Preface

Gopalswamy, Ν.; Nieves‐Chinchilla, Teresa; Hidalgo, M. A.; Zhang, J.; Riley, Pete; Driel-Gesztelyi, L. van; Mandrini, C. H.

doi:10.1007/s11207-013-0280-1

Cited by 13 publications

(11 citation statements)

References 3 publications

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“…Yashiro et al (2013) found that the structures of the post-eruption arcades of MCs and non-MC ICMEs during launch have no significant difference. Gopalswamy et al (2013b) observed that MCs and non-MC ICMEs have significant enhancement in Fe and O charge states, and Fe and O charge-state measurements are positively correlated with flare properties, including flare size and soft X-ray flare intensity. Their observations suggest that these CMEs have similar explosive environment and flux rope structures near the sun.…”

Section: Introductionmentioning

confidence: 93%

Comparison of counterstreaming suprathermal electron signatures of ICMEs with and without magnetic cloud: are all ICMEs flux ropes?

Wang

Zhao

Feng

et al. 2019

A&A

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Context. Magnetic clouds (MCs), as large-scale interplanetary magnetic flux ropes, are usually still connected to the sun at both ends near 1 AU. Many researchers believe that all non-MC interplanetary coronal mass ejections (ICMEs) also have magnetic flux rope structures, which are inconspicuous because the observing spacecraft crosses the flanks of the rope structures. If so, the field lines of non-MC ICMEs should also be usually connected to the Sun on both ends. Aims. Then we want to know whether the field lines of most non-MC ICMEs are still connected to the sun at both ends or not. Methods. This study examined the counterstreaming suprathermal electron (CSE) signatures of 266 ICMEs observed by the Advanced Composition Explorer (ACE) spacecraft from 1998 to 2008 and compared the CSE signatures of MCs and non-MC ICMEs.Results. Results show that only 10 of the 101 MC events (9.9% ) and 75 of the 171 non-MC events (43.9%) have no CSEs. Moreover, 21 of the non-MC ICMEs have high CSE percentages (more than 70%) and show relatively stable magnetic field components with slight rotations, which are in line with the expectations that spacecraft passes through the flank of magnetic flux ropes. So the 21 events may be magnetic flux ropes but the ACE spacecraft passes through their flanks of magnetic flux ropes. Conclusions.Considering that most other non-MC events have disordered magnetic fields, we suggest that some non-MC ICMEs inherently have disordered magnetic fields, namely have no magnetic flux rope structures.

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Section: Introductionmentioning

confidence: 93%

Comparison of counterstreaming suprathermal electron signatures of ICMEs with and without magnetic cloud: are all ICMEs flux ropes?

Wang

Zhao

Feng

et al. 2019

A&A

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“…Such a situation is expected for CMEs originating at large central meridian distances. However, eruptions originating within a longitudinal distance of 15º also ended up as EJs at 1 au (Gopalswamy et al 2013a).…”

Section: Introductionmentioning

confidence: 99%

Coronal flux ropes and their interplanetary counterparts

Gopalswamy

Akiyama

Yashiro

et al. 2018

Journal of Atmospheric and Solar-Terrestrial Physics

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Abstract:We report on a study comparing coronal flux ropes inferred from eruption data with their interplanetary counterparts constructed from in situ data. The eruption data include the sourceregion magnetic field, post-eruption arcades, and coronal mass ejections (CMEs). Flux ropes were fit to the interplanetary CMEs (ICMEs) considered for the 2011 and 2012 Coordinated Data Analysis Workshops (CDAWs). We computed the total reconnected flux involved in each of the associated solar eruptions and found it to be closely related to flare properties, CME kinematics, and ICME properties. By fitting flux ropes to the white-light coronagraph data, we obtained the geometric properties of the flux ropes and added magnetic properties derived from the reonnected flux. We found that the CME magnetic field in the corona is significantly higher than the ambient magnetic field at a given heliocentric distance. The radial dependence of the fluxrope magnetic field strength is faster than that of the ambient magnetic field. The magnetic field strength of the coronal flux rope is also correlated with that in interplanetary flux ropes constructed from in situ data, and with the observed peak magnetic field strength in ICMEs. The physical reason for the observed correlation between the peak field strength in MCs is the higher magnetic field content in faster coronal flux ropes and ultimately the higher reconnected flux in the eruption region. The magnetic flux ropes constructed from the eruption data and coronagraph observations provide a realistic input that can be used by various models to predict the magnetic properties of ICMEs at Earth and other destination in the heliosphere.

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“…Some ICMEs are traditionally categorized as magnetic clouds (MCs) that possess a specific set of signatures based on in situ spacecraft measurements of both magnetic field and bulk plasma properties. A more modern view of all ICMEs containing flux ropes is also emerging [ Gopalswamy et al , , ; Xie et al , ; Hu et al , ]. This seems reasonable especially considering that most origination mechanisms for CMEs involve magnetic flux ropes no matter whether they are considered to be preexisting prior to eruption or generated during the process.…”

Section: Introductionmentioning

confidence: 99%

Magnetic field line lengths inside interplanetary magnetic flux ropes

Qiu

Krucker

2015

JGR Space Physics

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We report on the detailed and systematic study of field line twist and length distributions within magnetic flux ropes embedded in interplanetary coronal mass ejections (ICMEs). The Grad‐Shafranov reconstruction method is utilized together with a constant‐twist nonlinear force‐free (Gold‐Hoyle) flux rope model to reveal the close relation between the field line twist and length in cylindrical flux ropes, based on in situ Wind spacecraft measurements. We show that the field line twist distributions within interplanetary flux ropes are inconsistent with the Lundquist model. In particular, we utilize the unique measurements of magnetic field line lengths within selected ICME events as provided by Kahler et al. () based on energetic electron burst observations at 1 AU and the associated type III radio emissions detected by the Wind spacecraft. These direct measurements are compared with our model calculations to help assess the flux rope interpretation of the embedded magnetic structures. By using the different flux rope models, we show that the in situ direct measurements of field line lengths are consistent with a flux rope structure with spiral field lines of constant and low twist, largely different from that of the Lundquist model, especially for relatively large‐scale flux ropes.

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Preface

Cited by 13 publications

References 3 publications

Comparison of counterstreaming suprathermal electron signatures of ICMEs with and without magnetic cloud: are all ICMEs flux ropes?

Comparison of counterstreaming suprathermal electron signatures of ICMEs with and without magnetic cloud: are all ICMEs flux ropes?

Coronal flux ropes and their interplanetary counterparts

Magnetic field line lengths inside interplanetary magnetic flux ropes

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