The Cluster Ion Spectrometry (CIS) Experiment

Rème, H.; Bosqued, J. M.; Sauvaud, J. A.; Cros, A.; Dandouras, J.; Aoustin, C.; Bouyssou, J.; Camus, Thierry; Cuvilo, J.; Martz, C.; Médale, J. L.; Perrier, Hideki; Romefort, D.; Rouzaud, Jean-Noël; d’Uston, C.; Möbius, E.; Crocker, Kyle; Granoff, M.; Kistler, L. M.; Popecki, M. A.; Hovestadt, D.; Klecker, B.; Paschmann, G.; Scholer, M.; Carlson, C. W.; Curtis, D. W.; Lin, R. P.; McFadden, J. P.; Formisano, V.; Amata, E.; Bavassano-Cattaneo, M. B.; Baldetti, P.; Belluci, G.; Bruno, R.; Chionchio, G.; Lellis, A. Di; Shelley, E. G.; Ghielmetti, A. G.; Lennartsson, W.; Korth, A.; Rosenbauer, H.; Lundin, R.; Olsen, Susanne Nautrup; Parks, G. K.; McCarthy, Michael; Balsiger, H.

doi:10.1007/978-94-011-5666-0_12

Cited by 211 publications

(196 citation statements)

References 18 publications

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“…All of these resonances change in frequency with plasma density, except the electron gyrofrequency and its harmonics. Cluster Ion Spectrometry (CIS) instrument (Rème et al, 1997(Rème et al, , 2001) measured the full 3-D distribution functions of major ions from thermal energies up to ∼40 keV. During 09:30 to 12:00 UT, the CIS-COmposition and DIstribution Function analyser (CODIF) measured peak ion fluxes in the energy range ∼1 keV to 10 keV in the plasma sheet-RC region, with the energy spread narrowing to ∼10 keV within the outer plasmasphere (L∼5).…”

Section: Cluster Satellite Observationsmentioning

confidence: 99%

An auroral westward flow channel (AWFC) and its relationship to field-aligned current, ring current, and plasmapause location determined using multiple spacecraft observations

Parkinson

Wild²,

Waters³

et al. 2007

Ann. Geophys.

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Abstract. An auroral westward flow channel (AWFC) is a latitudinally narrow channel of unstable F-region plasma with intense westward drift in the dusk-to-midnight sector ionosphere. AWFCs tend to overlap the equatorward edge of the auroral oval, and their life cycle is often synchronised to that of substorms: they commence close to substorm expansion phase onset, intensify during the expansion phase, and then decay during the recovery phase. Here we define for the first time the relationship between an AWFC, large-scale field-aligned current (FAC), the ring current, and plasmapause location. The Tasman International Geospace Environment Radar (TIGER), a Southern Hemisphere HF Super-DARN radar, observed a jet-like AWFC during ∼08:35 to 13:28 UT on 7 April 2001. The initiation of the AWFC was preceded by a band of equatorward expanding ionospheric scatter (BEES) which conveyed an intense poleward electric field through the inner plasma sheet. Unlike previous AWFCs, this event was not associated with a distinct substorm surge; rather it occurred during an interval of persistent, moderate magnetic activity characterised by AL∼ −200 nT. The four Cluster spacecraft had perigees within the dusk sector plasmasphere, and their trajectories were magnetically conjugate to the radar observations. The Waves of High frequency and Sounder for Probing Electron density by Relaxation (WHISPER) instruments on board Cluster were used to identify the plasmapause location. The Imager for Magnetopause-to-Aurora Global Exploration (IM-AGE) EUV experiment also provided global-scale observations of the plasmapause. The Cluster fluxgate magnetometers (FGM) provided successive measurements specifying the relative location of the ring current and filamentaryCorrespondence to: M. L. Parkinson (m.parkinson@latrobe.edu.au) plasma sheet current. An analysis of Iridium spacecraft magnetometer measurements provided estimates of large-scale ionospheric FAC in relation to the AWFC evolution. Peak flows in the AWFC were located close to the peak of a Region 2 downward FAC, located just poleward of the plasmapause. DMSP satellite observations confirmed the AWFC was located equatorward of the nightside plasmasheet, sometimes associated with ∼10 keV ion precipitation.

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Section: Cluster Satellite Observationsmentioning

confidence: 99%

An auroral westward flow channel (AWFC) and its relationship to field-aligned current, ring current, and plasmapause location determined using multiple spacecraft observations

Parkinson

Wild²,

Waters³

et al. 2007

Ann. Geophys.

