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VOYAGER 1 SATURN PLASMA DERIVED ION FITS BROWSE 96 SEC

THIS DATA SET CONTAINS THE ION DENSITIES, TEMPERATURES, AND VELOCITIES OBTAINED FROM VOYAGER 1 PLS DATA (VOLTAGE RANGE 10-5950 EV/Q) AT SATURN BY FITTING THE MEASURED SPECTRA WITH ISOTROPIC MAXWELLIAN DISTRIBUTIONS. IT IS A SUBSET OF THE DATA SET VG1-S-PLS-5-ION-FIT-96.0SEC WHICH SHOULD BE OBTAINED BEFORE THIS DATA IS USED. ONLY SPECTRA WHICH HAD DISTINCT CURRENT PEAKS WERE FIT. SPECTRA WERE FIT USING ONE OR TWO ION SPECIES, PROTONS AND/OR A HEAVY ION WHICH WAS TAKEN TO BE OXYGEN. OUTSIDE L=10-12 ION SPECTRA CHANGE RAPIDLY, SO THE VALUES IN THIS DATA SET DO NOT REPRESENT AVERAGE PLASMA CONDITIONS IN THE OUTER MAGNETOSPHERE. A COMPLETE DESCRIPTION OF THIS DATA SET IS GIVEN IN RICHARDSON (1986). DATA FORMAT: FIRST 5 COLUMNS ARE TIME TAG (YEAR, DAY, HOUR, MIN SEC.MSEC), FOLLOWED BY PROTON DENSITY (CM-3), PROTON TEMPERATURE (EV), HEAVY ION DENSITY (CM-3), HEAVY ION TEMPERATURE (EV), AND THREE VELOCITY COMPONENTS, (RHO, PHI,Z) IN KM/S. A CYLINDRICAL COORDINATE SYSTEM CENTERED ON THE PLANET IS USED, WITH RHO OUTWARDS FROM THE SPIN AXIS, PHI IN THE DIRECTION OF ROTATION, AND Z THE DISTANCE ABOVE THE EQUATOR. EACH ROW HAS THE FORMAT (2I4,2I3,F7.3,7E11.3). VALUES OF 1.E32 INDICATE THAT THE PARAMETER COULD NOT BE OBTAINED FROM THE DATA USING THE STANDARD ANALYSIS TECHNIQUE. ADDITIONAL INFORMATION ABOUT THIS DATASET AND THE INSTRUMENT WHICH PRODUCED IT CAN BE FOUND ELSEWHERE IN THIS CATALOG. AN OVERVIEW OF THE DATA IN THIS DATA SET CAN BE FOUND IN RICHARDSON (1986) AND A COMPLETE INSTRUMENT DESCRIPTION CAN BE FOUND IN BRIDGE (1977).

GO JUP HIC SURVEY ENERGETIC ION COUNT RATE V1.0

This data set provides energetic (MeV) ion count rates and events measured by the Heavy Ion Counter (HIC) instrument on the Galileo spacecraft. The data are derived from the raw real-time science (RTS) data. There are two basic types of data files associated with the full-rate reduced data: Detector Count Rates and Events (Pulse Heights).

ACE Electron Proton Alpha Monitor (EPAM) LEFS150 MFSA, Spacecraft Frame, Sectored Z>1 Ion Fluxes, 17 min Averages

17-min-averaged sectored Z>1 ion fluxes from the MF Spectrum Analyzer of the ACE/EPAM LEFS150 instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the spacecraft rest frame.

ACE Electron Proton Alpha Monitor (EPAM) LEFS60 MFSA, Solar Wind Frame, Sectored Z>1 Ion Fluxes, 17 min Averages

17-min-averaged sectored Z>1 ion fluxes from the MF Spectrum Analyzer of the ACE/EPAM LEFS60 instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the solar wind rest frame.

