Hasan Magnetic Coupling between the Interior and Atmosphere of the Sun

1. Auflage 2010
ISBN: 978-3-642-02859-5
Verlag: Springer
Format: PDF
Kopierschutz: Wasserzeichen (»Systemvoraussetzungen)

E-Book, Englisch, 538 Seiten

Solar physics in India has a tradition that can be traced to the setting up of the Kodaikanal Observatory in 1899 when the Madras Observatory was relocated to a high altitude site with a view to initiate observations of the sun. This conference on Magnetic Coupling between the Interior and the Atmosphere of the Sun during 2-5 December 2008 was planned to coincide with centenary of the Evershed effect discovery at Kodaikanal in 1909. The aim of this meeting was to bring to a critical focus a comprehensive - derstanding of the important issues pertaining to solar magnetism with particular emphasis on the various MHD processes that operate in the solar atmosphere. The current status of magnetic eld measurements and their implications in the light of recenttheoriesandnumericalmodelingthataddressthe fundamentalscalesandp- cessesinthehighlymagnetizedturbulentplasmawerereviewedduringthismeeting. The meeting was timely for the following reasons: Space observations such as from SOHO and TRACE have provided a wealth of multiwavelength observations onprocessesoccurringinregionsofthe atmosphereextendingfromthe photosphere up to the outer corona. With the launch of Hinode and STEREO in 2006 and of SDO (Solar Dynamics Observatory) shortly, this conference provided a platform for in-depth discussions on new results from various space missions as well as a comparison with ground-based observing facilities such as the Swedish 1-m Solar Telescope. Using sophisticated image processing techniques, such telescopes r- tinelygenerateobservationswitharesolutionbetterthan0. 1arcsec,therebyyielding more informative diagnostics for instance of the microstructure of ux tubes.

Autoren/Hrsg.

Hasan, Siraj

Inhaltsverzeichnis

1;Preface;5
2;Contents;7
3;Part I Preamble;24
3.1;Republication of: Radial Movement in Sunspots;25
3.2;Opening Remarks;33
3.3;Solar Physics at the Kodaikanal Observatory: A Historical Perspective;35
3.3.1;1 Background;35
3.3.2;2 Birth of the Kodaikanal Observatory;38
3.3.3;3 John Evershed (1864–1956);40
3.3.3.1;3.1 Evershed in Kodaikanal;43
3.3.3.2;3.2 Evershed Effect;45
3.3.3.3;3.3 Spectral Lines and Diagnostics;46
3.3.3.4;3.4 Prominences;47
3.3.4;4 Scientific Impact of the Evershed Effect;48
3.3.5;5 Kodaikanal Observatory: 1923–1960;51
3.3.5.1;5.1 Eclipse Expeditions;51
3.3.5.2;5.2 The Saha Committee;51
3.3.5.3;5.3 Ionospheric and Geomagnetic Laboratory;51
3.3.5.4;5.4 Solar Instrumentation;52
3.3.5.5;5.5 Scientific Highlights;53
3.3.6;6 Solar Physics Research at Kodaikanal from 1960 Onwards;54
3.3.6.1;6.1 Velocity Fields in the Solar Atmosphere;55
3.3.6.2;6.2 Magnetic Fields;56
3.3.6.3;6.3 Chromospheric Features and Dynamics;56
3.3.6.4;6.4 Coronal Studies;57
3.3.6.5;6.5 Solar Terrestrial Studies;57
3.3.6.6;6.6 Current Observational Facilities and Programmes;57
3.3.7;7 Future Programmes;58
3.3.7.1;7.1 National Large Solar Telescope;58
3.3.7.2;7.2 Space Coronagraph;58
3.3.8;References;59
3.4;Vainu Bappu Memorial Lecture: What is a Sunspot?;60
3.4.1;1 Introduction;60
3.4.2;2 Subsequent Milestones of Discovery;62
3.4.3;3 Superficial Sunspot Structure;64
3.4.4;4 The Sunspot Cycle;65
3.4.5;5 What Causes Sunspot Darkening?;70
3.4.6;6 The Rotation of the Sun;76
