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457 results for “voyager”
VOYAGER 2 SOLAR WIND PLS 1 HOUR AVERAGES V1.0
Voyager 2 plasma data of the solar wind, 1 hour averages.
VOYAGER 2 SOLAR WIND PLS 1 DAY AVERAGES V1.0
Voyager 2 plasma data of the solar wind, 1 day averages.
NASA 3D Models: Voyager Probe
Polygons: 99526 Vertices: 50502
VOYAGER 2 SOLAR WIND PLS FINE RES V1.0
Voyager 2 plasma data of the solar wind, fine resolution data.
VOYAGER 2 JUP LOW ENERGY CHARGED PARTICLE CALIB. 15MIN
THIS DATA SET CONSISTS OF RESAMPLED DATA FROM THE LOW ENERGY CHARGED PARTICLE (LECP) EXPERIMENT ON VOYAGER 2 WHILE THE SPACECRAFT WAS IN THE VICINITY OF JUPITER. THIS INSTRUMENT MEASURES THE INTENSITIES OF IN-SITU CHARGED PARTICLES (>26 KEV ELECTRONS AND >30 KEV IONS) WITH VARIOUS LEVELS OF DISCRIMINATION BASED ON ENERGY, MASS SPECIES, AND ANGULAR ARRIVAL DIRECTION. A SUBSET OF ALMOST 100 LECP CHANNELS ARE INCLUDED WITH THIS DATA SET. THE LECP DATA ARE GLOBALLY CALIBRATED TO THE EXTENT POSSIBLE (SEE BELOW) AND THEY ARE TIME AVERAGED TO ABOUT 15 MINUTE TIME INTERVALS WITH THE EXACT BEGINNING AND ENDING TIMES FOR THOSE INTERVALS MATCHING THE LECP INSTRUMENTAL CYCLE PERIODS (THE ANGULAR SCANNING PERIODS). THE LECP INSTUMENT HAS A ROTATING HEAD FOR OBTAINING ANGULAR ANISOTROPY MEASUREMENTS OF THE MEDIUM ENERGY CHARGED PARTICLES THAT IT MEASURES. THE CYCLE TIME FOR THE ROTATION IF VARIABLE, BUT DURING ENCOUNTERS IT IS ALWAYS FASTER THAN 15 MINUTES. THUS, THE FULL ANGULAR ANISOTROPY INFORMATION IS PRESERVED WITH THIS DATA. THE DATA IS IN THE FORM OF 'RATE' DATA WHICH HAS NOT BEEN CONVERTED TO THE USUAL PHYSICAL UNITS. THE REASON IS THAT SUCH A CONVERSION WOULD DEPEND ON UNCERTAIN DETERMINATIONS SUCH AS THE MASS SPECIES OF THE PARTICLES AND THE LEVEL OF BACKGROUND. BOTH MASS SPECIES AND BACKGROUND ARE GENERALLY DETERMINED FROM CONTEXT DURING THE STUDY OF PARTICULAR REGIONS. TO CONVERT 'RATE' TO 'INTENSITY' FOR A PARTICULAR CHANNEL ONE PERFORMS THE FOLLOWING TASKS: 1) DECIDE ON THE LEVEL OF BACKGROUND CONTAMINATION AND SUBTRACT THAT OFF THE GIVEN RATE LEVEL. BACKGROUND IS TO BE DETERMINED FROM CONTEXT AND FROM MAKING USE OF SECTOR 8 RATES (SECTOR 8 HAS A 2 mm AL SHIELD COVERING IT). 2) DIVIDE THE BACKGROUND CORRECTED RATE BY THE CHANNEL GEOMETRIC FACTOR AND BY THE ENERGY BANDPASS OF THE CHANNEL. THE GEOMETRIC FACTOR IS FOUND IN ENTRY 'channel_geometric_ factor' AS ASSOCIATED WITH EACH CHANNEL 'channel_id'. TO DETERMINE THE ENERGY BANDPASS, ONE MUST JUDGE THE MASS SPECIES OF THE OF THE DETECTED PARTICLES (FOR IONS BUT NOT FOR ELECTRONS). THE ENERGY BAND PASSES ARE GIVEN IN ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPENERGY', AND ARE GIVEN IN THE FORM 'ENERGY/NUCLEON'. FOR CHANNELS THAT BEGIN THEIR NAMES WITH THE DESIGNATIONS 'CH' THESE BANDPASSES