VG2 NEP PLS DERIVED RDR ION MAGNETOSPHERE 48SEC V1.0

This data set gives the best available values for ion densities, temperatures, and velocities near Neptune derived from data obtained by the Voyager 2 plasma experiment. All parameters are obtained by fitting the observed spectra (current as a function of energy) with Maxwellian plasma distributions, using a non-linear least squares fitting routine to find the plasma parameters which, when coupled with the full instrument response, best simulate the data. The PLS instrument measures energy/charge, so composition is not uniquely determined but can be deduced in some cases by the separation of the observed current peaks in energy (assuming the plasma is co-moving). In the upstream solar wind protons are fit to the M-long data since high energy resolution is needed to obtain accurate plasma parameters. In the magnetosheath the ion flux so low that several L-long spectra (3-5) had to be averaged to increase the signal-to-noise ratio to a level at which the data could be reliably fit. These averaged spectra were fit using 2 proton maxwellians with the same velocity. The values given in the upstream magnetosheath are the total density and the density-weighted temperature. In both the upstream solar wind and magnetosheath full vector velocities, densities and temperatures are derived for each fit component. In the magnetosphere spectra do not contain enough information to obtain full velocity vectors, so flow is assumed to be purely azimuthal. In some cases the azimuthal velocity is a fit parameter, in some cases rigid corotation is assumed. In the 'outer' magnetosphere (L>5) two distinct current peaks appear in the spectra H+ and N+. In the inner magnetosphere the plasma is hot and the composition is ambiguous, although two superimposed Maxwellians are still required to fit the data. These spectra are fit using two compositions, one with H+ and N+ and the second with two H+ components. The N+ composition is preferred by the data provider. All fit values in the magnetosphere come with one sigma errors. It should be noted that no attempt has been made to account for the spacecraft potential, which is probably about -10 V in this region and will effect the density and velocity values. In the outbound magnetosheath and solar wind both moment and fit values are given for velocity, density, and thermal speed. The signal-to-noise ratio in the M-longs is very low, especially near the magnetopause, which can result in the analysis giving incorrect values. The L-long spectra have too low an energy resolution to permit accurate determinations parameters in many regions temperature and non-radial velocity components may be inaccurate.

ACE Electron Proton Alpha Monitor (EPAM) LEFS150 MFSA, Solar Wind Frame, Sectored Z>1 Ion Fluxes, Hourly Averages

Hourly-averaged sectored Z>1 ion fluxes from the MF Spectrum Analyzer of the ACE/EPAM LEFS150 instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the solar wind rest frame.

VG2 NEP PLS DERIVED RDR ION OUTBND MAGSHTH M-MODE 12MIN V1.0

THEMIS-E: ESA electron/ion energy fluxes and moments

THEMIS-E: Electrostatic Analyzers (ESA): Electron/Ion Ground-Calculated Energy Fluxes (5eV - 25 keV for Ions and 6eV - 30 KeV for Electrons) and Moments (density, velocity, pressure, and temperature). The satellite has 2 modes Fast and Slow survey and 3 data types: FULL, REDUCED and BURST. FULL: 88 angles x 32 energies, time resolution of 128 spins(395 seconds) in slow survey and 32 spins(98 seconds) in fast survey. REDUCED: spin time resolution(3 sec) but angles averaged into 1 angular spectra x 32 energies in slow survey or 6 angular spectra(90 degree x 90 degree window) x 32 energies in fast survey. BURST: 88 angles x 32 energies and spin time resolution(3 sec) but only available sporadically and for short duration. Note that angular resolution affects moments since they are obtained integrating over the mode-specific angular distribution. These moments are processed on the ground. They should be regarded as approximations but will improve in quality as our processing routines are improved over the course of the mission to account for additional sources of variance.

ACE Electron Proton Alpha Monitor (EPAM) LEFS/LEMS MFSA, Spacecraft Frame, Spin-Averaged Z>1 Ion Fluxes, Daily Averages

Daily-averaged ion fluxes from the MF Spectrum Analyzer of the ACE/EPAM instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the spacecraft rest frame.

