Titlebook: Highlights of Astronomy; As Presented at the Richard M. West (General Secretary of the Union) Book 1983 International Astronomical Union 1

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Active Galactic Nucleiet of these observations, in particular those which I believe are most likely to be important in elucidating those properties of the central energy source to which we attribute the origin of all high energy phenomena. I will therefore restrict my remarks to certain aspects of BL LAc objects, optical

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Mass Loss Phenomena on stellar evolution, which was sumed up in his book The internal Constitution of the Stars (ICS) which appeard in 1926. Although he did no substantial work on mass loss from stars, the possible of mass loss is mentioned in several places in ICS and I shll mention these and other aspects of Eddingt

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Joint Commission Meeting on UV and X-Ray Observations of Interacting Binary Systemsorer (IUE). A comaparison of low dispersion UV-spectra reveals important differences between the central ionized source and the jet feature. The UV-continum flux F. between 1200-2000A that rises with decreasing wavelegth in the jet feature, essentially is independent with wavelength in the central c

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Joint Commission Meeting on Beams and Jets in Extragalactic SourcesC273) and we do not know if they are manifestations of the same basic phenomenon or whether Nature is fooling us in some way despite the morphological similarities. For the moment, it seems sensible to asume an underlying unity and to use the observations to explore the jet phenomenon in different g

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The Origin and Early History of the Sun and the Planetary System in the Context of Stellar Evolutiont for that long, and hence circumstellar activity may still be in progress around some young stars in the solar vicinity. The observed time decay of axial rotation and surface activity in solar-type stars can be extended backwards, and indicates that the ultra-violet radiation of the young sun would

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Origin and Development of Solar Flaress that several hours after a large flare extended loop-like structures appear of fairly high temperature (> 6 MK), emitting a very faint X-ray flux. They are the basic structures of a more extended configuration, visible on metric radio waves, and pointing out from the area where the flare occurred.

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