A coronal hole observed by 8-cm wavelength radioheliograph

Details A coronal hole observed by 8-cm wavelength radioheliograph A coronal hole observed by 8-cm wavelength radioheliograph

Jun 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977cosp.meets....s&link_type=abstract

COSPAR, Plenary Meeting, 20th, Tel Aviv, Israel, June 7-18, 1977, Paper. 15 p.

Computer Science

Centimeter Waves, Solar Corona, Solar Radio Emission, Spectroheliographs, Atmospheric Models, Brightness Temperature, Far Ultraviolet Radiation, Magnetic Storms

Scientific paper

Around the end of 1975, a low brightness region was detected by an 8-cm radioheliograph at Toyokawa. It was observed over a period of three solar rotations. It was accompanied by a high-speed solar wind stream and caused recurrent-type geomagnetic storms. This region was identified as a coronal hole. The brightness temperature of this coronal hole was 6000 K lower than that of the normal quiet region. A simple model of the solar atmosphere was used to calculate the brightness temperature at 8-cm wavelength in the coronal hole and the normal quiet region. The electron pressure at the base of the corona obtained by EUV and soft X-ray observations is too high to explain the present radio observations of the coronal hole and the normal quiet region.

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