Voyager 1 Plasma Spectrometer (PLS) Faraday Cups A-D Low Energy Resolution Current Ion Spectra, L Mode, for Proton Energies from 10 eV to 5950 eV, 96 s Data

These Ion Current Spectra in the Jovian Magnetosphere are from the Plasma Spectrometer (PLS) Instrument on Voyager 1 during March 1979 Flyby of Jupiter. The Instrument has four Faraday Cups A, B, C, and D, the Electron Data come only from Faraday Cup D. The Data are specified in Terms of Current per Faraday Cup in femto-amperes (10^-15 A equals 1 fA) versus Channel Number and Energy (eV). This Data Set is for the PLS L Mode covering Proton (H+ Ion) Energies from 10 eV to 5950 eV at Low Energy Resolution in 16 logarithmic Energy Channels. The PLS Instrument samples only one Mode of Electron (E1, E2) or Ion (L, M) Spectra in each Time Interval, so the L Mode Data are not continuous but consecutive with the other Modes in Time. Reference: Bridge, H.S., Belcher, J.W., Butler, R.J., Lazarus, A.J., Mavretic, A.M., Sullivan, J.D., Siscoe, G.L., and V.M. Vasyliunas, The Plasma Experiment on the 1977 Voyager Mission, Space Sci. Rev., 21, 259-287, 1977.

VG2 NEP PLS DERIVED RDR ION OUTBND MAGSHTH L-MODE 48SEC V1.0

This data set gives the best available values for ion densities, temperatures, and velocities near Neptune derived from data obtained by the Voyager 2 plasma experiment. All parameters are obtained by fitting the observed spectra (current as a function of energy) with Maxwellian plasma distributions, using a non-linear least squares fitting routine to find the plasma parameters which, when coupled with the full instrument response, best simulate the data. The PLS instrument measures energy/charge, so composition is not uniquely determined but can be deduced in some cases by the separation of the observed current peaks in energy (assuming the plasma is co-moving). In the upstream solar wind protons are fit to the M-long data since high energy resolution is needed to obtain accurate plasma parameters. In the magnetosheath the ion flux so low that several L-long spectra (3-5) had to be averaged to increase the signal-to-noise ratio to a level at which the data could be reliably fit. These averaged spectra were fit using 2 proton maxwellians with the same velocity. The values given in the upstream magnetosheath are the total density and the density-weighted temperature. In both the upstream solar wind and magnetosheath full vector velocities, densities and temperatures are derived for each fit component. In the magnetosphere, spectra do not contain enough information to obtain full velocity vectors, so flow is assumed to be purely azimuthal. In some cases the azimuthal velocity is a fit parameter, in some cases rigid corotation is assumed. In the 'outer' magnetosphere (L>5) two distinct current peaks appear in the spectra H+ and N+. In the inner magnetosphere the plasma is hot and the composition is ambiguous, although two superimposed Maxwellians are still required to fit the data. These spectra are fit using two compositions, one with H+ and N+ and the second with two H+ components. The N+ composition is preferred by the data provider. All fit values in the magnetosphere come with one sigma errors. It should be noted that no attempt has been made to account for the spacecraft potential, which is probably about -10 V in this region and will effect the density and velocity values. In the outbound magnetosheath and solar wind both moment and fit values are given for velocity, density, and thermal speed. The signal-to-noise ratio in the M-longs is very low, especially near the magnetopause, which can result in the analysis giving incorrect values. The L-long spectra have too low an energy resolution to permit accurate determinations parameters in many regions temperature and non-radial velocity components may be inaccurate.

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

ULYSSES JUPITER HISCALE W ION COUNTS

This data set consists of HISCALE W ion counts from the Ulysses Jupiter encounter 1991-Dec-31 to 1992-Feb-16. This includes 1 hour averaged inbound cruise data (1991-12-31 to 1992-02-01), and 15 minute averaged encounter data (1992-02-02 to 1992-02-16).

