Dynamics and Structure of Quiescent Solar Prominences

1 Introduction to Quiescent Solar Prominences (E R Priest).- 1.1 Basic Description.- 1.1.1 Different Types.- 1.1.2 Properties.- 1.1.3 Development.- 1.1.4 Structure.- 1.1.5 Eruption.- 1.2 Basic Equations of MHD.- 1.2.1 Magnetohydrostatics.- 1.2.2 Waves.- 1.2.3 Instabilities.- 1.3 Prominence Puzzles.- 2 Overall Properties and Steady Flows (B Schmieder).- 2.1 Basic Properties.- 2.1.1 Description and Classification.- 2.1.2 Fine Structure in H?.- 2.1.3 Evolution of Filaments During the Solar Cycle.- 2.2 Physical Characteristics: Density and Temperature.- 2.2.1 Density and Ionization Degree.- 2.2.2 Non LTE Models.- 2.2.3 Turbulent Velocity and Electron Temperature.- 2.3 Velocity Field and Mass Flux.- 2.3.1 Instrumentation.- 2.3.2 H? Profile Analysis.- 2.3.3 Vertical Motions.- 2.3.4 Horizontal Motions.- 2.3.5 Oscillations.- 2.4 Instability.- 2.4.1 Disparition Brusque of Filaments.- 2.4.2 Model Support.- 2.4.3 Post-Flare Loops and Loop Prominences.- 2.5 Conclusion.- 3 Prominence Environment (O Engvold).- 3.1 Introduction.- 3.2 Helmet Streamers.- 3.2.1 Eclipse Photography.- 3.2.2 Morphology.- 3.2.3 Location of Current Sheet.- 3.2.4 Brightness.- 3.3 Coronal Cavities.- 3.3.1 Brightness and Structure.- 3.3.2 Temperature and Density.- 3.4 Filament Channels.- 3.4.1 Association with Neutral Lines.- 3.4.2 Poleward Migration of Filament Channels.- 3.4.3 Presence of Prominences.- 3.4.4 Temperature and Electron Pressure.- 3.4.5 Cool Matter in the Filament Channels.- 3.5 Prominence-Corona Transition Region.- 3.5.1 Line Emission.- 3.5.2 Empirical Modelling.- 3.5.3 A Fragmented and Dynamic Transition Region.- 3.6 Prominences and Environment.- 3.6.1 Magnetic Fields and Chromospheric Structure.- 3.6.2 Association with Supergranulation Network.- 3.6.3 Dynamics.- 3.6.4 The Mass of Coronal Cavity and Prominence.- 3.6.5 Coronal Voids - a Source of Prominence Mass?.- 3.7 Modelling of the Helmet Streamer/Prominence Complex.- 3.7.1 Helmet Streamer and Cavity.- 3.7.2 Magnetic Field Topology.- 3.7.3 Siphon-Type Models.- 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.- 4.2.1 Zeeman Effect.- 4.2.2 HanleEffect.- 4.2.3 180 Ambiguity.- 4.2.4 Instrumental Achievements.- 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.- 4.5.1 Field Strength.- 4.5.2 Angle with Horizontal.- 4.5.3 Angle with Prominence Axis.- 4.5.4 Magnetic Structure with Normal or Inverse Polarity.- 4.5.5 Homogeneity of the Field.- 4.6 Some Important Problems.- 4.6.1 Magnetic Field in Sub Arc Second Structures.- 4.6.2 Paradox of Fine Vertical Structures.- 4.6.3 Determination of Currents.- 4.6.4 Evolution of Prominence Magnetic Structure.- 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.- 5.3.1 Radiative Thermal Instability.- 5.3.2 Resistive Instabilities.- 5.4 Steady Reconnection in Current Sheets.- 5.4.1 Incompressible and Compressible Theories.- 5.4.2 Unification of Different Regimes.- 5.5 Static Models.- 5.5.1 Condensation in a Loop.- 5.5.2 Condensation in an Arcade.- 5.5.3 Condensation in a Sheared Magnetic Field.- 5.5.4 Condensation in a Current Sheet.- 5.6 Dynamic Models: Injection from the Chromosphere into Closed Loops.- 5.6.1 Surge-Like Models.- 5.6.2 Evaporation Models.- 5.7 Dynamic Models: Condensation in Coronal Current Sheets.- 5.7.1 Numerical Simulations.- 5.7.2 Role of Shock Waves in Condensation Process.- 5.8 Unsolved Problems.- 5.9 Conclusion.- 6 Structure and Equilibrium of Prominences (U Anzer).- 6.1 Introduction.- 6.2 Prominence Models.- 6.2.1 Global Structure.- 6.2.1.1 Two-Dimensional Equilibria.- 6.2.1.1.1 Models with Normal Magnetic Polarity.- 6.2.1.1.2 Models with Inverse Magnetic Polarity.- 6.2.1.1.3 Force-Free Fields.- 6.2.1.2 Quasi-Three-Dimensional Models.- 6.2.1.3 Support by Alfven Waves.- 6.2.2 Internal Structure and Thermal Equilibrium.- 6.2.2.1 Hydrostatic Equilibrium.- 6.2.2.2 Thermal Equilibrium.- 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.- 7.3.1 Normal Modes.- 7.3.2 Energy Method.- 7.3.3 Non Equilibrium.- 7.4 Effect of the Dense Photosphere.- 7.4.1 Physical Arguments.- 7.4.2 Ballooning Modes.- 7.5 Coronal Arcades.- 7.5.1 Distributed Current Models - Eruptive Instability.- 7.5.2 Localised Modes - Small Scale Structure.- 7.5.3 Arcades Containing a Current Sheet.- 7.6 Thermal Stability.- 7.7 Resistive Instabilities - Tearing Modes.- 7.7.1 Introduction.- 7.7.2 Estimate of Tearing Mode Growth Rate.- 7.7.3 Effect of Line Tying.- 7.8 Simple Model of Prominence Eruption and a Coronal Mass Ejection.- 7.9 Conclusions and Future Work.- References.