Dynamics and Structure of Quiescent Solar Prominences

• 1 Introduction to Quiescent Solar Prominences (E R Priest).- 1.1 Basic Description.- 1.2 Basic Equations of MHD.- 1.3 Prominence Puzzles.- 2 Overall Properties and Steady Flows (B Schmieder).- 2.1 Basic Properties.- 2.2 Physical Characteristics: Density and Temperature.- 2.3 Velocity Field and Mass Flux.- 2.4 Instability.- 2.5 Conclusion.- 3 Prominence Environment (O Engvold).- 3.1 Introduction.- 3.2 Helmet Streamers.- 3.3 Coronal Cavities.- 3.4 Filament Channels.- 3.5 Prominence-Corona Transition Region.- 3.6 Prominences and Environment.- 3.7 Modelling of the Helmet Streamer/Prominence Complex.- 3.8 Conclusions.- 4 Observation of Prominence Magnetic Fields (J L Leroy).- 4.1 Historical Steps.- 4 2 Investigations Based on the Polarimetry of Spectral Lines.- 4.3 Indirect Magnetic Field Determinations.- 4.4 Magnetic Field at the Photospheric Level.- 4.5 Main Features of the Magnetic Field in Quiescent Prominences.- 4.6 Some Important Problems.- 5 The Formation of Solar Prominences (J M Malherbe).- 5.1 Introduction.- 5.2 Overview of Observations.- 5.3 Main MHD Instabilities Involved in Prominence Formation.- 5.4 Steady Reconnection in Current Sheets.- 5.5 Static Models.- 5.6 Dynamic Models: Injection from the Chromosphere into Closed Loops.- 5.7 Dynamic Models: Condensation in Coronal Current Sheets.- 5.8 Unsolved Problems.- 5.9 Conclusion.- 6 Structure and Equilibrium of Prominences (U Anzer).- 6.1 Introduction.- 6.2 Prominence Models.- 6.3 Concluding Remarks.- 7 Stability and Eruption of Prominences (A W Hood).- 7.1 Introduction.- 7.2 Description of MHD Instabilities.- 7.3 Methods of Solution.- 7.4 Effect of the Dense Photosphere.- 7.5 Coronal Arcades.- 7.6 Thermal Stability.- 7.7 Resistive Instabilities — Tearing Modes.- 7.8 Simple Model of Prominence Eruption and aCoronal Mass Ejection.- 7.9 Conclusions and Future Work.- References.

'This book is a wonderful contribution from the European solar physics community.' Space Sciences Review 61, 1992 'It certainly belongs in libraries or in the personal collection of a specialist.' American Scientist, 78