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STEREO-A In-Situ Measurements of Particles and CME Transients from the Magnetometer and the Plasma and Suprathermal Ion and Composition Instruments (IMPACT/MAG, PLASTIC) Solar Wind Plasma Data

STEREO-A In-situ Measurements of Particles and CME Transients, IMPACT, Magnetometer Instrument, MAG, Magnetic Field Vector and PLAsma and SupraThermal Ion Composition, PLASTIC, Solar Wind Parameter, Level 2, Data

Wind 3DP Solar Wind Plasma Corrected Electron Moments (EMFITS), 100 s Data

These Electron Parameters are Moments of Wind 3DP EESA-L and EESA-H Measurements, corrected for Spacecraft Potential and other Instrumental Effects. More Information can be found at: R. P. Lin et al., A Three-Dimensional Plasma and Energetic Particle Investigation for the Wind Spacecraft, Space Science Reviews, 71, 125-153, 1995. C. S. Salem et al., Precision Electron Measurements in the Solar Wind at 1 AU from NASA's Wind Spacecraft, J. Geophys. Res. Space Physics, 2017. M. Pulupa et al., Spin-Modulated Spacecraft Floating Potential: Observations and Effects on Electron Moments, J. Geophys. Res. Space Physics, 119, 647-657, doi:10.1002/2013JA019359, 2014.

ACE Solar Wind Electron, Proton, and Alpha Monitor (SWEPAM), Key Parameter, K1, Preliminary Browse Data

ACE Solar Wind Electron Proton Alpha Monitor (SWEPAM), Key Parameter, K1, Browse Data is designed for monitoring large scale particle and field behavior and for selecting interesting time periods. The data is automatically generated from the spacecraft data stream using simple algorithms provided by the instrument teams. It is not routinely checked for accuracy and is subject to revision. Use this data at your own risk, and consult with the appropriate instrument teams about citing it. SWEPAM browse data is not validated by the experimenters and should not be used except for preliminary examination prior to detailed Studies. See: https://izw1.caltech.edu/ACE/.

ISEE 1 Fast Plasma Experiment Solar Wind Weimer Propagated 60 s Resolution Data in GSM Coordinates

ISEE-1 Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution FPE data in GSM coordinates. This data set consists of propagated solar wind data that has first been propagated to a position just outside of the nominal bow shock (about 17, 0, 0 Re) and then linearly interpolated to 1 min resolution using the interp1.m function in MATLAB. The input data for this data set is a 1 min resolution processed solar wind data constructed by Dr. J.M. Weygand. The method of propagation is similar to the minimum variance technique and is outlined in Dan Weimer et al. [2003; 2004]. The basic method is to find the minimum variance direction of the magnetic field in the plane orthogonal to the mean magnetic field direction. This minimum variance direction is then dotted with the difference between final position vector minus the original position vector and the quantity is divided by the minimum variance dotted with the solar wind velocity vector, which gives the propagation time. This method does not work well for shocks and minimum variance directions with tilts greater than 70 degrees of the sun-earth line. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies References: Weimer, D. R. (2004), Correction to ‘‘Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique,’’ J. Geophys. Res., 109, A12104, doi:10.1029/2004JA010691. Weimer, D.R., D.M. Ober, N.C. Maynard, M.R. Collier, D.J. McComas, N.F. Ness, C. W. Smith, and J. Watermann (2003), Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique, J. Geophys. Res., 108, 1026, doi:10.1029/2002JA009405.

Wind 3DP PESA Moments Data

Wind 3DP proton and ion onboard calculated moments from the PESA instrument. Calibrated science quality data.

Wind Energetic Particle Acceleration Composition Transport (EPACT) SupraThermal Energetic Particle Telescope (STEP) Differential, Directional Carbon, Nitrogen, and Oxygen Fluxes, 10 min Data

The EPACT Instrument on Wind STEP - SupraThermal Energetic Particle Telescope measures Ion Fluxes of Protons (H) in 0.12.5 MeV Energy Range and He-Fe Nuclei in the ~0.032 MeV/nucleon Energy Ranges in two identical Telescopes, each with a Geometrical Factor of 0.4 cm^2 sr and a rectangular Field of View with an Angular Acceptance of 44° in Azimuth and 17° in Polar Angle.

