Dynamics of coronal mass ejections in the interplanetary medium

Borgazzi, A.; Lara, A.; Echer, E.; Alves, M. V.

doi:10.1051/0004-6361/200811171

Cited by 45 publications

(43 citation statements)

References 29 publications

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“…For distances >R m , we assume that the CME dynamics are governed exclusively by the aerodynamic drag it experiences due to momentum coupling with the ambient solar wind. For heliocentric distances >R m , we therefore use the widely used onedimensional differential equation to determine the CME velocity profile: (e.g., Borgazzi et al 2009)…”

Section: Third Shortlist: Cme Velocity Profilementioning

confidence: 99%

High-rigidity Forbush decreases: due to CMEs or shocks?

Arunbabu

Antia

Dugad

et al. 2013

A&A

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Aims. We seek to identify the primary agents causing Forbush decreases (FDs) in high-rigidity cosmic rays observed from the Earth. In particular, we ask if these FDs are caused mainly by coronal mass ejections (CMEs) from the Sun that are directed towards the Earth, or by their associated shocks. Methods. We used the muon data at cutoff rigidities ranging from 14 to 24 GV from the GRAPES-3 tracking muon telescope to identify FD events. We selected those FD events that have a reasonably clean profile, and can be reasonably well associated with an Earth-directed CME and its associated shock. We employed two models: one that considers the CME as the sole cause of the FD (the CME-only model) and one that considers the shock as the only agent causing the FD (the shock-only model). We used an extensive set of observationally determined parameters for both models. The only free parameter in these models is the level of MHD turbulence in the sheath region, which mediates cosmic ray diffusion (into the CME for the CME-only model, and across the shock sheath for the shock-only model). Results. We find that good fits to the GRAPES-3 multi-rigidity data using the CME-only model require turbulence levels in the CME sheath region that are only slightly higher than those estimated for the quiescent solar wind. On the other hand, reasonable model fits with the shock-only model require turbulence levels in the sheath region that are an order of magnitude higher than those in the quiet solar wind. Conclusions. This observation naturally leads to the conclusion that the Earth-directed CMEs are the primary contributors to FDs observed in high-rigidity cosmic rays.

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Section: Third Shortlist: Cme Velocity Profilementioning

confidence: 99%

High-rigidity Forbush decreases: due to CMEs or shocks?

Arunbabu

Antia

Dugad

et al. 2013

A&A

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“…Various drag forces have been investigated [16,17]. Typically the strongest deceleration occurs close to the Sun, and ICMEs have a nearly constant velocity in most of the heliosphere [outward of 0.3 AU, 1, 2, 7].…”

Section: Evolution Of the Velocitymentioning

confidence: 99%

Interaction of ICMEs with the Solar Wind

Démoulin¹

2010

AIP Conference Proceedings

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Modeling the global structure of the heliosphere during the recent solar minimum: Model improvements and unipolar streamers AIP Conf.Abstract. Interplanetary Coronal Mass Ejections (ICMEs) are formed of plasma and magnetic field launched from the Sun into the Solar Wind (SW). These coherent magnetic structures, frequently formed by a flux rope, interact strongly with the SW. This interaction is reviewed by comparing the results obtained from in situ observations and numerical simulations. Like fast ships in the ocean, fast ICMEs drive an extended shock in front. ICMEs expand in all directions while traveling away from the Sun, a sheath of SW plasma and magnetic field accumulates in front of the ICME, which partially reconnects with the ICME magnetic field. Furthermore, not only do ICMEs have a profound impact on the heliosphere, but the type of SW encountered by an ICME has an important impact on its evolution (e.g. increase of mass, global deceleration, lost of magnetic flux and helicity, distortion of the configuration). FIGURE 1. Schema showing three time steps. First, the crossing of the convective zone by a flux rope. Second, the launch of a CME (the photospheric emergence and the coronal evolution before the CME are not shown). Finally, depending on the speed and launch direction, the CME can be detected a few days later in the interplanetary space as a magnetic cloud (with a flux rope topology, as shown schematically), or more generally as an ICME. The CME image is from SOHO/LASCO.

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“…Gopalswamy et al 2000;Michałek et al 2004;Vršnak & Žic 2007), analytical propagation models (e.g. Smart & Shea 1985;Vršnak & Gopalswamy 2002;Cantó et al 2005;Vršnak & Žic 2007;Borgazzi et al 2009;), or numerical MHD simulations (e.g. González-Esparza et al 2003;Manchester et al 2004;Odstrcil et al 2004;Smith et al 2009;Taktakishvili et al 2009).…”

Section: Introductionmentioning

confidence: 99%

The role of aerodynamic drag in propagation of interplanetary coronal mass ejections

Vršnak

Žic

Falkenberg

et al. 2010

A&A

120

115

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Context. The propagation of interplanetary coronal mass ejections (ICMEs) and the forecast of their arrival on Earth is one of the central issues of space weather studies. Aims. We investigate to which degree various ICME parameters (mass, size, take-off speed) and the ambient solar-wind parameters (density and velocity) affect the ICME Sun-Earth transit time. Methods. We study solutions of a drag-based equation of motion by systematically varying the input parameters. The analysis is focused on ICME transit times and 1 AU velocities. Results. The model results reveal that wide ICMEs of low masses adjust to the solar-wind speed already close to the sun, so the transit time is determined primarily by the solar-wind speed. The shortest transit times and accordingly the highest 1 AU velocities are related to narrow and massive ICMEs (i.e. high-density eruptions) propagating in high-speed solar wind streams. We apply the model to the Sun-Earth event associated with the CME of 25 July 2004 and compare the results with the outcome of the numerical MHD modeling.

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Dynamics of coronal mass ejections in the interplanetary medium

Cited by 45 publications

References 29 publications

High-rigidity Forbush decreases: due to CMEs or shocks?

High-rigidity Forbush decreases: due to CMEs or shocks?

Interaction of ICMEs with the Solar Wind

The role of aerodynamic drag in propagation of interplanetary coronal mass ejections

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