\relax 
\@writefile{toc}{\contentsline {section}{\numberline {1}Introduction}{1}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces The emission functions used in the present study for the 14 lines or energy bands. Key numbers denoting the curves correspond to lines/bands given in Table\nobreakspace  {}1.}}{1}}
\@writefile{lot}{\contentsline {table}{\numberline {1}{\ignorespaces The set of lines/bands used in our DEM inversion}}{2}}
\newlabel{tab:table*}{{1}{2}}
\@writefile{toc}{\contentsline {section}{\numberline {2}The WS algorithm}{2}}
\@writefile{toc}{\contentsline {section}{\numberline {3}The results }{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces Left row: comparison of assumed (solid line) with calculated (dashed line) model in case the data does not contain errors. In the right row each of hundred calculated models was computed using perturbed lines fluxes. The perturbations have been taken according to average uncertainty values from the Table. }}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces DEM distributions calculated for 13 January 1992 flare. The lower panel show the ratio of observed to calculated fluxes in the particular line/band. In the upper panel the solid line represent results of present study while the dash-dotted line represents the shape of DEM as calculated by McTiernan (1997) using Maximum Entropy method.}}{3}}
\bibcite{Fludra86}{{1}{1986}{{Fludra}}{{}}}
\bibcite{McTiernan97}{{2}{1997}{{McTiernan}}{{}}}
\bibcite{Sylwester80}{{3}{1980}{{Sylwester}}{{}}}
\bibcite{Withbroe97}{{4}{1997}{{Withbroe}}{{}}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces  As in Figure 3. DEM distributions for 20\nobreakspace  {}October\nobreakspace  {}1995. The lower panel presents ratios of the observed to calculated flux in the particular line/band. }}{4}}
\@writefile{toc}{\contentsline {section}{\numberline {4}Summary}{4}}