Effect of Solar Wind Drag on the Determination of the Properties of Coronal Mass Ejections from Heliospheric Imager Data

Details Effect of Solar Wind Drag on the Determination of the Properties of Coronal Mass Ejections from Heliospheric Imager Data Effect of Solar Wind Drag on the Determination of the Properties of Coronal Mass Ejections from Heliospheric Imager Data

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh23c1969k&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH23C-1969

Physics

[2101] Interplanetary Physics / Coronal Mass Ejections, [2194] Interplanetary Physics / Instruments And Techniques

Scientific paper

Coronal mass ejections (CMEs) are the largest eruptions emitted from our sun, releasing large masses of charged particles into the heliosphere. With use of the Heliospheric Imagers (HIs) on the STEREO spacecraft, CMEs can now be tracked through the inner heliosphere up to 1 AU. A few methods fit the time-elongation data from the HIs to determine the CME velocity and direction of propagation. Here the Fixed-Phi (FP) and Harmonic Mean (HM) techniques are analyzed, both methods assume a constant velocity. A simple form of the equation for interplanetary drag is used to model the change in velocity of the CME as it propagate, so that time-elongation tracks can be constructed from them and in turn fitted with the FP and HM fitting methods. In this way, we are able to quantify the error in the fitting methods arising purely from the acceleration and deceleration of the CMEs. It is found that higher viewing angles and velocities give rise to greater error in both methods. Also notable is that the FP method in general gives rise to less error the HM method. For fast CMEs observed behind the limb, the error in the direction due to the deceleration can be as large as 30°.

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