STEREO-A Plasma and Supra-Thermal Ion Composition (PLASTIC) Beacon Browse Data

The STEREO-A PLASTIC Beacon data has not been validated and should not be used for publication purposes

VOYAGER 2 SATURN PLASMA DERIVED ION FITS BROWSE 96 SEC

THIS DATA SET CONTAINS THE ION DENSITIES, TEMPERATURES, AND VELOCITIES OBTAINED FROM VOYAGER 2 PLS DATA (VOLTAGE RANGE 10-5950 EV/Q) AT SATURN BY FITTING THE MEASURED SPECTRA WITH ISOTROPIC MAXWELLIAN DISTRIBUTIONS. IT IS A SUBSET OF THE DATA SET VG2-S-PLS-5-ION-FIT-96.0SEC WHICH SHOULD BE OBTAINED BEFORE THIS DATA IS USED. ONLY SPECTRA WHICH HAD DISTINCT CURRENT PEAKS WERE FIT. SPECTRA WERE FIT USING ONE OR TWO ION SPECIES, PROTONS AND/OR A HEAVY ION WHICH WAS TAKEN TO BE OXYGEN. OUTSIDE L=10-12 ION SPECTRA CHANGE RAPIDLY, SO THE VALUES IN THIS DATA SET DO NOT REPRESENT AVERAGE PLASMA CONDITIONS IN THE OUTER MAGNETOSPHERE. A COMPLETE DESCRIPTION OF THIS DATA SET IS GIVEN IN RICHARDSON (1986). DATA FORMAT: FIRST 5 COLUMNS ARE TIME TAG (YEAR, DAY, HOUR, MIN SEC.MSEC), FOLLOWED BY PROTON DENSITY (CM-3), PROTON TEMPERATURE (EV), HEAVY ION DENSITY (CM-3), HEAVY ION TEMPERATURE (EV), AND THREE VELOCITY COMPONENTS, (RHO, PHI,Z) IN KM/S. A CYLINDRICAL COORDINATE SYSTEM CENTERED ON THE PLANET IS USED, WITH RHO OUTWARDS FROM THE SPIN AXIS, PHI IN THE DIRECTION OF ROTATION, AND Z THE DISTANCE ABOVE THE EQUATOR. EACH ROW HAS THE FORMAT (2I4,2I3, F7.3,7E11.3). VALUES OF 1.E32 INDICATE THAT THE PARAMETER COULD NOT BE OBTAINED FROM THE DATA USING THE STANDARD ANALYSIS TECHNIQUE. ADDITIONAL INFORMATION ABOUT THIS DATASET AND THE INSTRUMENT WHICH PRODUCED IT CAN BE FOUND ELSEWHERE IN THIS CATALOG. AN OVERVIEW OF THE DATA IN THIS DATA SET CAN BE FOUND IN RICHARDSON (1986) AND A COMPLETE INSTRUMENT DESCRIPTION CAN BE FOUND IN BRIDGE (1977).

STEREO-A Plasma and Suprathermal Ion Composition (PLASTIC) 1-hour Proton Plasma Parameters

This data product contains 1-hour averaged values of solar wind proton flow speed, density, and temperature and corresponding thermal speed. The records also hold flow velocity vector components and direction angles in HERTN and RTN coordinates. Chi-squared and statistical uncertainties are included, as are various flags. STEREO position information is given in radial distance and HEE, HEEQ and HCI direction angles.

GIOTTO ION MASS SPECTROMETER HIGH INTENSITY DATA V1.0

A wide range of ion species and velocity distributions are expected to be found as the Giotto spacecraft traverses the coma of Halley's Comet. The outer coma is characterized by the interaction between solar wind and cometary plasmas, the inner coma by the outflow of cometary neutrals and their ionization products. The resultant demands on instrument dynamic range preclude use of a single sensor for measurements of ion composition. The Giotto Ion Mass Spectrometer (IMS) therefore consists of two sensors: one optimized for the outer and the other for the inner coma, with each obtaining complementary information in the region for which it is not optimized. Both sensors feature mass imaging characteristics, thereby permitting simultaneous measurements of several ion species by means of multi-detector arrays. The High Intensity Spectrometer (HIS) was designed to complement the HERS in the inner coma.

