Modeling a space weather event from the Sun to the Earth: CME generation and interplanetary propagation

Manchester, W.; Gombosi, T. I.; Roussev, I. I.; Ridley, A. J.; Zeeuw, Darren L. De; Соколов, И. В.; Powell, Kenneth G.; Tóth, G.

doi:10.1029/2003ja010150

Cited by 302 publications

(343 citation statements)

References 38 publications

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“…Using 2-D and 3-D numerical simulations, it is possible to show that a CME initiated at the solar surface (for example using a twisted flux rope) evolves through its interaction with the solar wind into a typical ICME (Riley, Gosling, and Pizzo, 1997;Odstrčil and Pizzo, 1999;Manchester et al, 2004;Chané et al, 2006;Shen et al, 2007). This idea has now been confirmed by STEREO observations (see, for example, Savani et al, 2010).…”

Section: Introductionmentioning

confidence: 79%

Magnetic Field Configuration Models and Reconstruction Methods for Interplanetary Coronal Mass Ejections

et al. 2013

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This study aims to provide a reference to different magnetic field models and reconstruction methods for interplanetary coronal mass ejections (ICMEs). In order to understand the differences in the outputs of those models and codes, we analyze 59 events from the Coordinated Data Analysis Workshop (CDAW) list, using four different magnetic field models and reconstruction techniques; force-free fitting (Goldstein, 1983; Burlaga, 1988;Lepping, Burlaga, and Jones, 1990), magnetostatic reconstruction using a numerical solution to the Grad-Shafranov equation (Hu and Sonnerup, 2001), fitting to a self-similarly expanding cylindrical configuration (Marubashi and Lepping, 2007) and elliptical, non-force free fitting (Hidalgo, 2003). The resulting parameters of the reconstructions for the 59 events are compared statistically, as well as in selected case studies. The ability of a method to fit or reconstruct an event is found to vary greatly: the Grad-Shafranov reconstruction is successful for most magnetic clouds (MCs) but for less than 10% of the non-MC ICMEs; the other three Al-Haddad et al methods provide a successful fit for more than 65% of all events. The differences between the reconstruction and fitting methods are discussed, and suggestions are proposed as to how to reduce them. We find that the magnitude of the axial field is relatively consistent across models but not the orientation of the axis of the ejecta. We also find that there are a few cases for which different signs of the magnetic helicity are found for the same event when we do not fix the boundaries, illustrating that this simplest of parameters is not necessarily always well constrained by fitting and reconstruction models. Finally, we look at three unique cases in depth to provide a comprehensive idea of the different aspects of how the fitting and reconstruction codes work.

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Section: Introductionmentioning

confidence: 79%

Magnetic Field Configuration Models and Reconstruction Methods for Interplanetary Coronal Mass Ejections

et al. 2013

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“…2.4). However, values of a larger than ≈ √ b are expected to be unphysical (in particular they were not found in MHD simulations, e.g., Riley et al 2003;Manchester et al 2004), so we claim that Fig. 11 represents a sufficiently broad range of the parameter space which covers most of the observed MC configurations.…”

Section: Bendingmentioning

confidence: 87%

“…In some MHD simulations, the flux rope is strongly compressed in the propagation direction, such that it becomes relatively flat (e.g., Vandas et al 2002), and it can even develop a bending of the lateral sides towards the front direction as it moves away from the Sun (e.g., Riley et al 2003;Manchester et al 2004). Owens et al (2006) proposed a kinematic model of this evolution with an initial Lundquist solution passively deformed by a given velocity flow.…”

