Titlebook: Solar Gamma-, X-, and EUV Radiation; Sharad R. Kane Book 1975 International Astronomical Union 1975 Corona.Solar flare.Variation.gamma-ray

变形

Interpretation of the X-Ray Spectra of Solar Active Regionsonal spectrum, and the currently available atomic rate constant data are reviewed first. Spectroscopic techniques which have been proposed for the determination of coronal temperature and density structure, and the results derived from their application to coronal spectra are also reviewed..A number

者变

Folklore

Time Variations in Coronal Active Regions regular 12±2 h synoptic observation rate. The form and brightness of coronal active region structures are seen to vary on time scales ranging from seconds, for flare associated changes, to several solar rotations for long term evolution of the regions. The extrapolation of photospheric magnetic fie

Dislocation

cinder

钝剑

Ultraviolet Emission Line Profiles of Flares and Active Regionsraph is given. The findings can be summarized as follows: (1) Line profiles of medium ionized lines (transition zone lines) show the most pronounced broadenings and shifts in flares and flare like events. (2) Typical full width at half maximum of these lines correspond to Doppler-velocities of 70 km

Irritate

处理

Interpretation of the X-Ray Spectra of Solar Active Regions of coronal models based on X-ray observations have been developed recently, and the coronal temperature structure and composition predicted by these models is discussed, and compared with models of the corona and transition region derived from studies of the solar EUV spectrum.

Confess

curriculum

X-Ray Spectra of Solar Active Regions to the discovery of weak satellite lines to helium-like ions; the quantitative theory for these lines is also discussed. The observed intensities of the Fe . lines are also investigated and found to be in agreement with calculations that allow for cascading processes.