%\documentclass[pdf,azure1,colorBG]{prosper}

% dvips -Ppdf -G0 talk2.dvi -o talk2.ps

% ps2pdf -dPDFsettings=/prepress talk2.ps talk2.pdf 

%%%%%%%%%%%%%%%%%%%%%%%%%

\documentclass[ps,azure1,colorBG]{prosper}
% dvips -Ppdf -G0 talk2.dvi -o talk2ps.ps


%\documentclass[pdf,slideColor,contemporain,colorBG]{prosper}

%\documentclass[pdf,slideColor, gdz1,colorBG]{prosper}

%\documentclass[pdf,slideColor,azure,colorBG]{prosper}

%\documentclass[ps,slideColor,darkblue,colorBG]{prosper}

% ~/ss/research/flare


\usepackage{amsmath, epsfig, amsfonts, amsbsy, pstricks, pst-node, pst-text, pst-3d}


\newcommand{\items}[1]{\begin{itemize} \item #1 \end{itemize}}
\newcommand{\itemss}[2]{\begin{itemize} \item #1 \item #2 \end{itemize}}
\newcommand{\itemsss}[3]{\begin{itemize} \item #1 \item #2 \item #3 
\end{itemize}}
\newcommand{\itemssss}[4]{\begin{itemize} \item #1 \item #2 \item #3 \item #4
\end{itemize}}

%\newcommand{\slidetextsize}{\footnotesize}
%\newcommand{\captionstyle}[1]{\scriptsize \textbf{#1}}


\newcommand{\Ne}{$N_{\rm e}$}
\newcommand{\Te}{$T_{\rm e}$}

\newcommand{\cmt}{cm$^{-3}$}
\newcommand{\cm}{cm$^{-1}$}
\def\rsun{R$_\odot$}

\newcommand{\bi}{\begin{itemize}}
\newcommand{\ei}{\end{itemize}}

\title{Spectroscopic observations of compact solar flares}
%\subtitle{

\author{Giulio Del Zanna \&  H.E. Mason \\
   A.\ Berlicki \&  B.\ Schmieder } 


%\centerline{Department of Applied Mathematics and Theoretical Physics \\
% University of Cambridge }
%\centerline{  A.\ Berlicki \&  B.\ Schmieder}
%\centerline{Observatoire de Paris,  Meudon }

\institution{Department of Applied Mathematics and Theoretical Physics \\
 University of Cambridge \\
 Observatoire de Paris,  Meudon }


\slideCaption{COSPAR 2004: compact solar flares}

\Logo(8.3,7.78){\includegraphics[scale=0.4]{UniversityLogo.eps}}

\DefaultTransition{Replace}

%Box dissolve replace wipe 

%\FontTitle{Large}{}



\begin{document}
\maketitle

%\FontText{ \white\usefont{T1}{phv}{m}{n}\fontsize{14.4pt}{14pt}\selectfont}

%\footnotesize

%---------------------------------------------------------------------- SLIDE -
%---------------------------------------------------------------------- SLIDE -
\overlays{5}{%
\begin{slide}{Introduction}



\begin{itemstep}

\item
The SOHO/Coronal Diagnostic Spectrometer provides essential  
spectroscopic information to understand the characteristics 
and dynamics of solar coronal features.

\item
We give a description of the main observational features
and what types of measurements (densities, temperatures, flows)
are obtained. 

\item
These provide important observational constraints 
for flare modeling.

\item
 CDS observations of a compact M1 flare 
that occurred on October 22 2002, also observed from the ground
in chromospheric lines  and by RHESSI.

\item
The flare occurred in a region of strong and mixed magnetic polarity,
was compact and lasted only a short time.

