GLOBAL STRUCTURE OF SOLAR-WIND PLASMA FLUX OUTPUT NEAR THE SUN

Based on the observational data for K-corona brightness, interplanetary scintillations (IPS) and the photosphere's magnetic fields in the ten Carrington rotations, 1733-1742, in 1983, the average global structures of solar wind mass, momentum and energy flux outputs, F(m), F(p) arid F(e), on the source surface (10R(s)) near the sun have been discussed and compared with these of the magnetic fields on the photosphere. New discoveries are: (i) there are the global structures similar to wave-like structures with bi-peak in F(m), F(e) and F(e); (ii) global structures of F(m), F(p) and F(e) are closely associated with those of the magnetic fields on the photosphere: most large flux outputs concentrate near the magneto-neutral line (MN) regions, less in the polar corona (PC) regions and middle in the strong magnetic fields (SM) regions; (iii) frequency spectra of F(m), F(p) and F(e) are evidently different for MN, PC and SM regions which are located in the high, low and middle, respectively; (iv) the total output rates of solar wind mass, momentum and energy from the positive and negative magnetic polarity regions on the source surface, respectively, are nearly equal to F(m),+/F(m),- =1.04, F(p),+/F(p),- =0.97 and F(e),+/F(e),- =0.90. These results imply that global structures of solar plasma outputs near the sun could be an important indicator for large scale global dynamical processes near the sun. There could be various source regions of the solar wind with different magnetic structures.