Dependence of Coronal Mass Ejection Properties on Their Solar Source Active Region Characteristics and Associated Flare Reconnection Flux

Pal, Sanchita; Nandy, Dibyendu; Srivastava, Nandita; Gopalswamy, N.; Panda, Suman

doi:10.3847/1538-4357/aada10

Cited by 35 publications

(27 citation statements)

References 91 publications

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“…Because of the pressure imbalance between the CME and the surrounding solar wind upon insertion in the heliospheric domain (leading to an expansion of the CME structure, as shown by Scolini et al 2019Scolini et al , 2021, the effective initial CME speed is ∼ 1100 km s −1 , which results in a fast CME that drives an interplanetary shock and sheath, as discussed in Section 3. Such a combination of initial parameters is representative of those of a typical fast CME with a reconnected flux of the order of 10 14 Wb (Pal et al 2018). The CME initial direction is chosen to reproduce two end-member scenarios of interaction with different solar wind structures (shown in panels (b) and (d) in Figure 1): in run A, the CME is inserted across the HCS/HPS at (θ, φ) = (0 • , 0 • ); in run B, the CME is inserted across the HSS at (θ, φ) = (5 • , 0 • ), in a configuration similar to that of CMEs originated from "anemone" active regions (e.g.…”

Section: Modeling Set-upmentioning

confidence: 99%

Evolution of Interplanetary Coronal Mass Ejection Complexity: A Numerical Study through a Swarm of Simulated Spacecraft

Scolini

Winslow

Lugaz

et al. 2021

ApJL

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In-situ measurements carried out by spacecraft in radial alignment are critical to advance our knowledge on the evolutionary behavior of coronal mass ejections (CMEs) and their magnetic structures during propagation through interplanetary space. Yet, the scarcity of radially aligned CME crossings restricts investigations on the evolution of CME magnetic structures to a few case studies, preventing a comprehensive understanding of CME complexity changes during propagation. In this paper, we perform numerical simulations of CMEs interacting with different solar wind streams using the linear force-free spheromak CME model incorporated into the EUropean Heliospheric FORecasting Information Asset (EUHFORIA) model. The novelty of our approach lies in the investigation of the evolution of CME complexity using a swarm of radially aligned, simulated spacecraft. Our scope is to determine under which conditions, and to what extent, CMEs exhibit variations of their magnetic structure and complexity during propagation, as measured by spacecraft that are radially aligned. Results indicate that the interaction with large-scale solar wind structures, and particularly with stream interaction regions, doubles the probability to detect an increase of the CME magnetic complexity between two spacecraft in radial alignment, compared to cases without such interactions. This work represents the first attempt to quantify the probability of detecting complexity changes in CME magnetic structures by spacecraft in radial alignment using numerical simulations, and it provides support to the interpretation of multi-point CME observations involving past, current (such as Parker Solar Probe and Solar Orbiter), and future missions.

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Section: Modeling Set-upmentioning

confidence: 99%

Evolution of Interplanetary Coronal Mass Ejection Complexity: A Numerical Study through a Swarm of Simulated Spacecraft

Scolini

Winslow

Lugaz

et al. 2021

ApJL

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“…Because of the difficulty in observing CME evolution and measuring CME acceleration in the low corona, many studies instead compare the CME velocity measured at a few solar radii after the peak acceleration phase, and the total magnetic flux reconnected during the flare. These studies found that, in fast CME events, these two quantities are positively correlated (Qiu & Yurchyshyn 2005;Deng & Welsch 2017;Toriumi et al 2017;Tschernitz et al 2018;Pal et al 2018). Note that most of these studies have focused on fast CMEs and strong flares, and it is unclear whether this relationship applies to a broader range of CMEs, in particular, slow CMEs.…”

Section: Introductionmentioning

confidence: 99%

How Does Magnetic Reconnection Drive the Early-stage Evolution of Coronal Mass Ejections?

