Quantitative relationship between the trajectories of CMEs and evolution of their magnetic fields

Details Quantitative relationship between the trajectories of CMEs and evolution of their magnetic fields Quantitative relationship between the trajectories of CMEs and evolution of their magnetic fields

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh23a1949k&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH23A-1949

Astronomy and Astrophysics

Astrophysics

[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields

Scientific paper

Coronal mass ejections (CMEs) are the solar drivers of large geomagnetic storms. With the new observations using the twin-spacecraft SECCHI/STEREO configuration, it is now possible to observe CME trajectories from the Sun to 1 AU from one spacecraft and, in cases where the ejecta is encountered by the other spacecraft, measure the in situ magnetic field and plasma properties of the CME ejecta. We have examined a number of CME events where the trajectories were continuously observed by one STEREO spacecraft and the ejecta were intersected by the another spacecraft at the L1 Lagrange point. We have applied the erupting flux rope model of CMEs (EFR) to these events and calculated the solutions that best fit the observed trajectories. Using these solutions, we have obtained a number of best-fit physical quantities such as the footpoint separation distance of the initial flux rope, the temporal profile of associated X-ray profiles, and the magnetic field strength at 1 AU. In this paper, we focus on the magnetic field and the ejecta plasma parameters. For each event, we find that there is a narrow range of solutions that fit the observed trajectory to within 1 to 2 percent of the position data throughout the 1-AU STEREO field of view (FOV). It is found that the magnitude of the magnetic field and plasma parameters at 1 AU predicted by the best-fit solutions are in good agreement with the in situ data for each event. In particular, the calculated average temperature is lower than the ambient temperature, consistent with being magnetic clouds. The paper shows how the magnetic field of a CME evolves through interplanetary space, emphasizing the quantitative relationship between the CME trajectory and the evolution of the CME magnetic field. The discussion will focus on a physical understanding that can be used to interpret observational data and numerical results of simulation models of CMEs. The arrival time and the magnetic field configuration inside a flux rope, however, depend on the detailed three dimensional geometry (e.g., orientation), which has not been addressed by the present work.

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