Observations of a prominence eruption and loop contraction

Abstract

Context. Prominence eruptions provide key observations to understand the launch of coronal mass ejections as their cold plasma traces a part of the unstable magnetic configuration. Aims. We select a well observed case to derive observational constraints for eruption models. Methods. We analyze the prominence eruption and loop expansion and contraction observed on 02 March 2015 associated with a GOES M3.7 class flare (SOL2015-03-02T15:27) using the data from Atmospheric Imaging Assembly (AIA) and the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI). We study the prominence eruption and the evolution of loops using the time-distance techniques. Results. The source region is a decaying bipolar active region where magnetic flux cancellation is present for several days before the eruption. AIA observations locate the erupting prominence within a flux rope viewed along its local axis direction. We identify and quantify the motion of loops in contraction and expansion located on the side of the erupting flux rope. Finally, RHESSI hard X-ray observations identify the loop top and two foot-point sources. Conclusions. Both AIA and RHESSI observations support the standard model of eruptive flares. The contraction occurs 19 min after the start of the prominence eruption indicating that this contraction is not associated with the eruption driver. Rather, this prominence eruption is compatible with an unstable flux rope where the contraction and expansion of the lateral loop is the consequence of a side vortex developing after the flux rope is launched.

Filament Eruption Driving EUV Loop Contraction then Expansion above a Stable Filament

“…These vortex flows drive the coronal loops and as a result of this the contraction/expansion in loops observed, depending where the loops are in the vortex. The careful analysis of the contraction/expansion of loops in some studied eruptions filament support the conclusion of the MHD simulations (Dudík et al 2017(Dudík et al , 2019Devi et al 2021).…”

“…This phenomenon is reported with various space borne observations in flare loops with the shrinkage of individual loops while the global loop system expand upwards as further flare loops are formed (Forbes & Acton 1996;Li & Gan 2006;Sui et al 2004;Zhou et al 2008;Joshi et al 2009). Moreover, since the launch of SDO in 2010, observational evidences of coronal loop contraction and expansion, not associated to flare loops, are increasing (Sun et al 2012;Gosain 2012;Liu et al 2012;Zhou et al 2013;Simões et al 2013;Shen et al 2014;Dudík et al 2017;Wang et al 2018;Dudík et al 2019;Devi et al 2021). This is a consequence of SDO continuous high temporal and spatial resolution observations.…”

“…The contraction of all the loops starts almost simultaneously ≈ 21 min after the filament eruption onset. This is in the range 4 to 40 min of the time difference between the onsets of filament eruption and loop contraction reported before (Shen et al 2014;Dudík et al 2016Dudík et al , 2017Wang et al 2018;Devi et al 2021). The speed of the contraction varies from 5 to 10 km s −1 .…”

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

“…Although solar eruptions are symmetric in most of the theoretical models (e.g., Antiochos et al 1999;Chen & Shibata 2000;Lin & Forbes 2000;Moore et al 2001;Jiang et al 2021), the eruptions of prominences are not always radial in observations. Occasionally, the propagations of prominences deviate from the vertical and are termed "non-radial eruptions" (Williams et al 2005;Gosain et al 2009;Shen et al 2011;Sun et al 2012;Bi et al 2013;Kliem et al 2013;Panasenco et al 2013;McCauley et al 2015;Yang et al 2018;Devi et al 2021;Mancuso et al 2021). The apparent inclination angles are between ∼45 • and ∼90 • .…”

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

“…Although solar eruptions are symmetric in most of the theoretical models (e.g., Antiochos et al 1999;Chen & Shibata 2000;Lin & Forbes 2000;Moore et al 2001;Jiang et al 2021), the eruptions of prominences are not always radial in observations. Occasionally, the propagations of prominences deviate from the vertical and are termed "non-radial eruption" (Williams et al 2005;Gosain et al 2009;Shen et al 2011;Sun et al 2012;Bi et al 2013;Kliem et al 2013;Panasenco et al 2013;McCauley et al 2015;Yang et al 2018;Devi et al 2021;Mancuso et al 2021). The apparent inclination angles are between ∼45 • and ∼90 • .…”