Wind SMS Key Parameter 4-hour Data

Combined SWICS and STICS data containing 4 hour averaged alpha particle velocity, C/O abundance ratio, and carbon and oxygen ionization temperatures. Time is for the start of the averaging interval. Computed are the average alpha velocity, average C/O abundance ratio, average carbon ionization temperature (in million degs K) from C6 and C5 (using the tables of Arnaud and Rothenflug, 1985), the average oxygen ionization temperature from O7 and O6 (in million degs K, using tables of Arnaud and Rothenflug, 1985). These averages are made over 4 hours. He velocity and He kinetic temperature are computed every 3 minutes and are contained in the K1 CDF. References: Space Science Reviews 71:79-124, 1995, Kluwer Academic Publishers, Belgium Instrument consist of: Solar Wind Ion Composition Spectrometer (SWICS); high resolution mass spectrometer (MASS); Supra-Thermal Ion Composition Spectrometer (STICS) and common DPU

ACE Solar Wind Electron Proton Alpha Monitor (SWEPAM) Suprathermal Electron Pitch Angle 128-Second Level 3 Data

Suprathermal Electron Pitch Angle data from ACE/SWEPAM. Level 3 data, 128-second averages. These pitch angle distributions are calculated automatically by a computer code, and have not been validated by a person. It is therefore likely that they include some artifacts and erroneous values. These data files contain suprathermal electron pitch angle distribution functions (s^3 cm^-6) at 272 eV from the ACE/SWEPAM-E instrument. The energy channel is ~12% wide, centered at 272 eV. Pitch angle bins are 9 degrees wide, and run from 0 to 180 degrees (so 0-9, 9-18, 18-27 degrees, etc.). The break between the core and suprathermal electrons is generally around 70 eV at 1 AU, but varies around this value, at times exceeding 100 eV. Electrons at 272 eV are generally well within the suprathermal range, and the distribution at this energy typically shows very little contribution from the core population. The measured count rates at 272 eV energy provide excellent statistical significance. In addition, because of the high count rates, very few artifacts (for example due to sunlight contamination) are seen in the data at this energy. The data are in the solar wind frame, and have been corrected for the spacecraft potential. The spacecraft potential determination requires measurement of the lower energy electrons, and so the potentials calcuated at these times have been interpolated to the times of the suprathermal electron measurements. Transformation to the solar wind frame requires interpolation of the measurements (each at a different energy in the solar wind frame) to the desired energy (272 eV). Also note that the detector gains on the SWEPAM-E instrument change over time, including both slowly decreasing gains and abrupt increases when the instrument voltages are increased. The use of these data for long-term studies of the distribution function amplitudes is therefore strongly discouraged.

Apollo 15 Solar Wind Measurements at the Lunar Surface 1-HR Data

This data set contains hourly averaged plasma parameters from the Apollo 15 Solar Wind Spectrometer. Four sets of hourly averaged parameters are computed, using as input data -- (1) all fine-time scale parameters (FTSP), (2) all FTSP computed from spectra with small rms error on curve fitting and thermal speeds less than one-half the bulk velocity, (3) all FTSP computed from spectra that satisfy the requirements of criterion 2 as well as having only one flow angle that can be directly measured, and (4) all FTSP computed from spectra that satisfy the requirements of criterion 2 as well as having both flow angles directly measureable. Contained in each of the 4 sets of averages are the proton density, alpha-to-proton ratio, bulk speed, angle of flow, number of spectra, and rms deviations of each average.

Wind Energetic Particle Acceleration Composition Transport (EPACT) SupraThermal Energetic Particle Telescope (STEP) Differential, Directional Helium Fluxes, 10 min Data

ACE SWICS 2.0 Solar Wind 2-Hour Data

The SWICS 2.0 dataset consists of time series measurements by ACE/SWICS of the elemental abundance, charge state composition, and kinetic distribution of heavy ions in the solar wind. This data set begins after August 23, 2011, when a radiation and age-induced hardware anomaly altered the instrument's operational state. It should not be confused with SWICS 1.1, the recalibrated data set extending from launch up to the anomaly. SWICS 2.0 continues to make heavy ion measurements which are not available from any other instrument, and new data analysis methods have been developed to address the statistical and calibration issues of the current instrument state.

