Hostname: page-component-5c6d5d7d68-ckgrl Total loading time: 0 Render date: 2024-08-23T23:10:55.486Z Has data issue: false hasContentIssue false
  • English
  • Français

X-Ray Evidence of Coronal Preflare Emission

Published online by Cambridge University Press:  14 August 2015

D. F. Webb
D. F. Webb*
Affiliation:
American Science and Engineering, Inc. Cambridge, Massachusetts 02139 USA

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Flares are believed to derive their energy from localized nonpotential magnetic fields; this energy is somehow stored and initially released in the low corona. Therefore, knowledge of coronal conditions prior to flares is essential to our understanding of the flare process. The coronal plasma is constrained by the magnetic field and its characteristic emission is easily observed at soft X-ray wavelengths. Therefore, X-ray imagery is well suited for observing changes in emission influenced by nonpotential magnetic fields in the low corona. This study used soft X-ray images from the Skylab AS&E telescope to search for evidence of coronal preflare emission.

Type
Part III. Solar Transient Phenomena Affecting the Corona and Interplanetary Medium: Dynamics Deduced from Observations
Information
Symposium - International Astronomical Union , Volume 91: Solar and Interplanetary Dynamics , 1980 , pp. 189 - 193
Copyright
Copyright © Reidel 1980 

References

Heyvaerts, J., Priest, E.R., and Rust, D. M.: 1977, Astrophys. J. 216, 123.Google Scholar
Kahler, S.W. : 1979, Solar Phys . 62, 347.Google Scholar
Kahler, S.W. and Buratti, B.J.: 1976, Solar Phys . 47, 157.Google Scholar
Kahler, S.W., Petrasso, R.D., and Kane, S.R. : 1976, Solar Phys . 50, 179.Google Scholar
Martin, S.F. and Ramsey, H.E. : 1972, in McIntosh, P.S. and Dryer, M. (eds.) Solar Activity Observations and Predictions , MIT Press, Cambridge, MA.Google Scholar