Solar Magnetic Phenomena

Invited Lectures.- Observations of Photosphere and Chromosphere.- Solar Flares — Observations and Theory.- Coronal Mass Ejections and Magnetic Helicity.- High Energy Radiation from the Sun.- Physics of Solar Prominences.- Eight Years of Soho: Some Highlights.- Contributed Papers.- 2 1/2-D Compressible Reconnection Model.- Waiting Time Distribution of CMES.- Simultaneous Visible and IR Spectropolarimetry of the Quiet Sun.- A Simple Topological Model of the Bastille Day Flare (July 14, 2000).- Spectropolarimetry in a Sunspot Penumbra at High Spatial Resolution.- X-Ray and H?Emission of the 20 Aug 2002 Flare*.- Center-to-Limb Variation of Facular Contrast Derived from MLSO RISE/PSPT Full Disk Images.- The Acceleration-Velocity Relationship in 5000 LASCO-CME’s.- Time Evolution of the Spectral Index in Solar Flares.- Analysis of Doppler Shifts of Spectral Lines Obtained by the CDS/SOHO Instrument.- On the Behaviour of a Blinker in Chromospheric and Transition Region Layers.- On the 24- and 155-Day Periodicity Observed in Solar H? Flares.- He-D3 Polarization Observed in Prominences.- Line-of-Sight Velocity and Magnetic Field in Sunspot Penumbrae.- Impulsive X-Ray Radiation Characteristics of Solar Flare Footpoints.- Velocity Fields in an Irregular Sunspot.- On the Dynamic Disconnection of Rising ?-Loops.- Searching for the Origins of the Fast Solar Wind.- Detectability of High Frequency Acoustic Waves with Trace.- Linking Coronal to Interplanetary Magnetic Helicity.- Debrecen Photoheliographic Data and Its Comparison with Other Sunspot Databases.- Properties of a Small Active Region in the Solar Photosphere.- Small Scale Events Seen in SXT Observations.- Properties of Type IV Radio Bursts with Periodical Fine Structures.- Testing the Neupert Effect.- The Faint YoungSun Problem.- CCD Spectroscopy of Solar Rotation.- The Observing Programs at Kanzelhöhe Solar Observatory.- Theoretical Modeling of Potential Magnetic Field Distribution in the Corona above Axially Symmetric Photospheric Active Regions in a Uniform Magnetic Field.

Is particularly useful for graduate students and young researchers working in solar physics