Strong coronal channelling and interplanetary evolution of a solar storm up to Earth and Mars

Möstl, Christian; Rollett, T.; Frahm, R. A.; Liu, Ying D.; Long, David M.; Colaninno, R. C.; Reiss, Martin A.; Temmer, Manuela; Farrugia, Charles J.; Posner, A.; Dumbović, Mateja; Janvier, Miho; Démoulin, P.; Boakes, Peter; Devos, Andy; Kraaikamp, E.; Mays, M. L.; Vršnak, Bojan

doi:10.1038/ncomms8135

Cited by 181 publications

(205 citation statements)

References 67 publications

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“…After the launch of twin Solar TErrestrial Relations Observatory spacecraft (STEREO: Kaiser et al 2008), the data from the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI: Howard et al 2008) have enabled us to continuously image CMEs from their lift-off in the corona up to the Earth and beyond Harrison et al, 2012;Liu et al, 2013;Möstl et al, 2015;Vemareddy and Mishra, 2015). These observations have also revealed direct evidence of CME-CME interaction when they are launched in close succession in the same direction Lugaz et al, 2012;Shen et al, 2012;Mishra, Srivastava, and Chakrabarty, 2015).…”

Section: Introductionmentioning

confidence: 84%

Interplanetary and Geomagnetic Consequences of Interacting CMEs of 13 – 14 June 2012

2018

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We report on the kinematics of two interacting CMEs observed on 13 and 14 June 2012. Both CMEs originated from the same active region NOAA 11504. After their launches which were separated by several hours, they were observed to interact at a distance of 100 R from the Sun. The interaction led to a moderate geomagnetic storm at the Earth with D st index of approximately, -86 nT. The kinematics of the two CMEs is estimated using data from the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) onboard the Solar Terrestrial Relations Observatory (STEREO). Assuming a head-on collision scenario, we find that the collision is inelastic in nature. Further, the signatures of their interaction are examined using the in situ observations obtained by Wind and the Advance Composition Explorer (ACE) spacecraft. It is also found that this interaction event led to the strongest sudden storm commencement (SSC) (≈ 150 nT) of the present Solar Cycle 24. The SSC was of long duration, approximately 20 hours. The role of interacting CMEs in enhancing the geoeffectiveness is examined.

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Section: Introductionmentioning

confidence: 84%

Interplanetary and Geomagnetic Consequences of Interacting CMEs of 13 – 14 June 2012

2018

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“…Next, we compare this with the expectation of a self-similar expansion model (e.g. Möstl et al 2015, and references therein) where the shape (axis or shock surface) is simply rescaled with a function of time f (t), so r(λ, t) = f (t) r(λ, t 0 ) where r(λ, t) is the distance to the Sun at λ and time t, and t 0 is a reference time. Then the radial velocity is:…”

Section: Property Variations Along the Icme Frontmentioning

confidence: 99%

“…Also, they are important information for possible impact prediction with the Earth's magnetosphere, their arrival time as well as their journey in the interplanetary medium (e.g. Möstl & Davies 2013;Möstl et al 2015). The ICME structure also affects the transport of energetic particles in the heliosphere over a large range of energies (e.g.…”