3.4.7;7 The Overall Structure of a Large Sunspot;80
3.4.8;8 On the Birth, Death, and Lifespan of Sunspots;84
3.4.9;9 Solar-Cycle Irradiance Variation;87
4;Part II Oral Presentations;90
4.1;Angular-Momentum Coupling Through the Tachocline;91
4.1.1;1 Introduction;91
4.1.2;2 Some Initial Remarks on Tachocline Dynamics;93
4.1.3;3 The Early History of Dynamical Tachocline Models;96
4.1.4;4 Some Consequences of Tachocline Circulation;99
4.1.5;5 The Quest for a Tachocline Simulation;102
4.1.6;6 Closing Remarks;105
4.1.7;References;107
4.2;Outstanding Issues in Solar Dynamo Theory;109
4.2.1;1 Introduction;109
4.2.2;2 Basic Concepts;111
4.2.3;3 Current State of Our Understanding;112
4.2.4;4 Outstanding Issues;113
4.2.4.1;4.1 Nature of the Dynamo -Effect;113
4.2.4.2;4.2 Treatment of Magnetic Buoyancy;114
4.2.4.3;4.3 Origin of Grand Minima;115
4.2.4.4;4.4 Parametrization of Turbulent Diffusivity;115
4.2.4.5;4.5 Role of Downward Flux Pumping;116
4.2.5;5 Concluding Remarks;116
4.2.5.1;5.1 A Story of Communication Timescales;116
4.2.5.2;5.2 Solar Cycle Predictions;117
4.2.6;References;118
4.3;Status of 3D MHD Models of Solar Global Internal Dynamics;119
4.3.1;1 Introduction: Solar Global MHD;119
4.3.2;2 Global Convection;119
4.3.3;3 Differential Rotation and Meridional Circulation;120
4.3.4;4 Global Dynamo;120
4.3.5;5 Solar Radiation Zone and Its Coupling to the Convection Zone;121
4.3.6;6 Towards a 3D Integrated Model of the Sun;122
4.3.7;References;123
4.4;Measuring the Hidden Aspects of Solar Magnetism;124
4.4.1;1 The Zeeman Effect as a Window to Cosmic Magnetism;124
4.4.2;2 Emergence of the Flux Tube Paradigm;126
4.4.3;3 The Hanle Effect as a Window to the Hidden Fields;129
4.4.4;4 The ``Standard Model'' and Its Shortcomings;132
4.4.5;5 The Second Solar Spectrum and Solar Magnetism;134
4.4.6;6 Scale Spectrum of the Magnetic Structures;136
4.4.7;7 Beyond the Standard Model: Scaling Laws and PDFs for a Fractal-Like Field;137
4.4.8;References;139
4.5;Recent Advances in Chromospheric and Coronal PolarizationDiagnostics;141
4.5.1;1 Introduction;141
4.5.2;2 The Physical Origin of the Spectral Line Polarization;142
4.5.3;3 The Zeeman Effect vs. the Hanle Effect;145
4.5.4;4 Diagnostic Tools Based on Spectral Line Polarization;146
4.5.4.1;4.1 Methods for the Chromosphere and Transition Region;146
4.5.4.2;4.2 Methods for Chromospheric and Coronal Structures;148
4.5.5;5 The Quiet Chromosphere;152
4.5.6;6 Plasma Structures in the Chromosphere and Corona;154
4.5.6.1;6.1 Off-Limb Diagnostics of Prominences and Spicules;155
4.5.6.2;6.2 On-Disk Diagnostics of Filaments;156
4.5.6.3;6.3 Magnetic Field ``Reconstruction" in Emerging Flux Regions;159
4.5.7;7 How to Map the Magnetic Fields of Coronal Loops?;160
4.5.8;8 Concluding Comments;161
4.5.9;References;162
4.6;Probability Density Functions to Represent Magnetic Fields at the Solar Surface;164
4.6.1;1 Introduction;164
4.6.2;2 Scalar PDFs;165
4.6.2.1;2.1 Asymmetric Voigt PDF;165
4.6.2.2;2.2 Asymmetric Stretched Exponential PDF;167
4.6.3;3 Angular PDFs;169
4.6.4;4 Vector Magnetic Field Distributions;170
4.6.5;5 Conclusions;170
4.6.6;References;172
4.7;Spectropolarimetry with CRISP at the Swedish 1-m Solar Telescope;173
4.7.1;1 Introduction;173
4.7.2;2 The June 2008 Campaign Data and Processing;174
4.7.3;3 Inversions and Results;175
4.7.4;4 Discussion;177
4.7.5;References;178
4.8;Spectropolarimetry with the NLST;179
4.8.1;1 Introduction;179
