The solar coronal density irregularity N squared bar/(n bar) squared derived from simultaneous measurements of the EUV and K-coronal brightness

Details The solar coronal density irregularity N squared bar/(n bar) squared derived from simultaneous measurements of the EUV and K-coronal brightness The solar coronal density irregularity N squared bar/(n bar) squared derived from simultaneous measurements of the EUV and K-coronal brightness

Feb 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...349..656o&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 349, Feb. 1, 1990, p. 656-666.

Astronomy and Astrophysics

Astrophysics

18

Brightness Distribution, Density Distribution, Extreme Ultraviolet Radiation, Solar Corona, Electron Distribution, Hydrostatics, Polarized Radiation, Ultraviolet Spectra

Scientific paper

Results are reported from a study of the low corona based on cospatial and cotemporal measurements of the K-coronal polarized brightness pB, and the intensity of the strong resonance line Mg x 625A as a function of height between 1.05 and 1.24 solar radius. Taken together, these measurements yield an estimate of the solar coronal density irregularity. This quantity, is found to be much greater than 1. On the basis of a simple two-component model, it is found that the well-studied resolved structures of the inner corona as presently understood are not capable of explaining the observed irregularity. It is conjectured that subresolution density fluctations associated with coronal dissipation and heating may be the source of the excess irregularity.

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