Three dimensional shape of the magnetopause: Global MHD results

Lu, J. Y.; Liu, Z.-Q.; Кабин, К.; Zhao, Ming-Xian; Liu, D. D.; Zhou, Quan; Xiao, Y. C.

doi:10.1029/2010ja016418

Cited by 48 publications

(76 citation statements)

References 39 publications

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“…However, at present they rather add to the confusion. In particular, Lu et al (2011) found that larger negative IMF B z causes the tailward magnetopause to shrink, contrary to the empirical models by both Shue et al (1998) and Lin et al (2010). Such a strange result is most likely due to the actual boundary studied in that work being not the magnetopause proper, but the fluopause , located inward from the magnetopause and gradually converging towards the plasma sheet owing to the dawn-dusk electric field caused by IMF B z < 0.…”

Section: Magnetopause Shape and The Imf 'Penetration'contrasting

confidence: 51%

Data-based modelling of the Earth's dynamic magnetosphere: a review

Tsyganenko

2013

Ann. Geophys.

119

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Abstract. This paper reviews the main advances in the area of data-based modelling of the Earth's distant magnetic field achieved during the last two decades. The essence and the principal goal of the approach is to extract maximum information from available data, using physically realistic and flexible mathematical structures, parameterized by the most relevant and routinely accessible observables. Accordingly, the paper concentrates on three aspects of the modelling: (i) mathematical methods to develop a computational "skeleton" of a model, (ii) spacecraft databases, and (iii) parameterization of the magnetospheric models by the solar wind drivers and/or ground-based indices. The review is followed by a discussion of the main issues concerning further progress in the area, in particular, methods to assess the models' performance and the accuracy of the field line mapping. The material presented in the paper is organized along the lines of the author Julius-Bartels' Medal Lecture during the General Assembly 2013 of the European Geosciences Union.

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Section: Magnetopause Shape and The Imf 'Penetration'contrasting

confidence: 51%

Data-based modelling of the Earth's dynamic magnetosphere: a review

Tsyganenko

2013

Ann. Geophys.

119

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“…Although they can predict widely divergent magnetopause locations for the same solar wind conditions (Samsonov et al 2016), global magnetohydrodynamic simulations all indicate that the solar wind dynamic pressure and north/south component of the IMF are the most important factors determining magnetopause location (Lu et al 2011). As illustrated in the top panel of Fig.…”

Section: Earth's Magnetopausementioning

confidence: 99%

Imaging Plasma Density Structures in the Soft X-Rays Generated by Solar Wind Charge Exchange with Neutrals

et al. 2018

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Both heliophysics and planetary physics seek to understand the complex nature of the solar wind's interaction with solar system obstacles like Earth's magnetosphere, the ionospheres of Venus and Mars, and comets. Studies with this objective are frequently conducted with the help of single or multipoint in situ electromagnetic field and particle observations, guided by the predictions of both local and global numerical simulations, and placed in con- text by observations from far and extreme ultraviolet (FUV, EUV), hard X-ray, and energetic neutral atom imagers (ENA). Each proposed interaction mechanism (e.g., steady or transient magnetic reconnection, local or global magnetic reconnection, ion pick-up, or the KelvinHelmholtz instability) generates diagnostic plasma density structures. The significance of each mechanism to the overall interaction (as measured in terms of atmospheric/ionospheric loss at comets, Venus, and Mars or global magnetospheric/ionospheric convection at Earth) remains to be determined but can be evaluated on the basis of how often the density signatures that it generates are observed as a function of solar wind conditions. This paper reviews efforts to image the diagnostic plasma density structures in the soft (low energy, 0.1-2.0 keV) X-rays produced when high charge state solar wind ions exchange electrons with the exospheric neutrals surrounding solar system obstacles. The introduction notes that theory, local, and global simulations predict the characteristics of plasma boundaries such the bow shock and magnetopause (including location, density gradient, and motion) and regions such as the magnetosheath (including density and width) as a function of location, solar wind conditions, and the particular mechanism operating. In situ measurements confirm the existence of time-and spatial-dependent plasma density structures like the bow shock, magnetosheath, and magnetopause/ionopause at Venus, Mars, comets, and the Earth. However, in situ measurements rarely suffice to determine the global extent of these density structures or their global variation as a function of solar wind conditions, except in the form of empirical studies based on observations from many different times and solar wind conditions. Remote sensing observations provide global information about auroral ovals (FUV and hard X-ray), the terrestrial plasmasphere (EUV), and the terrestrial ring current (ENA). ENA instruments with low energy thresholds (∼ 1 keV) have recently been used to obtain important information concerning the magnetosheaths of Venus, Mars, and the Earth. Recent technological developments make these magnetosheaths valuable potential targets for high-cadence wide-field-of-view soft X-ray imagers.Section 2 describes proposed dayside interaction mechanisms, including reconnection, the Kelvin-Helmholtz instability, and other processes in greater detail with an emphasis on the plasma density structures that they generate. It focuses upon the questions that remain as yet unanswered, such as the significanc...

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“…Most empirical magnetopause models [e.g., Sibeck et al, 1991;Petrinec and Russell, 1996;Shue et al, 1997;Kawano et al, 1999] also adopted the hypothesis that magnetopause is rotational symmetric about the aberrated Sun-Earth line and has a rounded section at magnetotail. Lu et al [2011] developed a numerical three-dimensional magnetopause model considering the impact of IMF B z and solar wind dynamic pressure (D p ) on the shape of magnetopause. They showed that the dayside magnetopause shape in the yz plane is an oval elongated along the y direction, and the magnetotail magnetopause is an oval elongated along the z direction.…”

Section: 1002/2013ja019257mentioning

confidence: 99%

Effects of the interplanetary magnetic field on the twisting of the magnetotail: Global MHD results

Wang

Huang

et al. 2014

JGR Space Physics

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We used the global magnetohydrodynamic (MHD) simulation to investigate effects of the interplanetary magnetic field (IMF) on the twisting of the magnetotail. It is shown that the cross section of the magnetotail is elongated along a certain direction close to the IMF orientation. The elongated direction twists with the IMF orientation, magnitude, and the distance away from Earth, and the quantitative relationship has been given. In addition, the current sheet has a similar twisting behavior as the magnetotail magnetopause, with a smaller twisting angle. Our simulated results fall within the range that people have deduced from observations.

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Three dimensional shape of the magnetopause: Global MHD results

Cited by 48 publications

References 39 publications

Data-based modelling of the Earth's dynamic magnetosphere: a review

Data-based modelling of the Earth's dynamic magnetosphere: a review

Imaging Plasma Density Structures in the Soft X-Rays Generated by Solar Wind Charge Exchange with Neutrals

Effects of the interplanetary magnetic field on the twisting of the magnetotail: Global MHD results

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