Observations of the Coronal Mass Ejection with a Complex Acceleration Profile

Abstract

We study the coronal mass ejection (CME) with a complex acceleration profile. The event occurred on April 23, 2009. It had an impulsive acceleration phase, an impulsive deceleration phase, and a second impulsive acceleration phase. During its evolution, the CME showed signatures of different acceleration mechanisms: kink instability, prominence drainage, flare reconnection, and a CME-CME collision. The special feature of the observations is the usage of the TESIS EUV telescope. The instrument could image the solar corona in the Fe 171Å line up to a distance of 2 R ⊙ from the center of the Sun. This allows us to trace the CME up to the LASCO/C2 field of view without losing the CME from sight. The onset of the CME was caused by kink instability. The mass drainage occurred after the kink instability. The mass drainage played only an auxiliary role: it decreased the CME mass, which helped to accelerate the CME. The first impulsive acceleration phase was caused by the flare reconnection. We observed the two ribbon flare and an increase of the soft X-ray flux during the first impulsive acceleration phase. The impulsive deceleration and the second impulsive acceleration phases were caused by the CME-CME collision. The studied event shows that CMEs are complex phenomena that cannot be explained with only one acceleration mechanism. We should seek a combination of different mechanisms that accelerate CMEs at different stages of their evolution.

Magnetic Structure of an Erupting Filament

“…The amplitudes of such dynamics are also significantly larger than those at the smaller scales, with velocities and displacements in the region of 30 -100 km s −1 and 110 Mm, respectively (e.g., Luna & Karpen 2012;Luna et al 2014;Liakh et al 2020). More recently, similarly large-scale and correlated mass motions occurring in the lead-up to a filament eruption have been added to the conditions for global flux rope stability (e.g., Bi et al 2014;Reva et al 2017;Jenkins et al 2018Jenkins et al , 2019Fan 2020), alongside the more commonly-considered stability conditions (e.g., torus/kink instability, breakout reconnection, tether cutting, etc. ; Antiochos et al 1999;Moore et al 2001;Török & Kliem 2005;Kliem & Török 2006).…”

Monochromatic X-Ray Imagers of the Sun Based on the Bragg Crystal Optics

“…In 2009, the Sun was in the minimum of the solar activity. The data were mainly used to study microflares (Kirichenko and Bogachev, 2017a,b) and hot plasma dynamics during Coronal Mass Ejection (CMEs) (Kirichenko and Bogachev, 2013;Reva et al, 2017).…”

KORTES Mission for Solar Activity Monitoring Onboard International Space Station

“…The effective focal length of all three telescopes equals to 1,740 mm giving a field of view (FoV) of 0.91 • to enable widefield observations of CME formation and flux-rope eruptions. The main advantage of the KORTES telescopes over other EUV telescopes and coronographs, e.g., LASCO/C2 and C3 (Brueckner et al, 1995) or SDO/AIA (Lemen et al, 2012), is that they may provide valuable observations in the so-called "blind zone"-the gap in solar altitudes between 1.2 and 2 solar radii (Reva et al, 2014(Reva et al, , 2017.…”