Uncovering erosion effects on magnetic flux rope twist

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Pal , S , Kilpua , E , Good , S , Pomoell , J & Price , D 2021 , ' Uncovering erosion effects on magnetic flux rope twist ' , Astronomy & Astrophysics , vol. 650 , 176 . https://doi.org/10.1051/0004-6361/202040070

Title: Uncovering erosion effects on magnetic flux rope twist
Author: Pal, Sanchita; Kilpua, Emilia; Good, Simon; Pomoell, Jens; Price, Daniel
Contributor: University of Helsinki, Particle Physics and Astrophysics
University of Helsinki, Space Physics Research Group
University of Helsinki, Particle Physics and Astrophysics
University of Helsinki, Department of Physics
University of Helsinki, Space Physics Research Group
Date: 2021-06-25
Language: eng
Number of pages: 7
Belongs to series: Astronomy & Astrophysics
ISSN: 0004-6361
URI: http://hdl.handle.net/10138/333496
Abstract: Context. Magnetic clouds (MCs) are transient structures containing large-scale magnetic flux ropes from solar eruptions. The twist of magnetic field lines around the rope axis reveals information about flux rope formation processes and geoeffectivity. During propagation MC flux ropes may erode via reconnection with the ambient solar wind. Any erosion reduces the magnetic flux and helicity of the ropes, and changes their cross-sectional twist profiles. Aims. This study relates twist profiles in MC flux ropes observed at 1 AU to the amount of erosion undergone by the MCs in interplanetary space. Methods. The twist profiles of two clearly identified MC flux ropes associated with the clear appearance of post eruption arcades in the solar corona are analyzed. To infer the amount of erosion, the magnetic flux content of the ropes in the solar atmosphere is estimated, and compared to estimates at 1 AU. Results. The first MC shows a monotonically decreasing twist from the axis to the periphery, while the second displays high twist at the axis, rising twist near the edges, and lower twist in between. The first MC displays a larger reduction in magnetic flux between the Sun and 1 AU, suggesting more erosion than that seen in the second MC. Conclusions. In the second cloud the rising twist at the rope edges may have been due to an envelope of overlying coronal field lines with relatively high twist, formed by reconnection beneath the erupting flux rope in the low corona. This high-twist envelope remained almost intact from the Sun to 1 AU due to the low erosion levels. In contrast, the high-twist envelope of the first cloud may have been entirely peeled away via erosion by the time it reaches 1 AU.
Subject: Sun: coronal mass ejections (CMEs)
magnetic reconnection
Sun: heliosphere
solar-terrestrial relations
Sun: magnetic fields
CORONAL MASS EJECTION
CLOUD EROSION
MODEL
RECONNECTION
HELICITY
TOPOLOGY
PROFILE
LOOP
115 Astronomy, Space science
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