4.8.2;2 Polarimetry Package;181
4.8.3;3 Spectropolarimetry with NLST;182
4.8.3.1;3.1 Multi-slit SP;183
4.8.3.2;3.2 Integral Field Unit;185
4.8.4;4 Concept Realization;186
4.8.5;5 Conclusions;187
4.8.6;References;188
4.9;Magnetic Coupling in the Quiet Solar Atmosphere;189
4.9.1;1 The Magnetic Field of the Quiet Sun;189
4.9.2;2 Coupling of Convection with Magnetic Fields;192
4.9.3;3 Coupling of Waves with Magnetic Fields;197
4.9.4;4 Coupling of Radiation with Magnetic Fields;202
4.9.5;5 Conclusion;205
4.9.6;References;206
4.10;The Evershed Effect with SOT/Hinode;209
4.10.1;1 Introduction;209
4.10.2;2 Elementary Structure of the Evershed Flow;210
4.10.3;3 Discussion;212
4.10.4;References;214
4.11;The Evershed Flow and the Brightness of the Penumbra;216
4.11.1;1 Introduction;216
4.11.2;2 The Evershed Flow at High Spatial Resolution;218
4.11.3;3 Heating of the Penumbra by the Evershed Flow;225
4.11.4;4 Convection in Penumbral Filaments;228
4.11.5;5 Conclusions;229
4.11.6;References;230
4.12;A Topology for the Penumbral Magnetic Fields;233
4.12.1;1 Introduction;233
4.12.2;2 Constraints on the Penumbral Structure;235
4.12.3;3 Model MISMA for Penumbral Filaments with Dark Core;240
4.12.4;4 Scenario for the Small-Scale Structure of the Penumbra;243
4.12.5;5 Qualitative Comparison with Observations;245
4.12.6;6 Discussion and Tests;248
4.12.7;References;249
4.13;Theoretical Models of Sunspot Structure and Dynamics;252
4.13.1;1 Introduction;252
4.13.2;2 Umbral Magnetoconvection;253
4.13.3;3 The Inner and Outer Penumbra;254
4.13.4;4 The Formation and Maintenance of the Penumbra;255
4.13.5;5 The Magnetic Field Configuration in the Penumbra;257
4.13.6;6 Numerical Simulations of a Sunspot;260
4.13.7;7 The Evershed Flow;262
4.13.8;8 Conclusions;263
4.13.9;References;264
4.14;Convection and the Origin of Evershed Flows;266
4.14.1;1 Introduction;266
4.14.2;2 Recent Modeling Results;268
4.14.2.1;2.1 Evershed Results;271
4.14.3;3 Local Penumbra Models;273
4.14.4;4 Conclusions and Concluding Remarks;275
4.14.5;References;277
4.15;The Magnetic Field of Solar Spicules;278
4.15.1;1 Introduction;278
4.15.2;2 Observations;279
4.15.3;3 Analysis;280
4.15.3.1;3.1 Detection of Zeeman-Induced Stokes V;281
4.15.3.2;3.2 Inversions;282
4.15.4;4 Conclusion;283
4.15.5;References;283
4.16;Three-Dimensional Magnetic Reconnection;284
4.16.1;1 Introduction;284
4.16.2;2 Characteristics of 2D and 3D Reconnection;286
4.16.3;3 3D Magnetic Interactions;288
4.16.3.1;3.1 Potential 3D Interaction;288
4.16.3.2;3.2 3D Resistive MHD Interaction;290
4.16.3.3;3.3 Recursive Reconnection and Reconnection Rates;293
4.16.4;4 Energetics;296
4.16.5;5 Conclusions;297
4.16.6;References;298
4.17;Signatures of Coronal Heating Mechanisms;300
4.17.1;1 Introduction;300
4.17.2;2 Signatures for Alfvén Wave Heating;301
4.17.3;3 Signatures for Nanoflare Reconnection Heating;302
4.17.4;4 Conclusion;303
4.17.5;References;303
4.18;Waves in Polar Coronal Holes;304
4.18.1;1 Introduction;304
4.18.2;2 Observation and Results;306
4.18.3;3 Conclusion;307
4.18.4;References;308
4.19;MHD Wave Heating Diagnostics;310
4.19.1;1 The State of the Art;310
4.19.2;References;311
4.20;Coronal Mass Ejections from Sunspot and Non-Sunspot Regions;312
4.20.1;1 Introduction;312
4.20.2;2 Summary of CME Properties;313
4.20.3;3 Special Populations of CMEs;316
4.20.3.1;3.1 Halo CMEs;316
4.20.3.2;3.2 CMEs Resulting in ICMEs;318
4.20.3.3;3.3 Shock-Driving CMEs;319
