Faraday Rotation Response to Coronal Mass Ejection Structure

Details Faraday Rotation Response to Coronal Mass Ejection Structure Faraday Rotation Response to Coronal Mass Ejection Structure

Aug 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010soph..265...31j&link_type=abstract

Solar Physics, Volume 265, Issue 1-2, pp. 31-48

Physics

2

Coronal Mass Ejections, Helicity, Magnetic, Observations, Theory, Instrumental Effects, Integrated Sun Observations, Magnetic Fields, Corona, Interplanetary, Models, Polarization, Radio, Radio Scintillation, Rotation, Solar Wind, Disturbances

Scientific paper

We present the results from modeling the coronal mass ejection (CME) properties that have an effect on the Faraday rotation (FR) signatures that may be measured with an imaging radio antenna array such as the Murchison Widefield Array (MWA). These include the magnetic flux rope orientation, handedness, magnetic-field magnitude, velocity, radius, expansion rate, electron density, and the presence of a shock/sheath region. We find that simultaneous multiple radio source observations (FR imaging) can be used to uniquely determine the orientation of the magnetic field in a CME, increase the advance warning time on the geoeffectiveness of a CME by an order of magnitude from the warning time possible from in-situ observations at L 1, and investigate the extent and structure of the shock/sheath region at the leading edge of fast CMEs. The magnetic field of the heliosphere is largely "invisible" with only a fraction of the interplanetary magnetic-field lines convecting past the Earth; remote sensing the heliospheric magnetic field through FR imaging from the MWA will advance solar physics investigations into CME evolution and dynamics.

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