Role of coronal mass ejections in the heliospheric Hale cycle

Details Role of coronal mass ejections in the heliospheric Hale cycle Role of coronal mass ejections in the heliospheric Hale cycle

Mar 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007georl..3406104o&link_type=abstract

Geophysical Research Letters, Volume 34, Issue 6, CiteID L06104

Astronomy and Astrophysics

Astrophysics

27

Interplanetary Physics: Solar Cycle Variations (7536), Interplanetary Physics: Interplanetary Magnetic Fields, Interplanetary Physics: Coronal Mass Ejections (7513), Solar Physics, Astrophysics, And Astronomy: Stellar Interiors And Dynamo Theory, Solar Physics, Astrophysics, And Astronomy: Corona

Scientific paper

The 11-year solar cycle variation in the heliospheric magnetic field strength can be explained by the temporary buildup of closed flux released by coronal mass ejections (CMEs). If this explanation is correct, and the total open magnetic flux is conserved, then the interplanetary-CME closed flux must eventually open via reconnection with open flux close to the Sun. In this case each CME will move the reconnected open flux by at least the CME footpoint separation distance. Since the polarity of CME footpoints tends to follow a pattern similar to the Hale cycle of sunspot polarity, repeated CME eruption and subsequent reconnection will naturally result in latitudinal transport of open solar flux. We demonstrate how this process can reverse the coronal and heliospheric fields, and we calculate that the amount of flux involved is sufficient to accomplish the reversal within the 11 years of the solar cycle.

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