4.20.3.4;3.4 Comparing the Properties of the Special Populations;320
4.20.3.5;3.5 Solar Sources of the Special Populations;321
4.20.4;4 Solar Cycle Variation;323
4.20.4.1;4.1 Solar Sources of the General Population;325
4.20.4.2;4.2 Implications to the Flare: CME Connection;326
4.20.5;5 Sunspot Number and CME Rate;327
4.20.6;6 Summary and Conclusions;328
4.20.7;References;329
4.21;CME Observations from STEREO;331
4.21.1;1 Introduction;331
4.21.2;2 What Have We Learnt from LASCO Observations?;333
4.21.3;3 CME Observations from SECCHI/STEREO Coronagraphs;335
4.21.4;4 Summary and Conclusion;337
4.21.5;References;339
4.22;Low-Frequency Radio Observations of Coronal Magnetic Fields;341
4.22.1;1 Introduction;341
4.22.2;2 Observations;342
4.22.3;3 Results and Discussion;344
4.22.4;References;346
4.23;Evolution of Near-Sun Solar Wind Turbulence;347
4.23.1;1 Introduction;347
4.23.2;2 Interplanetary Scintillation;348
4.23.3;3 Scintillation Spectrum Near the Sun;349
4.23.4;4 Radial Evolution of Small- and Large-Scale Turbulence;351
4.23.5;5 Discussion and Conclusion ;353
4.23.6;References;354
4.24;The Solar-Stellar Connection;355
4.24.1;1 Introduction;356
4.24.2;2 Sunspot Cycle and Total Solar Irradiance;357
4.24.3;3 The X-Ray Sun;358
4.24.4;4 The Ca II H & K Sun;360
4.24.5;5 Which Stars are X-Ray Emitters? ;361
4.24.6;6 Universality of Stellar X-Ray Emission;363
4.24.7;7 Connection of X-Ray Emission with Other Stellar Parameters;364
4.24.8;8 Coronal Structure;366
4.24.9;9 Conclusions;368
4.24.10;References;368
4.25;Summary and Perspective;369
4.25.1;1 A Double Centenary;369
4.25.2;2 The Solar Interior;370
4.25.3;3 Small-Scale Fields and Polarimetry;371
4.25.4;4 Sunspots;372
4.25.5;5 The Quiet Sun;374
4.25.6;6 Coupling to the Atmosphere and Corona;375
4.25.7;7 Eruptive Phenomena: CMEs and Flares;376
4.25.8;8 The Solar-Stellar Connection;376
4.25.9;9 Epilogue;378
4.25.10;References;378
5;Part III Poster Presentations;379
5.1;Evidence for Return Meridional Flows in the Convection Zone;380
5.1.1;1 Introduction;380
5.1.2;2 Measurements;381
5.1.3;3 Results;381
5.1.4;References;383
5.2;Long-Term Variations in Meridional Flows;384
5.2.1;1 Introduction;384
5.2.2;2 Data Analysis and Results;385
5.2.3;3 Discussion;386
5.2.4;References;386
5.3;Low-Degree High-Frequency p and g Modes in the Solar Core;387
5.3.1;1 Introduction;387
5.3.2;2 The Effect of Low-Degree High-Frequency p Modes;389
5.3.3;3 The Effect of g Modes in the Inversions;389
5.3.4;4 Conclusion;390
5.3.5;References;390
5.4;Interior and Exterior Clues of Solar Activity;391
5.4.1;1 Introduction;391
5.4.2;2 The Dynamics of the Radiative Zone;392
5.4.3;3 The Multichannel GOLF-NG Spectrometer;392
5.4.4;4 Building Secular Solar Dynamical Models;395
5.4.5;References;396
5.5;Do Active Regions Modify Oscillation Frequencies?;397
5.5.1;1 Introduction;397
5.5.2;2 Analysis and Results;397
5.5.3;References;400
5.6;Deep-Focus Diagnostics of Sunspot Structure;401
5.6.1;1 Introduction;401
5.6.2;2 The Flux Tube and Forward Models;402
5.6.3;3 Common Midpoint Deep-Focusing;403
5.6.4;4 Results and Discussion;405
5.6.5;5 Conclusion;407
5.6.6;References;407
5.7;Are Polar Faculae Generated by a Local Dynamo?;409
5.7.1;1 Introduction;409
5.7.2;2 Results;410
5.7.3;References;412
5.8;The Hanle Effect as Diagnostic Tool for Turbulent Magnetic Fields;413
5.8.1;1 Introduction;413
5.8.2;2 Transfer Equations;414
5.8.3;3 Results;414
5.8.3.1;3.1 Dependence on the Correlation Length;414
