LEADER 05510nam 22006135 450 001 9910813432303321 005 20240313131416.0 010 $a3-642-61523-6 024 7 $a10.1007/978-3-642-61523-8 035 $a(CKB)3400000000105287 035 $a(SSID)ssj0000808639 035 $a(PQKBManifestationID)11401193 035 $a(PQKBTitleCode)TC0000808639 035 $a(PQKBWorkID)10778989 035 $a(PQKB)10217964 035 $a(DE-He213)978-3-642-61523-8 035 $a(MiAaPQ)EBC3092371 035 $a(PPN)238028771 035 $a(EXLCZ)993400000000105287 100 $a20121227d1990 u| 0 101 0 $aeng 135 $aurnn#008mamaa 181 $ctxt 182 $cc 183 $acr 200 10$aStellar Structure and Evolution$b[electronic resource] /$fby Rudolf Kippenhahn, Alfred Weigert 205 $a1st ed. 1990. 210 1$aBerlin, Heidelberg :$cSpringer Berlin Heidelberg :$cImprint: Springer,$d1990. 215 $a1 online resource (XVI, 468 p. 7 illus.) 225 1 $aAstronomy and Astrophysics Library,$x0941-7834 300 $aBibliographic Level Mode of Issuance: Monograph 311 $a3-540-50211-4 311 $a3-540-58013-1 320 $aIncludes bibliographical references and index. 327 $aI The Basic Equations -- 1. Coordinates, Mass Distribution, and Gravitational Field in Spherical Stars -- 2. Conservation of Momentum -- 3. The Virial Theorem -- 4. Conservation of Energy -- 5. Transport of Energy by Radiation and Conduction -- 6. Stability Against Local, Non-spherical Perturbations -- 7. Transport of Energy by Convection -- 8. The Chemical Composition -- II The Overall Problem -- 9. The Differential Equations of Stellar Evolution -- 10. Boundary Conditions -- 11. Numerical Procedure -- 12. Existence and Uniqueness of Solutions -- III Properties of Stellar Matter -- 13. The Ideal Gas with Radiation -- 14. Ionization -- 15. The Degenerate Electron Gas -- 16. The Equation of State of Stellar Matter -- 17. Opacity -- 18. Nuclear Energy Production -- IV Simple Stellar Models -- 19. Polytropic Gaseous Spheres -- 20. Homology Relations -- 21. Simple Models in the U-V Plane -- 22. The Main Sequence -- 23. Other Main Sequences -- 24. The Hayashi Line -- 25. Stability Considerations -- V Early Stellar Evolution -- 26. The Onset of Star Formation -- 27. The Formation of Protostars -- 28. Pre-Main-Sequence Contraction -- 29. From the Initial to the Present Sun -- 30. Chemical Evolution on the Main Sequence -- VI Post-Main-Sequence Evolution -- 31. Evolution Through Helium Burning ? Massive Stars -- 32. Evolution Through Helium Burning ? Low-Mass Stars -- 33. Later Phases -- 34. Final Explosions and Collapse -- VII Compact Objects -- 35. White Dwarfs -- 36. Neutron Stars -- 37. Black Holes -- VIII Pulsating Stars -- 38. Adiabatic Spherical Pulsations -- 39. Non-adiabatic Spherical Pulsations -- 40. Non-radial Stellar Oscillations -- IX Stellar Rotation -- 41. The Mechanics of Rotating Stellar Models -- 42. The Thermodynamics of Rotating Stellar Models -- 43. The Angular-Velocity Distribution in Stars -- References. 330 $aThe attempt to understand the physics of the structure of stars and their change in time - their evolution - has been bothering many physicists and astronomers ever since the last century. This long chain of successful research is well documented not only by numerous papers in the corresponding journals but also by a series of books. Some of them are so excellently written that despite their age they can still be recommended, and not only as documents of the state of the art at that time. A few outstanding examples are the books of R. Emden (1907), A. S. Eddington (1926), S. Chandrasekhar (1939), and M. Schwarzschild (1958). But our science has rapidly expanded in the last few decades, and new aspects have emerged which could not even be anticipated, say, 30 years ago and which today have to be carefully explored. This does not mean, however, that our ambition is to present a complete account of the latest and most refined numerical results. This can well be left to the large and growing number of excellent review articles. The present book is intended rather to be a textbook that will help students and teachers to understand these results as far as possible and present them in a simple and clear manner. We know how difficult this is since we ourselves have tried for the largest part of our scientific career to understand "how the stars work" - and then to make others believe it. 410 0$aAstronomy and Astrophysics Library,$x0941-7834 606 $aObservations, Astronomical 606 $aAstronomy?Observations 606 $aAstrophysics 606 $aAstronomy, Observations and Techniques$3https://scigraph.springernature.com/ontologies/product-market-codes/P22014 606 $aAstrophysics and Astroparticles$3https://scigraph.springernature.com/ontologies/product-market-codes/P22022 615 0$aObservations, Astronomical. 615 0$aAstronomy?Observations. 615 0$aAstrophysics. 615 14$aAstronomy, Observations and Techniques. 615 24$aAstrophysics and Astroparticles. 676 $a523.8 700 $aKippenhahn$b Rudolf$4aut$4http://id.loc.gov/vocabulary/relators/aut$0754841 702 $aWeigert$b Alfred$4aut$4http://id.loc.gov/vocabulary/relators/aut 906 $aBOOK 912 $a9910813432303321 996 $aStellar structure and evolution$91519098 997 $aUNINA