IMP-8 PLS Solar Wind Weimer Propagated 60 s Resolution Data in GSM Coordinates

IMP-8 PLS Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution data in GSM coordinates. This data set consists of propagated solar wind data that has first been propagated to a position just outside of the nominal bow shock (about 17, 0, 0 Re) and then linearly interpolated to 1 min resolution using the interp1.m function in MATLAB. The input data for this data set is a 1 min resolution processed solar wind data constructed by Dr. J.M. Weygand. The method of propagation is similar to the minimum variance technique and is outlined in Dan Weimer et al. [2003; 2004]. The basic method is to find the minimum variance direction of the magnetic field in the plane orthogonal to the mean magnetic field direction. This minimum variance direction is then dotted with the difference between final position vector minus the original position vector and the quantity is divided by the minimum variance dotted with the solar wind velocity vector, which gives the propagation time. This method does not work well for shocks and minimum variance directions with tilts greater than 70 degrees of the sun-earth line. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies References: Weimer, D. R. (2004), Correction to ‘‘Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique,’’ J. Geophys. Res., 109, A12104, doi:10.1029/2004JA010691. Weimer, D.R., D.M. Ober, N.C. Maynard, M.R. Collier, D.J. McComas, N.F. Ness, C. W. Smith, and J. Watermann (2003), Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique, J. Geophys. Res., 108, 1026, doi:10.1029/2002JA009405.

Wind 3DP 92-sec Key Parameter Data

Wind 3DP (3-D Plasma Analyzer), 92-s key parameters, ion and electron fluxes (at 7 energy steps), flow velocities, densities and temperatures

DE 2 Fabry-Perot Interferometer (FPI), Thermospheric Neutral Gas Density, Meridional Wind, and Temperature, 8-sec data

The Fabry-Perot Interferometer, FPI, was a High-Resolution Remote Sensing Instrument designed to measure the Thermospheric Temperature, Meridional Wind, and Density of the following Metastable Atoms: Atomic Oxygen, Singlet S and D, and the 2P State of Ionic Atomic Oxygen. The FPI performed a Wavelength Analysis on the Light detected from the Thermospheric Emission Features by spatially scanning the Interference Fringe Plane with a Multichannel Array Detector. The Wavelength Analysis characterized the Doppler Line Profile of the emitting Species. A Sequential Altitude Scan performed by a Commandable Horizon Scan Mirror provided a Cross-Sectional View of the Thermodynamic and Dynamic State of the Thermosphere below the DE 2 Orbit. The Information obtained from this Investigation was used to Study the Dynamic Response of the Thermosphere to the Energy Sources caused by Magnetospheric Electric Fields and the Absorption of Solar Ultraviolet Light in the Thermosphere. The Instrument was based on the Visible Airglow Experiment, VAE, used in the AE Program. The Addition of a Scanning Mirror, the Fabry-Perot Etalon, an Image Plane Detector, and a Calibration Lamp were the Principal Differences. Interference Filters isolated Lines at 5577, 6300, 7320, 5896, and 5200, in Angstroms. The FPI had a Field of View of 0.53°, Half-Cone Angle. More Details are found in P. B. Hays et al., Space Sci. Instrum., 5(4), 395, 1981. From February 16, 1982 to September 11, 1982 the DE Satellite was inverted and the FPI measured Galactic Emissions. NOTE: Animations of DE2-FPI Science Products have been created as Daily Summary Files. The Animations contain Binned Averages displayed as a Color Code against a Geographic Background. The Bin Sizes are 7.5° Latitude and 24.0° Longitude. The Longitude Bin corresponds to the approximate Separation of adjacent Orbits, assuming that DE2 completed 15 Orbits per Day. The Animations are divided by Day, 06-18 LST, and Night, 18-06 LST, where LST is Local Standard Time. All Summary File Information and Animations employ Spacecraft Orbital Attitude Data. Users should note 1, that the DE2-FPI Experiment acquired Airglow Spectra by imaging the Terrestrial Limb below and ahead of the Spacecraft at an approximate Tangent Altitude of 250 km, 2, All Airglow Spectra were acquired while the DE2 Spacecraft orbited in it's Normal Configuration, which corresponded to Calendar Months August to February in 1981 to 1982 and n 1982 to 1983; 3, The Orbital Inclination of DE2 was 90° implying that DE2-FPI always viewed Ahead along the Meridian; 4, And that DE2 flew in an Elliptical Orbit with Perigee of 305 km and Apogee of 1300 km at Launch ans the Attitude of DE2 for each FPI Measurement is included with each reduced Data Point permitting Users to determine the Tangent Latitude corresponding to the 250 km Terrestrial Airglow Limb. The three GIF Animations are: 1. FPI_brightness.gif, which documents the OI, 630.0 nm,, Column Brightness in Units of log10 Rayleighs. Note different Scales for Day and Night. 2. FPI_temperature.gif, which documents the Neutral Thermosphere Temperature in Units of °Kelvin. 3. FPI_wind.gif, which documents the Line of Sight Neutral Wind Component in Units of m/s. The Wind Direction is positive when the Wind blows away from the approaching Spacecraft.

