The WIND magnetic field investigation

Lepping, R. P.; Acuña, M. H.; Burlaga, L. F.; Farrell, W. M.; Slavin, J. A.; Schatten, Kenneth H.; Mariani, F.; Ness, N. F.; Neubauer, F. M.; Whang, Y. C.; Byrnes, J.; Kennon, R. S.; Panetta, Peter V.; Scheifele, J. L.; Worley, E. M.

doi:10.1007/bf00751330

Cited by 1,384 publications

(985 citation statements)

References 34 publications

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“…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. The three-dimensional electron data from 3DP are binned into eight PA bins with a 22°.5 angular resolution (Wang 2009), according to the IMF direction measured by the WINDMFI instrument (Lepping et al 1995). In this study, we use the EESA (EESA-L and EESA-H) electron measurements to survey the suprathermal electrons in the solar wind during quiet times at the minimum April to 1997August, 2006June to 2010 and maximum (1999June to 2000July, 2011 June to 2014 January) of solar cycles 23 and 24, after correction for the spacecraft potential (Salem et al 2001; although the spacecraft potential has a very small effect on the electron measurements at 0.1-1.5 keV).…”

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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“…[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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“…For more details about the WAVES instrument, see Bougeret et al [1995], and for analysis, see Wilson III et al [2010]. High time resolution magnetic field data were obtained from the dual triaxial fluxgate magnetometers [Lepping et al, 1995]. The time resolution is~0.092 s or~11 samples/s.…”

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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The WIND magnetic field investigation

Cited by 1,384 publications

References 34 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

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

Electromagnetic waves and electron anisotropies downstream of supercritical interplanetary shocks

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