Wind was designed and manufactured by Martin Marietta Astro Space Division in East Windsor Township, New Jersey.

The SWE and 3DP experiments are meant to measure/analyze the lower energy (below 10 MeV) solar wind protons and electrons.

The WAVES and MFI experiments were designed to measure the electric and magnetic fields observed in the solar wind.

The Wind WAVES instrument also detects magnetic fields using three orthogonal search coil magnetometers (designed and built by the University of Iowa).

Electric (and magnetic) field waveform captures can be obtained from the Time Domain Sampler (TDS) receiver.

One should note that observation of the plasma line requires the dipole antenna to be longer than the local Debye length, λDe.

The instrument also has top-hat symmetrical spherical section electrostatic analyzers (ES) with microchannel plate detectors (MCPs) are used to measure ions and electrons from ~3 eV to 30 keV.

[9] The two types of detectors have energy resolutions ranging from ΔE/E ≈0.3 for the solid state telescopes (SST) and ΔE/E ≈ 0.2 for the top-hat ES analyzers.

The top-hat ES analyzers are composed of four separate detectors, each with different geometry factors to cover different ranges of energies.

One direction of the telescopes is covered in a thin lexan foil, ~1500 Angstrom (Å) of aluminum evaporated on each side to eliminate sunlight, (SST-Foil) where the thickness was chosen to stop protons up to the energy of electrons (~400 keV).

On the opposite side (SST-Open), a common broom magnet is used to refuse electrons below ~400 keV from entering but leaves the ions essentially unaffected.

Thus, if no higher energy particles penetrate the detector walls, the SST-Foil should only measure electrons and the SST-Open only ions.

[12] The Magnetic Field Instrument (MFI)[5] on board Wind is composed of dual triaxial fluxgate magnetometers.

[8] The SWE FCs can produce reduced ion distribution functions with up to 20 angular and 30 energy per charge bins every 92 seconds.

A circular aperture limits the effects of aberration near the modulator grid and defines the collecting area of the collector plates in each FC.

Since there are up to 30 energy bins for these detectors, a full reduced distribution function requires 30 rotations or slightly more than 90 seconds.

Notifications of astrophysical transients are sent worldwide instantly from KONUS, and are of importance in the subsequent positioning of telescopes everywhere.

The SWICS "stop" microchannel plate detector (MCP) experienced a failure resulting in reduced capabilities for this instrument and was eventually turned off in May 2000.

In 2010, MASS experienced a small degradation in the acceleration/deceleration power supply which reduced the efficiency of the instrument, though this does not seriously affect science data analysis.

For a complete list of refereed publications directly or indirectly using data from the Wind spacecraft, see https://wind.nasa.gov/bibliographies.php.