Multipoint Study of Successive Coronal Mass Ejections Driving Moderate Disturbances at 1 au

Palmerio, Erika; Scolini, Camilla; Barnes, David; Magdalenić, Jasmina; West, Matthew J.; Zhukov, A. N.; Rodriguez, L.; Mierla, M.; Good, Simon; Morosan, Diana; Kilpua, Emilia; Pomoell, Jens; Poedts, Stefaan

doi:10.3847/1538-4357/ab1850

Cited by 31 publications

(44 citation statements)

References 129 publications

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“…In such cases, employing a larger CME half-width may solve the issue (a detailed study of how the SSSE model performs with respect to different CME half-widths is shown in Barnes et al, 2020). Furthermore, we remark that Palmerio et al (2019) applied the (S)SSE model to two CMEs and noted that adding 15 • to the GCS-derived half-width improved arrival time predictions in both cases. Nevertheless, employing several models with different assumptions can provide an overall context useful to interpret in-situ observations, as was demonstrated in this study.…”

Section: Cme Propagationmentioning

confidence: 91%

CME Magnetic Structure and IMF Preconditioning Affecting SEP Transport

et al. 2021

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Coronal mass ejections (CMEs) and solar energetic particles (SEPs) are two phenomena that can cause severe space weather effects throughout the heliosphere. The evolution of CMEs, especially in terms of their magnetic structure, and the configuration of the interplanetary magnetic field (IMF) that influences the transport of SEPs are currently areas of active research. These two aspects are not necessarily independent of each other, especially during solar maximum when multiple eruptive events can occur close in time. Accordingly, we present the analysis of a CME that erupted on 2012 May 11 (SOL2012-05-11) and an SEP event following an eruption that took place on 2012 May 17 (SOL2012-05-17). After observing the May 11 CME using remote-sensing data from three viewpoints, we evaluate its propagation through interplanetary space using several models. Then, we analyse in-situ measurements from five predicted impact locations (Venus, Earth, the Spitzer Space Telescope, the Mars Science Laboratory en route to Mars, and Mars) in order to search for CME signatures. We find that all in-situ locations detect signatures of an SEP event, which we trace back to the May 17 eruption. These findings suggest that the May 11 CME provided a direct magnetic connectivity for the efficient transport of SEPs. We discuss the space weather implications of CME evolution, regarding in particular its magnetic structure, and CME-driven IMF preconditioning that facilitates SEP transport. Finally, this work remarks the importance of using data from multiple spacecraft, even those that do not include space weather research as their primary objective.

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Section: Cme Propagationmentioning

confidence: 91%

CME Magnetic Structure and IMF Preconditioning Affecting SEP Transport

et al. 2021

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“…Magdalenić et al 2008Magdalenić et al , 2010 and a 1-fold Leblanc density model for for the decametre to hectometre range (e.g. Palmerio et al 2019). Fig.…”

Section: Radio Eventmentioning

confidence: 99%

Using radio triangulation to understand the origin of two subsequent type II radio bursts

Jebaraj

Magdalenić

Podladchikova

et al. 2020

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Context. Eruptive events such as coronal mass ejections (CMEs) and flares accelerate particles and generate shock waves which can arrive at Earth and can disturb the magnetosphere. Understanding the association between CMEs and CME-driven shocks is therefore highly important for space weather studies. Aims. We present a study of the CME/flare event associated with two type II bursts observed on September 27, 2012. The aim of the study is to understand the relationship between the observed CME and the two distinct shock wave signatures. Methods. The multiwavelength study of the eruptive event (CME/flare) was complemented with radio triangulation of the associated radio emission and modelling of the CME and the shock wave employing MHD simulations. Results. We found that, although temporal association between the type II bursts and the CME is good, the low-frequency type II (LF-type II) burst occurs significantly higher in the corona than the CME and its relationship to the CME is not straightforward. The analysis of the EIT wave (coronal bright front) shows the fastest wave component to be in the southeast quadrant of the Sun. This is also the quadrant in which the source positions of the LF-type II were found to be located, probably resulting from the interaction between the shock wave and a streamer. Conclusions. The relationship between the CME/flare event and the shock wave signatures is discussed using the temporal association, as well as the spatial information of the radio emission. Further, we discuss the importance and possible effects of the frequently non-radial propagation of the shock wave.

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“…More sophisticated geometries for modelling CME morphology include the Graduated Cylindrical Shell (GCS) model (Thernisien, Howard, and Vourlidas, 2006), ElEvoHI (Rollett et al, 2016), which employs an elliptical CME front and includes the effects of drag, and 3DCORE (Möstl et al, 2018), which is used to measure CME rotation and deflection and also to give information about magnetic field orientation based on data from the Solar Dynamics Observatory. Both Volpes and Bothmer (2015) and Palmerio et al (2019) apply SSSE analysis to HI data, where the half-width of the CME is first determined using coronagraph observations. This is rather labour-intensive and so is more challenging to apply to large statistical studies, such as that which we present here.…”

Section: Introductionmentioning

confidence: 99%

CMEs in the Heliosphere: III. A Statistical Analysis of the Kinematic Properties Derived from Stereoscopic Geometrical Modelling Techniques Applied to CMEs Detected in the Heliosphere from 2008 to 2014 by STEREO/HI-1

et al. 2020

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We present an analysis of coronal mass ejections (CMEs) observed by the Heliospheric Imagers (HIs) onboard NASA’s Solar Terrestrial Relations Observatory (STEREO) spacecraft. Between August 2008 and April 2014 we identify 273 CMEs that are observed simultaneously, by the HIs on both spacecraft. For each CME, we track the observed leading edge, as a function of time, from both vantage points, and apply the Stereoscopic Self-Similar Expansion (SSSE) technique to infer their propagation throughout the inner heliosphere. The technique is unable to accurately locate CMEs when their observed leading edge passes between the spacecraft; however, we are able to successfully apply the technique to 151, most of which occur once the spacecraft-separation angle exceeds $180^{\circ }$ 180 ∘ , during solar maximum. We find that using a small half-width to fit the CME can result in inferred acceleration to unphysically high velocities and that using a larger half-width can fail to accurately locate the CMEs close to the Sun because the method does not account for CME over-expansion in this region. Observed velocities from SSSE are found to agree well with single-spacecraft (SSEF) analysis techniques applied to the same events. CME propagation directions derived from SSSE and SSEF analysis agree poorly because of known limitations present in the latter.

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Multipoint Study of Successive Coronal Mass Ejections Driving Moderate Disturbances at 1 au

Cited by 31 publications

References 129 publications

CME Magnetic Structure and IMF Preconditioning Affecting SEP Transport

CME Magnetic Structure and IMF Preconditioning Affecting SEP Transport

Using radio triangulation to understand the origin of two subsequent type II radio bursts

CMEs in the Heliosphere: III. A Statistical Analysis of the Kinematic Properties Derived from Stereoscopic Geometrical Modelling Techniques Applied to CMEs Detected in the Heliosphere from 2008 to 2014 by STEREO/HI-1

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