Section: Introductionmentioning

confidence: 99%

Magnetic cloud models with bent and oblate cross-section boundaries

Démoulin¹,

Dasso

2009

A&A

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Context. Magnetic clouds (MCs) are formed by magnetic flux ropes that are ejected from the Sun as coronal mass ejections. These structures generally have low plasma beta and travel through the interplanetary medium interacting with the surrounding solar wind. Thus, the dynamical evolution of the internal magnetic structure of a MC is a consequence of both the conditions of its environment and of its own dynamical laws, which are mainly dominated by magnetic forces. Aims. With in-situ observations the magnetic field is only measured along the trajectory of the spacecraft across the MC. Therefore, a magnetic model is needed to reconstruct the magnetic configuration of the encountered MC. The main aim of the present work is to extend the widely used cylindrical model to arbitrary cross-section shapes. Methods. The flux rope boundary is parametrized to account for a broad range of shapes. Then, the internal structure of the flux rope is computed by expressing the magnetic field as a series of modes of a linear force-free field. Results. We analyze the magnetic field profile along straight cuts through the flux rope, in order to simulate the spacecraft crossing through a MC. We find that the magnetic field orientation is only weakly affected by the shape of the MC boundary. Therefore, the MC axis can approximately be found by the typical methods previously used (e.g., minimum variance). The boundary shape affects the magnetic field strength most. The measurement of how much the field strength peaks along the crossing provides an estimation of the aspect ratio of the flux-rope cross-section. The asymmetry of the field strength between the front and the back of the MC, after correcting for the time evolution (i.e., its aging during the observation of the MC), provides an estimation of the cross-section global bending. A flat or/and bent cross-section requires a large anisotropy of the total pressure imposed at the MC boundary by the surrounding medium. Conclusions. The new theoretical model developed here relaxes the cylindrical symmetry hypothesis. It is designed to estimate the cross-section shape of the flux rope using the in-situ data of one spacecraft. This allows a more accurate determination of the global quantities, such as magnetic fluxes and helicity. These quantities are especially important for both linking an observed MC to its solar source and for understanding the corresponding evolution.

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“…They have studied with the use of global MHD simulations in 3D (Manchester et al 2004;Lugaz & Roussev 2011;Shiota & Kataoka 2016). Liu et al (2013) reported the first detailed examination of the Sun-to-Earth propagation characteristics of three fast CMEs and an associated shock front using the combination of wideangle heliospheric imaging observations by STEREO, interplanetary Type II radio bursts, and in situ observations of solar wind parameters at multiple points.…”

Section: Introductionmentioning

confidence: 99%

Sheath-accumulating Propagation of Interplanetary Coronal Mass Ejection

Takahashi

Shibata

2017

ApJL

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Fast interplanetary coronal mass ejections (ICMEs) are the drivers of strong space weather storms such as solar energetic particle events and geomagnetic storms. The connection between the space-weather-impacting solar wind disturbances associated with fast ICMEs at Earth and the characteristics of causative energetic CMEs observed near the Sun is a key question in the study of space weather storms, as well as in the development of practical space weather prediction. Such shock-driving fast ICMEs usually expand at supersonic speeds during the propagation, resulting in the continuous accumulation of shocked sheath plasma ahead. In this paper, we propose a "sheath-accumulating propagation" (SAP) model that describes the coevolution of the interplanetary sheath and decelerating ICME ejecta by taking into account the process of upstream solar wind plasma accumulation within the sheath region. Based on the SAP model, we discuss (1) ICME deceleration characteristics; (2) the fundamental condition for fast ICMEs at Earth; (3) the thickness of interplanetary sheaths; (4) arrival time prediction; and (5) the super-intense geomagnetic storms associated with huge solar flares. We quantitatively show that not only the speed but also the mass of the CME are crucial for discussing the above five points. The similarities and differences between the SAP model, the drag-based model, and the"snow-plow" model proposed by Tappin are also discussed.

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Modeling a space weather event from the Sun to the Earth: CME generation and interplanetary propagation

Cited by 302 publications

References 38 publications

Magnetic Field Configuration Models and Reconstruction Methods for Interplanetary Coronal Mass Ejections

Magnetic Field Configuration Models and Reconstruction Methods for Interplanetary Coronal Mass Ejections

Magnetic cloud models with bent and oblate cross-section boundaries

Sheath-accumulating Propagation of Interplanetary Coronal Mass Ejection

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