MHD simulation of an interaction of a shock wave with a magnetic cloud

Vandas, M.; Fischer, S.; Dryer, M.; Smith, Z.; Detman, T.; Geranios, A.

doi:10.1029/97ja01675

Cited by 59 publications

(51 citation statements)

References 10 publications

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“…However, the results of ejecta 1 in columns 2 and 4 were very different: due to the interaction with the shock wave driven by ejecta 2, ejecta 1 arrived at 1 AU compressed (with an approximate 79% smaller radial width) and with a much faster front speed (about 27% higher) and shorter transit time (about 10.5% less). These results agree with those by Vandas et al (1997), where they studied the interaction of a shock wave overtaking a magnetic cloud (MC) using a MHD model. They found that the passing of the shock through the MC produces an increment in the MC's field magnitude and the ejecta is compressed and accelerated in the radial direction.…”

Section: One-dimensional Simulationsupporting

confidence: 82%

A numerical study of the interaction between two ejecta in the interplanetary medium: one- and two-dimensional hydrodynamic simulations

2004

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Abstract.We studied the heliospheric evolution in one and two dimensions of the interaction between two ejecta-like disturbances beyond the critical point: a faster ejecta 2 overtaking a previously launched slower ejecta 1. The study is based on a hydrodynamic model using the ZEUS-3-D code. This model can be applied to those cases where the interaction occurs far away from the Sun and there is no merging (magnetic reconnection) between the two ejecta. The simulation shows that when the faster ejecta 2 overtakes ejecta 1 there is an interchange of momentum between the two ejecta, where the leading ejecta 1 accelerates and the tracking ejecta 2 decelerates. Both ejecta tend to arrive at 1 AU having similar speeds, but with the front of ejecta 1 propagating faster than the front of ejecta 2. The momentum is transferred from ejecta 2 to ejecta 1 when the shock initially driven by ejecta 2 passes through ejecta 1. Eventually the two shock waves driven by the two ejecta merge together into a single stronger shock. The 2-D simulation shows that the evolution of the interaction can be very complex and there are very different signatures of the same event at different viewing angles; however, the transferring of momentum between the two ejecta follows the same physical mechanism described above. These results are in qualitative agreement with in-situ plasma observations of "multiple magnetic clouds" detected at 1 AU.

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Section: One-dimensional Simulationsupporting

confidence: 82%

A numerical study of the interaction between two ejecta in the interplanetary medium: one- and two-dimensional hydrodynamic simulations

2004

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“…These shocks are likely associated to each of the two CMEs. We note that, while the flux ropes of the two CMEs are not able to penetrate through each other, the CME-driven shock of CME2 might pass through the slower CME1 (Vandas et al 1997). …”

Section: Remote-sensing Observationsmentioning

confidence: 99%

Long-lasting injection of solar energetic electrons into the heliosphere

Dresing

Gómez-Herrero

Heber

et al. 2018

A&A

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Context. The main sources of solar energetic particle (SEP) events are solar flares and shocks driven by coronal mass ejections (CMEs). While it is generally accepted that energetic protons can be accelerated by shocks, whether or not these shocks can also efficiently accelerate solar energetic electrons is still debated. In this study we present observations of the extremely widespread SEP event of 26 Dec 2013. To the knowledge of the authors, this is the widest longitudinal SEP distribution ever observed together with unusually long-lasting energetic electron anisotropies at all observer positions. Further striking features of the event are long-lasting SEP intensity increases, two distinct SEP components with the second component mainly consisting of high-energy particles, a complex associated coronal activity including a pronounced signature of a shock in radio type-II observations, and the interaction of two CMEs early in the event.Aims. The observations require a prolonged injection scenario not only for protons but also for electrons. We therefore analyze the data comprehensively to characterize the possible role of the shock for the electron event.Methods. Remote-sensing observations of the complex solar activity are combined with in-situ measurements of the particle event.We also apply a Graduated Cylindrical Shell (GCS) model to the coronagraph observations of the two associated CMEs to analyze their interaction. Results. We find that the shock alone is likely not responsible for this extremely wide SEP event. Therefore we propose a scenario of trapped energetic particles inside the CME-CME interaction region which undergo further acceleration due to the shock propagating through this region, stochastic acceleration, or ongoing reconnection processes inside the interaction region. The origin of the second component of the SEP event is likely caused by a sudden opening of the particle trap.

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“…8.ÈLASCO C2 images at 10 : 39 UT (left) and 10 : 54 UT (right), showing the halo CME on 2000 July 14. Burlaga 1982 ;Vandas et al 1997). The CME arrival was also accompanied by a severe magnetic storm, during which the Dst index decreased to [300 (see Fig.…”

Section: Halo Cme On 2000 July 14mentioning

confidence: 99%

Orientation of the Magnetic Fields in Interplanetary Flux Ropes and Solar Filaments

Yurchyshyn

Wang

Goode

et al. 2001

ApJ

127

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Coronal mass ejections (CMEs) are often associated with erupting magnetic structures or disappearing Ðlaments. The majority of CMEs headed directly toward the Earth are observed at 1 AU as magnetic cloudsÈthe region in the solar wind where the magnetic Ðeld strength is higher than average and there is a smooth rotation of the magnetic Ðeld vectors. The three-dimensional structure of magnetic clouds can be represented by a force-free Ñux rope. When CMEs reach the Earth, they may or may not cause magnetic storms, alter EarthÏs magnetic Ðeld, or produce the phenomena known as auroras. The geoe †ectiveness of a solar CME depends on the orientation of the magnetic Ðeld in it.Two M-class solar Ñares erupted on 2000 February 17. The second Ñare occurred near a small active region, NOAA Active Region 8872. This eruption was accompanied by a halo CME. However, the February 17 CME did not trigger any magnetic activity when it arrived at the Earth. Another powerful Ñare, on 2000 July 14, was also associated with a halo CME, which caused the strongest geomagnetic activity of solar cycle 23. Using ACE measurements of the interplanetary magnetic Ðelds, we study the orientation of the magnetic Ñux ropes in both sets of magnetic clouds and compare them with the orientation of the solar magnetic Ðelds and disappearing Ðlaments. We Ðnd that the direction of the axial Ðeld and helicity of the Ñux ropes are consistent with those of the erupted Ðlaments. Thus, the geoe †ectiveness of a CME is deÐned by the orientation and structure of the erupted Ðlament and by its magnetic helicity as well. We also suggest that the geoe †ectiveness of a CME can be forecasted using daily full-disk Ha and Y ohkoh images and MDI magnetograms as well.

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MHD simulation of an interaction of a shock wave with a magnetic cloud

Cited by 59 publications

References 10 publications

A numerical study of the interaction between two ejecta in the interplanetary medium: one- and two-dimensional hydrodynamic simulations

A numerical study of the interaction between two ejecta in the interplanetary medium: one- and two-dimensional hydrodynamic simulations

Long-lasting injection of solar energetic electrons into the heliosphere

Orientation of the Magnetic Fields in Interplanetary Flux Ropes and Solar Filaments

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