The Physics of the Solar Corona and Transition Region

1. Radio Versus EUV/X-Ray Observations of the Solar Atmosphere

   • S. M. White

   Pages 309-330

2. Non-Uniqueness of Atmospheric Modeling

   • Philip G. Judge, Scott W. Mcintosh

   Pages 331-350

3. Calibrated H i Lyman α Observations with TRACE

   • B. N. Handy, T. D. Tarbell, C. J. Wolfson, C. M. Korendyke, A. Vourlidas

   Pages 351-361

4. Measuring the Physical Properties of the Solar Corona: Results from SUMER/SOHO and TRACE

   • H. P. Warren

   Pages 363-377

5. Observations of Transition Region Plasma

   • Pål Brekke

   Pages 379-408

6. What is Moss?

   • T. E. Berger, B. De Pontieu, L. Fletcher, C. J. Schrijver, T. D. Tarbell, A. M. Title

   Pages 409-418

7. Dynamics of Transition Region ‘Moss’ at High Time Resolution

   • B. De Pontieu, T. E. Berger, C. J. Schrijver, A. M. Title

   Pages 419-435

8. On the Sunspot Transition Region

   • P. Maltby, N. Brynildsen, T. Fredvik, O. Kjeldseth-Moe, K. Wilhelm

   Pages 437-458

9. Variations of Photospheric Magnetic Field Associated with Flares and CMEs

   • A. G. Kosovichev, V. V. Zharkova

   Pages 459-466

10. Observations of a Propagating Disturbance in Trace

    • M. J. Wills-Davey, B. J. Thompson

    Pages 467-483

11. Ion Cyclotron Waves, Instabilities and Solar Wind Heating

    • Xing Li, Shadia R. Habbal

    Pages 485-497

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.

• Corona
• Solar wind
• Sunspot
• Variation
• solar
• solar physics

• Institute of Theoretical Astrophysics, Oslo, Norway

  Oddbjorn Engvold

• National Solar Observatory, Tucson, USA

  John W. Harvey

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