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Stellar Astrophysics for the Local Group
A review of the new subject of extragalactic stellar astrophysics - for both graduate students and researchers working in astrophysics.
Luminous Stars and Associations in Galaxies
Proceedings of the 116th Symposium of the International Astronomical Union, held at Porto Heli, Greece, May 26-31, 1985
Groups of Galaxies in the Nearby Universe
For every galaxy in the field or in clusters, there are about three galaxies in groups. The Milky Way itself resides in a group. Groups in the local universe offer the chance to study galaxies in environments characterized by strong interactions. In the cosmological context, groups trace large-scale structures better than clusters; the evolution of groups and clusters appears to be related. All these aspects of research are summarized in this book.
Wolf-Rayet Stars: Observations, Physics, Evolution
Proceedings of IAU Symposium No. 99, held at Cozumel, Mexico, September 18-22, 1981
Mass Loss and Evolution of O-Type Stars
The organization of this Symposium had its beginnings at the International Astronomical Union General Assembly in Grenoble in 1976. The initial "rounding up" of the Scienti fic Organizing Committee was begun by Drs. Snow and Swings; most of us who became the eventual organizing committee met a few times during the Assembly and formulated the essential outlines of the meeting. Extensive correspondence with all the committee subsequently established the program. The idea was to bring together both observers and theoreticians to discuss the stellar winds and mass loss rates and their effects on evolutions of O-type stars. On the observational side, there are now spectroscopic data from the far UV to the near IR regions concerning the stellar winds. There is also information about the free-free emission in the wind from the IR and radio portions of the spectrum. Fortunately, these different detection methods give more or less the same mass loss rate for the one star, s Pup" which has been observed at all wavelengths. One of the intents of the first three sessions of this Symposium is to outline the eXisting data on mass loss rates as it per tains to the O-type stars.
Stellar Populations
The concept of Stellar Populations has played a fundamental role in astronomy in the last few decades. It was introduced by Walter Baade after he was able to resolve the Andromeda Nebula and its companions into stars when he used red-sensitive plates and realised that there were two fundamentally different Herzsprung-Russell diagrams in our and these nearby galaxies (common stars in the solar neighborhood versus globular clusters). This result was published in two papers in 1944 in volume 100 of the Astrophysical Journal. Subsequent research gave the concept a much firmer basis and at the famous Vatican Symposium of 1957 resulted in a general scheme of the concept and a working hypothesis fo...
Globular Clusters
An accessible introduction to globular clusters for graduate students, and a comprehensive and up-to-date reference for researchers.
Evolution of Massive Stars
Massive stars occupy an exceptional place in general astrophysics. They trigger many if not all of the important processes in galactic evolution whereas due to their intrinsic brightness, they offer the (only until now) possibility to study the stellar content and stellar behaviour in distant galaxies. The last, say, 25 years, massive stars have been the subject of numerous meetings discussing the influence of massive stars on population synthesis, the number distribution of different types of massive stars, the LBV phenomenon, WR stars, X-ray binaries, stellar winds in massive stars, chemical pecularities in massive stars, supernova explosions of massive stars and the important SN1987A even...
Convection in Astrophysics (IAU S239)
Convection is ubiquitous throughout the Universe, and during the last three decades it has become the largest factor of uncertainty in theoretical models of stars and in the interpretation of observations on the basis of such models. Recently, numerical simulations of convection have dramatically improved in their potential to take into account both the large scale properties of the flow itself and the microphysical properties of the fluid. Observations have become accurate enough to provide stringent tests for both numerical simulations and models of convection. IAU S239 was held to further understanding of convection, bringing together leading researchers in solar and stellar physics, the physics of planets, and of accretion disks. With reviews, research contributions, and detailed recordings of plenary discussions, this book is a valuable resource for professional astronomers and graduate students interested in the interdisciplinary study of one of the key physical processes in astrophysics.
