A revised cone model and its application to non-radial prominence eruptions

Abstract

The traditional cone models achieve great success in studying the geometrical and kinematic properties of halo coronal mass ejections (CMEs). In this paper, a revised cone model is proposed to investigate the properties of CMEs as a result of non-radial prominence eruptions. The cone apex is located at the source region of an eruption instead of the Sun center. The cone axis deviates from the local vertical by an inclination angle of ${\theta }_1$ and an angle of ${\varphi }_1$. The length and angular width of the cone are $r$ and $\omega$, respectively. The model is successfully applied to two CMEs originating from the western limb on 2011 August 11 and 2012 December 7. By comparing the projections of the cones with the CME fronts simultaneously observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO) and the Extreme-Ultraviolet Imager (EUVI) on board the ahead Solar TErrestrial RElations Observatory (STEREO), the properties of the CMEs are derived, including the distance, angular width, inclination angle, deviation from the plane of the sky, and true speed in space. This revised cone model provides a new and complementary approach in exploring the whole evolutions of CMEs.

5 pages, 4 figures, accepted for publication in A&A Letters

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• On the three-dimensional relation between the coronal dimming, erupting filament and CME. Case study of the 28 October 2021 X1.0 event
• Reconfiguration and eruption of a solar filament by magnetic reconnection with an emerging magnetic field
• Understanding the deflection of the `Cartwheel CME': data analysis and modeling
• Rapid Rotation of an Erupting Prominence and the Associated Coronal Mass Ejection on 13 May 2013
• Analysis of solar eruptions deflecting in the low corona: influence of the magnetic environment
• Theoretical Studies on the Evolution of Solar Filaments in Response to New Emerging Flux
• The Kinematical Behavior of Solar Eruptive Filaments Affected by the Poloidal Magnetic Field