MHD waves in the solar atmosphere /
Develops a fresh mathematical approach to coronal seismology, explaining oscillatory phenomena by drawing upon original research and complex modelling techniques.
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| Formato: | Licensed eBooks |
| Idioma: | inglês |
| Publicado em: |
Cambridge ; New York, NY :
Cambridge University Press,
2019.
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| Acesso em linha: | https://search.ebscohost.com/login.aspx?direct=true&scope=site&db=nlebk&AN=2172636 |
Sumário:
- Cover; Half-title; Title page; Copyright information; Dedication; Contents; Preface; 1 General Principles; 1.1 Introduction; 1.2 A Variety of Plasmas; 1.2.1 The Sun; 1.3 The Magnetohydrodynamic Equations; 1.4 Some Properties of the MHD Equations; 1.4.1 Fundamental Speeds; 1.4.2 Magnetic Flux Tubes; 1.4.3 The Induction Equation; 1.4.4 Diffusion of Magnetic Field (R[sub(m)]> 1); 1.4.6 The j x B Force; 1.4.7 Energetics; 1.5 Aspects of Wave Propagation; 1.5.1 Linearization; 1.5.2 Fourier Representation
- 1.5.3 Dispersion Relations, Phase Speed and Group Velocity2 Waves in a Uniform Medium; 2.1 Introduction; 2.2 Wave Equations; 2.3 Plane Waves; 2.4 Sound Waves; 2.5 Magnetohydrodynamic Waves; 2.6 Alfvén Waves; 2.6.1 Phase Speed and Group Velocity; 2.6.2 Perturbations in an Alfvén Wave; 2.7 Magnetoacoustic Waves; 2.7.1 Dispersion Relation; 2.7.2 Phase Speed Diagrams; 2.7.3 Group Velocity of Magnetoacoustic Waves; 2.7.4 Perturbations in the Magnetoacoustic Waves; 2.8 Magnetoacoustic Waves: The Special Case c[sub(A)] = c[sub(s)]; 2.9 Two Physical Extremes; 2.9.1 The Incompressible Fluid