The purpose of this book is to give a detailed description of the planetary nebulae including the relevant astronomical observations and their interpretation. Considerable attention is given to the evolution of these objects as well as to their physical characteristics. I t is hoped that the book be useful to both advanced research workers and to students with some background in astronomy. In this regard, the book should serve as a text as well as a reference work. The many tables included are expected to be useful for both purposes. The references are generally not included in the text except…mehr
The purpose of this book is to give a detailed description of the planetary nebulae including the relevant astronomical observations and their interpretation. Considerable attention is given to the evolution of these objects as well as to their physical characteristics. I t is hoped that the book be useful to both advanced research workers and to students with some background in astronomy. In this regard, the book should serve as a text as well as a reference work. The many tables included are expected to be useful for both purposes. The references are generally not included in the text except for historical purposes in an effort to improve readability. References are given at the end of each chapter together with sufficient text to describe their content. No attempt has been made to make the list of references complete; on the contrary it has generally been limited to the most recent literature on the subject which in turn refers to earlier research. Again, exceptions have been made for references of historical interest.Hinweis: Dieser Artikel kann nur an eine deutsche Lieferadresse ausgeliefert werden.
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.
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.
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