Publications (20)3.61 Total impact
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Article: Highly periodic stormtime activations observed by THEMIS prior to substorm onset
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ABSTRACT: On March 24, 2007 THEMIS observed near the dusk flank several 10 minute quasi-periodic flow and magnetic field oscillations followed by the onset of a strong substorm (AL ~ -1000 nT). The substorm occurred during an interval of strongly southward IMF, near the start of the recovery phase of a small storm (SYM-H near -80 nT). Each magnetic oscillation was accompanied by a rapid flow variation, auroral intensification, energetic particle injection, and Pi2 pulsations. For several hours both prior to and following the substorm THEMIS observed highly periodic flow oscillations, with the same 10 minute periodicity. The average of these flow oscillations was non-zero and positive, indicating net sunward transport. We suggest that the long interval of oscillatory flow constituted a periodic convective mode of the magnetosphere, and further suggest that the quasi-periodic activations were associated with reconnection near the THEMIS location.Geophysical Research Letters - GEOPHYS RES LETT. 01/2008; 35(17). -
Article: Case studies of the dynamics of ionospheric ions in the Earth's magnetotail
Journal of Geophysical Research (Space Physics). 01/2004; 109:1212. -
Article: Cluster observations of the electric field structure of the reconnection region in the plasma sheet: an electrostatic nozzle
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ABSTRACT: Measurements from the Cluster spacecraft of electric fields, magnetic fields, and ions at distances of 18 Re in the geomagnetic tail are used to study the structure and dynamics of the reconnection region during a major geomagnetic storm on October 1, 2001. The paper focuses on the structure of the normal component of the electric field at the current sheet. Evidence is presented at "thin" current sheet crossings with widths of 1-2 c/ωpe for a +/- 60 mV/m symmetric bipolar electric field structure in the normal component of the electric field. The bipolar structure spatially coincides spatially with the bifurcated cross tail current sheet and reverses at the current sheet midplane with the vectors pointing towards the current sheet mid plane. The associated intE\cdotdl is ˜2 kV between the outer boundary of the current and the mid-plane. The data is consistent at these thin current sheet crossings with a picture in which the normal component of the electric field drives an E×B drift of the magnetized electrons which provides the cross tail current. Over these scales, 100 eV ions from the tail lobes should be largely un-magnetized and accelerated nearly ballistically through the 2 kV potential drop . A heuristic model is presented in which the normal component of the electric field spatially coincide with planar current sheet in an X line geometry forming a potential well creating a two dimensional "quasi-electrostatic nozzle". In this model, low energy ions accelerated into this nozzle gain a kinetic energy of ˜1/2 mV_A^2 (˜2 keV) and bounce several times between opposing walls. Each bounce converts ion velocity normal to the current sheet to that parallel to the x gse axis forming in ion jets with velocity ˜V_A flowing away from the separatrix region in a manner consistent with fluid pictures of reconnection. Measurements are also presented from thicker tail current sheet crossings (1000-2000 km˜1-2 c/ωpi) with normal components of the electric field of 5-20 mV/m and potential drops of 4-30 kV. It is expected that only higher energy ions are non- adiabatic in this portion of the current sheet structure. The bipolar electric field structure correlates with the magnetic field perturbations due to the Hall magnetic field perturbation. The associated Poynting flux provides a non-negligible contribution to the outgoing energy flux.03/2003; -1:13835. -
Article: Multi-spacecraft observations of the CPS and PSBL using the CIS instruments on CLUSTER
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ABSTRACT: We present multi-spacecraft observations of the Central Plasma Sheet (CPS) and the Plasma Sheet Boundary Layer (PSBL) as observed by the CIS-CODIF instrument on CLUSTER. During these passes the spacecraft have apogee (XGSE ~20 Re) in the midnight region. The CIS-CODIF instrument measured ion distribution functions of the major species, H+, He++, He+ and O+ over the energy range 20 eV - 40 keV. In this study we focus in the presence of earthward and tailward ion beams and flows in the CPS and PSBL where two types of ion populations were observed. Earthward ion flows at energies 1 keV - 10 keV and low energy (< ~100 eV) field aligned ions coming from the Earth with the O+ ions appearing predominately as field aligned tailward beams. The composition and directional information will be used to infer the source of the CPS and PSBL plasma. During the comissioning phase (September 2000) the spacecraft crossed the night side plasma sheet with a separation of ~600 km, while the current (September 2001) separation is ~2000 km. This bigger separation seems to be necessary (in contrast to the smaller separation) for the distinction between spatial and temporal structures.AGU Fall Meeting Abstracts. 11/2001; -1:0812. -
