Origin and Ion Charge State Evolution of Solar Wind Transients during 4 – 7 August 2011

Rodkin, Denis; Goryaev, F. F.; Pagano, Paolo; Gibb, G.; Slemzin, V. A.; Shugay, Yu. S.; Veselovsky, I. S.; Mackay, D. H.

doi:10.1007/s11207-017-1109-0

Cited by 25 publications

(23 citation statements)

References 81 publications

(110 reference statements)

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“…This arises because the global model does not follow the detailed dynamics within active regions, so that, for example, multiple eruptions from within the same active region can not be reproduced in the simulation. When higher resolution magnetograms are used as input to drive the model, it has been shown to reproduce well the formation and eruption of flux ropes within individual active regions (Gibb et al 2014;Rodkin et al 2017). But at present it is not possible to include such fine detail within globalscale simulations, not least because magnetogram data are not available simultaneously over the full solar surface.…”

Section: Coronal Magnetic Field Modelmentioning

confidence: 99%

Magnetic Flux Rope Identification and Characterization from Observationally Driven Solar Coronal Models

Lowder

Yeates

2017

ApJ

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Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. Submitted to ApJ ABSTRACT Formed through magnetic field shearing and reconnection in the solar corona, magnetic flux ropes are structures of twisted magnetic field, threaded along an axis. Their evolution and potential eruption are of great importance for space weather. Here we describe a new methodology for the automated detection of flux ropes in simulated magnetic fields, utilizing fieldline helicity. Our Flux Rope Detection and Organization (FRoDO) code is publicly available, and measures the magnetic flux and helicity content of pre-erupting flux ropes over time, as well as detecting eruptions. As a first demonstration the code is applied to the output from a time-dependent magnetofrictional model, spanning 1996 June 15 -2014 February 10. Over this period, 1561 erupting and 2099 non-erupting magnetic flux ropes are detected, tracked, and characterized. For this particular model data, erupting flux ropes have a mean net helicity magnitude of 2.66 × 10 43 Mx 2 , while non-erupting flux ropes have a significantly lower mean of 4.04 × 10 42 Mx 2 , although there is overlap between the two distributions. Similarly, the mean unsigned magnetic flux for erupting flux ropes is 4.04×10 21 Mx, significantly higher than the mean value of 7.05×10 20 Mx for non-erupting ropes. These values for erupting flux ropes are within the broad range expected from observational and theoretical estimates, although the eruption rate in this particular model is lower than that of observed coronal mass ejections. In future the FRoDO code will prove a valuable tool for assessing the performance of different non-potential coronal simulations and comparing them with observations.

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Section: Coronal Magnetic Field Modelmentioning

confidence: 99%

Magnetic Flux Rope Identification and Characterization from Observationally Driven Solar Coronal Models

Lowder

Yeates

2017

ApJ

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“…Amari et al (2014) model the solar eruption from AR 10930 by using the vector magnetograms taken from the Hinode/SOT. Rodkin et al (2017) coupled the NLFF and MHD model to produce the CME on 2 August 2011. They use the NLFF to obtain a flux rope.…”

