Solar and Heliospheric Physics
Coronal mass ejections and magnetic flux buildup in the heliosphere
Article first published online: 11 OCT 2006
Copyright 2006 by the American Geophysical Union.
Journal of Geophysical Research: Space Physics (1978–2012)
Volume 111, Issue A10, October 2006
How to Cite
2006), Coronal mass ejections and magnetic flux buildup in the heliosphere, J. Geophys. Res., 111, A10104, doi:10.1029/2006JA011641., and (
- Issue published online: 11 OCT 2006
- Article first published online: 11 OCT 2006
- Manuscript Accepted: 25 MAY 2006
- Manuscript Revised: 26 APR 2006
- Manuscript Received: 31 JAN 2006
- heliospheric flux;
- interplanetary magnetic field
 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.