Global Structure of the Out-of-ecliptic Solar Wind

Details Global Structure of the Out-of-ecliptic Solar Wind Global Structure of the Out-of-ecliptic Solar Wind

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh13a..03w&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SH13A-03

Other

2162 Solar Cycle Variations (7536), 2164 Solar Wind Plasma, 7511 Coronal Holes, 7524 Magnetic Fields, 7536 Solar Activity Cycle (2162)

Scientific paper

We use the observed photospheric field maps and the wind speed observed from Ulysses to study the out-of-ecliptic solar wind. The model calculates the wind speed from the rate of magnetic flux-tube expansion factor using a conversion function that is determined by least-squares fit of all currently available data from Ulysses. Using the best-fit conversion function we investigate the global solar wind at all latitudes, from 90º south to 90º north, covering a 36-year period from 1968 through 2003. The results complement and expand upon earlier studies conducted with IPS and other in situ spacecraft observations. The rotationally averaged wind speed is a function of two parameters: the heliolatitude and the phase of the solar cycle. The out-of-ecliptic solar wind has a recurrent stable structure, the average wind speed varies like a sine square of latitude profile spanning more than 5 years during the declining phase and solar minimum in each solar cycle. Near solar maximum the structure of the out-of-ecliptic solar wind is in a transient state lasting 2 to 3 years when the stable structure breaks down during the disappearance and reappearance of the polar coronal holes. We also report the Ulysses observations of the stable and transient structure.

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