摘要
Since 1958 when Parker predicted the existence of solar wind plasma in the interplanetary space, its source regions and acceleration mechanisms have been the problems presented to space physicists. We obtained some results for average 2-D large scale structures of solar wind mass flux output near the sun by means of a combination study of the interplanetary scintillation (IPS) observations and the K-coronameter data in 1983 and have compared them with the photospheric magnetic field observations for the
基金
Project supported by the National Natural Science Foundation of China.