Article: FAST Observations of Lower Hybrid Waves in the Cusp Regions
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ABSTRACT: The Fast Auroral Snapshot (FAST) spacecraft has encountered the Earth's cusp regions on numerous occasions during its first few years of operations. Intense plasma waves are consistent features of these cusp encounters which are characterized by localized keV dispersed ion "Injections". Emissions observed near the lower hybrid frequency are frequently, though not always, observed in conjunction with the precipitating cusp ions. The waves are clearly electrostatic and often exhibit a bifuncation in frequency about the lower hybrid frequency. In some cases, numerous ion Bernstein waves are present, separated in frequency at harmonics near the local proton cyclotron frequency. An analysis of the measurements of the electric field components of the plasma waves gathered with FAST's spaced receivers (or interferometers) reveals their short wavelength characteristics. We examine several examples of such waves in detail in order to understand their growth mechanisms and to relate them with the cusp energetic particle populations.02/1999; -
Article: Acceleration Processes in the Cusp: Observations by the FAST Satellite
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ABSTRACT: The Fast Auroral Snapshot (FAST) spacecraft has encountered the Earth's cusp regions near its apogee of 4175 km on numerous occasions during its first two and half years of operations. The cusp encounters are identified by their signatures of keV dispersed ion injections of solar wind origin. The FAST instruments reveal a complex microphysics inherent to many, but not all, of the cusp regions encountered by the spacecraft, that often include upgoing ion beams within regions of downgoing electrons that may appear as series of inverted-V features with energies near a few hundred eV. In many instances, upgoing electron beams have also been observed. Intense (> 100 mV/m) spikey DC-coupled electric fields and plasma waves are common features of the cusp encounters which also provide evidence for the presence of such local acceleration processes. In some cases, the FAST data show clear modulation of the precipitating magnetosheath ions indicative that they are affected by local electric potentials, as evidenced by simultaneous electron acceleration within such intervals. Furthermore, the acceleration events are sometimes organized with an apparent cellular structure that suggest Alfv6n waves or other large scale phenomena are controlling the localized potentials. We examine several cusp encounters in detail in order to study the complex relation of the cusp energetic particle populations with the plasma waves and DC electric fields.02/1999; -
Article: Acceleration Processes in the Cusp -- Observations by the FAST Satellite
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ABSTRACT: The FAST spacecraft has encountered the Earth's cusp regions near its apogee of 4175 km on numerous occasions during its first two and half years of operations. The cusp encounters are identified by their signatures of keV dispersed ion injections of solar wind origin. The FAST instruments reveal a complex microphysics inherent to many, but not all, of the cusp regions encountered by the spacecraft, that often include upgoing ion beams within regions of downgoing electrons that may appear as series of inverted-V features with energies near a few hundred eV. In many instances, upgoing electron beams have also been observed. Intense (> 100 mV/m) spikey DC-coupled electric fields and plasma waves are common features of the cusp encounters which also provide evidence for the presence of such local acceleration processes. In some cases, the FAST data show clear modulation of the precipitating magnetosheath ions indicative that they are affected by local electric potentials, as evidenced by simultaneous electron acceleration within such intervals. Furthermore, the acceleration events are sometimes organized with an apparent cellular structure that suggest Alfven waves or other large scale phenomena are controlling the localized potentials. We examine several cusp encounters in detail in order to study the complex relation of the cusp energetic particle populations with the plasma waves and DC electric fields.02/1999; -
Article: FAST Observations of Acceleration Processes in the Cusp--Evidence for Parallel Electric Fields
