Low frequency wave sources in the outer magnetosphere, magnetosheath, and near Earth solar wind

Constantinescu, Dragoş; Glaßmeier, Karl‐Heinz; Décréau, Pierrette; Fränz, M.; Fornaçon, K.‐H.

doi:10.5194/angeo-25-2217-2007

Cited by 25 publications

(21 citation statements)

References 27 publications

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“…They found a higher level of plasma and magnetic field fluctuations in the foreshock than in the undisturbed solar wind and in the quasi-parallel magnetosheath than in the quasi-perpendicular magnetosheath. Constantinescu et al [2007] found a source of low-frequency waves in the electron foreshock and in the cusp region. Gutynska et al [2012] suggested that the solar wind is the source of coherent low-frequency fluctuations (10 −4 − 10 −3 Hz) in the magnetosheath, whereas higher-frequency fluctuations (up to 10 −1 Hz) are generated by local sources.…”

Section: Introductionmentioning

confidence: 99%

Magnetosheath plasma structures and their relation to foreshock processes

2015

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We present simultaneous Time History of Events and Macroscale Interactions during Substormsobservations of plasma parameters upstream in the solar wind and downstream in the magnetosheath (MSH) from 2007 to 2008. We discuss the connection of foreshock (FSH) processes and magnetospheric disturbances to transmission mechanisms in the MSH. In 60% of the analyzed cases, the MSH was strongly influenced by the FSH. We analyze the results as a function of location, time scale, spatial orientation of the observed structures, and the prevailing interplanetary magnetic field (IMF) and solar wind plasma parameters. We find that plasma structures with density enhancement are mostly observed during radial IMF orientations and for small BN , the angle between the upstream magnetic field and the local bow shock normal; the observed structures are pressure balanced with strong anticorrelation between density and temperature; the scale size of the density fluctuations is about 0.4R E . We compare the observations with results from a 2.5-dimensional hybrid simulation to investigate the mechanisms by which the foreshock plasma structures are generated, propagate through the bow shock, and evolve.

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Section: Introductionmentioning

confidence: 99%

Magnetosheath plasma structures and their relation to foreshock processes

2015

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“…Pinçon and Lefeuvre (1991) expanded the method to include multidimensional (vectorial) observables and Motschmann et al (1996) further developed it in order to apply it to multipoint satellite measurements (e.g. Glassmeier et al, 2001;Narita et al, 2003;Constantinescu et al, 2007).…”

Section: Introductionmentioning

confidence: 99%

Statistical analysis of ground based magnetic field measurements with the field line resonance detector

et al. 2008

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Abstract. In this paper we introduce the field line resonance detector (FLRD), a wave telescope technique which has been specially adapted to estimate the spectral energy density of field line resonance (FLR) phase structures in a superposed wave field. The field line resonance detector is able to detect and correctly characterize several superposed FLR structures of a wave field and therefore constitutes a new and powerful tool in ULF pulsation studies. In our work we derive the technique from the classical wave telescope beamformer and present a statistical analysis of one year of ground based magnetometer data from the Canadian magnetometer network CANOPUS, now known as CARISMA. The statistical analysis shows that the FLRD is capable of detecting and characterizing superposed or hidden FLR structures in most of the detected ULF pulsation events; the one year statistical database is therefore extraordinarily comprehensive. The results of this analysis confirm the results of previous FLR characterizations and furthermore allow a detailed generalized dispersion analysis of FLRs.

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“…This data pool will be further enriched by the measurements of the upcoming ESA/Swarm mission, a constellation of three satellites in three different polar orbits between 400 and 550 km altitude, which will be launched in 2013. This data pool provides unique opportunities to study ULF pulsations in the magnetosphere (e.g., Constantinescu et al, 2007;Usanova et al, 2008;Sarris et al, 2009;Picket et al, 2010). New analysis tools that can cope with increased volume of measurements by numerous spacecraft located at different regions of the magnetosphere, similar to the ones employed in the present study, will effectively enhance the scientific exploitation of the continuously accumulated data.…”

Section: Discussionmentioning

confidence: 99%

“…These studies revealed that toroidal and poloidal mode field line resonances together with compressional Pc5 waves account for most of the observed coherent pulsations observed in the outer magnetosphere (Anderson et al, 1990). Multipoint observations show that upstream ULF waves in the Pc3-4 bands are generated in the foreshock region and entering and propagating through the magnetosphere as compressional waves (Sakurai et al, 1999;Constantinescu et al, 2007;Heilig et al, 2007;Clausen et al, 2009).…”

Section: Introductionmentioning

confidence: 98%

ULF wave activity during the 2003 Halloween superstorm: multipoint observations from CHAMP, Cluster and Geotail missions

Balasis

Daglis

Zesta³

et al. 2012

Ann. Geophys.

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Abstract. We examine data from a topside ionosphere and two magnetospheric missions (CHAMP, Cluster and Geotail) for signatures of ultra low frequency (ULF) waves during the exceptional 2003 Halloween geospace magnetic storm, when Dst reached ∼ −380 nT. We use a suite of waveletbased algorithms, which are a subset of a tool that is being developed for the analysis of multi-instrument multi-satellite and ground-based observations to identify ULF waves and investigate their properties. Starting from the region of topside ionosphere, we first present three clear and strong signatures of Pc3 ULF wave activity (frequency 15-100 mHz) in CHAMP tracks. We then expand these three time intervals for purposes of comparison between CHAMP, Cluster and Geotail Pc3 observations but also to be able to search for Pc4-5 wave signatures (frequency 1-10 mHz) into Cluster and Geotail measurements in order to have a more complete picture of the ULF wave occurrence during the storm. Due to the fast motion through field lines in a low Earth orbit (LEO) we are able to reliably detect Pc3 (but not Pc4-5) waves from CHAMP. This is the first time, to our knowledge, that ULF wave observations from a topside ionosphere mission are compared to ULF wave observations from magnetospheric missions. Our study provides evidence for the occurrence of a number of prominent ULF wave events in the Pc3 and Pc4-5 bands during the storm and offers a platform to study the wave evolution from high altitudes to LEO. The ULF wave analysis methods presented here can be applied to observations from the upcoming Swarm multi-satellite mission of ESA, which is anticipated to enable joint studies with the Cluster mission.

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Low frequency wave sources in the outer magnetosphere, magnetosheath, and near Earth solar wind

Cited by 25 publications

References 27 publications

Magnetosheath plasma structures and their relation to foreshock processes

Magnetosheath plasma structures and their relation to foreshock processes

Statistical analysis of ground based magnetic field measurements with the field line resonance detector

ULF wave activity during the 2003 Halloween superstorm: multipoint observations from CHAMP, Cluster and Geotail missions

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