\end{itemstep}
\end{slide}
}
%------------------------------------------------------------------------------

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{Papers -- I }

\begin{figure}[!htbp]
\centerline{\epsfig{file=p1.ps, width=4.0cm,angle=-90 }}
\end{figure}

- Del Zanna et al. (2004) in preparation
\end{slide}

\begin{slide}{Papers -- II }

\bi
\item
On general aspects of quiescent ARs:

-Del Zanna \& Mason 2003, A\&A, 406, 1089

-Del Zanna 2003, A\&A,  406, L5

\item 
On chromospheric evaporation:

-Mason et al. 1986, ApJ, 309,435 

-Zarro et al., 1988, ApJ, 333, L99

-Del Zanna et al.  (COSPAR 2000),  2002, Adv. Space Res., 30, 551

%-Gibson et al., 2002, ApJ, 574, 1021
%-Del Zanna,  Mason, \& Foley, 2002, 
% 10th European Sol. Phys. meeting, ESA-SP 506, 585
\item 
Time dependent and non-equilibrium effects:

-Bradshaw,  Del Zanna \& Mason, A\&A, 2004, in press

\ei


\end{slide}
%------------------------------------------------------------------------------

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{Overview I}

\begin{figure}[!htbp]
\centerline{\epsfig{file=fov.ps, width=4.0cm,angle=-90 }
\epsfig{file=wl.ps, width=4.0cm,angle=-90 }}
\centerline{\epsfig{file=blong.ps, width=4.0cm,angle=-90 }}
\caption{THEMIS/MSDP in  Na I ${\rm{D_{1}}}$
(15:41--16:29 UT) and line-of-sight magnetic field deduced from
           $I$ and $V$ Stokes overlaid with H$\alpha$ contours
observed by VTT/MSDP at 15:30:01 UT.}
\end{figure}

\end{slide}
%------------------------------------------------------------------------------
%---------------------------------------------------------------------- SLIDE -
\begin{slide}{Overview II}

\begin{itemstep}
\item
THEMIS observed continuously between 15:41--17:26 UT.
\item
TRACE and VTT/MSDP observations were performed during 
           the whole flare.
\item
VTT/MSDP observations in H$\alpha$
9 scans between 15:30 and 16:17 UT
\item
TRACE high cadence (40 s) in the 195 {\AA} band between 15:29 and
15:41 UT 

\end{itemstep}
\end{slide}

\begin{slide}{Overview III - GOES}

\begin{figure}[!htbp]
\centerline{\epsfig{file=goesp1.ps, width=6.0cm,angle=0 }
\epsfig{file=goesp2.ps, width=6.0cm,angle=0 }}
\end{figure}

\end{slide}

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{RHESSI } 

RHESSI counts rates (the 12--25 keV  band are 
multiplied by a factor of 10).

\begin{figure}[!htbp]
\centerline{\epsfig{file=rhessi_cr.ps, width=7.0cm,angle=-90 }}
%\caption).}
\end{figure}

\end{slide}

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{Movies}

{\bf MDI}
\href{run:movie_mdi_long.mpg}{\red MDI movie}

{\bf MDI - during the M1 flare}
\href{run:movie_mdi_15_16.mpg}{\red MDI movie}

{\bf TRACE 195 \AA}
\href{run:movie_trace.mpg}{\red TRACE movie}

\end{slide}

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{The M1 flare}

\begin{figure}[!htbp]
\centerline{\epsfig{file=trace_195_154039_mdi.ps, width=9.0cm,angle=0 }}
%\caption{TRACE 195 \AA\ + MDI contours}
\end{figure}
\end{slide}

%---------------------------------------------------------------------- SLIDE -

\begin{slide}{The M1 flare}

 CDS FOV - TRACE 195 \AA\ + contours of Fe XIX intensity

\begin{figure}[!htbp]
\centerline{\epsfig{file=trace_195_154039_FeXIX_int.ps, width=8.0cm,angle=0 }}
%\caption{\small}
\end{figure}

