First multispacecraft ion measurements in and near the Earth’s magnetosphere with the identical Cluster ion spectrometry (CIS) experiment

Rème, H.; Aoustin, C.; Bosqued, J. M.; Dandouras, I.; Lavraud, B.; Sauvaud, J. A.; Barthe, A.; Bouyssou, J.; Camus, Thierry; Cœur-Joly, O.; Cros, A.; Cuvilo, J.; Ducay, F.; Garbarowitz, Y.; Médale, J. L.; Penou, E.; Perrier, Hideki; Romefort, D.; Rouzaud, Jean-Noël; Vallat, C.; Alcaydé, D.; Jacquey, C.; Mazelle, C.; d’Uston, C.; Möbius, E.; Kistler, L. M.; Crocker, Kyle; Granoff, M.; Mouikis, C.; Popecki, M. A.; Vosbury, M.; Klecker, B.; Hovestadt, D.; Kucharek, H.; Kuenneth, E.; Paschmann, G.; Scholer, M.; Sckopke, N.; Seidenschwang, E.; Carlson, C. W.; Curtis, D. W.; Ingraham, C.; Lin, R. P.; McFadden, J. P.; Parks, G. K.; Phan, T. D.; Formisano, V.; Amata, E.; Bavassano-Cattaneo, M. B.; Baldetti, P.; Bruno, R.; Chionchio, G.; Lellis, A. Di; Marcucci, M. F.; Pallocchia, G.; Korth, A.; Daly, P. W.; Graeve, B.; Rosenbauer, H.; Vasyliūnas, V. M.; McCarthy, Michael; Wilber, M.; Eliasson, L.; Lundin, R.; Olsen, Susanne Nautrup; Shelley, E. G.; Fuselier, S. A.; Ghielmetti, A. G.; Lennartsson, W.; Escoubet, C. P.; Balsiger, H.; Friedel, R. H.; Cao, Jinbin; Kovrazhkin, R. A.; Papamastorakis, I.; Pellat, R.; Scudder, J.; Sonnerup, B. U. Ö.

doi:10.5194/angeo-19-1303-2001

Cited by 1,101 publications

(913 citation statements)

References 31 publications

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“…1. Data from the Flux Gate Magnetometer 31 , Cluster Ion Spectrometry Experiment 32 and Plasma Electron and Current Experiment 33 instruments onboard Cluster have been used for this study. The time-shifted 1 min OMNI data at the earth's bow shock is used to get the solar wind parameters and the IMF.…”

Section: Resultsmentioning

confidence: 99%

Solar wind entry into the high-latitude terrestrial magnetosphere during geomagnetically quiet times

et al. 2013

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An understanding of the transport of solar wind plasma into and throughout the terrestrial magnetosphere is crucial to space science and space weather. For non-active periods, there is little agreement on where and how plasma entry into the magnetosphere might occur. Moreover, behaviour in the high-latitude region behind the magnetospheric cusps, for example, the lobes, is poorly understood, partly because of lack of coverage by previous space missions. Here, using Cluster multi-spacecraft data, we report an unexpected discovery of regions of solar wind entry into the Earth's high-latitude magnetosphere tailward of the cusps. From statistical observational facts and simulation analysis we suggest that these regions are most likely produced by magnetic reconnection at the high-latitude magnetopause, although other processes, such as impulsive penetration, may not be ruled out entirely. We find that the degree of entry can be significant for solar wind transport into the magnetosphere during such quiet times.