CAN BE USED ON MASS SPECIES THAT ARE ACCEPTED INTO THAT CHANNEL (SEE ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPCHANZ', WHICH GIVE THE MINIMUM AND MAXIMUM 'Z' VALUE ACCEPTED -- THESE ENTRIES ARE BLANK FOR ELECTRON CHANNELS). FOR OTHER CHANNELS THE GIVEN BANDPASS REFERS ONLY TO THE LOWEST 'Z' VALUE ACCEPTED. THE BANDPASSES FOR OTHER 'Z' VALUES ARE NOT ALL KNOWN, BUT SOME ARE GIVEN IN THE LITERATURE (E.G. KRIMIGIS ET AL., 1979). THE FINAL PRODUCT OF THESE INSTRUCTIONS WILL BE THE PARTICLE INTENSITY WITH THE UNITS: COUNTS/(CM**2.STR.SEC.KEV). SOME CHANNELS ARE SUBJECT TO SERIOUS CONTAMINATIONS, AND MANY OF THESE CONTAMINATIONS CANNOT BE REMOVED EXCEPT WITH A REGION-BY-REGION ANALYSIS, WHICH HAS NOT BEEN DONE FOR THIS DATA. THUS, TO USE THIS DATA IT IS ABSOLUTELY VITAL THAT THE CONTAMINATION TYPES ('contamination_id' , 'contamination_desc') AND THE LEVELS OF CONTAMINATION ('data_quality_id' CORRESPONDING TO THE DEFINITIONS 'data_quality_desc') BE CAREFULLY EXAMINED FOR ALL REGIONS OF STUDY. A DEAD TIME CORRECTION PROCEDURE HAS BEEN APPLIED IN AN ATTEMPT TO CORRECT THE LINEAR EFFECTS OF DETECTOR OVERDRIVE (PULSE-PILEUP). THIS PROCEDURE DOES NOT FIX SEVERELY OVERDRIVEN DETECTORS. A PROCEDURE IS AVAILABLE FOR CORRECTING VOYAGER 2 LECP ELECTRON CONTAMINATION OF LOW ENERGY ION CHANNELS, BUT ITS EFFECTIVENESS HAS BEEN EVALUATED ONLY FOR THE URANUS DATA SET. THUS, CORRECTIONS HAVE BEEN APPLIED ONLY TO THE URANUS DATA SET. Also included with this data are one standard deviation statistical uncertainties for the directional data (sectors 1 through 8) expressed as a percent. Unknown values are generally coded as s
VOYAGER 1 JUP PLASMA SPECTROMETER EDITED SPEC 4.0SEC
This data set consists of 4-second edited, wave electric field intensities from the Voyager 1 Plasma Wave Receiver spectrum analyzer obtained in the vicinity of the Jovian magnetosphere. For each 4-second interval, a field strength is determined for each of the 16 spectrum analyzer channels whose center frequencies range from 10 Hertz to 56.2 kiloHertz and which are logarithmically spaced in frequency, four channels per decade. The time associated with each set of intensities (16 channels) is the time of the beginning of the scan. During data gaps where complete 4-second spectra are missing, no entries exist in the file, that is, the gaps are not zero-filled or tagged in any other way. When one or more channels are missing within a scan, the missing measurements are zero-filled. Data are edited but not calibrated. The data numbers in this data set can be plotted in raw form for event searches and simple trend analysis since they are roughly proportional to the log of the electric field strength. Calibration procedures and tables are provided for use with this data set described below.
