Atmospheric models of coronal hole network

Details Atmospheric models of coronal hole network Atmospheric models of coronal hole network

Sep 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989chjss...8...81z&link_type=abstract

(Chinese Journal of Space Science, vol. 8, Apr. 1988, p. 81-90) Chinese Physics (ISSN 0273-429X), vol. 9, July-Sept. 1989, p. 70

Physics

1

Coronal Holes, Magnetohydrodynamic Waves, Solar Atmosphere, Solar Magnetic Field, Stellar Models, Chromosphere, Conductive Heat Transfer, Electron Density (Concentration), Energy Dissipation, Radiative Heat Transfer

Scientific paper

Energy balance models of the chromosphere-corona transition region are computed for a segment of coronal hole assuming a nonradial magnetic field geometry. The energy fluxes considered include radiation, conduction, convection, and mechanical wave heating. The calculated results show that the temperature is about 60 percent lower, the electron density is twice as small, and the thickness of the transition region is four times larger in the coronal hole network than in the quiet region. This atmospheric model can satisfactorily explain the distribution of emission measurements obtained from the EUV observations for temperatures above 100,000 K.

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