\documentstyle{preprint}
\begin{document}
\title{UV SPECTRAL MORPHOLOGY: THE LBV--Ofpe/WN9
CONNECTION\/\thanks{Based on observations with the NASA/ESA Hubble
Space Telescope, obtained at the Space Telescope Science Instiute, which
is operated by AURA for NASA under contract NAS5--26555.}}
\author{Anna Pasquali\\
\\
Space Telescope Science Institute\\
\\
3700 San Martin Drive\\
\\
Baltimore, MD  21218}

\pub{{\em the proceedings of}\\
~\\
Luminous Blue Variables: Massive Stars in Transition,\\
~\\
{\em held 6--10 October 1996 in Kona, Hawaii}}

\maketitle

\abstract{IUE and HST observations have greatly improved our knowledge
of the UV spectral domain of massive stars.  The data show that the
spectral types derived from the 1200--2000~\AA\ range agree well with
those determined from the optical spectrum for all the {\it normal\/}
stars. Nevertheless, in the case of {\it LBVs\/} the picture becomes more
intricate.  For example, in AG~Carinae the UV and optical spectral types
disagree at minimum, being B and Ofpe/WN9 respectively.  Wind asymmetry
could be a plausible reason, implying that an equatorial density
enhancement may ``mimic'' a hotter spectral type like Ofpe/WN9.  It also
seems that such a spectral discrepancy did not occur in P~Cygni and
HR~Carinae, which have long displayed a B~spectral type in both UV and
optical ranges.  The example of AG~Carinae indicates how significantly
spectral morphology may relate to stellar wind geometry.  The comparison
between the UV and optical spectral types of LBVs has linked them to the
class of {\it Ofpe/WN9\/} stars, and suggested Ofpe/WN9 stars be
quiescent LBVs. We discuss the stellar parameters and the evolutionary
status of a sample of Ofpe/WN9 stars in the LMC, in order to indirectly
trace the evolutionary path of LBVs.}

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