Overview

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.

Full Product Details

Author:   Oddbjorn Engvold ,  C.J. Schrijver ,  John W. Harvey ,  Neal E. Hurlburt
Publisher:   Springer
Imprint:   Springer
Edition:   Softcover reprint of hardcover 1st ed. 2000
Weight:   0.771kg
ISBN:  

9789048154746

ISBN 10:   904815474
Pages:   497
Publication Date:   01 December 2010
Audience:   Professional and scholarly ,  Professional & Vocational
Format:   Paperback
Publisher's Status:   Active
Availability:   Out of stock  
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Table of Contents

Aspects of Three-Dimensional Magnetic Reconnection.- The Topological Behaviour of Stable Magnetic Separators.- Does Magnetic Flux Submerge at Flux Cancelation Sites?.- Magnetic Reconnection as the Cause of a Photospheric Canceling Feature and Mass Flows in a Filament.- Forward Modeling of the Coronal Response to Reconnection in an X-Ray Bright Point.- Different Spatial Structures between Network Regions and Active Regions Indicated by TRACE 171 Å Observation.- The Global Dynamics of the High-Temperature Corona.- CME Associated with Transequatorial Loops and a Bald Patch Flare.- Long-Lived Coronal Loop Profiles from TRACE.- Inclination of Large Coronal Loops Observed by TRACE.- Structure and Dynamics of Interconnecting Loops and Coronal Holes in Active Longitudes.- Counter-Streaming Mass Flow and Transient Brightening in Active Region Loops.- High-Resolution Observations of Plasma Jets in the Solar Corona.- Dynamics of Polar Plumes Observed at the 1998 February 26 Eclipse.- Coronal Heating Events in High-Cadence TRACE Data.- Do EUV Nanoflares Account for Coronal Heating?.- Time Variability of EUV Brightenings in Coronal Loops Observed with TRACE.- Flares in Sigmoidal Coronal Structures — A Case Study.- Post-Impulsive-Phase Acceleration in a Wide Range of Solar Longitudes.- Radio versus EUV/X-Ray Observations of the Solar Atmosphere.- Non-Uniqueness of Atmospheric Modeling.- Calibrated H i Lyman ? Observations with TRACE.- Measuring the Physical Properties of the Solar Corona: Results from SUMER/SOHO and TRACE.- Observations of Transition Region Plasma.- What is Moss?.- Dynamics of Transition Region ‘Moss’ at High Time Resolution.- On the Sunspot Transition Region.- Variations of Photospheric Magnetic Field Associated with Flares and CMEs.- Observations of aPropagating Disturbance in TRACE.- Ion Cyclotron Waves, Instabilities and Solar Wind Heating.

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