Latitudinal dependence of solar wind speed

Details Latitudinal dependence of solar wind speed Latitudinal dependence of solar wind speed

Jul 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987p%26ss...35..913f&link_type=abstract

Planetary and Space Science (ISSN 0032-0633), vol. 35, July 1987, p. 913-920.

Physics

12

Geomagnetic Latitude, Magnetic Flux, Solar Cycles, Solar Wind Velocity, Coronal Holes, Stellar Models, Time Dependence

Scientific paper

The authors study the solar-cycle evolution of solar wind bulk speed as a function of source magnetic field strength. Effects of solar transient events are removed. The background solar wind speed follows a function of the form vsw = v0+v1(1-cosnλm), where λm is the magnetic latitude, set equal to the arc sine of the normalized field strength. The authors find the value of n is largest at solar minimum, and smallest at solar maximum, while v0 and v1 remain fairly constant throughout the solar cycle. This implies the latitudinal gradient in background solar wind speed is steepest at solar minimum and most broad at solar maximum. The lowest and highest background speeds remain fairly constant throughout the solar cycle. The new function is inserted into the improved kinematic code of Hakamada and Akasofu (1982), and solar wind speed and IMF are simulated for two periods in the solar cycle. The authors are able to reproduce observed parameters for specific coronal hole passages.

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