Size and shape of the distant magnetotail

Sibeck, D. G.; Lin, Ray-Qing

doi:10.1002/2013ja019471

Cited by 39 publications

(44 citation statements)

References 51 publications

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“…Observations discussed by Lavraud et al [] confirmed this and also showed that this asymmetry is more pronounced in the case of low Mach numbers. Similar conclusions were also reached by Sibeck and Lin [] in their modeling study.…”

Section: Introductionsupporting

confidence: 90%

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: Introductionsupporting

confidence: 90%

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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“…For example, bow shock reflection should create hot electrons predominantly in the duskside magnetosheath [ Sibeck and McEntire , ]. The locations of the magnetopause reconnection in the tail have a dawn‐dusk asymmetry depending on the IMF B y direction [ Sibeck and Lin , ]. The magnetosphere electrons may be hotter on the dawnside due to drift effect, thus may result in stronger enhancements in the dawnside magnetosheath [e.g., Imada et al ., ].…”

Section: Discussionmentioning

confidence: 99%

Source and structure of bursty hot electron enhancements in the tail magnetosheath: Simultaneous two‐probe observation by ARTEMIS

et al. 2014

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Bursty enhancements of hot electrons (≳0.5 keV) with duration of minutes sometimes occur in the tail magnetosheath. In this study we used the unique simultaneous measurements from the two Acceleration Reconnection Turbulence and Electrodynamics of Moon's Interaction with the Sun probes to investigate the likely sources, spatial structures, and responsible processes for these hot electron enhancements. The enhancements can be seen at any distance across the magnetosheath, but those closer to the magnetopause are more often accompanied by magnetosheath density and flow magnitudes changing to more magnetosphere-like values. From simultaneous measurements with the two probes being on either side of magnetopause or both in the magnetosheath, it is evident that these hot electrons come from the magnetosphere near the current sheet without further energization and that the enhancements are a result of bursty lateral magnetosphere intrusion into the magnetosheath, the enhancements and changes in the magnetosheath properties becoming smaller with increasing outward distance from the intrusion. From limited events having specific separation distances and alignments between the probes, we estimated that a single isolated enhancement can have a thin and elongated structure as narrow as 2 R E wide in the X direction, as long as over 7 R E in the Y direction, and as thin as 1 R E in the Z direction. We propose that Kelvin-Helmholtz perturbations at the magnetopause and subsequent magnetosphere-magnetosheath particle mixing due to reconnection or diffusion can plausibly play an important role in generating the bursty magnetosphere intrusion into the magnetosheath and the hot electron enhancements.

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“…A Figura 1 apresenta as regiões mais importantes que compõem a magnetosfera terrestre [2,9,10]. O lado diurno, queé a região voltada para o Sol no lado esquerdo da Figura 1, estende-se, tipicamente, por 10 raios terrestres 3 em condições de vento solar calmo.…”

Section: A Interação Vento Solarmagnetosfera Terrestreunclassified

“…A magnetocauda pode chegar a distâncias superiores a 200 raios terrestres, sendo considerado um grande reservatório de energia e plasma [2,9,10].…”

Section: A Interação Vento Solarmagnetosfera Terrestreunclassified

Conceitos básicos sobre a física da formação de tubos de fluxo magnético nas proximidades da Terra

Ferreira

Silveira

Cardoso

et al. 2017

Rev. Bras. Ensino Fís.

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Em 1978 Christopher T. Russell e Richard C. Elphic detectaram tubos de fluxo magnético na região de fronteira da magnetosfera terrestre por meio de dados observacionais obtidos pelos satélites ISEE-1 e -2, que foram denominados eventos de transferência de fluxo, ou simplesmente FTE (do inglês, flux transfer events). O vento solar, juntamente com o campo magnético interplanetário, oriundos do Sol, atingem a região de campo magnético terrestre, produzindo fenômenos como a reconexão magnética e os tubos de fluxo. Esse artigo apresenta uma introdução sobre a conexão Sol-Terra e o processo de reconexão magnética, e principalmente, os conceitos básicos sobre a geração e a formação dos tubos de fluxo magnético. Os modelos que descrevem o tipo de reconexão e as características dos tubos, como por exemplo Russell-Elphic, Lee-Fu e Southwood-Scholer, e as propriedades dos eventos FTE, são apresentados de forma clara e concisa. Por fim, o artigo trata de um exemplo de identificação dos tubos em simulação computacional, realizado nesse trabalho. Palavras-chave: eventos de transferência de fluxo, física espacial, vento solar, reconexão magnética.In 1978 Christopher T. Russell and Richard C. Elphic detected magnetic flux tubes in magnetosphere boundary region through observational data obtained from the satellites ISEE-1 and -2, which were named flux transfer events (FTE). The solar wind together with the interplanetary magnetic field, both originated in the Sun, reach the earth magnetic field region, producing the magnetic reconnection and the flux tubes phenomena. This paper presents an introduction on the Sun-Earth connection and the magnetic reconnection process, and mainly the basic concepts on the tubes generation and formation. The models which describe the type of reconnection and the tubes signatures, for example, Russell-Elphic, Lee-Fu, Southwood-Scholer, and the FTE event characteristics, are presented in a clear and concise way. Finally, this paper brings an example of the tubes identification in computing simulation, performed in this work.

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Size and shape of the distant magnetotail

Cited by 39 publications

References 51 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

Source and structure of bursty hot electron enhancements in the tail magnetosheath: Simultaneous two‐probe observation by ARTEMIS

Conceitos básicos sobre a física da formação de tubos de fluxo magnético nas proximidades da Terra

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