Icko IbenCambridge University PressEdition: Illustrated, 11/29/2012EAN 9781107016569, ISBN10: 1107016568Hardcover, 906 pages, 25.1 x 19.3 x 4.3 cmLanguage: EnglishOriginally published in EnglishThis text describes the microscopic physics operating in stars and demonstrates how stars respond from formation, through hydrogen-burning phases, up to the onset of helium burning. Intended for beginning graduate students and senior undergraduates with a solid background in physics, it illustrates the intricate interplay between the microscopic physical processes and the stars' macroscopic responses. The volume starts with the gravitationally contracting phase which carries the star from formation to the core hydrogen-burning main sequence, through the main sequence phase, through shell hydrogen-burning phases as a red giant, up to the onset of core helium burning. Particular emphasis is placed on describing the gravothermal responses of stars to nuclear transformations in the interior and energy loss from the surface, responses which express the very essence of stellar evolution. The volume is replete with many illustrations and detailed numerical solutions to prepare the reader to program and calculate evolutionary models.Part I. Introduction and Overview1. Qualitative description of single and binary star evolution2. Quantitative foundations of stellar evolution theoryPart II. Basic Physical Processes in Stellar Interiors3. Properties of and physical processes in the interiors of main sequence stars – order of magnitude estimates4. Statistical physics, thermodynamics, and equations of state5. Polytropes and single zone modelselementary tools for understanding some aspects of stellar structure and evolution6. Hydrogen-burning nuclear reactions and energy-generation rates7. Photon-matter interactions and opacity8. Equations of stellar evolution and methods of solutionPart III. Pre-Main Sequence, Main Sequence, and Shell Hydrogen Burning Evolution of Single Stars9. Star formation and evolution to the main-sequence10. Solar structure and neutrino physics11. Evolution during core hydrogen-burning phases up to the onset of helium burningIndex.
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