Physics
Scientific paper
Oct 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986azh....63.1029b&link_type=abstract
Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 63, Sept.-Oct. 1986, p. 1029-1039. In Russian.
Physics
12
Brightness Distribution, Coronal Holes, Plasma Diagnostics, Polarization Characteristics, Solar Corona, Density Distribution, Solar Physics, Solar Wind Velocity
Scientific paper
A method for determining the coronal plasma parameters is used, in which the brightness B and the polarization brightness pB of the white coronal emission are computed and are then compared with observational data. The computations are performed under the assumption that the density distribution is hydrostatic at heliocentric distances r < 2 R_sun; and hydrodynamic expansion of the corona (of the type of Parker solution) is taken into account at r > 2 R_sun;. The density at the base of the large coronal hole of 1973 is found to be equal to ≈0.6×108cm-3. For the usual polar and equatorial holes the characteristic value is ≡108cm-3 at the temperature (1.2 - 1.4)×106K. Up tp 2 R_sun; the plasma outflow velocities are small. At larger distances, though the plasma outflow does influence the brightness distribution, the flux of particles from the polar holes is considerably less than in the quiet solar wind at low latitudes. The method has also been applied to the quiet corona and to the streamers, which allowed to suggest a model of the expanding corona.
Badalyan Olga G.
Livshits Moisey A.
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