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“…Once the magnetic energy distribution P (ω, k) is calculated, it can be used to identify the existing propagating modes (Sahraoui et al, 2003): for each given frequency ω 0 , and using an isocontour representation, the distribution of energy in k-space is displayed as cuts in the (k x , k y ) plane along the k z axis. For each k z corresponding to an identified peak, the theoretical dispersion relations of the plasma LF linear modes (MHD and mirror modes) are then superposed after being Doppler shifted using the flow velocities from the CIS experiment (Rème et al, 1997). The mirror mode is assumed to have approximately a zero frequency in the plasma frame, which means that it is observed in the satellite frame with the dispersion ω=k.v.…”

Section: Wave Identification Using the K-filtering Techniquementioning

confidence: 99%

Magnetic turbulent spectra in the magnetosheath: new insights

Sahraoui¹,

Belmont²,

Pinçon

et al. 2004

Ann. Geophys.

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Abstract. The spectrum of the magnetic fluctuations measured by the Cluster satellites in the inner magnetosheath is investigated using the k-filtering technique. On a case study, it is shown first that the wave vectors calculated from the Flux Gate Magnetometer (FGM) data fit well with those determined from the Spatio-Temporal Analysis of Field Fluctuations (STAFF) data for their common range of frequency, which allows one to confirm that the high pass filter applied to STAFF data does not alter the spatial characteristics of its spectra. Both analyses confirm the dominance of the mirror mode for frequencies up to 1.4 Hz. Furthermore, by comparing the experimental charateristics of the identified mirror mode to the prediction of the linear theory, it is shown that the predicted maximum growth rate is observed in the frequency range 0-0.15 Hz, i.e. the FGM range. All the rest of the mirror mode, identified for higher frequencies is more likely to be a non linear extension of the most instable one. This cascade on the spatial scales is, in turn, observed in the satellite frame as a temporal spread due to Doppler shift. Further implications on the real nature of the observed spectrum are discussed.

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“…This study is based on the following data sets: interplanetary plasma and magnetic field observations from SOHO/CELIAS (Hovestadt et al, 1995) and ACE/MAG (Smith et al, 1998), supported by magnetic field measurements from Geotail (Kokubun et al, 1994); particle and magnetic field data from Cluster 1 ("Rumba") CIS (Rème et al, 1997) and FGM (Balogh et al, 1997); particle precipitation data (Carlson et al, 2001) and magnetic field (Elphic et al, 2001) from FAST; local radar measurements of plasma convection from the Søndrestrøm radar; and global patterns of ionospheric convection from the SuperDARN HF radars (Greenwald et al, 1995 starting at 14:00 UT at the second discontinuity and terminating at 14:30 UT. After the pressure release, this quantity remains steady at slightly lower-than-normal values of 1.5 nPa.…”

Section: Observationsmentioning

confidence: 99%

Pulsed flows at the high-altitude cusp poleward boundary, and associated ionospheric convection and particle signatures, during a Cluster - FAST - SuperDARN- Søndrestrøm conjunction under a southwest IMF

et al. 2004

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Abstract. Particle and magnetic field observations during a magnetic conjunction Cluster 1-FAST-Søndrestrøm within the field of view of SuperDARN radars on 21 January 2001 allow us to draw a detailed, comprehensive and selfconsistent picture at three heights of signatures associated with transient reconnection under a steady south-westerly IMF (clock angle ≈130 • ). Cluster 1 was outbound through the high altitude (∼12R E ) exterior northern cusp tailward of the bifurcation line (geomagnetic B x >0) when a solar wind dynamic pressure release shifted the spacecraft into a boundary layer downstream of the cusp. The centerpiece of the investigation is a series of flow bursts observed there by the spacecraft, which were accompanied by strong field perturbations and tailward flow deflections. Analysis shows these to be Alfvén waves. We interpret these flow events as being due to a sequence of reconnected flux tubes, with fieldaligned currents in the associated Alfvén waves carrying stresses to the underlying ionosphere, a view strengthened by the other observations. At the magnetic footprint of the region of Cluster flow bursts, FAST observed an ion energylatitude disperison of the stepped cusp type, with individual cusp ion steps corresponding to individual flow bursts. Simultaneously, the SuperDARN Stokkseyri radar observed very strong poleward-moving radar auroral forms (PMRAFs) which were conjugate to the flow bursts at Cluster. FAST was traversing these PMRAFs when it observed the cusp ion

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The Cluster Ion Spectrometry (CIS) Experiment

Cited by 211 publications

References 18 publications

An auroral westward flow channel (AWFC) and its relationship to field-aligned current, ring current, and plasmapause location determined using multiple spacecraft observations

An auroral westward flow channel (AWFC) and its relationship to field-aligned current, ring current, and plasmapause location determined using multiple spacecraft observations

Magnetic turbulent spectra in the magnetosheath: new insights

Pulsed flows at the high-altitude cusp poleward boundary, and associated ionospheric convection and particle signatures, during a Cluster - FAST - SuperDARN- Søndrestrøm conjunction under a southwest IMF

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