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ABSTRACT: The existence of precipitating keV ions in the Earth's cusp originating at the magnetosheath provide unique means to test our understanding of particle acceleration and parallel electric fields in the lower altitude acceleration region. On numerous occasions, the FAST (The Fast Auroral Snapshot) spacecraft has encountered the Earth's cusp regions near its apogee of 4175 km which are characterized by their signatures of dispersed keV ion injections. The FAST instruments also reveal a complex microphysics inherent to many, but not all, of the cusp regions encountered by the spacecraft, that include upgoing ion beams and conics, inverted-V electrons, upgoing electron beams, and spikey DC-coupled electric fields and plasma waves. Detailed inspection of the FAST data often show clear modulation of the precipitating magnetosheath ions that indicate that they are affected by local electric potentials. For example, the magnetosheath ion precipitation is sometimes abruptly shut off precisely in regions where downgoing localized inverted-V electrons are observed. Such observations support the existence of a localized process, such as parallel electric fields, above the spacecraft which accelerate the electrons downward and consequently impede the precipitating ion precipitation. Other acceleration events in the cusp are sometimes organized with an apparent cellular structure that suggests Alfven waves or other large-scale phenomena are controlling the localized potentials. We examine several cusp encounters by the FAST satellite where the modulation of energetic session on acceleration particle populations reveals evidence of localized acceleration, most likely by parallel electric fields.02/1999; -
Article: Initial FAST observations of acceleration processes in the cusp
grl. 06/1998; 25:2037-2040. -
Article: Observations of the 3-D distribution of interplanetary electrons and ions from solar wind plasma to low energy cosmic rays
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ABSTRACT: The 3-D Plasma and Energetic Particle instrument on the GGS Wind spacecraft (launched November 1, 1994) is designed to make measurements of the full three-dimensional distribution of suprathermal electrons and ions from solar wind plasma to low energy cosmic rays, with high sensitivity, wide dynamic range, good energy and angular resolution, and high time resolution. Three pairs of double-ended telescopes, each with two or three closely sandwiched passivated ion implanted silicon detectors measure electrons and ions from approximately 20 keV to greater than or equal to 300 keV. Four top-hat symmetrical spherical section electrostatic analyzers with microchannel plate detectors, a large and a small geometric factor analyzer for electrons and a similar pair for ions, cover from approximately 3 eV to 30 keV. We present preliminary observations of the electron and ion distributions in the absence of obvious solar impulsive events and upstream particles. The quiet time electron energy spectrum shows a smooth approximately power law fall-off extending from the halo population at a few hundred eV to well above approximately 100 keV The quiet time ion energy spectrum also shows significant fluxes over this energy range. Detailed 3-D distributions and their temporal variations will be presented.07/1995; -
Article: A three-dimensional plasma and energetic particle investigation for the wind spacecraft
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ABSTRACT: This instrument is designed to make measurements of the full three-dimensional distribution of suprathermal electrons and ions from solar wind plasma to low energy cosmic rays, with high sensitivity, wide dynamic range, good energy and angular resolution, and high time resolution. The primary scientific goals are to explore the suprathermal particle population between the solar wind and low energy cosmic rays, to study particle accleration and transport and wave-particle interactions, and to monitor particle input to and output from the Earth's magnetosphere.Three arrays, each consisting of a pair of double-ended semi-conductor telescopes each with two or three closely sandwiched passivated ion implanted silicon detectors, measure electrons and ions above 20 keV. One side of each telescope is covered with a thin foil which absorbs ions below 400 keV, while on the other side the incoming 1 MeV) and ions (up to 11 MeV) are identified by the two double-ended telescopes which have a third detector. The telescopes provide energy resolution of E/E0.3 and angular resolution of 22.536, and full 4 steradian coverage in one spin (3 s).Top-hat symmetrical spherical section electrostatic analyzers with microchannel plate detectors are used to measure ions and electrons from 3 eV to 30 keV. All these analyzers have either 180 or 360 fields of view in a plane, E/E0.2, and angular resolution varying from 5.6 (near the ecliptic) to 22.5. Full 4 steradian coverage can be obtained in one-half or one spin. A large and a small geometric factor analyzer measure ions over the wide flux range from quiet-time suprathermal levels to intense solar wind fluxes. Similarly two analyzers are used to cover the wide range of electron fluxes. Moments of the electron and ion distributions are computed on board.In addition, a Fast Particle Correlator combines electron data from the high sensitivity electron analyzer with plasma wave data from the WAVE experiment (Bougeretet al., in this volume) to study wave-particle interactions on fast time scales. The large geometric factor electron analyzer has electrostatic deflectors to steer the field of view and follow the magnetic field to enhance the correlation measurements.Space Science Reviews 01/1995; 71(1):125-153. · 3.61 Impact Factor -
