Large non-radial propagation of a coronal mass ejection on 2011 January 24

Abstract

Understanding the deflection of coronal mass ejections (CMEs) is of great interest to the space weather community because of their implications for improving the prediction of CME. This paper aims to shed light into the effects of the coronal magnetic field environment on CME trajectories. We analyze the influence of the magnetic environment on the early development of a particular CME event. On 2011 January 24 an eruptive filament was ejected in association with a CME that suffered a large deflection from its source region and expected trajectory. We characterize the 3D evolution of the prominence material using the tie-pointing/triangulation reconstruction technique on EUV and white-light images. To estimate the coordinates in 3D space of the apex of the CME we use a forwardmodeling technique that reproduces the large-scale structure of the flux rope-like CME, the Graduated Cylindrical Shell model. We found that the deflection amounts to 42 in latitude and 20 in longitude and that most of it occurs at altitudes below 4R . Moreover, we found a non-negligible deflection at higher altitudes. Combining images of different wavelengths with the extrapolated magnetic field obtained from a potential field source surface model we confirm the presence of two magnetic structures near the erupting event. The magnetic field environment suggests that field lines from the southern coronal hole act as a magnetic wall that produces the large latitudinal deflection; while a nearby pseudostreamer and a northward extension of the southern coronal hole may be responsible for the eastward deflection of the CME.

Polarity relevance in flux-rope trajectory deflections triggered by coronal holes

“…Studies based on the evolution of CMEs in the high corona agree on the hypothesis that CHs and open magnetic fluxes, acting as strong 'magnetic walls', repel neighbouring CMEs by deflecting their trajectories (Cremades et al 2006;Gopalswamy et al 2009;Gui et al 2011;Yang et al 2018;Cécere et al 2020). However, there are a few peculiar examples for which CME paths behave differently.…”

LUCI onboard Lagrange, the next generation of EUV space weather monitoring

“…The event is described in O'Hara et al 2019, where the eruption, dimmings, and EUV waves associated with the event were tracked. Other studies of eruptions using large FOV EUV observations include Sarkar et al (2019) and Cécere et al (2020). The de-centred configuration of the LUCI FOV will allow it to produce continual observations of the extended EUV solar atmosphere, and provide important observations of the early development of eruptions, during the crucial acceleration phase.…”

Pseudostreamer influence on flux rope evolution

“…It is widely known that the magnetic structures in the vicinity of FRs are capable of deflecting them both in latitude and longitude. While coronal holes (e.g., Cremades et al 2006;Gopalswamy et al 2009;Sahade et al 2020Sahade et al , 2021 and active regions (e.g., Kay et al 2015;Möstl et al 2015;Wang et al 2015) deflect FRs against their location, heliospheric current sheets (e.g., Liewer et al 2015;Wang et al 2020), helmet-streamers (e.g., Zuccarello et al 2012;Yang et al 2018) and pseudostreamers (PSs) (e.g., Bi et al 2013;Wang 2015;Cécere et al 2020;Wang et al 2020) attract FRs to their low magnetic energy regions. Combined effects of the several structures at different heights can be seen in, for example, Sieyra et al (2020).…”