Structure of coronal holes from UV and radio observations

Details Structure of coronal holes from UV and radio observations Structure of coronal holes from UV and radio observations

Feb 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977soph...51..143c&link_type=abstract

Solar Physics, vol. 51, Jan.-Feb. 1977, p. 143-158.

Physics

14

Solar Corona, Solar Radio Emission, Ultraviolet Spectra, Coronagraphs, Far Ultraviolet Radiation, Solar X-Rays, Spectroheliographs

Scientific paper

EUV (Fe XV at 284 A) and radio (at 169 and 408 MHz) observations were made of the coronal hole on May 31, 1973. An inhomogeneous model consisting of hot (a temperature of about 2 x 10 to the 6th K) elements covering 10% of the hole surface surrounded by regions of colder gas (a temperature of about 8 x 10 to the 5th K) is able to explain both observations.

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