Chapter: Spatial and Temporal Cusp Structures Observed by Multiple Spacecraft and Ground Based Observations
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ABSTRACT: Downward precipitating ions in the cusp regularly exhibit sudden changes in ion energy distributions, forming distinctive structures that can be used to study the temporal/spatial nature of reconnection at the magnetopause. When observed simultaneously with the Polar, FAST, and Interball satellites, such cusp structures revealed remarkably similar features. These similar features could be observed for up to several hours during stable solar wind conditions. Their similarities led to the conclusion that large-scale cusp structures are spatial structures related to global ionospheric convection patterns created by magnetic merging and not the result of temporal variations in reconnection parameters. The launch of the Cluster fleet allows cusp structures to be studied in great detail and during changing solar wind conditions using three spacecraft with identical plasma and field instrumentation. In addition, Cluster cusp measurements are linked with ionospheric convection cells by combining the satellite observations with SuperDARN radar observations that are used to derive the convection patterns in the ionosphere. The combination of satellite observations with ground-based observations during variable solar wind conditions shows that large-scale cusp structures can be either spatial or temporal. Cusp structures can be described as spatial features observed by satellites crossing into spatially separated flux tubes. Cusp structures can also be observed as poleward-traveling (temporal) features within the same convection cell, most probably caused by variations in the reconnection rate at the magnetopause.01/1970: pages 281-305; -
Article: Evidence for impulsive solar wind plasma penetration through the dayside magnetopause
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ABSTRACT: This paper presents in situ observational evidence from the Cluster Ion Spectrometer (CIS) on Cluster of injected solar wind "plasma clouds" protruding into the day-side high-latitude magnetopause. The plasma clouds, presumably injected by a transient process through the day-side magnetopause, show characteristics implying a generation mechanism denoted impulsive penetration (Lemaire and Roth, 1978). The injected plasma clouds, hereafter termed "plasma transfer events", (PTEs), (Woch and Lundin, 1991), are temporal in nature and relatively limited in size. They are initially moving inward with a high velocity and a magnetic signature that makes them essentially indistinguishable from regular magnetosheath encounters. Once inside the magnetosphere, however, PTEs are more easily distinguished from magnetopause encounters. The PTEs may still be moving while embedded in an isotropic background of energetic trapped particles but, once inside the magnetosphere, they expand along magnetic field lines. However, they frequently have a significant transverse drift component as well. The drift is localised, thus constituting an excess momentum/motional emf generating electric fields and currents. The induced emf also acts locally, accelerating a pre-existing cold plasma (e.g. Sauvaud et al., 2001). Observations of PTE-signatures range from "active" (strong transverse flow, magnetic turbulence, electric current, local plasma acceleration) to "evanescent" (weak flow, weak current signature). PTEs appear to occur independently of Interplanetary Magnetic Field (IMF) Bz in the vicinity of the polar cusp region, which is consistent with observations of transient plasma injections observed with mid- and high-altitude satellites (e.g. Woch and Lundin, 1992; Stenuit et al., 2001). However the characteristics of PTEs in the magnetosphere boundary layer differ for southward and northward IMF. The Cluster data available up to now indicate that PTEs penetrate deeper into the magnetosphere for northward IMF than for southward IMF. This may or may not mark a difference in nature between PTEs observed for southward and northward IMF. Considering that flux transfer events (FTEs), (Russell and Elphic, 1979), are observed for southward IMF or when the IMF is oriented such that antiparallel merging may occur, it seems likely that PTEs observed for southward IMF are related to FTEs.01/2001; -
Article: Intermittent thermal plasma acceleration linked to sporadic motions of the magnetopause, first Cluster results
