By Peter S. Conti (auth.), C. Chiosi, R. Stalio (eds.)

The IAU Colloquium No. fifty nine, "The results of mass loss on Stellar Evolution" used to be hung on September 15-19, 1980 on the foreign Centre for Theoretical Physics, Miramare, Trieste (Italy), lower than the auspices of the IAU govt Co~ mittee and the Italian nationwide Council of analysis. The making plans of this convention begun years in the past du­ ring the IAU Symposium No. eighty three "Mass loss and evolution of zero variety stars" (Qualicum seashore, Victoria, Canada) after we felt that mass loss and its results at the evolution of stars used to be too large an issue for being restrained to zero variety stars simply. accordingly we concept convention facing the final challenge of mass loss around the complete HR diagram might were of curiosity to every person operating within the box. the most notion used to be that bringing jointly Astronomers and Astrophysicists of the widest diversity of pursuits and e~ pertize - all ultimately with regards to the matter of mass loss from stars - could have spurred thorough discussions at the many facets and implications of this subject. we are hoping this objective has been completed. in addition, the newest observational and theoreti­ cal advancements at the challenge of mass loss from early ty­ pe stars kept away from this assembly to be an easy updating of the Qualicum seashore Symposium so far as this factor is concerned.

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However, HM Sge does not display a H/He anomaly that is inherent in WR-stars. The solution of the HM Sge' s eni,gma may be the following. We are observing the WR-star birth when an emitting gas is not yet the outflowed layers of a stellar atmosphere of a hydrogen depleted composition but a placenta nebula of a WR-star; this young star of hi,gh luminosity excites and drives the gas of the placenta nebula. During three years we observe the systematic increase in the excitation level of the HM Sge spectrum.

For example, in 9 Sgr, the radio rate gives a number similar to that for "strongest" or stars, yet there is no optical emission; similarly for most Of stars the major UV P Cygni lines are saturated but they are not in 9 Sgr. If the radio detection is not spurious we would have to conclude that some of our understanding of stellar winds is incomplete perhaps the spherical symmetry or homogeneity assumptions are not valid in all cases. VANBEVEREN: If one determines the M from spectral analysis (UV or Ha) one assumes that the star has a solar abundance.

If the radio detection is not spurious we would have to conclude that some of our understanding of stellar winds is incomplete perhaps the spherical symmetry or homogeneity assumptions are not valid in all cases. VANBEVEREN: If one determines the M from spectral analysis (UV or Ha) one assumes that the star has a solar abundance. However one only has to remove some 20% to 30% of the stellar mass in order to see layers that were originally in the convective hydrogen burning core. Computations reveal that these layers have the equilibrium CNO abundances Which are very different from the solar ones.

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