Helium burning stars with masses between 10 Mo and 40 Mo are evolved up to core helium exhaustion including mass loss by stellar wind at rates between 10-5 Mo/yr and 10-4 Mo/yr appropriate for WR stars. Different M formalisms were used. It should however be noted that the results presented here are only marginally dependent on this formalism. The initial models contain a small hydrogen shell. The atmospherical hydrogen abundance Xatm = 0.2-0.3. These models correspond to primary remnants (with hydrogen ZAMS masses between 30 M0 and 100 M0) after a case B mode of mass transfer in close binaries, or to stars after a red giant phase of huge mass loss comparable to late case B remnants after Roche lobe overflow. Evolutionary details can be found elsewhere (Vanbeveren, D., Ph.D. Thesis, Vrije Universiteit Brussel) and will not be discussed here. I want to focus on two applications