A three-dimensional plasma and energetic particle investigation for the wind spacecraft

Lin, R. P.; Anderson, K. A.; Ashford, S.; Carlson, C. W.; Curtis, D. W.; Ergun, R.; Larson, D. E.; McFadden, J. P.; McCarthy, Michael; Parks, G. K.; Rème, H.; Bosqued, J. M.; Coutelier, J.; Cotin, F.; d’Uston, C.; Wenzel, K.‐P.; Sanderson, T. R.; Henrion, J.; Ronnet, J. C.; Paschmann, G.

doi:10.1007/bf00751328

Cited by 797 publications

(579 citation statements)

References 22 publications

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“…The onboard 3DP instrument provides the full three-dimensional measurements of electrons from solar wind thermal plasma to ∼400 keV (Lin et al 1995). Silicon semiconductor telescopes (SST) measure ∼20-400 keV electrons with energy channel resolution of D = E E 0.3, while electron electrostatic analyzers (EESA-L and EESA-H) measure ∼3 eV-30 keV electrons with energy resolution of D = E E 0.2.…”

Section: Resultsmentioning

confidence: 99%

QUIET-TIME SUPRATHERMAL (∼0.1–1.5 keV) ELECTRONS IN THE SOLAR WIND

Tao

Wang

Zong

et al. 2016

ApJ

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We present a statistical survey of the energy spectrum of solar wind suprathermal (∼0.1-1.5 keV) electrons measured by the WIND3DP instrument at 1 AU during quiet times at the minimum and maximum of solar cycles 23 and 24. After separating (beaming) strahl electrons from (isotropic) halo electrons according to their different behaviors in the angular distribution, we fit the observed energy spectrum of both strahl and halo electrons at ∼0.1-1.5 keV to a Kappa distribution function with an index κ and effective temperature T eff . We also calculate the number density n and average energy E avg of strahl and halo electrons by integrating the electron measurements between ∼0.1 and 1.5 keV. We find a strong positive correlation between κ and T eff for both strahl and halo electrons, and a strong positive correlation between the strahl n and halo n, likely reflecting the nature of the generation of these suprathermal electrons. In both solar cycles, κ is larger at solar minimum than at solar maximum for both strahl and halo electrons. The halo κ is generally smaller than the strahl κ (except during the solar minimum of cycle 23). The strahl n is larger at solar maximum, but the halo n shows no difference between solar minimum and maximum. Both the strahl n and halo n have no clear association with the solar wind core population, but the density ratio between the strahl and halo roughly anti-correlates (correlates) with the solar wind density (velocity).

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Section: Resultsmentioning

confidence: 99%

QUIET-TIME SUPRATHERMAL (∼0.1–1.5 keV) ELECTRONS IN THE SOLAR WIND

Tao

Wang

Zong

et al. 2016

ApJ

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“…[10] We obtained full 4p steradian low energy (<30 keV) electron and ion distributions from the Wind/3DP EESA and PESA particle detectors [Lin et al, 1995]. Both EESA Low and PESA High can return full 4p steradian distribution functions once every spin period (~3 s) in burst mode.…”

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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“…[6] The present study uses Wind plasma data obtained by the 3DP instrument [Lin et al, 1995] with a temporal resolution of 49s except during one magnetopause crossing (20:29:56 -20:35:55 UT) when 3s resolution data (collected in the burst memory mode) were available. Geotail plasma data are taken from the Low Energy Particle instrument [Mukai et al, 1994] (also at 3 s resolution) for the magnetosphere and magnetopause intervals, and from the Comprehensive Plasma Instrument [Frank, 1994] (at 20 s resolution) for the magnetosheath intervals adjacent to the magnetopause.…”

Section: Orbit and Instrumentationsmentioning

confidence: 99%

Simultaneous Geotail and Wind observations of reconnection at the subsolar and tail flank magnetopause

Phan¹,

Hasegawa²,

Fujimoto³

et al. 2006

Geophysical Research Letters

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[1] We report a fortuitous two-spacecraft conjunction when Geotail and Wind observed the occurrence of reconnection simultaneously at the subsolar and dawn tail flank magnetopause during stable B y dominated IMF. Furthermore, bi-directional jets were observed by Geotail which indicate the presence of an X-line in the subsolar region. These observations are consistent with the presence of a tilted X-line hinged near the subsolar point and spanning the entire dayside (from subsolar to X GSE = À10 R E ) magnetopause, as expected from component reconnection. In addition, our observations do not reveal any thickening of the boundary layer down the flanks, the plasma boundary layer being confined to the reconnecting magnetopause current layer. This suggests that reconnection dominates over diffusive entry or Kelvin-Helmholtz instability at the low latitude magnetopause even when the IMF clock angle is 90°. Citation: Phan, T.

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A three-dimensional plasma and energetic particle investigation for the wind spacecraft

Cited by 797 publications

References 22 publications

QUIET-TIME SUPRATHERMAL (∼0.1–1.5 keV) ELECTRONS IN THE SOLAR WIND

QUIET-TIME SUPRATHERMAL (∼0.1–1.5 keV) ELECTRONS IN THE SOLAR WIND

Electromagnetic waves and electron anisotropies downstream of supercritical interplanetary shocks

Simultaneous Geotail and Wind observations of reconnection at the subsolar and tail flank magnetopause

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