Voyager 1 Plasma Spectrometer (PLS) High Resolution Plasma Density, Thermal Speed, and Velocity (RTN) Data in CDF Format
Voyager 1 High-Resolution Plasma Data. The files in this directory contain the Voyager fine resolution plasma data. The plasma parameters are obtained by finding the best fit of a convected isotropic Maxwellian distribution to the data. One sigma errors are typically less than 0.5% in the speed and VR, less than 5% for the density and thermal speed, and vary greatly for VT and VN. Sampling times range from 12 to 192 sec., with sampling generally more frequent early in the mission. The velocity components are given in the RTN coordinate system, where R is radially outward, T is in a plane parallel to the solar equatorial plane and positive in the direction of solar rotation, and N completes a right-handed system. Warning: the V_t and V_n parameters are often not reliable after 1989. Please consult with us, or at least send preprints, when you use these data to prevent grievous errors or misconceptions, John Richardson, jdr@space.mit.edu.
Voyager 2 1.92-s Averaged Triaxial Fluxgate Magnetometer (MAG) Interplanetary Magnetic Field in CDF Format
This data set includes the Voyager spacecraft number (1 or 2), the date-time in decimal year (90.00000 is day 1 of 1990), the magnetic field strength, F1, computed from high-resolution magnitudes, the elevation and azimuth angles in heliographic (RTN) coordinates, and the magnetic field strength, F2, computed from 1-hr averages of the components. The vector components of B can be computed from F2 and the two angles. The elevation angle is the latitude angle above or below the solar equatorial plane, and the azimuth angle is in the direction orbital motion around the Sun from the projection of the Sun-to-spacecraft axis into the solar equatorial plane. The Voyager MAG experiment and coordinates are further described in the following publication: Behannon, K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, and F.M. Neubauer, Magnetic-Field Experiment for Voyager-1 and Voyager-2, Space Sci. Rev., 21 (3), 235-257, 1977. At the time of experiment proposal, it was expected that the required accuracy of the measurements would be 0.1 nT, determined by the combined noise of the sensors and the spacecraft field. The spacecraft magnetic field at the outboard magnetic field sensor, referred to as the primary unit, was expected to be 0.2 nT and highly variable, consistent with current estimates. Hence, the dual magnetometer design (Ness et al., 1971, 1973; Behannon et al., 1977). At distances > 40 AU, the heliospheric magnetic fields are generally much weaker than 0.4 nT; the average magnetic field strength near 40 AU and 85 AU is about 0.15 nT and 0.05 nT, respectively. The use of roll calibrations lasting about 6 hours permits determination of the effective zero levels for the two independent magnetic axes that are perpendicular to the roll axis, which is nearly parallel to the radius vector to the Sun, at intervals of about 3 months. There is no roll calibration for the third magnetic axis. Comparison of the two derived magnetic vectors from the two magnetometers permits validation of the primary magnetometer data with an accuracy of 0.02 to 0.05 nT. A discussion of the uncertainties that must be considered when using these data is given in the Appendix of Burlaga et al. (1994) and in Appendix A of Burlaga et al. (2002). References: Behannon, K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, and F.M. Neubauer, Magnetic-Field Experiment for Voyager-1 and Voyager-2, Space Science Reviews, 21 (3), 235-257, 1977. Burlaga, L.F., Merged interaction regions and large-scale magnetic field fluctuations during 1991 - Voyager-2 observations, J. Geophys. Res., 99 (A10), 19341-19350, 1994. Burlaga, L.F., N.F. Ness, Y.-M. Wang, and N.R. Sheeley, Jr., Heliospheric magnetic field strength and polarity from 1 to 81 AU during the ascending phase of solar cycle 23, J. Geophys. Res., 107 (A11), 1410, 2002. Ness, N., K.W. Behannon, R. Lepping, and K.H. Schatten, J. Geophys. Res., 76, 3564, 1971. Ness et al., 1973. Coordinate Systems: Interplanetary magnetic field studies make use of two important coordinate systems, the Heliographic Inertial (HGI) coordinate system and the Heliographic (HG) coordinate system. The HGI coordinate system is used to define the spacecraft's position. The HGI system is defined with its origin at the Sun. There are three orthogonal axes, X(HGI), Y(HGI), and Z(HGI). The Z(HGI) axis points northward along the Sun's spin axis. The X(HGI)-Y(HGI) plane lays in the solar equatorial plane. The intersection of the solar equatorial plane with the ecliptic plane defines a line, the longitude of the ascending node, which is taken to be the X(HGI) axis. The X(HGI) axis drifts slowly with time, approximately one degree per 72 years. The magnetic field orientation is defined in relation to the spacecraft. Drawing a line from the Sun's center (HGI origin) to the spacecraft defines the X axis of the HG coordinate system. The HG coordinate system is defined with its origin centered at the spacecraft. Three orthogonal axes are defined, X(HG), Y(HG), and Z(HG). The X(HG) axis points radially away from the Sun and the Y(HG) axis is parallel to the solar equatorial plane and therefore parallel to the X(HGI)-Y(HGI) plane as well. The Z(HG) axis is chosen to complete the orthonormal triad. An excellent reference guide with diagrams explaining the HGI and HG systems may be found in L.F. Burlaga, MHD Processes in the Outer Heliosphere, Space Sci. Rev., 39, 255-316, 1984.
