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

CÉCERE, M., SIEYRA, M.V., CREMADES, H., MIERLA, M., SAHADE, A., STENBORG, G., COSTA, A., WEST, M.J., HUYS, E.D

ADVANCES IN SPACE RESEARCH

ELSEVIER SCI LTD

Lugar: Amsterdam; Año: 2020 vol. 65 p. 1654 - 1662

0273-1177

This paper aims to shed light into the effects of the coronal magnetic field environment on CME trajectories. We analyze the influence of themagnetic environment on the early development of a particular CME event. On 2011 January 24 an eruptive filament is ejected in association witha coronal mass ejection that suffers a large deflection from its source region. We characterize the 3D evolution of the prominence material usingthe tie-pointing/triangulation reconstruction technique on EUV and white-light images. To estimate the coordinates in 3D space of the apex of theCME we use a forward-modeling technique that reproduces the large-scale structure of the flux rope-like CME, the Graduated Cylindrical Shellmodel. We found that the deflection amounts 42 ◦ in latitude and 20 ◦ in longitude and that most of it occurs at altitudes below 4R . Moreover, wefound a non-negligible deflection at higher altitudes. Combining images of different wavelengths with the interpolated magnetic field obtainedfrom a potential field source surface model we found 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 CME eastward deflection.