5.8.3.2;3.2 Dependence on the Magnetic Field Vector PDF;415
5.8.4;4 Conclusions;416
5.8.5;References;416
5.9;Phase III of the USO Solar Vector Magnetograph ;418
5.9.1;1 Introduction;418
5.9.2;2 Recent Developments;419
5.9.3;3 Ongoing Developments;419
5.9.4;4 Conclusions;420
5.9.5;References;420
5.10;Revisit of the Classic Wilson Effect;421
5.10.1;1 Introduction;421
5.10.2;2 Observations and Measurements;422
5.10.3;3 Results and Conclusion;423
5.10.4;References;424
5.11;The Waldmeier Effect in Sunspot Cycles;425
5.11.1;1 Introduction;425
5.11.2;2 Observational Study;426
5.11.3;3 Preliminary Theoretical Results;427
5.11.4;References;427
5.12;Flare-Driven Acoustic Modes in the Sun;428
5.12.1;1 Introduction;428
5.12.2;2 Data and Analysis;430
5.12.3;3 Discussion and Conclusions;430
5.12.4;References;432
5.13;Dynamics of Active Regions Revealed by Tracking of Doppler Features;433
5.13.1;1 Introduction;433
5.13.2;2 The Data and Method;434
5.13.3;3 Results and Conclusions;434
5.13.4;References;435
5.14;The Growth of a Primitive Penumbra;436
5.14.1;1 Introduction;436
5.14.2;2 Observations;437
5.14.3;3 Results and Conclusions;437
5.14.4;References;439
5.15;Evershed Flow Velocities During 100 Years;440
5.15.1;1 Introduction;440
5.15.2;2 Data and Results;441
5.15.3;3 Discussion and Conclusion;441
5.15.4;References;442
5.16;The Thermal Structure of Sunspots;444
5.16.1;1 Introduction;444
5.16.2;2 Data and Analysis ;445
5.16.3;3 Results and Conclusions;445
5.16.4;References;446
5.17;Bright Points in G-Band and CaiiH Images from Hinode;447
5.17.1;1 Observations, Analysis, and Results;447
5.18;Waves in the Transition Region;449
5.18.1;1 Introduction;449
5.18.2;2 Evidence;449
5.18.3;References;451
5.19;Viscous Damping of Alfvén Surface Waves with Steady Flows;452
5.19.1;1 Introduction;452
5.19.2;2 Dispersion Relation;453
5.19.3;3 Discussion and Conclusion;453
5.19.4;References;454
5.20;Statistical Detection of Propagating Waves in a Polar Coronal Hole;456
5.20.1;1 Introduction;456
5.20.2;2 Observations and Data Analysis;457
5.20.3;3 Results and Discussion;457
5.20.4;References;459
5.21;Network Loop Oscillations with EIS/Hinode ;460
5.21.1;1 Introduction;460
5.21.2;2 Observations;460
5.21.3;3 Magnetoacoustic Oscillations;461
5.21.4;References;462
5.22;Dynamical Evolution of X-Ray Bright Points with Hinode/XRT;463
5.22.1;1 Introduction;463
5.22.2;2 Results and Discussion;464
5.22.3;References;465
5.23;Helicity at Photospheric and Chromospheric Heights;466
5.23.1;1 Introduction;466
5.23.2;2 Sign of Magnetic Helicity ;467
5.23.3;3 Data;468
5.23.4;4 Results and Discussion;468
5.23.5;References;470
5.24;Evolution of Coronal Helicity in a Twisted Emerging Active Region;471
5.24.1;1 Introduction;471
5.24.2;2 Results;472
5.24.3;3 Discussion;474
5.24.4;References;474
5.25;Power-Law Nanoflare Heating;475
5.25.1;1 Introduction;475
5.25.2;2 Power-Law Estimates;475
5.25.3;References;476
5.26;Spectroscopic Diagnostics of Polar Coronal Plumes;477
5.26.1;1 Introduction;477
5.26.2;2 Spectroscopic Observations of Coronal Plumes;478
5.26.3;3 Results and Discussion;479
5.26.4;References;481
5.27;A Flaring Polar Filament;482
5.27.1;1 Introduction;482
5.27.2;2 Observations ;483
5.27.3;References;485
5.28;Solar X-Ray Processes;486
5.28.1;References;487
5.29;Time-Varying Thermal Emission in Solar Flares;488
5.29.1;1 Introduction;488
5.29.2;2 Observations, Analysis, Results;490
5.29.3;3 Conclusion;492
