 \documentclass[12pt] {article}

% ~/bin-linux/tth -e2haicV -Lsummary < summary.tex > summary.html

%\input{definitions.tex}
%\input{def_journals.tex}

\def\hyperlink#1#2{\special{html:<a href="\##1">}#2\special{html:</a>}}
  % Incorrect link name in \TeX\ because # can't be passed properly to a special.
\def\hypertarget#1#2{\special{html:<a name="#1">}#2\special{html:</a>}}
\long\def\tthdump#1{#1} % Do nothing. The following are not done for TtH.
\tthdump{%
\def\title#1{\bgroup\leftskip 0 pt plus1fill \rightskip 0 pt plus1fill
\pretolerance=100000 \lefthyphenmin=20 \righthyphenmin=20
\noindent #1 \par\egroup}% Centers a possibly multi-line title.
 \let\author=\title % Actually smaller font than title in \LaTeX.
 \input epsf     % PD package defines \epsfbox for figure inclusion
  % Macro for http reference inclusion, per hypertex.
 \def\href#1#2{\special{html:<a href="#1">}#2\special{html:</a>}}
 \def\urlend#1{#1\endgroup}
 \def\url{\begingroup \tt 
  \catcode`\_=13 % Don't know why this works.
  \catcode`\~=11 \catcode`\#=11 \catcode`\^=11 
  \catcode`\$=11 \catcode`\&=11 \catcode`\%=11
\urlend}% \url for plain \TeX.
}


%\usepackage{mnstyle}
%\usepackage{array}
%\usepackage{latexsym}
\usepackage{longtable}
\usepackage{rotating}
\usepackage{epsfig}
\usepackage{psfig}

\setlength{\textheight}{250mm}                           %NORM=250
\setlength{\headheight}{0.0mm}
\setlength{\headsep}{0.0mm}
\setlength{\topmargin}{-5mm}
%\setlength{\footheight}{-5mm} 
%\setlength{\footskip}{15mm}
\setlength{\textwidth}{150mm} 
\setlength{\oddsidemargin}{13mm} 
 \setlength{\evensidemargin}{13mm}  
\setlength{\LTcapwidth}{150mm}                 %Width of longtable captions
\setlength{\belowcaptionskip}{4.2ex} 

%\parindent 0.6cm
\parindent 0.cm

\parskip 8pt
\oddsidemargin 0.5cm
\evensidemargin 0.5cm
\baselineskip 18 pt
%\textwidth 15cm
%\textheight 21cm

\def\ap{'\hskip 1pt}
\def\skf{\vskip 0.2truecm\noindent}
\def\skp{\vskip 1.truecm\noindent}
\def\skt{\vskip 0.5truecm}

\pagestyle{empty}

\large

\begin{document}


\section{Overview }

\begin{figure*}[!htbp]
\centerline{\epsfig{file=20031028_xray.ps, width=12.0cm , angle=0 }}
\centerline{\epsfig{file=goes_bw.ps, width=10.0cm , angle=90 }}
\caption{\large Time evolution of the GOES   X-ray fluxes.
Here we focus on the  October 28, 2003 X17 flare. 
In the bottom plot, the timings of the 5 successive CDS rasters 
are indicated.
CDS observed the two precursor M-class flares F1 and F2
with the third raster.
}
  \label{fig:goes_plot}
% Fig.~\ref{fig:goes_plot}
\end{figure*}


\section{The two pre-events, M-class flares}


SOHO CDS observed with the 3rd raster during
 09:37-11:02 UT.
CDS observed two distinct M-class flares,
with strong Fe~XIX emission 
(saturated in the two cores).
The first one (F1) was observed during 10:00-10:19 UT,
while the second (F2) during 10:33-10:47 UT.
The first flare was also observed by TRACE.