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ABSTRACT: This paper presents the first observations with Cluster of a very dense population of thermal ionospheric ions (H<sup>+</sup>, He<sup>+</sup>, O<sup>+</sup>) locally "accelerated" perpendicularly to the local magnetic field in a region adjacent to the magnetopause and on its magnetospheric side. The observation periods follow a long period of very weak magnetic activity. Recurrent motions of the magnetopause are, in the presented cases, unexpectedly associated with the appearance inside closed field lines of recurrent energy structures of ionospheric ions with energies in the 5 eV to ~1000 eV range. The heaviest ions were detected with the highest energies. Here, the ion behaviour is interpreted as resulting from local electric field enhancements/decreases which adiabatically enhance/lower the bulk energy of a local dense thermal ion population. This drift effect, which is directly linked to magnetopause motions caused by pressure changes, allows for the thermal ions to overcome the satellite potential and be detected by the suprathermal CIS Cluster experiment. When fast flowing, i.e. when detectable, the density (~ 1 cm<sup>-3</sup>) of these ions from a terrestrial origin is (in the cases presented here) largely higher than the local density of ions from magnetospheric/plasma sheet origin which poses again the question of the relative importance of solar and ionospheric sources for the magnetospheric plasma even during very quiet magnetic conditions.01/2001; -
Article: Cusp structures: combining multi-spacecraft observations with ground-based observations
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ABSTRACT: Recent simultaneous observations of cusp structures with Polar, FAST and Interball revealed remarkably similar features at spacecraft crossing the cusp. Such stable cusp structures could be observed up to several hours only during stable solar wind conditions. Their similarities led to the conclusion that for such conditions large-scale cusp structures are spatial structures related to a global ionospheric convection pattern and not the result of temporal variations in reconnection parameters. With the launch of the Cluster fleet we are now able to observe precipitating ion structures in the cusp with three spacecraft and identical instrumentation. The orbit configuration of the Cluster spacecraft allows for delay times between spacecraft of about 45 min in crossing the cusp. The compact configuration of three spacecraft at about the same altitude allows for the analysis of cusp structures in great de-tail and during changing solar wind conditions. Cluster observations on 25 July 2001 are combined with SuperDARN radar observations that are used to derive a convection pattern in the ionosphere. We found that large-scale cusp structures for this Cluster cusp crossing are in agreement with structures in the convection pattern and conclude that major cusp structures can be consistent with a spatial phenomenon. -
Article: Cluster observations of the high-latitude magnetopause and cusp: initial results from the CIS ion instruments
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ABSTRACT: Launched on an elliptical high inclination orbit (apogee: 19.6 R<sub>E</sub> ) since January 2001 the Cluster satellites have been conducting the first detailed three-dimensional studies of the high-latitude dayside magnetosphere, including the exterior cusp, neighbouring boundary layers and magnetopause regions. Cluster satellites carry the CIS ion spectrometers that provide high-precision, 3D distributions of low-energy (<35 keV/e) ions every 4 s. This paper presents the first two observations of the cusp and/or magnetopause behaviour made under different interplanetary magnetic field (IMF) conditions. Flow directions, 3D distribution functions, density profiles and ion composition profiles are analyzed to demonstrate the high variability of high-latitude regions. In the first crossing analyzed (26 January 2001, dusk side, IMF-BZ < 0), multiple, isolated boundary layer, magnetopause and magnetosheath encounters clearly occurred on a quasi-steady basis for ~ 2 hours. CIS ion instruments show systematic accelerated flows in the current layer and adjacent boundary layers on the Earthward side of the magnetopause. Multi-point analysis of the magnetopause, combining magnetic and plasma data from the four Cluster spacecraft, demonstrates that oscillatory outward-inward motions occur with a normal speed of the order of ± 40 km/s; the thickness of the high-latitude current layer is evaluated to be of the order of 900–1000 km. Alfvénic accelerated flows and D-shaped distributions are convincing signatures of a magnetic reconnection occurring equatorward of the Cluster satellites. Moreover, the internal magnetic and plasma structure of a flux transfer event (FTE) is analyzed in detail; its size along the magnetopause surface is ~ 12 000 km and it convects with a velocity of ~ 200 km/s. The second event analyzed (2 February 2001) corresponds to the first Cluster pass within the cusp when the IMF-BZ component was northward directed. The analysis of relevant CIS plasma data shows temporal cusp structures displaying a reverse energy-latitude "saw tooth" dispersion, typical for a bursty reconnection between the IMF and the lobe field lines. The observation of D-shaped distributions indicates that the Cluster satellites were located just a few R<sub>E</sub> from the reconnection site. -
Article: Alfven wave produced auroras, dynamic signatures of magnetospheric boundaries