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Section: Resultsmentioning

confidence: 99%

Solar wind entry into the high-latitude terrestrial magnetosphere during geomagnetically quiet times

et al. 2013

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“…There is a decrement of less than 10% in V x . Magnetic field data have a resolution of 5 vect/s [Balogh et al, 2001] and plasma moments from the Cluster Ion Spectrometry (CIS) instrument [Rème et al, 2001] are once per spin. Ion data from the CIS (HIA) experiment yield both the bulk solar wind plasma parameters and the threedimensional distribution functions of suprathermal ions in the range 0-32 keV.…”

Section: Cluster Observations Of Foreshock Cavitonsmentioning

confidence: 99%

Foreshock cavitons for different interplanetary magnetic field geometries: Simulations and observations

et al. 2011

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[1] Global hybrid (kinetic ions, fluid electrons) simulations have shown the existence of foreshock cavitons characterized by large depressions in plasma density and magnetic field magnitude, bounded by enhancements in these two parameters. Foreshock cavitons share some characteristics with reported foreshock cavities, but in contrast to the cavities that often appear as isolated structures, cavitons are always found surrounded by a sea of ultra low frequency (ULF) waves. They always occur in regions deep in the foreshock, downstream from the ion and ULF wave boundaries. We perform global hybrid simulations to show that cavitons can form for a variety of interplanetary magnetic field (IMF) geometries and different solar wind Mach numbers. We use Cluster data to show that cavitons are a common foreshock feature, and that they can form for different IMF orientations, consistent with our simulation results. We find that cavitons show density and field decrements as large as 60% of the ambient values. They are immersed in regions where waves show transverse and compressive components and the presence of diffuse ion distributions. We use linear kinetic theory to estimate wave growth for the two types of waves responsible for caviton formation, i.e., the weakly compressive waves and oblique propagating linearly polarized waves. Some of the cavitons observed by Cluster show trains of high-frequency waves inside them and this is consistent with the predictions of local higher-resolution hybrid simulations.Citation: Blanco-Cano, X., P. Kajdič, N. Omidi, and C. T. Russell (2011), Foreshock cavitons for different interplanetary magnetic field geometries: Simulations and observations,

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“…Planetary missions usually do not have particle data of sufficient resolution, so wave observations can then be used instead to infer the presence of DFs. In this letter we present statistics of whistlers in relation to DFs observed by Cluster [Escoubet et al, 1997] [Balogh et al, 2001], (b) electron density from PEACE [Owen et al, 2001], (c) ion velocity (X GSM) from both CIS [Rème et al, 2001] and v E×B using Electric Fields and Waves (EFW) [Gustafsson et al, 2001], (d) electron differential energy flux, (e) pitch angle distribution for energies of 3-10 keV, (f ) power spectral density of the wave magnetic field, (g) the degree of polarization, (h) the ellipticity, and (i) the wave angle with respect to the magnetic field. Data for Figures 1f-1i are calculated from spectral matrices produced by onboard STAFF Spectrum Analyzer [Cornilleau-Wehrlin et al, 2003], using the PRASSADCO program [Santolík, 2000;Santolík et al, 2003].…”

Section: Introductionmentioning

confidence: 99%

Whistler mode waves at magnetotail dipolarization fronts

et al. 2014

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We report the statistics of whistler mode waves observed in relation to dipolarization fronts (DFs) in Earth's magnetotail using data from the four Cluster spacecraft spanning a period of 9 years, 2001-2009. We show that whistler mode waves are common in a vicinity of DFs: between 30 and 60% of all DFs are associated with whistlers. Whistlers are about 7 times more likely to be observed near a DF than at any random location in the magnetotail. Therefore, whistlers are a characteristic signature of DFs. We find that whistlers are most often detected in the flux pileup region (FPR) following the DF, close to the center of the current sheet (B x ∼ 0) and in association with anisotropic electron distributions (T ⟂ > T ∥ ). This suggests that we typically observe emissions in the source region where they are generated by the anisotropic electrons produced by the betatron process inside the FPR.

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First multispacecraft ion measurements in and near the Earth’s magnetosphere with the identical Cluster ion spectrometry (CIS) experiment

Cited by 1,101 publications

References 31 publications

Solar wind entry into the high-latitude terrestrial magnetosphere during geomagnetically quiet times

Solar wind entry into the high-latitude terrestrial magnetosphere during geomagnetically quiet times

Foreshock cavitons for different interplanetary magnetic field geometries: Simulations and observations

Whistler mode waves at magnetotail dipolarization fronts

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