.8 \textheight}{images/JHV_1700.mp4}\\
\tiny{NASA Solar Dynamics Observatory / Atmospheric Imaging Assembly}
\end{center}


\foilhead[0.25in]{160\,nm, CIV + Continuum; $10^4 - 10^5$\,K?}
\begin{center}
\includemovie[
  autoplay,
  poster,
  controls,
  % autoclose,
  % text=()
  repeat,
  %palindrome
]{0.8 \textheight}{0.8 \textheight}{images/JHV_1600.mp4}\\
\tiny{NASA Solar Dynamics Observatory / Atmospheric Imaging Assembly}
\end{center}

\foilhead[0.25in]{30.4\,nm, He II; $5\times 10^4$\,K}
\begin{center}
\includemovie[
  autoplay,
  poster,
  controls,
  % autoclose,
  % text=()
  repeat,
  %palindrome
]{0.8 \textheight}{0.8 \textheight}{images/JHV_304.mp4}\\
\tiny{NASA Solar Dynamics Observatory / Atmospheric Imaging Assembly}
\end{center}







\foilhead[0.25in]{13.1\,nm, Fe VIII, XX, XXIII; $4\times 10^5, 10^7, 1.6\times 10^7$\,K}
\begin{center}
\includemovie[
  autoplay,
  poster,
  controls,
  % autoclose,
  % text=()
  repeat,
  %palindrome
]{0.8 \textheight}{0.8 \textheight}{images/JHV_131.mp4}\\
\tiny{NASA Solar Dynamics Observatory / Atmospheric Imaging Assembly}
\end{center}


\foilhead[0.25in]{17.1\,nm, Fe IX; $6.3\times 10^5$\,K}
\begin{center}
\includemovie[
  autoplay,
  poster,
  controls,
  % autoclose,
  % text=()
  repeat,
  %palindrome
]{0.8 \textheight}{0.8 \textheight}{images/JHV_171.mp4}\\
\tiny{NASA Solar Dynamics Observatory / Atmospheric Imaging Assembly}
\end{center}


\foilhead[0.25in]{19.3\,nm, Fe XII, XXIV; $1.2\times 10^6, 2\times 10^7$\,K}
\begin{center}
\includemovie[
  autoplay,
  poster,
  controls,
  % autoclose,
  % text=()
  repeat,
  %palindrome
]{0.8 \textheight}{0.8 \textheight}{images/JHV_193.mp4}\\
\tiny{NASA Solar Dynamics Observatory / Atmospheric Imaging Assembly}
\end{center}


\foilhead[0.25in]{21.1\,nm, Fe XIV; $2\times 10^6$\,K}
\begin{center}
\includemovie[
  autoplay,
  poster,
  controls,
  % autoclose,
  % text=()
  repeat,
  %palindrome
]{0.8 \textheight}{0.8 \textheight}{images/JHV_211.mp4}\\
\tiny{NASA Solar Dynamics Observatory / Atmospheric Imaging Assembly}
\end{center}


\foilhead[0.25in]{33.5\,nm, Fe XVI; $2.5\times 10^6$\,K}
\begin{center}
\includemovie[
  autoplay,
  poster,
  controls,
  % autoclose,
  % text=()
  repeat,
  %palindrome
]{0.8 \textheight}{0.8 \textheight}{images/JHV_335.mp4}\\
\tiny{NASA Solar Dynamics Observatory / Atmospheric Imaging Assembly}
\end{center}


\foilhead[0.25in]{9.4\,nm, Fe XVIII; $6.3\times 10^6$\,K}
\begin{center}
\includemovie[
  autoplay,
  poster,
  controls,
  % autoclose,
  % text=()
  repeat,
  %palindrome
]{0.8 \textheight}{0.8 \textheight}{images/JHV_94.mp4}\\
\tiny{NASA Solar Dynamics Observatory / Atmospheric Imaging Assembly}
\end{center}


\foilhead[0.25in]{13.1\,nm, Fe VIII, XX, XXIII; $4\times 10^5, 10^7, 1.6\times 10^7$\,K}
\begin{center}
\includemovie[
  autoplay,
  poster,
  controls,
  % autoclose,
  % text=()
  repeat,
  %palindrome
]{0.8 \textheight}{0.8 \textheight}{images/JHV_131.mp4}\\
\tiny{NASA Solar Dynamics Observatory / Atmospheric Imaging Assembly}
\end{center}


\foilhead[0.25in]{SDO/AIA Channels Summary}
\begin{center}
   \includegraphics[width=0.9\textwidth]{images/AIA_channels.png}
\end{center}
\begin{enumerate}\zerolistvertdimens
   \item Why are the wavelengths not inversely proportional to temperature?
   \item Why are there no coronal H or He lines?
   \item Why is the corona hotter than the photosphere?
\end{enumerate}


\foilhead[0.25in]{Solar Atmosphere Summary}
\begin{itemize} \zerolistvertdimens
   \item Photosphere
   \begin{itemize} \zerolistvertdimens
      %\item IR-Visible-UV continuum.
      \item Convection zone is dense and opaque, with a well-defined surface.
      \item Energy to escapes at the photosphere as continuum radiation.
      \item Spectrum at a given depth depends mainly on temperature (LTE).
      \item To first approximation, can ignore magnetic field.
   \end{itemize}
   \item Corona (\& Transition Region)
   \begin{itemize} \zerolistvertdimens
      %\item EUV \& x-ray emission line spectrum.
      \item Optically thin (transparent).
      \item Ionization (and therefore source spectrum) determined by temperature.
      \item Magnetic field confines plasma to 1D atmospheres (loops).
   \end{itemize}
   \item In the Chromosphere, everything matters:
   \begin{itemize} \zerolistvertdimens
      %\item Visible \& UV absorption \& emission lines, and continuum.
      \item Neither opaque nor transparent. Messy radiative transfer.
      \item Non-LTE (radiation field out of equilibrium with temperature).
      \item Magnetic field competes with hydrodynamic forces.
   \end{itemize}
\end{itemize}

\end{document}