VOYAGER 1 JUP LOW ENERGY CHARGED PARTICLE CALIB. BR 15MIN
THIS BROWSE DATA CONSISTS OF RESAMPLED DATA FROM THE LOW ENERGY CHARGED PARTICLE (LECP) EXPERIMENT ON VOYAGER 1 WHILE THE SPACECRAFT WAS IN THE VICINITY OF JUPITER. THIS INSTRUMENT MEASURES THE INTENSITIES OF IN-SITU CHARGED PARTICLES (>26 KEV ELECTRONS AND >30 KEV IONS) WITH VARIOUS LEVELS OF DISCRIMINATION BASED ON ENERGY, MASS SPECIES, AND ANGULAR ARRIVAL DIRECTION. A SUBSET OF ALMOST 100 LECP CHANNELS ARE INCLUDED WITH THIS DATA SET. THE LECP DATA ARE GLOBALLY CALIBRATED TO THE EXTENT POSSIBLE (SEE BELOW) AND THEY ARE TIME AVERAGED TO ABOUT 15 MINUTE TIME INTERVALS WITH THE EXACT BEGINNING AND ENDING TIMES FOR THOSE INTERVALS MATCHING THE LECP INSTRUMENTAL CYCLE PERIODS (THE ANGULAR SCANNING PERIODS). THE LECP INSTUMENT HAS A ROTATING HEAD FOR OBTAINING ANGULAR ANISOTROPY MEASUREMENTS OF THE MEDIUM ENERGY CHARGED PARTICLES THAT IT MEASURES. THE CYCLE TIME FOR THE ROTATION IF VARIABLE, BUT DURING ENCOUNTERS IT IS ALWAYS FASTER THAN 15 MINUTES. FOR THIS BROWSE DATA SET ONLY SCAN AVERAGE DATA IS GIVEN (NO ANGULAR INFORMATION). THE DATA IS IN THE FORM OF 'RATE' DATA WHICH HAS NOT BEEN CONVERTED TO THE USUAL PHYSICAL UNITS. THE REASON IS THAT SUCH A CONVERSION WOULD DEPEND ON UNCERTAIN DETERMINATIONS SUCH AS THE MASS SPECIES OF THE PARTICLES AND THE LEVEL OF BACKGROUND. BOTH MASS SPECIES AND BACKGROUND ARE GENERALLY DETERMINED FROM CONTEXT DURING THE STUDY OF PARTICULAR REGIONS. TO CONVERT 'RATE' TO 'INTENSITY' FOR A PARTICULAR CHANNEL ONE PERFORMS THE FOLLOWING TASKS: 1) DECIDE ON THE LEVEL OF BACKGROUND CONTAMINATION AND SUBTRACT THAT OFF THE GIVEN RATE LEVEL. BACKGROUND IS TO BE DETERMINED FROM CONTEXT AND FROM MAKING USE OF SECTOR 8 RATES (SECTOR 8 HAS A 2 mm AL SHIELD COVERING IT). 