Implications of a direct photometric comparison of the EUV-corona and the K-Corona

  • F. Q. Orrall
  • R. R. Fisher
  • R. H. Munro
  • G. J. Rottman
Session V: Mass Loss and Pulsation
Part of the Lecture Notes in Physics book series (LNP, volume 254)


We report results of co-temporal and co-spatial measurements of the K-coronal brightness (pB) and the intensity of the coronal emission line λ625 Mg X in the inner corona. The pB measurements were made with the Mark III K-coronameter on Mauna Loa (HAO/NCAR), and the EUV measurements were obtained on rocket flights of the LASP EUV Coronal Spectrometer in 1980 and 1983. The data consist of radial limb profiles of pB and λ625 intensity as a function of height above the limb that overlap between 1.10 and 1.25 solar radii. One result of this comparison is that the quantity [Ac/Ap] \([(\overline {N^2 } )/(\bar N)^2 ]\) is much greater than unity in the coronal regions sampled (a polar coronal hole and an old active region). Here Ac and Ap are the abundances of magnesium in the corona and photosphere, respectively and \([(\overline {N^2 } )/(\bar N)^2 ]\) is the electron density “irregularity factor.” If as recent work suggest the photospheric and coronal abundances of magnesium are about equal (cf Meyer 1985), then the corona is more highly structured on small scale than is visible on existing coronal images of high spatial resolution. Some implications of this for coronal physics are discussed.


Polar Coronal Hole Rocket Flight Coronal Emission Line Coronal Abundance High Altitude Observatory 
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Copyright information

© Springer-Verlag 1986

Authors and Affiliations

  • F. Q. Orrall
    • 1
  • R. R. Fisher
    • 3
  • R. H. Munro
    • 3
  • G. J. Rottman
    • 2
  1. 1.Institute for AstronomyUniversity of HawaiiHonoluluHawaii
  2. 2.Laboratory for Atmospheric and Space PhysicsUniversity of Colorado
  3. 3.High Altitude ObservatoryNational Center for Atmospheric ResearchBoulder

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