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\@writefile{toc}{\contentsline {section}{\numberline {1.}Introduction}{38}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces A montage of the morphological sequence from late-O super{\discretionary {-}{}{}}giants to WNL stars around 1$\mu $m (CTIO--IRS observations).}}{39}}
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\@writefile{toc}{\contentsline {section}{\numberline {2.}Observations}{39}}
\@writefile{toc}{\contentsline {section}{\numberline {3.}Analysis}{40}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces Synthetic fits (dotted lines, Model\nobreakspace  {}K) to near-IR CTIO--IRS spectra for HD\nobreakspace  {}152408 (O8:\,Iafpe, solid lines). He\,{\sc  ii} 3.09$\mu $m provides an important temperature diagnostic for WNL stars in heavily reddened environments since it is unblended and is much stronger than He\,{\sc  ii} 2.1885$\mu $m. The P$\beta $ synthetic profile is in excellent agreement with ESO--IRSPEC observations of HD\,152408 by Najarro (1996, personal communication).}}{41}}
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\@writefile{lot}{\contentsline {table}{\numberline {1}{\ignorespaces }}{42}}
\newlabel{table1}{{1}{42}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces  Line profiles (solid lines) calculated from blanketed model atmospheres reproduce He\,{\sc  i} 2.0581$\mu $m observations (dotted lines) for WN9h stars -- NS4 in our Galaxy and BE381 in the LMC -- where profiles from unblanketed models, assuming identical stellar parameters, were discrepant (Crowther et al. 1995a, Bohannan \& Crowther 1998).}}{43}}
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\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces Ground-based UKIRT/CGS4 observations of HD\nobreakspace  {}177230 (WR123, WN8) showing the prominent He\,{\sc  ii} 3.09-$\mu $m emission feature.}}{44}}
\newlabel{fig3}{{4}{44}}
\@writefile{lot}{\contentsline {table}{\numberline {2}{\ignorespaces A comparison between observed nebular-flux ratios (H$\beta $=100) in M1--67 (Esteban et\nobreakspace  {}al.\ 1993) and those predicted by photo{\discretionary {-}{}{}}ionization models of the central star 209\,BAC (WN8), using both unblanketed and blanketed flux distributions with parameters ($T_{\ast }$=33kK, log\,$L/L_{\odot }$=5.4) obtained by Crowther et\nobreakspace  {}al.\ (1995b). Observed nebular abundances and densities ($n_{\rm  e}$=1050 cm$^{-3}$) are fed into calculations.}}{44}}
\newlabel{table2}{{2}{44}}
\@writefile{toc}{\contentsline {section}{\numberline {4.}H\,{\relax \fontsize  {9}{11}\normalfont  \abovedisplayskip 8\p@ plus2\p@ minus4\p@ \abovedisplayshortskip \z@ plus\p@ \belowdisplayshortskip 4\p@ plus2\p@ minus2\p@ \def \leftmargin \leftmargini \parsep 4.5\p@ plus2\p@ minus\p@ \topsep 9\p@ plus3\p@ minus5\p@ \itemsep 4.5\p@ plus2\p@ minus\p@ {\leftmargin \leftmargini \topsep 4\p@ plus2\p@ minus2\p@ \parsep 2\p@ plus\p@ minus\p@ \itemsep \parsep }\belowdisplayskip \abovedisplayskip {\bf  II}} Regions as Probes of EUV Fluxes in Early-Type Stars}{44}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces Comparison between unblanketed (dotted) and blanketed (solid) flux distributions for 209\,BAC (WR124, WN8) using stellar parameters obtained by Crowther et\nobreakspace  {}al.\ (1995b), together with an indication of various important ionization edges.}}{45}}
\newlabel{fig4}{{5}{45}}
\@writefile{toc}{\contentsline {paragraph}{\relax Acknowledgments.}{45}}