SWE, a comprehensive plasma instrument for the WIND spacecraft

Ogilvie, K. W.; Chornay, D.; Fritzenreiter, R. J.; Hunsaker, F.; Keller, John W.; Lobell, J.; Miller, G.; Scudder, J. D.; Sittler, E. C.; Torbert, R. B.; Bodet, D.; Needell, G.; Lazarus, A. J.; Steinberg, J. T.; Tappan, J. H.; Mavretic, Anton; Gergin, E.

doi:10.1007/bf00751326

Cited by 1,200 publications

(869 citation statements)

References 8 publications

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“…[9] In addition to Polar ion data, solar wind context measurements observed by the Wind Magnetic Field Instrument (MFI) [Lepping et al, 1995] and the Wind Solar Wind Experiment (SWE) [Ogilvie et al, 1995] are used. These data are provided by the International Solar-Terrestrial Physics key parameter Web page.…”

Section: Instrumentation and Methodsologymentioning

confidence: 99%

Probing the boundary between antiparallel and component reconnection during southward interplanetary magnetic field conditions

et al. 2007

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[1] One of the major outstanding questions about magnetic reconnection is where reconnection will occur at the Earth's magnetopause for specific conditions of the solar wind and the interplanetary magnetic field (IMF). There are two scenarios discussed in the literature: (1) antiparallel reconnection, which occurs where the magnetospheric magnetic field and the IMF are antiparallel (shear angle of approximately 180°) and (2) component reconnection, where shear angles between the magnetospheric field and the IMF as low as 50°have been reported. The distinction between the two reconnection scenarios is important for the energy and momentum transfer from the solar wind to the magnetosphere. Here we report on a method using three-dimensional plasma observations from the Toroidal Imaging Mass-Angle Spectrograph instrument on the Polar spacecraft as it passes through the northern magnetospheric cusp to calculate the distance to the reconnection line and subsequently trace the distance along model magnetic field lines back to the magnetopause. Results from 130 events reveal that in general, magnetic reconnection occurs along an extended line across the dayside magnetopause (i.e., consistent with the component reconnection scenario). During strong sunward or antisunward IMF conditions (B X ), however, the reconnection location resembles the antiparallel reconnection model at high latitudes and does not cross the dayside magnetopause as a single tilted reconnection line. These results show that either reconnection scenario can occur at the magnetopause, depending on the specific IMF conditions. Citation: Trattner, K. J., J. S. Mulcock, S. M. Petrinec, and S. A. Fuselier (2007), Probing the boundary between antiparallel and component reconnection during southward interplanetary magnetic field conditions,

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Section: Instrumentation and Methodsologymentioning

confidence: 99%

Probing the boundary between antiparallel and component reconnection during southward interplanetary magnetic field conditions

et al. 2007

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“…[12] Supplemental ion distributions were calculated from the two Faraday Cup (FC) ion instruments from the Wind SWE experiment [Ogilvie et al, 1995]. The SWE FCs can produce reduced ion distribution functions with up to 20 angular and 30 energy per charge bins every 92 s over an energy range of~150 eV to~8 keV (~1200 km/s proton) [Kasper et al, 2006].…”

Section: Data Sets and Analysismentioning

confidence: 99%

Electromagnetic waves and electron anisotropies downstream of supercritical interplanetary shocks

et al. 2013

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[1] We present waveform observations of electromagnetic lower hybrid and whistler waves with f ci ≪ f < f ce downstream of four supercritical interplanetary shocks using the Wind search coil magnetometer. The whistler waves were observed to have a weak positive correlation between dB and normalized heat flux magnitude and an inverse correlation with T eh /T ec . All were observed simultaneous with electron distributions satisfying the whistler heat flux instability threshold and most with T ⊥ h /T k h > 1.01. Thus, the whistler mode waves appear to be driven by a heat flux instability and cause perpendicular heating of the halo electrons. The lower hybrid waves show a much weaker correlation between dB and normalized heat flux magnitude and are often observed near magnetic field gradients. A third type of event shows fluctuations consistent with a mixture of both lower hybrid and whistler mode waves. These results suggest that whistler waves may indeed be regulating the electron heat flux and the halo temperature anisotropy, which is important for theories and simulations of electron distribution evolution from the Sun to the Earth.

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“…[9] Interplanetary conditions measured by the Wind spacecraft (the Solar Wind Plasma Experiment (SWE) [Ogilvie et al, 1995] and the Magnetic Field Investigation (MFI) ) at a solar ecliptic location (X = 87, Y = À7, Z = À3 R E ) are displayed in Figure 2. The clock angle, CA, is defined such that 0°is northward, plus or minus 180°is southward, and plus and minus 90°a re equatorial in the positive and negative Y direction, respectively.…”

Section: Spacecraft Position and Interplanetary Conditionsmentioning

confidence: 99%

Waves on the dusk flank boundary layer during very northward interplanetary magnetic field conditions: Observations and simulation

et al. 2007

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[1] The Geotail spacecraft made an inbound passage perpendicular to the dusk equatorial magnetopause on 1 August 1998 when the interplanetary magnetic field had been very northward for more than 10 hours. As the spacecraft moved through the low-latitude boundary layer, it detected waves with $3 min period that caused transitions between cool dense magnetosheath plasma and mixed magnetosheath and magnetosphere plasmas. A region of highly fluctuating magnetic fields with variations up to 50 nT/s was observed on leaving the magnetosheath plasma but not on its return to this region. This observation suggests that the boundary region is not laminar but more likely consists of KelvinHelmholtz vortices. Such fluctuations are probably caused by twisting of the field by the vortices, and they could be important in transporting plasma to the magnetosphere where densities of 5/cc were observed. A global MHD simulation of the event reproduced the observed low-frequency waves, their counterclockwise polarization, and a region of high-velocity magnetosheath flow outside the magnetopause. This flow was associated with a decreased density and increased field strength which are characteristics of a plasma depletion layer. When Geotail moved further inward into the magnetosphere, it detected waves that are probably the magnetotail vortices which had been detected earlier by the ISEE spacecraft.

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SWE, a comprehensive plasma instrument for the WIND spacecraft

Cited by 1,200 publications

References 8 publications

Probing the boundary between antiparallel and component reconnection during southward interplanetary magnetic field conditions

Probing the boundary between antiparallel and component reconnection during southward interplanetary magnetic field conditions

Electromagnetic waves and electron anisotropies downstream of supercritical interplanetary shocks

Waves on the dusk flank boundary layer during very northward interplanetary magnetic field conditions: Observations and simulation

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