MHD simulation of energy transfer across magnetopause during sudden changes of the IMF orientation

Jing, Hao; Lu, J. Y.; Кабин, К.; Zhao, Jinsong; Liu, Z. Q.; Yang, Yi; Zhao, Ming-Xian; Wang, M.

doi:10.1016/j.pss.2014.04.001

Cited by 16 publications

(16 citation statements)

References 42 publications

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“…This model has been applied to study numerous aspects of the magnetospheric physics in the past [e.g., Song and Russell , ; Gombosi et al , ; Kabin et al , ; Zhang et al , ; Tóth et al , ] and is thoroughly validated [e.g., Welling and Ridley , ; Rae et al , ]. Recently, we have used the SWMF to study the global magnetopause shape and its dependence on the solar wind conditions [ Lu et al , , , ; Liu et al , , ], as well as the energy transfer across the magnetopause [ Lu et al , ; Jing et al , ]. This model was also used by Wang et al [] to analyze the influence of the dipole tilt angle on the shape and size of the bow shock.…”

Section: Methodsmentioning

confidence: 99%

“…Recently, we have used the SWMF to study the global magnetopause shape and its dependence on the solar wind conditions [Lu et al, 2010[Lu et al, , 2013aLiu et al, 2012Liu et al, , 2015, as well as the energy transfer across the magnetopause [Lu et al, 2013b;Jing et al, 2014]. This model was also used by Wang et al [2015] to analyze the influence of the dipole tilt angle on the shape and size of the bow shock.…”

Section: Methodsmentioning

confidence: 99%

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The influence of IMF clock angle on the cross section of the tail bow shock

Wang

Кабин

et al. 2016

JGR Space Physics

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We study effects of the interplanetary magnetic field (IMF) orientation on the terrestrial tail bow shock location and shape by using global MHD magnetosphere model and empirical bow shock models. It is shown that the tail bow shock cross section is well approximated by an ellipse with the direction of the major axis roughly perpendicular to the IMF clock angle direction. With the increasing IMF clock angle, the eccentricity of the bow shock cross section increases for northward IMF but decreases for southward IMF.

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Section: Methodsmentioning

confidence: 99%

Section: Methodsmentioning

confidence: 99%

The influence of IMF clock angle on the cross section of the tail bow shock

Wang

Кабин

et al. 2016

JGR Space Physics

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“…Recently, we have used the SWMF to check the global magnetopause structure and their dependence on the solar wind conditions and interplanetary magnetic fields (Lu et al, 2010(Lu et al, , 2013aLiu et al, 2012). Lu et al (2013b) and Jing et al (2014) further used the SWMF to investigate the energy transfer across magnetopause under different solar wind conditions. Especially Liu et al (2012) demonstrated the significant influence of the dipole tilt angle on the magnetopause, which motivates to see how important the dipole tilt angle affects the bow shock.…”

Section: Global Mhd Model and Identification Of The Bow Shockmentioning

confidence: 99%

The dipole tilt angle dependence of the bow shock for southward IMF: MHD results

Wang

Yuan

et al. 2015

Planetary and Space Science

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“…Several studies have demonstrated that different solar wind conditions, for example, the sheath and the ejecta, lead to differences in the solar wind‐magnetosphere coupling and magnetospheric activity [ Huttunen et al , , , ; Pulkkinen et al , ; Nikolaeva et al , ; Guo et al , ; Yermolaev et al , ; Lu et al , ; Jing et al , ]. Huttunen and Koskinen [] showed by analyzing the behavior of various geomagnetic indices that sheath regions typically lead to strong enhancements of high‐latitude ionospheric currents ( A E , A L , and also K p ), while magnetic clouds are more effective in enhancing the equatorial ring current ( D s t and S Y M ‐ H ).…”

Section: Introductionmentioning

confidence: 99%

Solar wind‐magnetosphere coupling efficiency during ejecta and sheath‐driven geomagnetic storms

et al. 2016

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We have investigated the effect of key solar wind driving parameters on solar wind‐magnetosphere coupling efficiency during sheath and magnetic cloud‐driven storms. The particular focus of the study was on the coupling efficiency dependence with Alfvén Mach number (MA). The efficiency has been estimated using the dawn‐dusk component of the interplanetary electric field (EY), Newell and Borovsky functions as a proxy for the energy inflow and the polar cap potential (PCN), and auroral electrojet (AE) and SYM‐H indices as the measure of the energy output. We have also performed a time delay analysis between the input parameters and the geomagnetic indices. The optimal time lag and smoothing window length depend on the coupling function used and on the solar wind driver. For example, turbulent sheaths are more sensitive to the time shift and the averaging interval than smoother magnetic clouds. The results presented in this study show that the solar wind‐magnetosphere coupling efficiency depends strongly on the definition used, and it increases with increasing MA. We demonstrate that the PCN index distinctively shows both a Mach number dependent saturation and a Mach number independent saturation, pointing to the existence of at least two underlying physical mechanisms for the saturation of the index. By contrast, we show that the AE index saturates but that the saturation of this index is independent of the solar wind Mach number. Finally, we find that the SYM‐H index does not seem to saturate and that the absence of saturation is independent of the Mach number regime. We highlight the difference between the typical MA conditions during sheath regions and magnetic clouds. The lowest MA values are related to the magnetic clouds. As a consequence, sheaths typically have higher solar wind‐magnetosphere coupling efficiencies than magnetic clouds.

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MHD simulation of energy transfer across magnetopause during sudden changes of the IMF orientation

Cited by 16 publications

References 42 publications

The influence of IMF clock angle on the cross section of the tail bow shock

The influence of IMF clock angle on the cross section of the tail bow shock

The dipole tilt angle dependence of the bow shock for southward IMF: MHD results

Solar wind‐magnetosphere coupling efficiency during ejecta and sheath‐driven geomagnetic storms

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