2) DIVIDE THE BACKGROUND CORRECTED RATE BY THE CHANNEL GEOMETRIC FACTOR AND BY THE ENERGY BANDPASS OF THE CHANNEL. THE GEOMETRIC FACTOR IS FOUND IN ENTRY 'channel_geometric_ factor' AS ASSOCIATED WITH EACH CHANNEL 'channel_id'. TO DETERMINE THE ENERGY BANDPASS, ONE MUST JUDGE THE MASS SPECIES OF THE OF THE DETECTED PARTICLES (FOR IONS BUT NOT FOR ELECTRONS). THE ENERGY BAND PASSES ARE GIVEN IN ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPENERGY', AND ARE GIVEN IN THE FORM 'ENERGY/NUCLEON'. FOR CHANNELS THAT BEGIN THEIR NAMES WITH THE DESIGNATIONS 'CH' THESE BANDPASSES CAN BE USED ON MASS SPECIES THAT ARE ACCEPTED INTO THAT CHANNEL (SEE ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPCHANZ', WHICH GIVE THE MINIMUM AND MAXIMUM 'Z' VALUE ACCEPTED -- THESE ENTRIES ARE BLANK FOR ELECTRON CHANNELS). FOR OTHER CHANNELS THE GIVEN BANDPASS REFERS ONLY TO THE LOWEST 'Z' VALUE ACCEPTED. THE BANDPASSES FOR OTHER 'Z' VALUES ARE NOT ALL KNOWN, BUT SOME ARE GIVEN IN THE LITERATURE (E.G. KRIMIGIS ET AL., 1979). THE FINAL PRODUCT OF THESE INSTRUCTIONS WILL BE THE PARTICLE INTENSITY WITH THE UNITS: COUNTS/(CM**2.STR.SEC.KEV). SOME CHANNELS ARE SUBJECT TO SERIOUS CONTAMINATIONS, AND MANY OF THESE CONTAMINATIONS CANNOT BE REMOVED EXCEPT WITH A REGION-BY-REGION ANALYSIS, WHICH HAS NOT BEEN DONE FOR THIS DATA. THUS, TO USE THIS DATA IT IS ABSOLUTELY VITAL THAT THE CONTAMINATION TYPES ('contamination_id' , 'contamination_desc') AND THE LEVELS OF CONTAMINATION ('data_quality_id' CORRESPONDING TO THE DEFINITIONS 'data_quality_desc') BE CAREFULLY EXAMINED FOR ALL REGIONS OF STUDY. A DEAD TIME CORRECTION PROCEDURE HAS BEEN APPLIED IN AN ATTEMPT TO CORRECT THE LINEAR EFFECTS OF DETECTOR OVERDRIVE (PULSE-PILEUP). THIS PROCEDURE DOES NOT FIX SEVERELY OVERDRIVEN DETECTORS. A PROCEDURE IS AVAILABLE FOR CORRECTING VOYAGER 2 LECP ELECTRON CONTAMINATION OF LOW ENERGY ION CHANNELS, BUT ITS EFFECTIVENESS HAS BEEN EVALUATED ONLY FOR THE URANUS DATA SET. THUS, CORRECTIONS HAVE BEEN APPLIED ONLY TO THE URANUS DATA SET.
VOYAGER 2 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 2 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). 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).