\end{slide}

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{The M1 flare - CDS }

\begin{figure}[!htbp]
\centerline{
\epsfig{file=s26058r00_OV_int_mdi.ps, width=4.5cm,angle=0 }
\epsfig{file=s26058r00_OV_pos_mdi.ps, width=4.5cm,angle=0}
}
\end{figure}

\begin{figure}[!htbp]
\centerline{
\epsfig{file=s26058r00_SiXII_int_mdi.ps, width=4.5cm,angle=0 }
\epsfig{file=s26058r00_SiXII_pos_mdi.ps, width=4.5cm,angle=0}
}
\end{figure}


\end{slide}

%------------------------------------------------------------------------------
\begin{slide}{The M1 flare - CDS -- Zoom in }

\begin{figure}[!htbp]
\centerline{
\epsfig{file=s26058r00_FeXIX_int_mdi.ps, width=4.5cm,angle=0 }
\epsfig{file=s26058r00_FeXIX_int_SiXII_pos.ps, width=4.5cm,angle=0}
}
\end{figure}

\begin{figure}[!htbp]
\centerline{
\epsfig{file=s26058r00_FeXIX_pos_SiXII_pos.ps, width=5.0cm,angle=0}
\epsfig{file=trace_195_154039_SiXII_pos.ps, width=5.0cm,angle=0}
}
\end{figure}


\end{slide}
%------------------------------------------------------------------------------

%---------------------------------------------------------------------- SLIDE -

\begin{slide}{Wavelength calibration}


The  wavelength calibration was remarkably stable.

Uncertainty 
in the derivation of velocities of the order of 
5--10 km/s.

\ptsize{8}

\begin{table*}[ht]
\begin{center}
%\footnotesize
%\tiny
\scriptsize
\begin{tabular}{lcccccccccccc}
%[511.455, 0.116225, 7.71135e-07]
\hline\noalign{\smallskip}
\hline\noalign{\smallskip}

$\lambda_{st}$ (\AA) & 520.665& 522.210&  542.07& 550.06& 553.34& 555.263&
 557.765& 558.594& 562.803& 592.60& 624.941& 629.732 \\

$\lambda$ (s26055) & 520.675 & 522.208   &    542.031  &     550.070   &    553.365  &     555.252    &   557.758     &  558.590    &   562.791    &   592.590   &    624.936
   &    629.735 \\

$v$ (s26055) & 5 &   -1 &  -21  &   5 &   13 &   -6 &   -3  &  -2 &   -6 &   -5 &   -2  &   1 \\

$\lambda$ (s26059) & 520.664 & 522.211 & 542.061 & 550.066 &
 553.354 & 555.260 & 557.769 & 558.622 & 562.812 & 592.597 & 624.932 & 629.747 \\


$v$ (s26059)      & 0 &   0 &  -4 &   3  &  7 &  -1  &  1 &  15  &  5  & -1 & -4  &  6 \\

\hline\noalign{\smallskip}
\end{tabular}
\end{center}
\normalsize
\label{tab:wvl_cal}
\end{table*}

\end{slide}

%---------------------------------------------------------------------- SLIDE -

\begin{slide}{The Fe XIX case}

Our calibration, based on this small sample,
provides a wavelength of 592.16 \AA, in excellent 
agreement with  Skylab measurements.


Lawson \& Peackok (1980)
reviewed  $n=2 \to n=2$ 
transitions, and suggested  an energy 
for the 2s 2 2p 4 $^1$D$_{2}$ level 
of 168770 \cm.

$\to \lambda=$ 592.522 \AA

$\to $ the considerable difference of  
 183. km/s compared to our result.


\end{slide}

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{Selected areas }

\begin{figure}[!htbp]
\centerline{\epsfig{file=s26058r00_sixii_areas.ps, width=5.0cm,angle=90}}
%\caption{\small }
  \label{fig:}
\end{figure}
% Figure~\ref{fig:}

Si XII velocity map, with the areas selected for further
  analysis.
Areas A,B,C correspond to regions of strong blue-shifts,
while area D of red-shift. Region LP corresponds to 
the area of peak Fe XIX intensity, while region L1 is where 
the central part of the flare loop is located. 
Region BG is a `background' reference region.

