Planetary Nebulae - Stuart R. Pottasch

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Sommaire:
I: History, Morphology and Evolution.- A Historical Review.- II: Distribution of Planetary Nebulae in the Galaxy.- A. Methods of discovering planetary nebulae.- B. Distribution in galactic coordinates.- C. Radial velocities of the nebulae.- D. Extragalactic planetary nebulae.- III: Interpretation of Emission Lines and Nebular Abundances.- A. Recombination lines.- B. Collisionally excited lines.- C. Line formation in heavier elements by other processes.- D. Nebular models.- E. Abundances in planetary nebulae.- IV: Nebular Continuum Emission.- A.Sources of continuum emission.- B. Comparison of theory with observations.- C. Separation of continuum radiation from the nebula and the exciting star.- D. Radio continuum radiation.- E. Comparison of radio continuum with hydrogen line emission.- V: Distance to the Nebulae.- A. Extinction.- B. Distances to individual nebulae.- C. Mass of the nebula.- D. Statistical methods for determining distances.- E. Absolute nebular flux.- F. The space density of nearby nebulae and their distribution with height above the galactic plane.- VI: Morphology, Expansion and Mass Loss.- A. Morphology: measurements.- B. Nebular expansion.- C. Morphology: models and classification.- D. Morphology: 'halo' structures.- E. Morphology: four individual cases.- F. Mass loss from the central star: ultraviolet lines.- G. Other evidence for mass loss: visual lines.- VII: The Temperature of the Central Stars.- A. The line spectra.- B. The continuous spectrum of the central star.- C. Model atmospheres.- D. 'Zanstra' temperatures.- E. 'Stoy' temperatures.- F. Temperatures derived from nebular ionization equilibrium.- VIII: Infrared and Millimeter Radiation.- A. Infrared continuous emission.- B. Interpretation as dust emission.- C. Energy input to thedust.- D. Consequences for the central star temperature determination.- E. Broad and narrow infrared emission features.- F. Molecular hydrogen.- G. Carbon monoxide emission.- IX: Evolution of the Central Star.- A. Observational evidence.- B. Theoretical models.- C. Comparison of theory and observation.- X: Evolution from Red Giant to Planetary Nebula.- A. The cool giants.- B. The Mira variables.- C. The OH/IR masers.- D. Protoplanetary nebulae and symbiotic stars.- E. FG Sge and its nebula.- F. Discussion of the evolution.- XI: Influence of Planetary Nebulae on the Interstellar Medium.- A. The mass input.- B. The dust input.- C. Kinetic energy input.- D. Element abundance changes.- E. The far-ultraviolet radiation field.- Appendix I: Positions and other Information of the Brightest Planetary Nebulae and Their Central Stars.- Appendix II: Infrared Continuum Flux from Planetary Nebulae.- Author Index.- Index of Individual Objects.