Quantitative Characterization of Magnetic Flux Rope Properties for Two Solar Eruption Events

He, Wen; Hu, Qiang; Jiang, Chaowei; Qiu, Jiong; Prasad, Avijeet

doi:10.48550/arxiv.2201.03149

Cited by 3 publications

(3 citation statements)

References 75 publications

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“…However, such a comparison is not feasible because the current flux rope models based on in situ measurements lack the capability of determining the field-line lengths L. Therefore, the proper evaluation of the total field-line twist based on in situ MC modeling remains challenging. In addition, a 3D field-line configuration also leads to difficulty in defining the poloidal flux of a flux rope, as we discussed in He et al (2022), simply because of the difficulty in defining a central axis.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Validation and Interpretation of a Three-dimensional Configuration of a Magnetic Cloud Flux Rope

Zhu

et al. 2022

ApJ

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One strong magnetic cloud (MC) with a magnetic field magnitude reaching ∼40 nT at 1 au during 2012 June 16–17 is examined in association with a preexisting magnetic flux rope (MFR) identified on the Sun. The MC is characterized by a quasi-three-dimensional (3D) flux rope model based on in situ measurements from the Wind spacecraft. The contents of the magnetic flux and other parameters are quantified. In addition, a correlative study with the corresponding measurements of the same structure crossed by the Venus Express (VEX) spacecraft at a heliocentric distance of 0.7 au and with an angular separation of ∼6° in longitude is performed to validate the MC modeling results. The spatial variation between the Wind and VEX magnetic field measurements is attributed to the 3D configuration of the structure appearing as a knotted bundle of flux. A comparison of the magnetic flux contents between the MC and the preexisting MFR on the Sun indicates that the 3D reconnection process accompanying an M1.9 flare may correspond to the magnetic reconnection between the field lines of the preexisting MFR rooted in the opposite polarity footpoints. Such a process reduces the amount of the axial magnetic flux in the erupted flux rope, by approximately 50%, in this case.

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Section: Conclusion and Discussionmentioning

confidence: 99%

Validation and Interpretation of a Three-dimensional Configuration of a Magnetic Cloud Flux Rope

Zhu

et al. 2022

ApJ

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“…However such a comparison is not feasible because the current flux rope models based on in situ measurements lack the capability to determine the field-line lengths L. Therefore the proper evaluation of the total field-line twist based on in situ MC modeling remains challenging. In addition, a 3D field-line configuration also leads to difficulty in defining the poloidal flux of a flux rope, as we discussed in He et al (2022), simply because of the difficulty in defining a central axis.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Validation and interpretation of three-dimensional configuration of a magnetic cloud flux rope

Hu,

Zhu,

et al. 2022

Preprint

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One "strong" magnetic cloud (MC) with the magnetic field magnitude reaching ∼ 40 nT at 1 au during 2012 June 16-17 is examined in association with a pre-existing magnetic flux rope (MFR) identified on the Sun. The MC is characterized by a quasi-three dimensional (3D) flux rope model based on in situ measurements from the Wind spacecraft. The magnetic flux contents and other parameters are quantified. In addition, a correlative study with the corresponding measurements of the same structure crossed by the Venus Express (VEX) spacecraft at a heliocentric distance 0.7 au and with an angular separation ∼ 6 • in longitude is performed to validate the MC modeling results. The spatial variation between the Wind and VEX magnetic field measurements is attributed to the 3D configuration of the structure as featured by a knotted bundle of flux. The comparison of the magnetic flux contents between the MC and the source region on the Sun indicates that the 3D reconnection process accompanying an M1.9 flare may correspond to the magnetic reconnection between the field lines of the pre-existing MFR rooted in the opposite polarity footpoints.

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“…In addition, important validations to the FS model fitting results were provided through multi-spacecraft studies of CME/ ICME flux ropes by using both multi-point in-situ measurements through one ICME structure [20,21], and multi-spacecraft measurements from both in-situ spacecraft crossing an ICME and the corresponding remote-sensing observations of the CME source region [22,23]. For example, in Hu [20], an MC event observed in May 2007 by both STEREO Behind (STB) and the Advanced Composition Explorer (ACE) spacecraft was examined by fitting the FS model to the STB in-situ data.…”

Section: Introductionmentioning

confidence: 99%

A magnetic flux rope configuration derived by optimization of two-spacecraft In-situ measurements

Chen

2022

Front. Phys.

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Increasingly one interplanetary coronal mass ejection (ICME) structure can propagate across more than one spacecraft in the solar wind. This usually happens when two or more spacecraft are nearly radially aligned with a relatively small longitudinal separation angle from one another. This provides multi-point measurements of the same structure and enables better characterization and validation of modeling results of the structures embedded in these ICMEs. We report such an event during October 13-14, 2019 when the Solar TErrestrial RElations Observatory Ahead (STA) spacecraft and the Parker Solar Probe (PSP) crossed one ICME structure at two different locations with nominal separations in both heliocentric distances and the longitudinal angles. We first perform an optimal fitting to the STA in-situ measurements, based on an analytic quasi-three dimensional (3D) model, yielding a minimum reduced χ2 = 0.468. Then we further apply the optimization approach by combining the magnetic field measurements from both spacecraft along their separate paths across the ICME structure. We find that the output based on the optimization (with the minimum reduced χ2 = 3.15) of the combined two-spacecraft dataset yields a more consistent result, given the much improved agreement of the model output with PSP data. The result demonstrates a magnetic flux rope configuration with clear 3D spatial variations.

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Quantitative Characterization of Magnetic Flux Rope Properties for Two Solar Eruption Events

Cited by 3 publications

References 75 publications

Validation and Interpretation of a Three-dimensional Configuration of a Magnetic Cloud Flux Rope

Validation and Interpretation of a Three-dimensional Configuration of a Magnetic Cloud Flux Rope

Validation and interpretation of three-dimensional configuration of a magnetic cloud flux rope

A magnetic flux rope configuration derived by optimization of two-spacecraft In-situ measurements

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