  An eclipsing binary with an orbital period of 62 days has been discovered in
HD 328058 and studied by UBVIcHalpha photometry. Combining the results of light
curve modelling with existing stellar models and known B3-shell spectral type
of the primary star then allowed a reliable estimation of the mass, radius and
effective temperature of both components: about 6.9 Msun, 5.2 Rsun and 17600 K
for the primary star, and about 0.78 Msun, 1.20 Rsun and 56000 K for the hot
subdwarf companion of type sdO. Obviously, this binary has been created by mass
transfer of the envelope of the sdO progenitor to our primary star, now being a
rapidly rotating shell star. Its spheroidal distortion and its decretion disk
can be studied here unusually well.