Section: Introductionmentioning

confidence: 99%

New data-driven method of simulating coronal mass ejections

Liu

Chen

Zhao

2019

A&A

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Context. Coronal mass ejections (CMEs) are large eruptions of plasma and magnetic field from the Sun’s corona. Understanding the evolution of the CME is important to evaluate its impact on space weather. Using numerical simulation, we are able to reproduce the occurrence and evolution process of the CME. Aims. The aim of this paper is to provide a new data-driven method to mimic the coronal mass ejections. By using this method, we can investigate the phsical mechanisms of the flux rope formation and the cause of the CME eruption near the real background. Methods. Starting from a potential magnetic field extrapolation, we have solved a full set of magnetohydrodynamic (MHD) equations by using the conservation element and solution element (CESE) numerical method. The bottom boundary is driven by the vector magnetograms obtained from SDO/HMI and vector velocity maps derived from DAVE4VM method. Results. We present a three-dimensional numerical MHD data-driven model for the simulation of the CME that occurred on 2015 June 22 in the active region NOAA 12371. The numerical results show two elbow-shaped loops formed above the polarity inversion line (PIL), which is similar to the tether-cutting picture previously proposed. The temporal evolutions of magnetic flux show that the sunspots underwent cancellation and flux emergence. The signature of velocity field derived from the tracked magnetograms indicates the persistent shear and converging motions along the PIL. The simulation shows that two elbow-shaped loops were reconnected and formed an inverse S-shaped sigmoid, suggesting the occurrence of the tether-cutting reconnection, which was supported by observations of the Atmospheric Imaging Assembly (AIA) telescope. Analysis of the decline rate of the magnetic field indicates that the flux rope reached a region where the torus instability was triggered. Conclusions. We conclude that the eruption of this CME was caused by multiple factors, such as photosphere motions, reconnection, and torus instability. Moreover, our simulation successfully reproduced the three-component structures of typical CMEs.

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“…The most possible sources of this event were two CMEs erupted from the Sun on 3 -4 August 2011 (see Table 3). A case study of this complex event consisting of several solar wind transients detected by ACE on 4 -7 August 2011 was presented by Rodkin et al (2017). Contrary to the case of merged CMEs shown in Figure 4, one can see here one shock and one ejecta coinciding with the ICME in the RC list.…”

Section: Complex Ejecta With Strong Interactionmentioning

confidence: 96%

Single ICMEs and Complex Transient Structures in the Solar Wind in 2010 – 2011

et al. 2018

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We analyzed statistics, solar sources and properties of interplanetary coronal mass ejections (ICMEs) in the solar wind. In comparison with the first eight years of Cycle 23, during the same period of Cycle 24 the yearly numbers of ICMEs were less correlated with the flare numbers (0.68 vs 0.78) and sunspot numbers (0.66 vs 0.81), whereas the ICME correlation with coronal mass ejections (CMEs) was higher (0.77 vs 0.70). For the period Space Research Institute (IKI RAS) 84/32, Profsoyznaya str., Moscow, 117810, Russia SOLA: ICME_and_their_Solar_Origins_rev-2.tex; 19 February 2018; 2:58; p. 1 D.Rodkin et al.of the Earth-directed CMEs supplemented by modeling of their propagation in the heliosphere using the kinematic models (the ballistic and drag-based model) and the Wang-Sheeley-Arge Enlil Cone MHD-based model. A detailed analysis of the ICME solar sources in the period under study showed that in 11 cases out of 23 (48 %) the observed ICME might be associated with two or more sources. In cases of multiple-source events, the resulting solar wind disturbances may be described as complex (merged) structures occurred due to the stream interactions with properties depending on the type of participating streams. As a reliable marker for identification of interacting streams and their sources, we used the plasma ion composition, as it becomes frozen in the low corona and remains unchanged in the heliosphere. According to the ion composition signatures, we classified these cases into three types: complex ejecta originating from weak and strong CME-CME interactions, as well as merged interaction regions (MIRs) originating from the CME-high-speed stream (HSS) interactions. We described temporal profiles of the ion composition for the single-source and multi-source solar wind structures and compared them with the ICME signatures determined from the kinematic and magnetic field parameters of the solar wind. In singlesource events, the ion charge state, as a rule, has one-peak enhancement with average duration of ∼ 1 day, which is similar to the mean ICME duration of 1.12 days derived from the Richardson and Cane list. In the multi-source events, the total profile of the ion charge state consists of a sequence of enhancements associated with interaction between the participating streams. On average, the total duration of complex structures appearing due to the CME-CME and CME-HSS interactions as determined from their ion composition is 2.4 days, which is more than 2 times longer than that of the single-source events.

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Origin and Ion Charge State Evolution of Solar Wind Transients during 4 – 7 August 2011

Cited by 25 publications

References 81 publications

Magnetic Flux Rope Identification and Characterization from Observationally Driven Solar Coronal Models

Magnetic Flux Rope Identification and Characterization from Observationally Driven Solar Coronal Models

New data-driven method of simulating coronal mass ejections

Single ICMEs and Complex Transient Structures in the Solar Wind in 2010 – 2011

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