%Fe XIX is saturated in two points.
%Also O IV is saturated in one slit position
%(X = 14)

\begin{figure*}[!htbp]
\centerline{\epsfig{file=seq_trace_195_10_11.ps, width=16.0cm , angle=0 }} 
\caption{\large Sequence of TRACE 195 \AA\ images, showing 
the two M-class flares. Between 10:24 and 10:49 UT 
TRACE did not observe. Note the contours of Fe~XIX 
emission of the two flares observed by CDS.}
  \label{fig:}
\end{figure*}

\begin{figure*}[!htbp]
\centerline{\epsfig{file=seq_trace_1600_10_11.ps, width=16.0cm , angle=0 }} 
\caption{\large Sequence of TRACE 1600 \AA\ images, showing 
the two M-class flares. Between 10:24 and 10:49 UT 
TRACE did not observe.
}
  \label{fig:}
\end{figure*}



\begin{figure*}[!htbp]
\centerline{\epsfig{file=trace_1019_mdi.ps, width=12.0cm , angle=0 }} 
\centerline{\epsfig{file=trace_1600_1019_mdi.ps, width=12.0cm , angle=0 }}
 \caption{\large TRACE 195,1600 \AA\ 
with contours from SOHO/MDI magnetogram.
The M-class flare occurred in the region of mixed polarity.
Note also the filament eruption associated with this flare.}
  \label{fig:}
\end{figure*}

\begin{figure*}[!htbp]
\centerline{\epsfig{file=mdi_1019.ps, width=13.0cm , angle=0 }}
\caption{\large SOHO/MDI magnetogram.}
 \label{fig:}
\end{figure*}

\begin{figure*}[!htbp]
\centerline{\epsfig{file=cds_int_9_11.ps, width=19.0cm , angle=0 }} 
\caption{\large CDS monochromatic images at transition region 
(O V), coronal (Mg X) and flare (Fe XIX) temperatures, during the 
long CDS scan which observed the two F1,F2 M-class flares.
Overlaid are contours of TRACE 1600 \AA.
Notice the complex structure of the second flare (left) in the 
enhanced Fe XIX image. }
  \label{fig:}
\end{figure*}


\section{The  X17 flare}


\begin{figure*}[!htbp]
\centerline{\epsfig{file=seq_trace_195_1055_1122.ps, width=13.0cm , angle=0 }} 
\caption{Sequence of TRACE 195 \AA\ images
during the X17 flare. The first three images are 
shown with a different intensity scale, compared to the 
following ones.
}
  \label{fig:}
\end{figure*}

\begin{figure*}[!htbp]
\centerline{\epsfig{file=2003oct28_trace_rhsi_int3_high_low.ps, width=13.0cm , angle=0 }} 
\caption{TRACE + RHESSI (from Sam Krucker)}
  \label{fig:}
\end{figure*}

\href{031028_eit_195.mpg}{SOHO/EIT 195 A movie}

\href{031028_c3.mpg}{SOHO/LASCO movie}


\begin{figure*}[!htbp]
\centerline{\epsfig{file=hsi_wind_20031028_1000_a.ps, width=13.0cm , angle=0 }} 
\caption{GOES + RHESSI + ... }
  \label{fig:}
\end{figure*}


\skt
{\bf Post-flare arcade }
\skt

Here we show results concerning the 5th CDS observation
(12:28-12:52 UT). During this time, 
TRACE 195 and 1600~\AA\ images show that the 2-ribbon 
structure and the arcade of loops is approximately stationary,
with some apparent flows along the loops.

\begin{figure*}[!htbp]
\centerline{
\epsfig{file=trace_seq_195.ps, width=8.0cm , angle=0 }
\epsfig{file=trace_seq_1600.ps, width=8.0cm , angle=0 }
} 
\caption{Sequence of TRACE 195, 1600 \AA\ images during the CDS
raster, shown with the 
same intensity scale. The FOV of the CDS raster, and the 
position of the slit. Notice that overall the loop structures
seen in TRACE 195~\AA\ and the ribbon structures
seen in TRACE 1600~\AA\ remain largely unchanged.
}
 \label{fig:trace_seq}
% Fig.~\ref{fig:trace_seq}
\end{figure*}