DE 1 Energetic Ion Composition Spectrometer (EICS) Validated Summary Data

This Validated Summary (VS) data set from the DE 1 Energetic Ion Composition Spectrometer (EICS) contains 96-second averaged fluxes (in units of 1/(cm^2-sec-sr-keV) ) for H+, O+, and He+ ions in 15 energy (~0.01 to ~20 keV) and 14 pitch angle bins. It also includes data uncertainties, data quality indicators, and spacecraft position. Data are in CDF format from CDAWeb.

VOYAGER 1 SATURN PLASMA DERIVED ION MOMENTS 96 SEC

THIS DATA SET CONTAINS ESTIMATES OF THE ION MOMENT DENSITY IN THE PLS VOLTAGE RANGE (10-5950 EV/Q) AT SATURN DURING THE VOYAGER 1 ENCOUNTER. RIGID COROTATION IS ASSUMED, WHICH LEADS TO AN UNDERESTIMATE OF THE DENSITY IN SOME REGIONS, AS DOES THE USE OF AN ACCEPTANCE AREA RELEVANT FOR A COLD BEAM FOR PLASMA WHICH IS TRANSONIC IS SOME REGIONS. DENSITIES MAY BE UNDERESTIMATED BY A FACTOR OF 2-3 IN THE INNER MAGNETOSPHERE, SO THIS DATA SET SHOULD BE USED PRIMARILY FOR STUDIES USING VARIATIONS IN PLASMA DENSITY. THE FIT DENSITIES GIVE A BETTER ESTIMATE OF THE ABSOLUTE DENSITY. THIS IS THE DATA SHOWN AND DESCRIBED IN DETAIL IN LAZARUS AND MCNUTT (1983). DATA FORMAT: COLUMNS 1-5 ARE TIME (YEAR, DAY, HOUR, MIN, SEC) AND COLUMN 6 IS THE MOMENT DENSITY IN CM-3. EACH ROW HAS FORMAT (I5,I4,2I3,I4,F8.3). VALUES OF 1.E32 INDICATE THAT THE PARAMETER COULD NOT BE OBTAINED FROM THE DATA USING THE STANDARD ANALYSIS TECHNIQUE. ADDITIONAL INFORMATION ABOUT THIS DATASET AND THE INSTRUMENT WHICH PRODUCED IT CAN BE FOUND ELSEWHERE IN THIS CATALOG. AN OVERVIEW OF THE DATA IN THIS DATA SET CAN BE FOUND IN LAZARUS AND MCNUTT (1983) AND A COMPLETE INSTRUMENT DESCRIPTION CAN BE FOUND IN BRIDGE (1977).

CNOFS CINDI IVM 500 ms Ion Drift Data

This data set contains plasma parameters of the equatorial F-region in the ionosphere measured by the Ion Velocity Meter (IVM) of the Coupled Ion-Neutral Dynamics Investigation (CINDI) payload on board the CNOFS spacecraft. Data are available in HDF format, with an IDL program to read and plot them. Each file contains data from one day of spacecraft operation and the file contains eight primary geophysical parameters: the ion temperature (Ti) in degrees Kelvin, the ion flow in m/s in the ram (i.e.--spacecraft velocity) direction (+Vx in the direction of spacecraft velocity), the ion flows in m/s in the horizontal and vertical directions (Vy and Vz) at right angles to the ram direction (+Vz is downward, +Vy is roughly southward), the total ion density (Ni) (the sum of O+ and H+ and He+ concentrations) in ions/cc, and the individual H+, He+, and O+ concentrations in ions/cc. In addition, ion velocities also are given in the coordinate system of the local magnetic field (parallel, perpendicular, and meridional) in the plots and as ASCII data on the UT Dallas website. Based on the IGRF model, the data are transformed into magnetic coordinates only if all three ion velocities in the spacecraft coordinates are available and good.