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Spectral Line Shapes in Astrophysics and Related Topics
Spectral lines, widths, and shapes are powerful tools for emitting/absorbing gas diagnostics in different astrophysical objects (from the solar system to the most distant objects in the universe—quasars). On the other hand, experimental and theoretical investigations of laboratory plasma have been applied in spectroscopic astrophysical research, especially in research on atomic data needed for line shape calculations. Data on spectral lines and their profiles are also important for diagnostics, analysis, and the modelling of fusion plasma, laser-produced plasma, laser design and development, and various plasmas in industry and technology, like light sources based on plasmas or the welding ...
Spectral Line Shapes in Astrophysics
The VI Serbian Conference on Spectral Line Shapes in Astrophysics was about the investigation of spectral line shapes in extragalactic objects, such as, active galactic nuclei, stellar atmospheres, and astrophysical spectra in general. Atomic spectral line shapes in various discharges and plasma devices was also discussed. The main purpose of the Conference was to present and discuss new results found by participants working in this research field, and to review significant topics.
Pulsation, Rotation and Mass Loss in Early-Type Stars
In this Symposium, researchers specializing in pulsation, rotation, magnetic fields and stellar winds are brought together for the first time in order to broaden our understanding of O and B stars. Thanks to advances in digital spectroscopy, new types of pulsating B stars have been discovered. The pulsations can be understood in terms of the recent revision of metal opacities, but the effects of rapid rotation and magnetic fields need further study. Observations in the UV and X-ray regions demonstrate that many B and Be stars show other activity, besides pulsation which is not yet understood. The reason for the enhanced mass loss in Be stars is a question which dominates the Symposium and which remains unanswered, although it is surely to be found in activity at or near the photosphere coupled with rotation. It is shown that the geometry of the circumstellar envelopes around Be stars is indeed a flattened disk as they can now be optically resolved. The variability of radiatively-driven winds from O and B stars are likely related to the rotation of the star. This underlines the central theme of the book: that the various phenomena seen in these stars cannot be studied in isolation.
Sun and Planetary System
Proceedings of the Sixth European Regional Meeting in Astronomy, held in Dubrovnik, Yugoslavia, October 19-23, 1981
