Coronal mass ejections and magnetic flux buildup in the heliosphere

Details Coronal mass ejections and magnetic flux buildup in the heliosphere Coronal mass ejections and magnetic flux buildup in the heliosphere

Oct 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006jgra..11110104o&link_type=abstract

Journal of Geophysical Research, Volume 111, Issue A10, CiteID A10104

Astronomy and Astrophysics

Astrophysics

42

Interplanetary Physics: Interplanetary Magnetic Fields, Interplanetary Physics: Coronal Mass Ejections (7513), Interplanetary Physics: Solar Cycle Variations (7536), Interplanetary Physics: Solar Wind Sources, Solar Physics, Astrophysics, And Astronomy: Solar And Stellar Variability (1650)

Scientific paper

To test for magnetic flux buildup in the heliosphere from coronal mass ejections (CMEs), we simulate heliospheric flux as a constant background open flux with a time-varying interplanetary CME (ICME) contribution. As flux carried by ejecta can only contribute to the heliospheric flux budget while it remains closed, the ICME flux opening rate is an important factor. Two separate forms for the ICME flux opening rate are considered: (1) constant and (2) exponentially decaying with time. Coronagraph observations are used to determine the CME occurrence rates, while in situ observations are used to estimate the magnetic flux content of a typical ICME. Both static equilibrium and dynamic simulations, using the constant and exponential ICME flux opening models, require flux opening timescales of ~50 days in order to match the observed doubling in the magnetic field intensity at 1 AU over the solar cycle. Such timescales are equivalent to a change in the ICME closed flux of only ~7-12% between 1 and 5 AU, consistent with CSE signatures; no flux buildup results. The dynamic simulation yields a solar cycle flux variation with high variability that matches the overall variability of the observed magnetic field intensity remarkably well, including the double peak forming the Gnevyshev gap.

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