\end{slide}
%---------------------------------------------------------------------- SLIDE -

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{ }

\begin{figure}[!htbp]
\centerline{\epsfig{file=s26058r00_oiv_win.ps, width=4.0cm , angle=90 }
\epsfig{file=s26058r00_fe_xix_win.ps, width=4.0cm , angle=90 }}
\centerline{\epsfig{file=s26058r00_mgx_win.ps, width=4.0cm , angle=90 }}
%\caption{ }
  \label{fig:}
\end{figure}
% Figure~\ref{fig:}

\end{slide}

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{ }

\begin{figure}[!htbp]
\centerline{\epsfig{file=s26058r00_he_i_prof.ps, width=4.0cm , angle=90 }
\epsfig{file=s26058r00_si_xii_prof.ps, width=4.0cm , angle=90 }}
\centerline{\epsfig{file=s26058r00_fe_xix_prof.ps, width=4.0cm , angle=90 }}
%\caption{ }
  \label{fig:}
\end{figure}
% Figure~\ref{fig:}

\end{slide}
%---------------------------------------------------------------------- SLIDE -

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{ }

\begin{table}[!htbp]
%\caption[]{ }
\begin{center}
%\footnotesize
%\tiny
%\scriptsize

\begin{tabular}{llrccclll}
\hline\noalign{\smallskip}

\hline\noalign{\smallskip}
Region         & A &   B    & C    & D   & L1 & LP & BG & \\
\hline\noalign{\smallskip}
%
v He I (km/s)   &  13  & -27  & -30  & -17 &  & & & \\
v Si XII (km/s) & -64  & -84  & -54  &  17 & -6 & -40 & & \\
v Fe XIX (km/s) & -141 & -140 & -56  & 22  & -13 & -26 & -  & \\  
%
%Ne   &  & & & & & & & \\
%  &  & & & & & & & \\
\hline\noalign{\smallskip}
\end{tabular}
\end{center}
\normalsize
\label{tab:}
\end{table}


\end{slide}
%---------------------------------------------------------------------- SLIDE -

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{Post-flare CDS raster 15:43--17:07 UT }

\begin{figure}[!htbp]
\centerline{
\epsfig{file=s26059r00_ima.ps, width=5.5cm,angle=0}
\epsfig{file=s26059r00_pos.ps, width=5.5cm,angle=0}
}
\end{figure}

\end{slide}
%---------------------------------------------------------------------- SLIDE -

%---------------------------------------------------------------------- SLIDE -
\begin{slide}{Post-flare CDS raster -- II }

\begin{figure}[!htbp]
\centerline{
\epsfig{file=trace_1627_FeXIX_int.ps, width=6.0cm,angle=0}
\epsfig{file=rhessi_1625_1628_3kev.ps, width=6.0cm,angle=0}
}
\end{figure}


\end{slide}
%---------------------------------------------------------------------- SLIDE -


\begin{slide}{Summary of preliminary results}

\bi
\item
Strong blue-shifts in lines emitted in the 1-8 MK range are observed
at the bases of hot Fe XIX structures.

\item
The hot structures are also clearly visible in the TRACE 195~\AA\ band

\item
The hot structures match the thermal emission as seen by RHESSI

\item
The peak Fe~XIX emission, recorded between 15:35 and 
15:43 UT, occurred just above the region of 
strong mixed polarity.

\item
The  TRACE 195 \AA\ emission is co-spatial 
with the CDS  Fe~XIX emission, which suggests that 
the bulk of the  TRACE 195 \AA\ emission 
 at the flare site is due to Fe~XXIV.

\item
Transition region densities can be estimated using 
 O~IV.
%1.5 $\times 10$^{11}$ cm$^{-3}$.


\ei


{\bf Acknowledgements}

Support from  PPARC is acknowledged. \\

SOHO is a project of international collaboration between ESA and NASA.

We acknowledge the use of the SURF, TRACE 
on-line databases.

\end{slide}


%---------------------------------------------------------------------- SLIDE -


\end{document}