Wind Magnetic Field Investigation (MFI) Solar Wind Experiment (SWE) 1-min field and plasma data at bow shock nose

Solar wind magnetic field and plasma data at 1-min resolution created from Wind data shifted to the Earth's bow shock nose (BSN).

Wind Magnetic Field Investigation (MFI) Composite Data in RTN Coordinates

Wind MFI composite data in RTN coordinates. The files contain multiple time resolution data: 3-second, 1-minute, and 1-hour. Final Version 5 data are accessible to within about 3 months of current date, newly defined Version 4 data (with final Bz offsets and not-yet-final spacecraft position vectors) between 3 months and about 2 weeks of current date, and newly defined Version 3 data (with the most recently determined Bz offset value, not yet final for the Version 3 interval) from 2 weeks to about 2 days of current.

Wind EPACT/LEMT 1-Hr He,C,O,Ne,Si,Fe Solar Energetic Particle Intensities Level 2 Data

Hourly-averaged fluxes of He, C, O Ne,Si, Fe nuclei in the general range 2-11 MeV/n. Poisson uncertainties are given for each flux.

Apollo 15 Solar Wind Measurements at the Lunar Surface 28-s Data

This data set contains the highest time resolution plasma data available (28 sec per spectrum) from the solar wind experiment onboard Apollo 15. Contained in each record are: time, proton density, alpha-to-proton ratio, bulk speed, angle of flow, most probable thermal speed, and various housekeeping and fit parameters relating to the reliability of the calculated plasma parameters. During the local lunar night there is no solar wind signal so there are data gaps of about 15 days each lunation.

ISEE 3 Merged Vector Helium Magnetometer (MAG), and Solar WInd Plasma (SWP), 2 min CDF Data

These Files provides access to ISEE 3 Merged Field and Plasma 2-min data generated at the NSSDC as part of preparing ISEE 3 data for the creation of new OMNI data sets. Input to the data set were ISEE 3 Magnetometer, MAG, 1 min Data, Solar Wind Plasma, SWP, 24 s data, and spacecraft position 1 day data, all obtained from ftps://spdf.gsfc.nasa.gov/pub/data/isee/isee3/. Pertinent documentation may be found at the same FTP directory. The annual files of this ASCII data set may be accessed at ftps://spdf.gsfc.nasa.gov/pub/data/isee/isee3/2_min_merged_mag_plasma/as well. Time span: magnetic field from 1978-09-11 to 1982-10-12 and solar wind plasma from 1978-09-11 to 1980-02-19. Note that the magnetic field is given in Spacecraft-Centered, Solar Ecliptic, SE, coordinates.