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Record Nr. |
UNINA9910143706703321 |
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Autore |
Salaris Maurizio |
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Titolo |
Evolution of stars and stellar populations / / Maurizio Salaris, Santi Cassisi |
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Pubbl/distr/stampa |
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West Sussex, England : , : John Wiley & Sons Ltd, , [2005] |
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©2005 |
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ISBN |
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1-280-28769-1 |
9786610287697 |
0-470-03345-2 |
0-470-09222-X |
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Descrizione fisica |
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1 online resource (388 p.) |
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Disciplina |
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Soggetti |
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Stars - Evolution |
Electronic books. |
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Lingua di pubblicazione |
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Formato |
Materiale a stampa |
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Livello bibliografico |
Monografia |
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Note generali |
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Description based upon print version of record. |
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Nota di bibliografia |
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Includes bibliographical references and index. |
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Nota di contenuto |
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Evolution of Stars and Stellar Populations; Contents; Preface; 1 Stars and the Universe; 1.1 Setting the stage; 1.2 Cosmic kinematics; 1.2.1 Cosmological redshifts and distances; 1.3 Cosmic dynamics; 1.3.1 Histories of R(t); 1.4 Particle- and nucleosynthesis; 1.5 CMB fluctuations and structure formation; 1.6 Cosmological parameters; 1.7 The inflationary paradigm; 1.8 The role of stellar evolution; 2 Equation of State of the Stellar Matter; 2.1 Physical conditions of the stellar matter; 2.1.1 Fully ionized perfect gas; 2.1.2 Electron degeneracy; 2.1.3 Ionization; 2.1.4 Additional effects |
3 Equations of Stellar Structure3.1 Basic assumptions; 3.1.1 Continuity of mass; 3.1.2 Hydrostatic equilibrium; 3.1.3 Conservation of energy; 3.1.4 Energy transport; 3.1.5 The opacity of stellar matter; 3.1.6 Energy generation coefficient; 3.1.7 Evolution of chemical element abundances; 3.1.8 Virial theorem; 3.1.9 Virial theorem and electron degeneracy; 3.2 Method of solution of the stellar structure equations; 3.2.1 Sensitivity of the solution to the boundary conditions; 3.2.2 More complicated cases; 3.3 Non-standard physical processes; 3.3.1 Atomic diffusion and radiative levitation |
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3.3.2 Rotation and rotational mixings4 Star Formation and Early Evolution; 4.1 Overall picture of stellar evolution; 4.2 Star formation; 4.3 Evolution along the Hayashi track; 4.3.1 Basic properties of homogeneous, fully convective stars; 4.3.2 Evolution until hydrogen burning ignition; 5 The Hydrogen Burning Phase; 5.1 Overview; 5.2 The nuclear reactions; 5.2.1 The p-p chain; 5.2.2 The CNO cycle; 5.2.3 The secondary elements: the case of (2)H and (3)He; 5.3 The central H-burning phase in low main sequence (LMS) stars; 5.3.1 The Sun |
5.4 The central H-burning phase in upper main sequence (UMS) stars5.5 The dependence of MS tracks on chemical composition and convection efficiency; 5.6 Very low-mass stars; 5.7 The mass-luminosity relation; 5.8 The Schönberg-Chandrasekhar limit; 5.9 Post-MS evolution; 5.9.1 Intermediate-mass and massive stars; 5.9.2 Low-mass stars; 5.9.3 The helium flash; 5.10 Dependence of the main RGB features on physical and chemical parameters; 5.10.1 The location of the RGB in the H-R diagram; 5.10.2 The RGB bump luminosity; 5.10.3 The luminosity of the tip of the RGB |
5.11 Evolutionary properties of very metal-poor stars6 The Helium Burning Phase; 6.1 Introduction; 6.2 The nuclear reactions; 6.3 The zero age horizontal branch (ZAHB); 6.3.1 The dependence of the ZAHB on various physical parameters; 6.4 The core He-burning phase in low-mass stars; 6.4.1 Mixing processes; 6.5 The central He-burning phase in more massive stars; 6.5.1 The dependence of the blue loop on various physical parameters; 6.6 Pulsational properties of core He-burning stars; 6.6.1 The RR Lyrae variables; 6.6.2 The classical Cepheid variables; 7 The Advanced Evolutionary Phases |
7.1 Introduction |
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Sommario/riassunto |
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Evolution of Stars and Stellar Populations is a comprehensive presentation of the theory of stellar evolution and its application to the study of stellar populations in galaxies. Taking a unique approach to the subject, this self-contained text introduces first the theory of stellar evolution in a clear and accessible manner, with particular emphasis placed on explaining the evolution with time of observable stellar properties, such as luminosities and surface chemical abundances. This is followed by a detailed presentation and discussion of a broad range of related techniques, that are widely |
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