Validation of a global 3D heliospheric model with observations for the May 12, 1997 CME event

Cohen, Ofer; Соколов, И. В.; Roussev, I. I.; Lugaz, Noé; Manchester, W.; Gombosi, T. I.; Arge, C. N.

doi:10.1016/j.jastp.2007.08.065

Cited by 18 publications

(24 citation statements)

References 34 publications

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“…Thompson et al 1998;Webb et al 2000;Attrill et al 2006) and several different groups have modeled it (e.g. Wu et al 2007;Cohen et al 2008;Titov et al 2008). We use a more simplified magnetic field distribution at 1 R s than in previous models of the 12 May 1997 event, in order to investigate a configuration based on a realistic case without introducing unnecessary complexity.…”

Section: Model Descriptionmentioning

confidence: 99%

Exploring Plasma Heating in the Current Sheet Region in a Three-dimensional Coronal Mass Ejection Simulation

Reeves

Török

Mikić

et al. 2019

ApJ

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We simulate a coronal mass ejection (CME) using a three-dimensional magnetohydrodynamic (MHD) code that includes coronal heating, thermal conduction, and radiative cooling in the energy equation. The magnetic flux distribution at 1 R s is produced by a localized subsurface dipole superimposed on a global dipole field, mimicking the presence of an active region within the global corona. Transverse electric fields are applied near the polarity inversion line to introduce a transverse magnetic field, followed by the imposition of a converging flow to form and destabilize a flux rope, producing an eruption. We examine the quantities responsible for plasma heating and cooling during the eruption, including thermal conduction, radiation, adiabatic effects, coronal heating, and ohmic heating. We find that ohmic heating is an important contributor to hot temperatures in the current sheet region early in the eruption, but in the late phase adiabatic compression plays an important role in heating the plasma there. Thermal conduction also plays an important role in the transport of thermal energy away from the current sheet region throughout the reconnection process, producing a "thermal halo" and widening the region of high temperatures. We simulate emission from solar telescopes for this eruption and find that there is evidence for emission from heated plasma above the flare loops late in the eruption, when the adiabatic heating is the dominant heating term. These results provide an explanation for hot supra-arcade plasma sheets that are often observed in X-rays and extreme ultraviolet wavelengths during the decay phase of large flares.

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Section: Model Descriptionmentioning

confidence: 99%

Exploring Plasma Heating in the Current Sheet Region in a Three-dimensional Coronal Mass Ejection Simulation

Reeves

Török

Mikić

et al. 2019

ApJ

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“…Images of numerical CME models have been made in this fashion before (e.g., Wu et al 1999;Odstrcil 2003;Manchester et al 2004c;Lugaz et al 2005). More recently, synthetic images have been made for models of specific CME events and qualitatively compared to LASCO images (e.g., Lugaz et al 2007;Cohen et al 2008). Here we go further and for the first time make truly quantitative comparisons with the data (see Fig.…”

Section: Comparisons With Lasco Observationsmentioning

confidence: 99%

“…This work by Tóth et al (2007) is groundbreaking in two regards. First, like those by Lugaz et al (2007) and Cohen et al (2008) it is the first 3D numerical full MHD simulation to reproduce observed CMEs as they are magnetically driven from active regions in the low corona. The earliest attempt to model an observed CME (including the magnetic field) propagating from the Sun to the Earth is that of Wu et al (1999).…”

Section: Introductionmentioning

confidence: 95%

Three‐dimensional MHD Simulation of the 2003 October 28 Coronal Mass Ejection: Comparison with LASCO Coronagraph Observations

Manchester

Vourlidas

Tóth

et al. 2008

Astrophysical Journal

160

118

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We numerically model the coronal mass ejection (CME) event of 2003 October 28 that erupted from AR 10486 and propagated to Earth in less than 20 hr, causing severe geomagnetic storms. The magnetohydrodynamic (MHD) model is formulated by first arriving at a steady state corona and solar wind employing synoptic magnetograms. We initiate two CMEs from the same active region, one approximately a day earlier that preconditions the solar wind for the much faster CME on the 28th. This second CME travels through the corona at a rate of over 2500 km s À1 , driving a strong forward shock. We clearly identify this shock in an image produced by the Large Angle Spectrometric Coronagraph (LASCO) C3 and reproduce the shock and its appearance in synthetic white-light images from the simulation. We find excellent agreement with both the general morphology and the quantitative brightness of the model CME with LASCO observations. These results demonstrate that the CME shape is largely determined by its interaction with the ambient solar wind and may not be sensitive to the initiation process. We then show how the CME would appear as observed by wide-angle coronagraphs on board the Solar Terrestrial Relations Observatory (STEREO) spacecraft. We find complex time evolution of the white-light images as a result of the way in which the density structures pass through the Thomson sphere. The simulation is performed with the Space Weather Modeling Framework (SWMF).