\href{test_195.mpg}{195 A movie}

\href{test_1600.mpg}{1600 A movie}

\href{test_halpha.html}{halpha}


\begin{figure*}[!htbp]
\centerline{
\epsfig{file=trace_195_1240_bw_mdi.ps, width=8.0cm , angle=90 }
\epsfig{file=trace_1600_1240_bw_mdi.ps, width=7.0cm , angle=90 }
} 
\centerline{
\epsfig{file=trace_195_1240_zbw_mdi.ps, width=8.0cm , angle=90 }
\epsfig{file=trace_1600_1240_zbw_mdi.ps, width=8.0cm , angle=90 }
} 
\caption{TRACE 195, 1600 \AA\ images, with contours from the
SOHO/MDI magnetogram (200, 500, 1000 G).
Notice the arcade of loops seen in TRACE 195~\AA\ 
connecting the ribbon structures R1, R2 which are located above the 
sunspot regions of opposite polarity.
Also note the system of loops in TRACE 195~\AA\ 
which connects the ribbon R3
to R1 and R2. The ribbon R3 is seen in TRACE 1600~\AA\
as an almost straight line of emission.
 Flows in TRACE 1600~\AA\ from R3 to R1 are seen.
The cantral part of R3 is also the loaction of the 
strongest emission in  TRACE 195~\AA.
}
 \label{fig:trace}
% Fig.~\ref{fig:trace}
\end{figure*}


%\centerline{\epsfig{file=trace_195_1240_civ.ps, width=14.0cm , angle=0 }} 
%\centerline{\epsfig{file=trace_1600_1240.ps, width=14.0cm , angle=0 }}
%  \caption{\large Top: TRACE 195 \AA\ with contours of CIV.
%Bottom: TRACE 1600~\AA }


\begin{figure}[!htbp]
\centerline{\epsfig{file=wro124059_mdimag0935_map.ps, width=12.0cm , angle=0 }}
\caption{H$\alpha$ observation from Bialkov, with contours
of SOHO/MDI magnetograms.
Note the similarity with the TRACE 1600~\AA\ image and 
the presence of the three ribbon structures.}
 \label{fig:halpha}
% Fig.~\ref{fig:halpha}
\end{figure}


\skt
{\bf  }
\skt

\begin{figure*}[!htbp]
\centerline{\epsfig{file=ov_int_civ.ps, width=10.0cm , angle=90 }
\epsfig{file=mgx_int_civ.ps, width=10.0cm , angle=90 } }
\centerline{\epsfig{file=si_xii_int_civ.ps, width=10.0cm , angle=90 }
\epsfig{file=fexix_int_civ.ps, width=10.0cm , angle=90 }}
\caption{\large CDS intensity maps with contours of TRACE 1600 (showing the ribbons).
The post-flare loops show emission at all temperatures}
  \label{fig:}
% Fig.~\ref{fig:}
\end{figure*}

\begin{figure*}[!htbp]
\centerline{\epsfig{file=fexix_int_1600.ps, width=7.0cm , angle=90 }
\epsfig{file=fexix_int_195.ps, width=7.0cm , angle=90 }}
\caption{ intensity in Fe~XIX with 
contours of TRACE  1600,195 \AA\ intensities.}
\end{figure*}


\clearpage

\begin{figure*}[!htbp]
\centerline{\epsfig{file=ov_vel_civ.ps, width=17.0cm , angle=0 }}
\caption{\large CDS velocity map in the transition region (O~V)
with contours of TRACE 1600 (showing the ribbons).
Strong downflows ($v \simeq 50-100$ km/s ) in the ribbons 
are observed.
}
  \label{fig:}
% Fig.~\ref{fig:}
\end{figure*}

\begin{figure*}[!htbp]
\centerline{\epsfig{file=mgx_vel_civ.ps, width=14.0cm , angle=0 }}
\centerline{\epsfig{file=si_xii_vel_civ.ps, width=14.0cm , angle=0 }}
\caption{\large CDS velocity maps in coronal lines
with contours of TRACE 1600 (showing the ribbons).
Strong downflows ($v \simeq 50-100$ km/s ) in the ribbons 
are observed.
}
  \label{fig:}
% Fig.~\ref{fig:}
\end{figure*}

\clearpage

\begin{itemize}

\item
The X17 flare presented great complexity. 
We have used the CDS to understand the temperature
structure of the various events.

\item
Two precursor M-class events have been observed with CDS.
The first one was also observed by TRACE, while the second,
more important one, was not observed by TRACE.
The second one had a complex structure of hot loops.

\item
During the precursor events the filament 
becomes activated. 

\item
During the X17 flare the ribbons quickly separate
and an arcade system of loops forms.
These loops are multi-thermal, with the 
hottest part in the central region.

\item
Strong downflows ($v \simeq 50-100$ km/s ), in 
particular at transition region temperatures
are observed in the ribbons.


\end{itemize}



\end{document}
