Interplanetary Propagation Behavior of the Fast Coronal Mass Ejection from 23 July 2012

Abstract

The fast coronal mass ejection (CME) from 23 July 2012 raised attention due to its extremely short transit time from Sun to 1 AU of less than 21 h. In-situ data from STEREO-A revealed the arrival of a fast forward shock with a speed of more than 2200 km s${}^{-1}$ followed by a magnetic structure moving with almost 1900 km s${}^{-1}$. We investigate the propagation behavior of the CME shock and magnetic structure with the aim to reproduce the short transit time and high impact speed as derived from in-situ data. We carefully measure the 3D kinematics of the CME using the graduated cylindrical shell model, and obtain a maximum speed of 2580$\pm$280 km s${}^{-1}$ for the CME shock and of 2270$\pm$420 km s${}^{-1}$ for its magnetic structure. Based on the 3D kinematics, the drag-based model (DBM) reproduces the observational data reasonably well. To successfully simulate the CME shock, we find that the ambient flow speed should be of average value close to the slow solar wind speed (450 km s${}^{-1}$), and the initial shock speed at a distance of 30 $R_{\odot }$ should not exceed $\approx$2300 km s${}^{-1}$, otherwise it would arrive much too early at STEREO-A. The model results indicate that an extremely low aerodynamic drag force is exerted on the shock, smaller by one order of magnitude compared to the average. As a consequence, the CME hardly decelerates in interplanetary space and maintains its high initial speed. The low aerodynamic drag can only be reproduced when reducing the density of the ambient solar wind flow, in which the massive CME propagates, to ${\rho }_{\mathrm{sw}}$=1-2 cm${}^{-3}$ at the distance of 1 AU. This result is consistent with the preconditioning of interplanetary space owing to a previous CME.

in press for Solar Physics

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