Dense and stagnant ions in the low‐latitude boundary region under northward interplanetary magnetic field

Hasegawa, Hiroshi; Fujimoto, M.; Saito, Y.; Mukai, T.

doi:10.1029/2003gl019120

Cited by 40 publications

(43 citation statements)

References 14 publications

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“…The northward IMF is a condition for such transportation through the LLBL. Ions from the LLBL are relatively cold, while ions from the distant tail are relatively hot (Nishida, 2000;Hasegawa et al, 2004a). When the solar wind speed is higher, more ions with low temperature enter the near-Earth plasma sheet through the LLBL, thus the temperature of the plasma sheet becomes colder.…”

Section: Results Of the Correlations Between Solar Wind And The Plasmmentioning

confidence: 99%

A statistical study on the correlations between plasma sheet and solar wind based on DSP explorations

et al. 2005

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Abstract. By using the data of two spacecraft, TC-1 and ACE (Advanced Composition Explorer), a statistical study on the correlations between plasma sheet and solar wind has been carried out. The results obtained show that the plasma sheet at geocentric distances of about 9∼13.4 Re has an apparent driving relationship with the solar wind. It is found that (1) there is a positive correlation between the duskward component of the interplanetary magnetic field (IMF) and the duskward component of the geomagnetic field in the plasma sheet, with a proportionality constant of about 1.09. It indicates that the duskward component of the IMF can effectively penetrate into the near-Earth plasma sheet, and can be amplified by sunward convection in the corresponding region at geocentric distances of about 9∼13.4 Re; (2) the increase in the density or the dynamic pressure of the solar wind will generally lead to the increase in the density of the plasma sheet; (3) the ion thermal pressure in the near-Earth plasma sheet is significantly controlled by the dynamic pressure of solar wind; (4) under the northward IMF condition, the ion temperature and ion thermal pressure in the plasma sheet decrease as the solar wind speed increases. This feature indicates that plasmas in the near-Earth plasma sheet can come from the magnetosheath through the LLBL. Northward IMF is one important condition for the transport of the cold plasmas of the magnetosheath into the plasma sheet through the LLBL, and fast solar wind will enhance such a transport process.

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Section: Results Of the Correlations Between Solar Wind And The Plasmmentioning

confidence: 99%

A statistical study on the correlations between plasma sheet and solar wind based on DSP explorations

et al. 2005

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“…Most recent simulations have been conducted using fully kinetic particle codes (Matsumoto and Hoshino, 2006;Nakamura et al, 2011), which demonstrate that particle transport through vortexinduced reconnection or turbulent mixing can occur within and/or around a developed KH vortex. It has been suggested that the plasma transport enhanced by the KHI is the key to the formation of the LLBL and the cold-dense plasma sheet (CDPS) that become prominent under northward IMF conditions (Mitchell et al, 1987;Terasawa et al, 1997;Wing and Newell, 2002;Hasegawa et al, 2004b) when reconnection is unlikely to occur at the low-latitude magnetopause.…”

Section: Possible Roles Of the Kelvin-helmholtz Instabilitymentioning

confidence: 99%

Structure and Dynamics of the Magnetopause and Its Boundary Layers

Hasegawa¹

2012

Monogr. Environ. Earth Planets

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The magnetopause is the key region in space for the transfer of solar wind mass, momentum, and energy into the magnetosphere. During the last decade, our understanding of the structure and dynamics of Earth's magnetopause and its boundary layers has advanced considerably, thanks largely to the advent of multi-spacecraft missions such as Cluster and THEMIS. Moreover, various types of physics-based techniques have been developed for visualizing two-or threedimensional plasma and field structures from data taken by one or more spacecraft, providing a new approach to the analysis of the spatiotemporal properties of magnetopause processes, such as magnetic reconnection and the Kelvin-Helmholtz instability (KHI). Information on the size, shape, orientation, and evolution of magnetic flux ropes or flow vortices generated by those processes can be extracted from in situ measurements. Observations show that magnetopause reconnection can be globally continuous for both southward and northward interplanetary magnetic field (IMF) conditions, but even under such circumstances, more than one X-line may exist within a certain (low-latitude or high-latitude) portion on the magnetopause and some X-lines may retreat anti-sunward. The potential global effects of such behavior are discussed. An overview is also given of the identification, excitation, evolution, and possible consequences of the magnetopause KHI: there is evidence for nonlinear KHI growth and associated vortex-induced reconnection under northward IMF. Observation-based estimates indicate that reconnection tailward of both polar cusps can be the dominant mechanism for solar wind plasma entry into the dayside magnetosphere under northward IMF. However, the mechanism by which the transferred plasma is transported into the central portion of the magnetotail, and the role of magnetopause processes in this transport, remain unclear. Future prospects of magnetopause and other relevant studies are also discussed.

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“…The Kelvin-Helmoltz instability is an MHD instability driven by a flow shear between the magnetosheath and the magnetosphere (Seki et al 2015). Hasegawa et al (2004a) noted that the plasma content in the outer terrestrial magnetosphere increases during northward solar wind magnetic field conditions (Mitchell et al 1987;Hasegawa et al 2004b), contrary to what would be expected in case reconnection were dominant. Hasegawa et al (2004b) showed that during northward solar wind magnetic field conditions -in the absence of active reconnection at low latitudes -there is a solar wind transport mechanism associated with the nonlinear phase of the Kelvin-Helmholtz instability, supplying plasma sources for various space weather phenomena in the circum-terrestrial space.…”

Section: Plasma and Magnetic Fieldsmentioning

confidence: 50%

Planetary space weather: scientific aspects and future perspectives

Plainaki

Lilensten

Radioti

et al. 2016

J. Space Weather Space Clim.

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In this paper, we review the scientific aspects of planetary space weather at different regions of our Solar System, performing a comparative planetology analysis that includes a direct reference to the circum-terrestrial case. Through an interdisciplinary analysis of existing results based both on observational data and theoretical models, we review the nature of the interactions between the environment of a Solar System body other than the Earth and the impinging plasma/radiation, and we offer some considerations related to the planning of future space observations. We highlight the importance of such comparative studies for data interpretations in the context of future space missions (e.g. ESA JUICE; ESA/JAXA BEPI COLOMBO). Moreover, we discuss how the study of planetary space weather can provide feedback for better understanding the traditional circumterrestrial space weather. Finally, a strategy for future global investigations related to this thematic is proposed.

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Dense and stagnant ions in the low‐latitude boundary region under northward interplanetary magnetic field

Cited by 40 publications

References 14 publications

A statistical study on the correlations between plasma sheet and solar wind based on DSP explorations

A statistical study on the correlations between plasma sheet and solar wind based on DSP explorations

Structure and Dynamics of the Magnetopause and Its Boundary Layers

Planetary space weather: scientific aspects and future perspectives

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