VOYAGER 1 SATURN MAGNETOMETER RESAMPLED DATA 9.60 SEC
This data set includes Voyager 1 Saturn encounter magnetometer data that have been resampled at a 9.6 second sample rate. The data set is composed of 6 columns: 1) ctime - this column contains the data acquisition time. The time is always output in the ISO standard spacecraft event time format (yyyy-mm-dd-Thh:mm:ss.sss) but is stored internally in Cline time which is measured in seconds after 00:00:00.000 Jan 01, 1966, 2) br - this column contains the radial component of the magnetic field, 3) bphi - this column contains the phi component of the magnetic field, 4) btheta - this column contains the theta component of the magnetic field, 5) bmag - this column contains the magnitude of the magnetic field, 6) flag - a flag value that indicates either software error or spacecraft hardware interference reduced confidence in this record (flag value of 1 is bad , 0 is good or unchecked). All magnetic field observations are measured in nanoTeslas. The coordinate system for this dataset is Minus Saturn Longitude System (-SLS). All of the magnetic field data are calibrated (see the instrument calibration description for more details). The SLS coordinate system is defined in Desch and Kaiser, 1981 and the reference documents for this dataset are: Ness et al, 1982 Acuna,Connerney,and Ness, 1983 Connerney,Acuna,and Ness, 1983 Behannon,Lepping,and Ness, 1983
Voyager 2 48-s Triaxial Fluxgate Magnetometer (MAG) Magnetic Field Data in CDF Format
This data set includes the Voyager spacecraft number (1 or 2), the date-time in decimal year (90.00000 is day 1 of 1990), the magnetic field strength, F1, computed from high-resolution magnitudes, the elevation and azimuth angles (degrees) in heliographic (RTN) coordinates, and the magnetic field strength, F2, computed from hour averages of the components. The vector components of B can be computed from F2 and the two angles. The elevation angle is the latitude angle above or below the solar equatorial plane, and the azimuth angle is in the direction of orbital motion around the Sun from the projection of the Sun-to-spacecraft axis into the solar equatorial plane. The Voyager MAG experiment and coordinates are further described in the following publication: Behannon, K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, and F.M. Neubauer, Magnetic-Field Experiment for Voyager-1 and Voyager-2, Space Science Reviews, 21 (3), 235-257, 1977. At the time of experiment proposal, it was expected that the required accuracy of the measurements would be 0.1 nT, determined by the combined noise of the sensors and the spacecraft field. The spacecraft magnetic field at the outboard magnetic field sensor, referred to as the primary unit, was expected to be 0.2 nT and highly variable, consistent with current estimates. Hence, the dual magnetometer design (Ness et al., 1971, 1973; Behannon et al. 1977) was adopted. At distances > 40 AU, the heliospheric magnetic fields are generally much weaker than 0.4 nT; the average magnetic field strength near 40 AU and 85 AU is about 0.15 nT and 0.05 nT, respectively. The use of roll calibrations lasting about 6 hours permits determination of the effective zero levels for the two independent magnetic axes that are perpendicular to the roll axis (which is nearly parallel to the radial vector to the Sun) at intervals of about 3 months. There is no roll calibration for the third magnetic axis. Comparison of the two derived magnetic vectors from the two magnetometers permits validation of the primary magnetometer data with an accuracy of 0.02 to 0.05 nT. A discussion of the uncertainties that must be considered when using these data is given in the Appendix of Burlaga et al. (1994) and in Appendix A of Burlaga et al. (2002). References: Behannon, K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, and F.M. Neubauer, Magnetic-Field Experiment for Voyager-1 and Voyager-2, Space Science Reviews, 21 (3), 235-257, 1977. Burlaga, L.F., Merged interaction regions and large-scale magnetic field fluctuations during 1991 - Voyager-2 observations, J. Geophys. Res., 99 (A10), 19341-19350, 1994. Burlaga, L.F., N.F. Ness, Y.