Evidence of Posteruption Reconnection Associated with Coronal Mass Ejections in the Solar Wind

Details Evidence of Posteruption Reconnection Associated with Coronal Mass Ejections in the Solar Wind Evidence of Posteruption Reconnection Associated with Coronal Mass Ejections in the Solar Wind

Oct 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002apj...578..972r&link_type=abstract

The Astrophysical Journal, Volume 578, Issue 2, pp. 972-978.

Astronomy and Astrophysics

Astronomy

29

Sun: Solar Wind, Sun: Activity, Sun: Corona, Sun: Coronal Mass Ejections (Cmes), Sun: Magnetic Fields

Scientific paper

Using a coupled 2.5-dimensional, time-dependent MHD model of the solar corona and inner heliosphere, we have simulated the eruption and evolution of a coronal mass ejection containing a flux rope all the way from the Sun to 1 AU. Although idealized, we find that the simulation reproduces many generic features of magnetic clouds. In this paper we report on a new, intriguing aspect of these comparisons. Specifically, the results suggest that jetted outflow, driven by posteruptive reconnection underneath the flux rope, occurs and may remain intact out to 1 AU and beyond. We present an example of a magnetic cloud with precisely these signatures and show that the velocity perturbations are consistent with reconnection outflow. We suggest that other velocity and/or density enhancements observed trailing magnetic clouds may be signatures of such reconnection and, in some cases, may not be associated with prominence material, as has previously been suggested.

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