Section: Introductionmentioning

confidence: 99%

Quantitative model for the generic 3D shape of ICMEs at 1 AU

Démoulin

Janvier

Masías-Meza

et al. 2016

A&A

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Context. Interplanetary imagers provide 2D projected views of the densest plasma parts of interplanetary coronal mass ejections (ICMEs) while in situ measurements provide magnetic field and plasma parameter measurements along the spacecraft trajectory, so along a 1D cut. As such, the data only give a partial view of their 3D structures. Aims. By studying a large number of ICMEs, crossed at different distances from their apex, we develop statistical methods to obtain a quantitative generic 3D shape of ICMEs. Methods. In a first approach we theoretically obtain the expected statistical distribution of the shock-normal orientation from assuming simple models of 3D shock shapes, including distorted profiles, and compare their compatibility with observed distributions. In a second approach we use the shock normal and the flux rope axis orientations, as well as the impact parameter, to provide statistical information across the spacecraft trajectory. Results. The study of different 3D shock models shows that the observations are compatible with a shock symmetric around the Sunapex line as well as with an asymmetry up to an aspect ratio around 3. Moreover, flat or dipped shock surfaces near their apex can only be rare cases. Next, the sheath thickness and the ICME velocity have no global trend along the ICME front. Finally, regrouping all these new results and the ones of our previous articles, we provide a quantitative ICME generic 3D shape, including the global shape of the shock, the sheath and the flux rope.Conclusions. The obtained quantitative generic ICME shape will have implications for several aims. For example, it constrains the output of typical ICME numerical simulations. It is also a base to develop deeper studies of the transport of high energy solar and cosmic particles during an ICME propagation, as well as for modeling and forecasting space weather conditions near Earth.

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“…With the triangulation method, it is revealed that fast CMEs impulsively accelerate until even after the X-ray flare maximum, and then rapidly decelerate to a nearly constant speed or gradual deceleration phase (Liu et al 2013), while slow CMEs experience a slow acceleration phase and then travel with a roughly constant speed around the average solar wind level . A CME could also propagate in a non-radial direction (e.g., Wang et al 2004;Gopalswamy et al 2009;Möstl et al 2015;Liewer et al 2015;Wang et al 2015), interact with other CMEs (e.g., Lugaz et al 2009;Gopalswamy et al 2001b;Liu et al 2012Liu et al , 2014 or co-rotating interaction regions (e.g., Reiner et al 1998;Rouillard et al 2010;Liu et al 2016), or rotate in interplanetary space (e.g., Thernisien et al 2006;Liu et al 2010b;Vourlidas et al 2011), which increases difficulty to predict the CME arrival characteristics at the Earth.…”

Section: Introductionmentioning

confidence: 99%

Sun-to-Earth Characteristics of the 2012 July 12 Coronal Mass Ejection and Associated Geo-Effectiveness

Liu

Wang

et al. 2016

ApJ

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We analyze multi-spacecraft observations associated with the 2012 July 12 Coronal Mass Ejection (CME), covering the source region on the Sun from SDO, stereoscopic imaging observations from STEREO, magnetic field characteristics at MESSENGER, and type II radio burst and in situ measurements from Wind. A triangulation method based on STEREO stereoscopic observations is employed to determine the kinematics of the CME, and the outcome is compared with the result derived from the type II radio burst with a solar wind electron density model. A Grad-Shafranov technique is applied to Wind in situ data to reconstruct the flux-rope structure and compare it with the observation of the solar source region, which helps understand the geo-effectiveness associated with the CME structure. Conclusions are as follows: (1) the CME undergoes an impulsive acceleration, a rapid deceleration before reaching MESSENGER, and then a gradual deceleration out to 1 AU, which should be noticed in CME kinematics models; (2) the type II radio burst was probably produced from a high-density interaction region between the CME-driven shock and a nearby streamer or from the shock flank with lower heights, which implies uncertainties in the determination of CME kinematics using solely type II radio bursts; (3) the flux-rope orientation and chirality deduced from in situ reconstruction at Wind agree with those obtained from solar source observations; (4) the prolonged southward magnetic field near the Earth is mainly from the axial component of the largely southward inclined flux rope, which indicates the importance of predicting both the flux-rope orientation and magnetic field components in geomagnetic activity forecasting.

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Strong coronal channelling and interplanetary evolution of a solar storm up to Earth and Mars

Cited by 181 publications

References 67 publications

Interplanetary and Geomagnetic Consequences of Interacting CMEs of 13 – 14 June 2012

Interplanetary and Geomagnetic Consequences of Interacting CMEs of 13 – 14 June 2012

Quantitative model for the generic 3D shape of ICMEs at 1 AU

Sun-to-Earth Characteristics of the 2012 July 12 Coronal Mass Ejection and Associated Geo-Effectiveness

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