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

Abstract

Context. The traditional cone models achieve great success in studying the geometrical and kinematic properties of halo coronal mass ejections (CMEs). Aims. In this Letter, a revised cone model is proposed to investigate the properties of CMEs as a result of non-radial prominence eruptions. Methods. 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 θ1 and an angle of ϕ1. The length and angular width of the cone are r and ω, respectively. Results. The model was 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 on board the Solar Dynamics Observatory and the Extreme-Ultraviolet Imager on board the ahead Solar TErrestrial RElations Observatory, the properties of the CMEs were derived, including the distance, angular width, inclination angle, deviation from the plane of the sky, and true speed in space. Conclusions. This revised cone model provides a new and complementary approach in exploring the whole evolutions of CMEs.

Reconfiguration and Eruption of a Solar Filament by Magnetic Reconnection with an Emerging Magnetic Field

“…Magnetic reconnection, rearranging the magnetic field topology, is considered to play an important role in the formation mechanisms of filaments (van Ballegooijen and Martens 1989; Kaneko & Yokoyama 2017;Li et al 2021b). Filaments sometimes erupt (Zhang & Wang 2001;Zhou et al 2006;Chen et al 2018;Zhang 2021). Successful filament eruptions are closely associated with other explosive activities on the Sun, such as flares and coronal mass ejections (CMEs; Li et al 2012;Yang et al 2012;Feng et al 2013;Song et al 2015;Yang & Zhang 2018).…”

Tracking the 3D evolution of a halo coronal mass ejection using the revised cone model

“…Isavnin et al (2014) explored the whole propagations of 14 CMEs from the Sun to 1 AU, finding that the deflection of flux ropes occurs below 30 R in most cases. Zhang (2021) applied the revised cone model to two CMEs as a result of nonradial prominence eruptions. Similarly, the inclination angles are 60 • −70 • at the very beginning, and the directions of CMEs become radial in the LASCO FOV.…”

“…To investigate the 3D evolution of CMEs as a result of nonradial filament eruptions, Zhang (2021) proposed a revised cone model (see Fig. 1).…”

Quantifying errors in 3D CME parameters derived from synthetic data using white-light reconstruction techniques

“…For example, the Graduated Cylindrical Shell (GCS; Thernisien et al, 2006Thernisien et al, , 2009Thernisien, 2011) model can use both STEREO viewpoints, together with the additional view from SOHO, and an ad-hoc geometrical CME model to recover the 3D structure of CMEs in the solar corona. Three viewpoints can be employed in a variety of other models, including the Space Weather Prediction Center CME Analysis Tool (SWPC CAT; Millward et al, 2013), the empirical model of Wood & Howard (2009)-applied to 31 events in Wood et al (2017), the Flux Rope in 3D (FRi3D; Isavnin, 2016) model, and the revised cone model (Zhang, 2021(Zhang, , 2022.…”