-M. Wang, and N.R. Sheeley Jr., Heliospheric magnetic field strength and polarity from 1 to 81 AU during the ascending phase of solar cycle 23, J. Geophys. Res., 107 (A11), 1410, 2002. Ness, N., K.W. Behannon, R. Lepping, and K.H. Schatten, J. Geophys. Res., 76, 3564, 1971. Ness et al., 1973. Coordinate Systems: Interplanetary magnetic field studies make use of two important coordinate systems, the Heliographic Inertial (HGI) coordinate system and the Heliographic (HG) coordinate system. The HGI coordinate system is use to define the spacecraft's position. The HGI system is defined with its origin at the Sun. There are three orthogonal axes, X(HGI), Y(HGI), and Z(HGI). The Z(HGI) axis points northward along the Sun's spin axis. The X(HGI)-Y(HGI) plane lays in the solar equatorial plane. The intersection of the solar equatorial plane with the ecliptic plane defines a line, the longitude of the ascending node, which is taken to be the X(HGI) axis. The X(HGI) axis drifts slowly with time, approximately one degree per 72 years. Magnetic field orientation is defined in relation to the spacecraft. Drawing a line from the Sun's center, the HGI origin, to the spacecraft defines the X axis of the HG coordinate system. The HG coordinate system is defined with its origin centered at the spacecraft. Three orthogonal axes are defined, X(HG), Y(HG), and Z(HG). The X(HG) axis points radially away from the Sun and the Y(HG) axis is parallel to the solar equatorial plane and therefore parallel to the X(HGI)-Y(HGI) plane too. The Z(HG) axis is chosen to complete the orthonormal triad. An excellent reference guide with diagrams explaining the HGI and HG systems may be found in L. F. Burlaga, MHD Processes in the Outer Heliosphere, Space and Science Reviews, 39, 255-316. Support data calib_flag_on, calib_flag_MF, and calib_flag_offset are added to file version 2. Variable calib_flag_on consists of points where bit 4 or 5 in variable magStatus equal 1. Variable calib_flag_MF represents observations where magnetometer was in cailbration mode. Variable calib_flag_offset represent delay between data points when the magnetometer was in calibration mode and data points where magStatus variable indicated calibration periods. Due to specific shape of magnetometer data profile variable calibration_flag_
VOYAGER 2 JUPITER/SHOEMAKER-LEVY 9 UVS NULL RESULTS V1.0
A preliminary examination of the Ultraviolet Spectrometer (UVS) data revealed no obvious detections of anything which might correspond with the impact phenomena. In order to investigate the possibility that more subtle impact-related events were present in the data and to establish a formal statistical upper limit for the non-detection of the impacts, we performed a statistical analysis as described in the DPS poster paper 'Voyager 2 UVS Observations of Jupiter During the Comet Shoemaker-Levy 9 Impact Events', by R. J. Vervack et al. [VERVACKETAL1995]
Voyager 2 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 2 during July 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.
VOYAGER 2 SATURN MAGNETOMETER RESAMPLED DATA 9.60 SEC
This data set includes Voyager 2 Saturn encounter magnetometer data that have been resampled at a 9.6 second sample rate. The data set is composed of 6 columns: 1) ctime - this column contains the data acquisition time. The time is always output in the ISO standard spacecraft event time format (yyyy-mm-dd-Thh:mm:ss.sss) but is stored internally in Cline time which is measured in seconds after 00:00:00.000 Jan 01, 1966, 2) br - this column contains the radial component of the magnetic field, 3) bphi - this column contains the phi component of the magnetic field, 4) btheta - this column contains the theta component of the magnetic field, 5) bmag - this column contains the magnitude of the magnetic field, 6) flag - a flag value that indicates either software error or spacecraft hardware interference reduced confidence in this record (flag value of 1 is bad , 0 is good or unchecked). All magnetic field observations are measured in nanoTeslas. The coordinate system for this dataset is Minus Saturn Longitude System (-SLS). All of the magnetic field data are calibrated (see the instrument calibration description for more details). The SLS coordinate system is defined in Desch and Kaiser, 1981 and the reference documents for this dataset are: Ness et al, 1982 Acuna,Connerney,and Ness, 1983 Connerney,Acuna,and Ness, 1983 Behannon,Lepping,and Ness, 1983
VOYAGER 2 SATURN PLASMA DERIVED ELECTRON BROWSE 96 SEC
THIS DATA SET CONTAINS THE THERMAL ELECTRON DENSITY AND TEMPERATURE IN THE PLS ENERGY RANGE (10-5950 EV) FROM VOYAGER 2 AT SATURN DERIVED BY FITTING THE LOW ENERGY ELECTRON COMPONENT WITH A MAXWELLIAN DISTRIBUTION, AND THE MOMENT DENSITY AND TEMPERATURE OF THE HOT ELECTRONS CALCULATED AFTER THE SIGNAL FROM THE THERMAL COMPONENT IS SUBTRACTED FROM THE ELECTRON SPECTRA. IT IS A SUBSET OF THE DATA SET VG2-S-PLS-5-ELE-FIT-96.0SEC WHICH SHOULD BE OBTAINED BEFORE THIS DATA IS USED. SPACECRAFT CHARGING MAY RESULT IN FACTOR OF 2-3 ERRORS IN THE THERMAL ELECTRON DENSITY. THE FIRST SIX COLUMNS ARE THE TIME TAG (YEAR, DAY, HOUR, MIN, SEC, MSEC), COLUMN 7 AND 8 ARE THE FIT DENSITY AND TEMPERATURE OF THE THERMAL ELECTRON COMPONENT, AND 9 AND 10 ARE THE MOMENT DENSITY AND TEMPERATURE OF THE SUPRATHERMAL ELECTRONS. EACH ROW HAS THE FORMAT (6I5,4E12.4). 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 SITTLER ET AL. (1983) AND A COMPLETE INSTRUMENT DESCRIPTION CAN BE FOUND IN BRIDGE (1977).
