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Solar Physics

, Volume 78, Issue 2, pp 225–228 | Cite as

On the color of the 26 February 1981 white light flare

  • Donald F. Neidig
  • Ronald O. Beck
Research Notes

Abstract

We describe visual observations of a white light flare which displayed a pink color in a part of the flare which covered a sunspot umbra. We then show that visible pink tint, if attributable to strong Hα emission, requires a minimum equivalent emission line width of approximately 140 A, or three times larger than in any flare previously measured. Such extreme line broadening might be interpreted to result from flare penetration to unusually high chromospheric densities (≳ 1014 cm−3), or from anomalous Stark broadening due to turbulent electric fields in an unstable plasma (Spicer and Davis, 1975) at lower density.

Keywords

Color Flare Line Width Emission Line Visual Observation 
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References

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Copyright information

© D. Reidel Publishing Company 1982

Authors and Affiliations

  • Donald F. Neidig
    • 1
  • Ronald O. Beck
    • 2
  1. 1.Air Force Geophysics Laboratory, Sacramento Peak ObservatorySunspotU.S.A.
  2. 2.Det 4, 3rd WWAir Weather Service, United States Air Force, Holloman AFBU.S.A.

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