Unusual solar wind structure observed during the 2008 sunspot minimum

Details Unusual solar wind structure observed during the 2008 sunspot minimum Unusual solar wind structure observed during the 2008 sunspot minimum

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh23a1619t&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH23A-1619

Other

2164 Solar Wind Plasma, 7536 Solar Activity Cycle (2162), 7537 Solar And Stellar Variability (1650)

Scientific paper

The solar wind during the sunspot minimum is known to have a stable bimodal structure, which is composed of a low-speed stream in a narrow latitude range around the equator and a high-speed stream over the poles. However, the solar wind structure determined from interplanetary scintillation (IPS) observations of the Solar-Terrestrial Environment Laboratory (STEL) for the current minimum period significantly differs from this typical feature. The STEL IPS observations indicate that the slow wind region extends to higher latitudes, while the fast wind exists over the poles. Furthermore, it is revealed from our IPS observations that another fast wind component is located near the equator, and the slow wind region split into northern and southern parts. This solar wind structure is consistent with a marked increase of the occurrence of fast winds at the Earth. Such an unusual feature may be attributed to the weak magnetic field intensity at the poles in the 2008 solar minimum. We consider that the evolution of the solar wind in the sunspot cycle 24 is likely to be significantly different from the previous ones.

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