Uncovering erosion effects on magnetic flux rope twist

Pal, Sanchita; Kilpua, Emilia; Good, Simon; Pomoell, Jens; Price, Daniel J.

doi:10.1051/0004-6361/202040070

Cited by 25 publications

(14 citation statements)

References 55 publications

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“…Magnetic erosion affects ∼30% of the ICMEs at 1 au, and it can be most reliably identified from the presence of reconnection exhausts and bifurcated current sheets near FR boundaries (Ruffenach et al 2015). Erosion also implies large-scale magnetic field topological changes occurring within ICMEs (Ruffenach et al 2012;Pal et al 2021), and yet, the full breadth of effects on magnetic field configurations within MEs and FRs therein remains unclear. In the following, we investigate the relationship between ME and FR duration as a potential proxy for magnetic erosion.…”

Section: Fr-to-me Duration Scaling With Heliocentric Distancementioning

confidence: 99%

Causes and Consequences of Magnetic Complexity Changes within Interplanetary Coronal Mass Ejections: a Statistical Study

Scolini,

Winslow,

Lugaz

et al. 2021

Preprint

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We present the first statistical analysis of complexity changes affecting the magnetic structure of interplanetary coronal mass ejections (ICMEs), with the aim of answering the questions: How frequently do ICMEs undergo magnetic complexity changes during propagation? What are the causes of such changes? Do the in situ properties of ICMEs differ depending on whether they exhibit complexity changes? We consider multi-spacecraft observations of 31 ICMEs by MESSENGER, Venus Express, ACE, and STEREO between 2008 and 2014 while radially aligned. By analyzing their magnetic properties at the inner and outer spacecraft, we identify complexity changes which manifest as fundamental alterations or significant re-orientations of the ICME. Plasma and suprathermal electron data at 1 au, and simulations of the solar wind enable us to reconstruct the propagation scenario for each event, and to identify critical factors controlling their evolution. Results show that ∼65% of ICMEs change their complexity between Mercury and 1 au and that interaction with multiple large-scale solar wind structures is the driver of these changes. Furthermore, 71% of ICMEs observed at large radial (>0.4 au) but small longitudinal (< 15 • ) separations exhibit complexity changes, indicating that propagation over large distances strongly affects ICMEs. Results also suggest ICMEs may be magnetically coherent over angular scales of at least 15 • , supporting earlier theoretical and observational estimates. This work presents statistical evidence that magnetic complexity changes are consequences of ICME interactions with large-scale solar wind structures, rather than intrinsic to ICME evolution, and that such changes are only partly identifiable from in situ measurements at 1 au.

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Section: Fr-to-me Duration Scaling With Heliocentric Distancementioning

confidence: 99%

Causes and Consequences of Magnetic Complexity Changes within Interplanetary Coronal Mass Ejections: a Statistical Study

Scolini,

Winslow,

Lugaz

et al. 2021

Preprint

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“…It exhibits a tail-like structure after around June 26 02:00 UT where the field components remain essentially constant. This is often interpreted as a sign of flux-rope erosion by magnetic reconnection with the ambient wind (e.g., Dasso et al 2007;Pal et al 2021).…”

Section: June 23 Cmementioning

confidence: 99%

Multipoint Interplanetary Coronal Mass Ejections Observed with Solar Orbiter, BepiColombo, Parker Solar Probe, Wind, and STEREO-A

Möstl

Weiss²,

Reiss³

et al. 2022

Preprint

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<p>We present the results of a search for multipoint in situ and imaging observations of interplanetary coronal mass ejections (ICMEs) with the Heliophysics System Observatory, from 2020 April to present day. This builds up on our recent publication in ApJ Letters introducing the living ICME lineup catalog available at https://helioforecast.space/lineups. We highlight a few new lineup events captured by those spacecraft from September to November 2021, when all were located within 50 degrees east of the Sun-Earth line. Multi-messenger observations of ICME flux ropes and shocks are much needed to make progress on the understanding of the global magnetic configuration of ICMEs, space weather forecasting, the magnetic connectivity of the solar wind to the Sun and the propagation of solar energetic particles.</p>

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“…Moreover, the percentage of eroded magnetic flux is very case dependent and so this needs to be taken into account in MC studies. In particular, from the analysis of two studiedcases, Pal et al (2021) concluded that the erosion has significant effects on the obtained magnetic flux rope twist, as it is expected mainly due to the lack of its external part, which typically is highly twisted.…”

Section: Introductionmentioning

confidence: 99%

A robust estimation of the twist distribution in magnetic clouds

Lanabere

Démoulin

Dasso

2022

A&A

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Context. Magnetic clouds (MCs) are observed in situ by spacecraft. The rotation of their magnetic field is typically interpreted as the crossing of a twisted magnetic flux tube, or flux rope, which was launched from the solar corona. Aims. The detailed magnetic measurements across MCs permit us to infer the flux rope characteristics. Still, the precise spatial distribution of the magnetic twist is challenging, and thus is debated. Methods. In order to improve the robustness of the results, we performed a superposed epoch analysis (SEA) of a set of well observed MCs at 1 au. While previous work was done using the MC central time, we here used the result of a fitted flux rope model to select the time of the closest approach to the flux rope axis. This implies a precise separation of the in-and outbound regions to coherently phase the observed signals. We also searched for and minimised the possible biases such as magnetic asymmetry and a finite impact parameter.Results. We applied the SEA to derive the median profiles both for the flux rope remaining when crossed by the spacecraft and to recover the one present before erosion. In particular, the median azimuthal B component is nearly a linear function of the radius. More generally, the results confirm our previous results realised without such a deep analysis. The twist profile is nearly uniform in the flux rope core, with a steep increase at the border of the flux rope and with similar profiles in the in-and outbound regions. The main difference with our previous study is a larger twist by ∼ 20%.

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Uncovering erosion effects on magnetic flux rope twist

Cited by 25 publications

References 55 publications

Causes and Consequences of Magnetic Complexity Changes within Interplanetary Coronal Mass Ejections: a Statistical Study

Causes and Consequences of Magnetic Complexity Changes within Interplanetary Coronal Mass Ejections: a Statistical Study

Multipoint Interplanetary Coronal Mass Ejections Observed with Solar Orbiter, BepiColombo, Parker Solar Probe, Wind, and STEREO-A

A robust estimation of the twist distribution in magnetic clouds

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