Titlebook: Birth and Evolution of Massive Stars and Stellar Groups; Proceedings of a Sym Wilfried Boland,Hugo Woerden Conference proceedings 1985 D. R

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Abbau des Wassers. Der Wasserstoff,ith other investigations. Along the entire main sequence (O-K5) close binaries appear to form with nearly circular orbits. When the orbital dimensions are close to the stellar dimensions complete circularization takes place.

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Die Lehre von den Atomen und Molekeln,e determination of ages of the associations and their subgroups by means of isochrone fitting are investigated. The influence of stellar rotation and undetected duplicity is discussed. Future work on the stellar content of the nearby OB-associations is suggested, in connection with the . mission.

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,Das Gesetz der festen Gewichtsverh?ltnisse,WR + 0) are, at the explosion of their initially more massive component, expected to produce runaway 0? stars with velocities typically in the range 30 to 90 km/s, and in a few cases > 100 km/s..At somewhat lower masses, ~ 9–30 M., also relatively wide binaries (ζ Aurigae type), with little mass tra

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Abbau des Wassers. Der Wasserstoff,tific career. His own contributions to that history include supernova explosions in close binary systems as an origin for runaway OB stars (most pulsars are also high-velocity objects), and studies of expanding stellar associations that have prompted explanations in terms of supernovae. Of the more

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Abbau des Wassers. Der Wasserstoff,ir rate of occurrence and theoretical considerations on stellar evolution (the latter only for type II supernovae). The pre-explosion masses are derived from the lightcurves (types II and V) and from the absolute magnitude before the explosion (only for type V’s). We find mass ranges of 6 to 16 M.,

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https://doi.org/10.1007/978-94-009-5478-6Galaxy; astronomy; star; stars; stellar

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Birth and Evolution of Massive Stars and Stellar Groups978-94-009-5478-6Series ISSN 0067-0057 Series E-ISSN 2214-7985

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Lehrbuch der Chemie für H?here Lehranstalteno the few hundredths of a parsec structure observed in dense cloud cores. Explanations of both the temporal and spatial progress of star formation are reviewed, and factors which may dominate the process on all scales are considered.