Relationships of quasi-stationary solar wind flows with their sources on the sun

Details Relationships of quasi-stationary solar wind flows with their sources on the sun Relationships of quasi-stationary solar wind flows with their sources on the sun

Jan 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992soph..137..179e&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 137, Jan. 1992, p. 179-197.

Physics

3

Magnetic Field Configurations, Solar Magnetic Field, Solar Rotation, Solar Wind, Center Of Gravity, Coronal Holes, Current Sheets, Solar Activity Effects, Solar Terrestrial Interactions

Scientific paper

By considering an example of four Carrington rotations (1671, 1672, 1681, and 1682), it is shown that there generally exists an exhaustive correspondence between quasi-stationary flows of 'fast' and 'slow' solar wind (SW), on the one hand, and their sources on the sun, coronal holes (CHs) and the heliospheric current sheet (HCS), on the other. It is also shown that by knowing characteristics such as the coordinate of the center of gravity of CHs on the sun, their areas S and the positions of the neutral line (NL) and of the HCS without the NL on the sun, it becomes possible to calculate the time of appearance and the amplitude of three points on the SW velocity profile at the earth's orbit, namely time and velocity amplitude V(F) corresponding to the mean point of the forward front of the SW flow velocity profile, the value of V = Vm in the central part of the flow, and angular width of the flow at level V = V(F). Calculated values agree with those observed.

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