5.29.4;References;493
5.30;Multi-Wavelength View of Flare Events on 20 November 2003;494
5.30.1;1 Flare Events on 20 November 2003;494
5.30.2;2 Reorganization of Magnetic Structures;495
5.30.3;3 Results and Discussion;496
5.30.4;References;497
5.31;Time-Delay Between Solar Soft X-Ray and EUV Flare Emissions;498
5.31.1;1 Introduction;498
5.31.2;2 Results and Discussion;499
5.31.3;References;500
5.32;Major Surge Activity of Super-Active Region NOAA 10484;501
5.32.1;1 Introduction;501
5.32.2;2 Observations;502
5.32.3;3 Results and Discussion;504
5.32.4;References;504
5.33;Coronal Magnetic Field Estimation Using Type-II Radio Bursts;505
5.33.1;1 Observations, Analysis, Results;505
5.33.2;References;507
5.34;Acceleration of CMEs Associated with Eruptive Prominences;508
5.34.1;1 Introduction;508
5.34.2;2 Observations;508
5.34.3;3 Discussion and Summary;509
5.34.4;4 Future Plan;511
5.34.5;References;511
5.35;Interplanetary Consequences of a Large CME;512
5.35.1;1 Introduction: Intense Flare and CME;512
5.35.2;2 Radio Spectra, Particle Fluxes, and Scintillation Images;512
5.35.3;3 Conclusion;516
5.35.4;References;516
5.36;Solar System Resonances on Light-Travel Time ScalesSet Up before Proto-Sun's Nuclear Ignition;517
5.36.1;1 Introduction;517
5.36.2;2 Fourier Frequencies in Momentum Transfer;518
5.36.3;3 Resonance Set-Up During the Approach to and Onset of Steady State;519
5.36.4;4 Conclusion;519
5.36.5;References;519
6;Part IV Summaries of Presentations Published Elsewhere;520
6.1;Cycle Prediction from Dynamo Theory;521
6.1.1;References;522
6.2;Why Does the Torsional Oscillation Precede the Sunspot Cycle?;523
6.2.1;References;524
6.3;The Subsurface Magnetic Structure of Solar Active Regions;525
6.4;Sunspot Magnetometry from Kodaikanal;527
6.4.1;References;527
6.5;Vector Magnetic Field in Emerging Flux Regions;528
6.5.1;References;529
6.6;Evolution of Umbral Dots and Penumbral Grains;530
6.7;Strong, Localized Downflows in a Sunspot Light Bridge;532
6.8;Small-Scale Velocities in Sunspot Penumbrae;533
6.9;Photospheric Temperatures from CaiiH;534
6.9.1;References;535
6.10;Dual-Line Spectral Imaging of the Chromosphere;536
6.11;Inversions of High-Cadence SOLIS-VSM Stokes Observations;538
6.11.1;References;538
6.12;Flows in Flaring and Dormant Active Regions;539
6.12.1;References;539
6.13;Magnetic and Velocity Field Changes Related to the Solar Flares of 28 and 29 October 2003;540
6.13.1;References;540
6.14;A Numerical Investigation of Unsheared Flux Cancelation;541
6.15;Wave Heating of Coronal Loops with Steady Flows;543
6.15.1;References;543
6.16;Damping of Prominence Oscillations in Steady Equilibrium;544
6.17;Variation of Network Contrast with Height;545
6.18;A Flaring Twisted Emerging Flux Region;546
6.18.1;Reference;547
6.19;Evidence of Magnetic Reconnection Outflows in a Flare seenby Hinode/EIS;548
6.20;Does Coronal Rotation Period Depend on the Sunspot Number?;549
6.20.1;1 Introduction;549
6.20.2;2 Feature Tracking;549
6.20.3;3 Spectral Measurements;550
6.20.4;4 Rotation Measurements from Flux Modulation;550
6.20.5;5 Data Analysis and Results;550
6.20.6;References;551
6.21;Coronal Magnetic Field from an Extreme Radio Burst;552
6.22;CME Kinematics and Dynamics;553
6.22.1;References;553
6.23;Solar Wind Monitoring with SWIM-SARA Onboard Chandrayaan-1;554
6.24;Coupling of the Solar Wind and the Magnetosphere;556
6.25;The FIP Effect in RV Tauri Stars;558
7;Author Index;559