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“…In practice, the numerical study of space weather events has used pressure/velocity pulses to represent a CME to simulate the propagation of a CME event [Groth et al, 2000;Odstrcil and Pizzo, 2009;Shen et al, 2007;Wood et al, 2012;Wu et al, 2007Wu et al, , 2011Liou et al, 2014]. To include the internal CME magnetic structure, there are semitoroidal flux rope models [Chen et al, 1997;Wu et al, 1999;Manchester et al, 2004aManchester et al, , 2004bToth et al, 2007;Cohen et al, 2008;Lugaz et al, 2010;Roussev et al, 2004;Shen et al, 2007], magnetized plasma blob models [Detman et al, 1991;Chane et al, 2008;Shen et al, 2011Shen et al, , 2012, and spheromak-type flux rope models [Vandas et al, 1998;Zhou and Feng, 2013]. Some of these studies computed the disturbance propagation from near the Sun to 1 AU in a near realistic background solar wind [Shen et al, 2007;Manchester et al, 2008;Cohen et al, 2008;Lugaz et al, 2010;Zhou et al, 2012Zhou et al, , 2014Zhou and Feng, 2013].…”

Section: Introductionmentioning

confidence: 99%

“…To include the internal CME magnetic structure, there are semitoroidal flux rope models [Chen et al, 1997;Wu et al, 1999;Manchester et al, 2004aManchester et al, , 2004bToth et al, 2007;Cohen et al, 2008;Lugaz et al, 2010;Roussev et al, 2004;Shen et al, 2007], magnetized plasma blob models [Detman et al, 1991;Chane et al, 2008;Shen et al, 2011Shen et al, , 2012, and spheromak-type flux rope models [Vandas et al, 1998;Zhou and Feng, 2013]. Some of these studies computed the disturbance propagation from near the Sun to 1 AU in a near realistic background solar wind [Shen et al, 2007;Manchester et al, 2008;Cohen et al, 2008;Lugaz et al, 2010;Zhou et al, 2012Zhou et al, , 2014Zhou and Feng, 2013]. Plunkett and Wu [2000] used a streamer and flux rope model [Wu et al, 1999] to study the January 1997 Sun-Earth connection event.…”

Section: Introductionmentioning

confidence: 99%

A data‐constrained three‐dimensional magnetohydrodynamic simulation model for a coronal mass ejection initiation

Zhou

Jiang

et al. 2016

JGR Space Physics

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In this study, we present a three‐dimensional magnetohydrodynamic model based on an observed eruptive twisted flux rope (sigmoid) deduced from solar vector magnetograms. This model is a combination of our two very well tested MHD models: (i) data‐driven 3‐D magnetohydrodynamic (MHD) active region evolution (MHD‐DARE) model for the reconstruction of the observed flux rope and (ii) 3‐D MHD global coronal‐heliosphere evolution (MHD‐GCHE) model to track the propagation of the observed flux rope. The 6 September 2011, AR11283, event is used to test this model. First, the formation of the flux rope (sigmoid) from AR11283 is reproduced by the MHD‐DARE model with input from the measured vector magnetograms given by Solar Dynamics Observatory/Helioseismic and Magnetic Imager. Second, these results are used as the initial boundary condition for our MHD‐GCHE model for the initiation of a coronal mass ejection (CME) as observed. The model output indicates that the flux rope resulting from MHD‐DARE produces the physical properties of a CME, and the morphology resembles the observations made by STEREO/COR‐1.

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Validation of a global 3D heliospheric model with observations for the May 12, 1997 CME event

Cited by 18 publications

References 34 publications

Exploring Plasma Heating in the Current Sheet Region in a Three-dimensional Coronal Mass Ejection Simulation

Exploring Plasma Heating in the Current Sheet Region in a Three-dimensional Coronal Mass Ejection Simulation

Three‐dimensional MHD Simulation of the 2003 October 28 Coronal Mass Ejection: Comparison with LASCO Coronagraph Observations

A data‐constrained three‐dimensional magnetohydrodynamic simulation model for a coronal mass ejection initiation

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