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

Wu, S. T.; Zhou, Yufen; Jiang, Chaowei; Feng, Xueshang; Wu, Chin‐Chun; Hu, Qiang

doi:10.1002/2015ja021615

Cited by 13 publications

(6 citation statements)

References 73 publications

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“…In summary, a data-driven MHD modelling like the one shown here, which is able to realistically simulate the whole process from origin to onset of a solar eruption, can be used as a new way for studying the cause of solar eruptions. Furthermore, utilizing the output of such realistic model as the CME initiation input for models of solar storms travelling from the Sun to Earth 57 58 59 will be, we believe, a step forward in developing sophisticated modelling for space weather.…”

Section: Discussionmentioning

confidence: 99%

Data-driven magnetohydrodynamic modelling of a flux-emerging active region leading to solar eruption

et al. 2016

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Solar eruptions are well-recognized as major drivers of space weather but what causes them remains an open question. Here we show how an eruption is initiated in a non-potential magnetic flux-emerging region using magnetohydrodynamic modelling driven directly by solar magnetograms. Our model simulates the coronal magnetic field following a long-duration quasi-static evolution to its fast eruption. The field morphology resembles a set of extreme ultraviolet images for the whole process. Study of the magnetic field suggests that in this event, the key transition from the pre-eruptive to eruptive state is due to the establishment of a positive feedback between the upward expansion of internal stressed magnetic arcades of new emergence and an external magnetic reconnection which triggers the eruption. Such a nearly realistic simulation of a solar eruption from origin to onset can provide important insight into its cause, and also has the potential for improving space weather modelling.

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Section: Discussionmentioning

confidence: 99%

Data-driven magnetohydrodynamic modelling of a flux-emerging active region leading to solar eruption

et al. 2016

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“…We conclude that solar wind modeling tools can be used to provide solar wind context at Mars' orbital location for planetary studies. Although this study focused on the WSA‐ENLIL + Cone model, other solar wind models [e.g., Hakamada and Akasofu , ; Tóth et al ., ; Hayashi , ; Feng et al ., , , ; Wu et al ., ; Yang et al ., , ; Liou et al ., ; Intriligator et al ., ; Wu et al ., ] could also be utilized to provide continuous upstream conditions at Mars. A particular advantage of the continuous conditions provided by models is that they can be used to fill any data gaps in in situ observations.…”

Section: Discussionmentioning

confidence: 99%

“…Modeling of continuous solar wind conditions throughout the inner heliosphere continues to advance in capability and accuracy [e.g., Pizzo et al, 2011;Tóth et al, 2012;Lee et al, 2013;Intriligator et al, 2015a;Wu et al, 2016aWu et al, , 2016b and has been applied to study solar wind-body interactions [e.g., Baker et al, 2013;Dewey et al, 2015]. While many solar wind models exist [e.g., Hakamada and Akasofu, 1982;Tóth et al, 2005;Hayashi, 2012;Feng et al, 2011Feng et al, , 2012Feng et al, , 2014Yang et al, 2011Yang et al, , 2012Liou et al, 2014;Intriligator et al, 2015b;Wu et al, 2016], here we present upstream solar wind conditions at Mars modeled by the Wang-Sheeley-Arge (WSA)-ENLIL + Cone model over the period from late November 2014 to mid-March 2015. This period corresponds to the beginning of the science mapping phase of the Mars Atmosphere and Volatile Evolution (MAVEN) spacecraft until its last observations of the pristine upstream solar wind for several months due to its orbit.…”