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ABSTRACT: A survey of substorm observations with IMAGE FUV and FAST satellite in situ data provided many cases in which the onset events occurred in the proximity of the FAST particle and field measurements. The IMAGE FUV experiment took a 10 second duration exposure every two minutes and the substorm onset was determined with this timing accuracy. The time when FAST observed the largest electron fluxes was used to determine the observation time phase related to onset. In the FAST satellite data, Alfven wave produced aurora can be recognized by the dominance of intense fluxes of magnetic field-aligned electrons having a broad, structured energy spectrum and accompanying intense wave activity. These events can be distinguished from "inverted V" auroras produced by quasi-static field aligned electric fields from their characteristic mono- energetic spectral signature. The Alfven wave accelerated electron auroras are produced by converting high intensity wave energy (Poynting) fluxes into electron energy and therefore these auroras can be regarded as the footprints of regions where large amplitude Alfven waves are produced by magnetic reconfigurations. During the substorm expansion phase Alfven wave accelerated electrons occur at the poleward boundary of the expanding substorm surge, while equatorward of the surge there is a broader region of electron precipitation with embedded strong quasi-static "inverted V" electric fields. This is consistent with wave signatures of dipolarization and the motion of a magnetospheric boundary. Ion conics and intense ion outflow is often seen in the region of Alfvenic auroras. Nearer to the onset time, Alfvenic aurora is seen deep within the auroral oval near the point of the initial brightening. This is consistent with prior observations that the most equatorward arc breaks up first at substorm onset. In all cases the Alfven wave accelerated auroras, unlike inverted V-s, do not appear to carry strong net field aligned return currents from the ionosphere into the magnetosphere. -
Article: Simultaneous Cluster and IMAGE observations of cusp reconnection and auroral proton spot for northward IMF
Geophysical Research Letters, v.30 (2003). -
Article: Investigation of the source region of ionospheric oxygen outflow in the cleft/cusp using multi-spacecraft observations by CIS onboard Cluster
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ABSTRACT: Beams of singly ionized oxygen with narrow energy distributions originating in the dayside cleft/cusp region are frequently observed in the cleft, cusp and polar cap regions by the CODIF sensor of the CIS instrument onboard Cluster. During summer and fall of 2001, the high separation distances of ∼1Re between the spacecraft provided a good opportunity to estimate the size and location of the source of outgoing O+ ions. A statistical study shows that the source region is located near the equatorward edge of the cleft/cusp region, within a latitudinal range of around 1.5°. The longitudinal extension cannot be resolved, except that it is more than the satellite separations that was 14° in average. Cluster observations inside the source region, at 4.5–6Re, show high transverse heating of the O+ population. This process is accompanied with a sudden enhancement of low-frequency electric field waves measured by the EFW and STAFF instruments. We suggest that O+ ion outflow is caused by resonant heating by BBELF waves.Advances in Space Research. -
Article: Cluster Survey of the Occurrence of Reconnection Tailward of the Cusp and its IMF Dependence: Implications for Component and Anti-Parallel Merging
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ABSTRACT: We have surveyed the occurrence of earthward directed reconnection jets at the poleward edge of the cusp detected by Cluster as a function of the interplanetary magnetic field (IMF) clock angle. The survey covers 3 years (2001-2003) of cusp and magnetopause crossings and is restricted to periods of relatively stable IMF. Our survey indicates that these jets occur only when the IMF clock angle is within ~ 90 degrees of the GSM +z direction. This finding at first seems inconsistent with the component merging model which should allow reconnection to occur for large than 90 degrees clock angle (or less than 90 degrees in magnetic shear angle). However, it is possible that this is a geophysical rather than a physical effect. When the IMF has a southward component, reconnection equatorward of the cusp could prevent the formation of a plasma depletion layer adjacent to the low- and high-latitude magnetopause, resulting in super-Alfvenic magnetosheath flows next to the high-latitude magnetopause. No accelerated reconnecton jets can be detected sunward of the X-line in this regime. On the other hand, our survey also found that the dawn-dusk location of reconnection jet detection is independent of the IMF By which seems inconsistent with anti-parallel merging.35:876.
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1–1970
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University of California, Berkeley
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