Acceleration and Deceleration of CMEs in Interplanetary Space

Details Acceleration and Deceleration of CMEs in Interplanetary Space Acceleration and Deceleration of CMEs in Interplanetary Space

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh32a..04c&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH32A-04

Astronomy and Astrophysics

Astrophysics

[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7519] Solar Physics, Astrophysics, And Astronomy / Flares

Scientific paper

STEREO observations have yielded a number of well observed CME trajectories from the Sun to 1 AU. The measured acceleration and deceleration provide stringent observational constraints on the theoretical understanding of the physical forces acting on CMEs. Recent theory-data comparisons have shown that the dominant contributions to the net force arise from the Lorentz and drag forces acting on flux ropes expanding into the ambient corona and interplanetary medium. In particular, the erupting flux rope (EFR) model of CMEs has been shown to produce model CME trajectories in good agreement, to within 1% of the data, with those of several observed CMEs in the STEREO field of view from the Sun to 1 AU. This is evidence that the EFR equations correctly capture the macroscopic forces acting on the observed CMEs. If these equations are indeed correct for CMEs in general, they can provide the answer to the long-standing question of what drives CMEs and serve as a basis for interpreting observations as well as simulation results. In this talk, I will discuss in quantitative detail the forces responsible for the acceleration and deceleration of observed CMEs using the EFR equations of motion.

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