VOYAGER 1&2 JUPITER IRIS DERIVED NORTH/SOUTH PARAMETERS V1.0
The data set contains Jovian atmospheric parameters derived from spectra obtained with the Voyager infrared interferometer spectrometer (IRIS). The data set is ordered by time as measured by the Flight Data System Count (FDSC). This represents the data frame number modulo 60. Also included in the data set are information on pointing and associated geometry of the measurements and brightness temperatures obtained from measured radiances at selected wavenumbers.
Academy of Program/Project & Engineering Leadership: Shared Voyage: Learning and Unlearning from Remarkable Projects
Shared Voyage is about four remarkable projects:the Advanced Composition Explorer (NASA), the Joint Air-to-Surface Standoff Missile (U.S. Air Force), the Pathfinder Solar-Powered Airplane (NASA), and the Advanced Medium Range Air-to-Air Missile (U.S. Air Force).
VOYAGER 2 JUPITER MAGNETOMETER RESAMPLED DATA 48.0 SEC
This data set includes Voyager 2 Jupiter encounter magnetometer data that have been resampled at a 48.0 second sample rate. The data set is composed of 6 columns: 1) ctime - this column contains the data acquisition time. The time is always output in the ISO standard spacecraft event time format (yyyy-mm-dd-Thh:mm:ss.sss) but is stored internally in Cline time which is measured in seconds after 00:00:00.000 Jan 01, 1966, 2) br - this column contains the radial component of the magnetic field, 3) bphi - this column contains the phi component of the magnetic field, 4) btheta - this column contains the theta component of the magnetic field, 5) bmag - this column contains the magnitude of the magnetic field, 6) flag - a flag value that indicates either software error or spacecraft hardware interference reduced confidence in this record (flag value of 1 is bad , 0 is good or unchecked). All magnetic field observations are measured in nanoTeslas. The coordinate system for this dataset is Minus System III. All of the magnetic field data are calibrated (see the instrument calibration description for more details). The Jupiter System III coordinate system is defined in Dessler 1983 and the reference documents for this dataset are: Ness et al, 1979A Lepping et al, 1981 Connerney,Acuna,Ness, 1981 Behannon,Burlaga,Ness, 1981
VOYAGER 1&2 JUPITER BRIGHTNESS NORTH/SOUTH MAP SET V1.0
This data set contains Voyager 1 and 2 measurements of the brightness of Jupiter at H Lyman alpha and in the H2 Lyman and Werner bands shortward of H Lyman alpha. Pointing has been corrected by the C-Smithing process, and these data were derived from the pre-encounter North-South Map sequences. In this sequence, the UVS field of view was located near the central meridian of the planet. The field of view stepped slowly from north to south, and then rapidly repositioned to the north. These scans were repeated until all Jovian longitudes had been sampled. Coverage in longitude was not continuous in time. Rather, some longitude ranges were covered on the preceding or following rotation of Jupiter.
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Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.