Physics of the Solar Corona and Transition Region : Proceedings of the Monterey Workshop, held in Monterey, California, August 1999

Solar Physics publishes up to two Topical Issues per year that focus on areas of especially vigorous and active research. The present Topical Issue contains papers of recent results on the solar corona, as well as on the transition region and low solar wind. The majority of these papers, which were all refereed in accordance with the standards of Solar Physics, were presented in August 1999 at a workshop held in Monterey, California. The authors were offered the opportunity to present relevant parts of their contributions on an accompanying CD ROM of this Topical Issue. The Sun's magnetic field is responsible for the spectacularly dynamic and intri­ cate phenomenon that we call the corona. The past decade has seen an enormous increase in our understanding of this part of the solar outer atmosphere, both as a result of observations and because of rapid advances in numerical studies. The Yohkoh satellite has observed the Sun now for over eight years, producing spectac­ ular sequences of images that convey the complexity of the corona. The imaging and spectroscopic instruments on SOHO have added information on the cooler part of the corona. And since April of 1998 TRACE has given us very high resolution images of the 1-2 MK corona, at cadences that allow detailed observations of field oscillations, loop evolution, mass ejecta, etc. Front Matter....Pages i-vii Aspects of Three-Dimensional Magnetic Reconnection....Pages 1-24 The Topological Behaviour of Stable Magnetic Separators....Pages 25-33 Does Magnetic Flux Submerge at Flux Cancelation Sites?....Pages 35-44 Magnetic Reconnection as the Cause of a Photospheric Canceling Feature and Mass Flows in a Filament....Pages 45-58 Forward Modeling of the Coronal Response to Reconnection in an X-ray Bright Point....Pages 59-77 Different Spatial Structures between Network Regions and Active Regions Indicated by TRACE 171 Å Observation....Pages 79-90 The Global Dynamics of the High-Temperature Corona....Pages 91-106 CME Associated with Transequatorial Loops and a Bald Patch Flare....Pages 107-129 Long-Lived Coronal Loop Profiles from TRACE....Pages 131-138 Inclination of Large Coronal Loops Observed by TRACE....Pages 139-144 Structure and Dynamics of Interconnecting Loops and Coronal Holes in Active Longitudes....Pages 145-151 Counter-Streaming Mass Flow and Transient Brightening in Active Region Loops....Pages 153-165 High-Resolution Observations of Plasma Jets in the Solar Corona....Pages 167-184 Dynamics of Polar Plumes Observed at the 1998 February 26 Eclipse....Pages 185-206 Coronal Heating Events in High-Cadence Trace Data....Pages 207-232 Do EUV Nanoflares Account for Coronal Heating?....Pages 233-247 Time Variability of EUV Brightenings in Coronal Loops Observed with Trace....Pages 249-265 Flares in Sigmoidal Coronal Structures — A Case Study....Pages 267-293 Post-Impulsive-Phase Acceleration in a Wide Range of Solar Longitudes....Pages 295-307 Radio Versus EUV/X-Ray Observations of the Solar Atmosphere....Pages 309-330 Non-Uniqueness of Atmospheric Modeling....Pages 331-350 Calibrated H i Lyman α Observations with TRACE....Pages 351-361 Measuring the Physical Properties of the Solar Corona: Results from SUMER/SOHO and TRACE....Pages 363-377 Observations of Transition Region Plasma....Pages 379-408 What is Moss?....Pages 409-418 Dynamics of Transition Region ‘Moss’ at High Time Resolution....Pages 419-435 On the Sunspot Transition Region....Pages 437-458 Variations of Photospheric Magnetic Field Associated with Flares and CMEs....Pages 459-466 Observations of a Propagating Disturbance in Trace....Pages 467-483 Ion Cyclotron Waves, Instabilities and Solar Wind Heating....Pages 485-497 The Sun's magnetic field is responsible for the spectacularly dynamic and intricate phenomenon that we call the corona. The past decade has seen an enormous increase in our understanding of this part of the solar outer atmosphere, both as a result of observations and because of rapid advances in numerical studies. The YOHKOH satellite has observed the Sun now for over six years, producing spectacular sequences of images that convey the complexity of the corona. The imaging and spectroscopic instruments on SOHO have added information on the cooler part of the corona. And since April of 1998 TRACE has given us very high resolution images of the 1-2 MK corona, at cadences that allow detailed observations of field oscillations, loop evolution, mass ejecta, etc. This volume contains papers contributed to a workshop (held in August 1999 in Monterey, California) that was dedicated to an exploration of the most recent results on the solar corona, as well as on the transition region and low solar wind. The diverse presentations at the meeting revolved around one key theme: the entire outer atmosphere of the Sun is intrinsically dynamic, evolving so rapidly that even the concept of a single local temperature for a single fluid often breaks down. Moreover, the corona is an intrinsically nonlinear and nonlocal medium. These aspects are discussed in these proceedings that include both papers that review recent developments (both based on observations and on theoretical/numerical modeling), and original research papers based on observations from many different observatories. The papers presented at the meeting add up to such a volume that they are distributed over two Topical Issues of Solar Physics (December 1999 and April 2000), which are reprinted in these bound volumes, of which this is the second. The Sun's magnetic field is responsible for the spectacularly dynamic and intricate phenomenon that we call the corona. The past decade has seen an enormous increase in our understanding of this part of the solar outer atmosphere, both as a result of observations and because of rapid advances in numerical studies. The YOHKOH satellite has observed the Sun now for over six years, producing spectacular sequences of images that convey the complexity of the corona. The imaging and spectroscopic instruments on SOHO have added information on the cooler part of the corona. And since April of 1998 TRACE has given us very high resolution images of the 1-2 MK corona, at cadences that allow detailed observations of field oscillations, loop evolution, mass ejecta, etc. This volume contains papers contributed to a workshop (held in August 1999, in Monterey, California) that was dedicated to an exploration of the most recent results on the solar corona, as well as on the transition region and low solar wind. The diverse presentations at the meeting revolved around one key theme: the entire outer atmosphere of the Sun is intrinsically dynamic, evolving so rapidly that even the concept of a single local temperature for a single fluid often breaks down. Moreover, the corona is an intrinsically nonlinear and nonlocal medium. These aspects are discussed in these proceedings that include both papers that review recent developments (both based on observations and on theoretical/numerical modeling), and original research papers based on observations from many different observatories. The papers presented at the meeting add up to such a size that they are distributed over two Topical Issues of Solar Physics (December 1999 and April 2000), which are reprinted in these bound volumes.