Zhu

Qiu

Liewer

et al. 2020

ApJ

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Theoretically, CME kinematics are related to magnetic reconnection processes in the solar corona. However, the current quantitative understanding of this relationship is based on the analysis of only a handful of events. Here we report a statistical study of 60 CME-flare events from August 2010 to December 2013. We investigate kinematic properties of CMEs and magnetic reconnection in the low corona during the early phase of the eruptions, by combining limb observations from STEREO with simultaneous on-disk views from SDO. For a subset of 42 events with reconnection rate evaluated by the magnetic fluxes swept by the flare ribbons on the solar disk observed from SDO, we find a strong correlation between the peak CME acceleration and the peak reconnection rate. Also, the maximum velocities of relatively fast CMEs ( 600 km s −1 ) are positively correlated with the reconnection flux, but no such correlation is found for slow CMEs. A time-lagged correlation analysis suggests that the distribution of the time lag of CME acceleration relative to reconnection rate exhibits three peaks, approximately 10 minutes apart, and on average, acceleration-lead events have smaller reconnection rates. We further compare the CME total mechanical energy with the estimated energy in the current sheet. The comparison suggests that, for small-flare events, reconnection in the current sheet alone is insufficient to fuel CMEs. Results from this study suggest that flare reconnection may dominate

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“…It is thus not possible to extract information for the magnetic flux of the CME using cotemporal magnetogram-based approaches (e.g. see Dissauer et al 2018a,b;Pal et al 2018;Dissauer et al 2019;Sarkar et al 2020). In this case, a base value of 80.0 × 10 12 Wb was used for the EUHFORIA runs, which represents the toroidal flux and is related to the magnetic field strength via equation 7 given in Verbeke et al (2019b).…”

Section: Magnetic Flux and Helicity Signmentioning

confidence: 99%

Modelling a multi-spacecraft coronal mass ejection encounter with EUHFORIA

Asvestari

Pomoell

Kilpua

et al. 2021

A&A

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Context. Coronal mass ejections (CMEs) are a manifestation of the Sun's eruptive nature. They can have a great impact on Earth, but also on human activity in space and on the ground. Therefore, modelling their evolution as they propagate through interplanetary space is essential. Aims. EUropean Heliospheric FORecasting Information Asset (EUHFORIA) is a data-driven, physics-based model, tracing the evolution of CMEs through background solar wind conditions. It employs a spheromak flux rope, which provides it with the advantage of reconstructing the internal magnetic field configuration of CMEs. This is something that is not included in the simpler cone CME model used so far for space weather forecasting. This work aims at assessing the spheromak CME model included in EUHFORIA. Methods. We employed the spheromak CME model to reconstruct a well observed CME and compare model output to in situ observations. We focus on an eruption from 6 January 2013 that was encountered by two radially aligned spacecraft, Venus Express and STEREO-A. We first analysed the observed properties of the source of this CME eruption and we extracted the CME properties as it lifted off from the Sun. Using this information, we set up EUHFORIA runs to model the event.Results. The model predicts arrival times from half to a full day ahead of the in situ observed ones, but within errors established from similar studies. In the modelling domain, the CME appears to be propagating primarily southward, which is in accordance with white-light images of the CME eruption close to the Sun. Conclusions. In order to get the observed magnetic field topology, we aimed at selecting a spheromak rotation angle for which the axis of symmetry of the spheromak is perpendicular to the direction of the polarity inversion line (PIL). The modelled magnetic field profiles, their amplitude, arrival times, and sheath region length are all affected by the choice of radius of the modelled spheromak.

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Dependence of Coronal Mass Ejection Properties on Their Solar Source Active Region Characteristics and Associated Flare Reconnection Flux

Cited by 35 publications

References 91 publications

Evolution of Interplanetary Coronal Mass Ejection Complexity: A Numerical Study through a Swarm of Simulated Spacecraft

Evolution of Interplanetary Coronal Mass Ejection Complexity: A Numerical Study through a Swarm of Simulated Spacecraft

How Does Magnetic Reconnection Drive the Early-stage Evolution of Coronal Mass Ejections?

Modelling a multi-spacecraft coronal mass ejection encounter with EUHFORIA

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