Section: Introductionmentioning

confidence: 99%

Continuous solar wind forcing knowledge: Providing continuous conditions at Mars with the WSA‐ENLIL + Cone model

et al. 2016

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Knowledge of solar wind conditions at Mars is often necessary to study the planet's magnetospheric and ionospheric dynamics. With no continuous upstream solar wind monitor at Mars, studies have used a variety of methods to measure or predict Martian solar wind conditions. In situ measurements, when available, are preferred, but can often be limited in continuity or scope, and so studies have also utilized solar wind proxies, spacecraft flybys, and Earth‐Mars alignment to provide solar wind context. Despite the importance of solar wind knowledge and the range of methods used to provide it, the use of solar wind models remains relatively unutilized. This study uses the Wang‐Sheeley‐Arge (WSA)‐ENLIL + Cone solar wind model to calculate solar wind parameters at Mars' orbital location to provide a new approach to determining solar wind conditions at Mars. Comparisons of the model results with observations by the MAVEN spacecraft indicate that the WSA‐ENLIL + Cone model can forecast solar wind conditions at Mars as accurately as it has predicted them historically at the Earth, although at Mars the model systematically mispredicts solar wind speed and density, likely a result of magnetogram calibration. Particular focus is placed on modeling the early March 2015 interplanetary coronal mass ejections (ICMEs) that interacted with Mars. Despite the complexity of the ICMEs, the model accurately predicted the speed and arrival time of the ICME‐driven interplanetary shock, although it underpredicted other solar wind parameters. These results suggest that solar wind models can be used to provide the necessary general context of the heliospheric conditions to planetary studies.

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“…An immediate approach is to parameterize the relationship functions and seek a set of optimal parameters for each solar rotation period and express them as functions of time, or other relevant parameters, such as magnetic field strength or proxy of coronal magnetic field structure, in addition to flow speed. Furthermore, such improved relation functions can represent the state of solar wind plasma near the Sun that cannot be well measured with remote sensing technique or space probes today; therefore, the modified functions can offer a good constraint or requirement to models of coronal heating and accelerations [e.g., Usmanov et al, 2000Usmanov et al, , 2011Yang et al, 2016] and enhance MHD simulation models for the trans-Alfvenic solar corona [e.g., Hayashi, 2005;Feng et al, 2010;Riley et al, 2011;Yang et al, 2012;Feng et al, 2012Feng et al, , 2015Wu et al, 2016] and interplanetary space [e.g., Dryer, 1994;Wu et al, 2005;Kataoka et al, 2009;Odstrcil and Pizzo, 2009;Intriligator et al, 2010;Detman et al, 2011;Wu et al, 2011;Hayashi, 2012;Kim et al, 2014] and heliospheric models [e.g., Washimi et al, 2011;Pogorelov et al, 2013].…”

Section: Introductionmentioning

confidence: 99%

MHD‐IPS analysis of relationship among solar wind density, temperature, and flow speed

2016

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The solar wind properties near the Sun are a decisive factor of properties in the rest of heliosphere. As such, determining realistic plasma density and temperature near the Sun is very important in models for solar wind, specifically magnetohydrodynamics (MHD) models. We had developed a tomographic analysis to reconstruct three‐dimensional solar wind structures that satisfy line‐of‐sight‐integrated solar wind speed derived from the interplanetary scintillation (IPS) observation data and nonlinear MHD equations simultaneously. In this study, we report a new type of our IPS‐MHD tomography that seeks three‐dimensional MHD solution of solar wind, matching additionally near‐Earth and/or Ulysses in situ measurement data for each Carrington rotation period. In this new method, parameterized relation functions of plasma density and temperature at 50 Rs are optimized through an iterative forward model minimizing discrepancy with the in situ measurements. Satisfying three constraints, the derived 50 Rs maps of plasma quantities provide realistic observation‐based information on the state of solar wind near the Sun that cannot be well determined otherwise. The optimized plasma quantities exhibit long‐term variations over the solar cycles 21 to 24. The differences in plasma quantities derived from the optimized and original IPS‐MHD tomography exhibit correlations with the source‐surface magnetic field strength, which can in future give new quantitative constrains and requirements to models of coronal heating and acceleration.

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

Cited by 13 publications

References 73 publications

Data-driven magnetohydrodynamic modelling of a flux-emerging active region leading to solar eruption

Data-driven magnetohydrodynamic modelling of a flux-emerging active region leading to solar eruption

Continuous solar wind forcing knowledge: Providing continuous conditions at Mars with the WSA‐ENLIL + Cone model

MHD‐IPS analysis of relationship among solar wind density, temperature, and flow speed

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