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Observations of the 12.3 micron Mg I emission line during a major solar flareThe extremely Zeeman-sensitive 12.32 micron Mg I solar emission line was observed during a 3B/X5.7 solar flare on October 24, 1989. When compared to postflare values, Mg I emission-line intensity in the penumbral flare ribbon was 20 percent greater at the peak of the flare in soft X-rays, and the 12 micron continuum intensity was 7 percent greater. The flare also excited the emission line in the umbra where it is normally absent. The umbral flare emission exhibits a Zeeman splitting 200 G less than the adjacent penumbra, suggesting that it is excited at higher altitude. The absolute penumbral magnetic field strength did not change by more than 100 G between the flare peak and postflare period. However, a change in the inclination of the field lines, probably related to the formation and development of the flare loop system, was seen.
Document ID
19910031919
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Deming, Drake (NASA Goddard Space Flight Center Greenbelt, MD, United States)
Jennings, Donald E. (NASA Goddard Space Flight Center Greenbelt, MD, United States)
Osherovich, Vladimir (NASA Goddard Space Flight Center Greenbelt, MD, United States)
Wiedemann, Gunter (NASA Goddard Space Flight Center Greenbelt, MD, United States)
Hewagama, Tilak (NASA Goddard Space Flight Center Greenbelt; Maryland, University, College Park, United States)
Date Acquired
August 15, 2013
Publication Date
December 1, 1990
Publication Information
Publication: Astrophysical Journal, Part 2 - Letters
Volume: 364
ISSN: 0004-637X
Subject Category
SOLAR PHYSICS
Distribution Limits
Public
Copyright
Other