Showing 1 - 24 |

1) | ISEE 3 Elemental Abundance Ratios | |||||||||||||||||
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Resource ID:spase://VEPO/NumericalData/ISEE3/ElemAbun | ||||||||||||||||||

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This ASCII file contains values and their uncertainties for 25 abundance ratios of various pairs of chemical elements. The ratios are based on 1978-1981 observations of ~50-500 MeV/n cosmic rays by the U. Chicago cosmic ray experiment on ISEE 3. Each of the ratios is linked in the ASCII file to the publication where its derivation is discussed. |

2) | ISEE 3 12-min Trajectory Data | |||||||||||||||||
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Resource ID:spase://VEPO/NumericalData/ISEE3/Ephemeris/PT12M | ||||||||||||||||||

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ISEE 3 positions. |

3) | ISEE 3 Daily Trajectory Data | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/ISEE3/Ephemeris/PT24H | ||||||||||||||||||

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This data set contains orbital parameters for ISEE-3: heliospheric radial distance in AU, solar ecliptical latitude, solar ecliptical longitude, solar heliographic latitude, solar heliographic longitude, and solar solar heliographic inertial longitude with respect to the ascending node of solar equator on the ecliptic. These data were obtained from running the program HELICOOR in the public directory NSSDCA::ANON_DIR:[ACTIVE.HELIO]. These data are based on predicted trajectories calculated with the GTDS code by the NSSDC Satellite Situation Center and converted to solar ecliptic and heliographic coordinates by the HELIOCOOR program. The HELICOOR code was written by R. Parthasarathy. The program GENTRJCON added the HILLON longitude. Note that the solar ecliptic coordinates are given with respect to true equinox and ecliptic of date. The solar ascending node was located at ecliptic longitude +74.367 degrees as of 1 Jan. 1900 at 1200 UT; this longitude increases by 1.4 degrees/century. |

4) | ISEE 3 64-min Trajectory Data | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/ISEE3/Ephemeris/PT64M | ||||||||||||||||||

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This data set was generated at NSSDC by selecting data parameters from the ISEE 3 data pool tape (binary) and converting to ASCII. The time resolution is about an hour and 4 minutes. Data records that contained fill data for the spacecraft position were not included in this data set. Only data items that are not instrument-specific are included here. The data items, in order, are: year, day of year (Jan. 1 = 001), seconds of day, bit rate code, maneuver code, spin period average (in seconds) over the hour, and the GSE X,Y,Z components of the spacecraft position (in km). The bit rate code is 1,2, or 4 for bit rates of 512, 1024, or 4028 bps, respectively. The maneuver code is 0 if there were no maneuvers during that time period (which can be up to an hour and four minutes starting at the given time), and is 7 if there were any maneuvers during that time. Record length is 78 bytes. The time period covered is from soon after launch through the end of the primary mission, i.e., August 13, 1978 through February 7, 1987. |

5) | ISEE 3 Isotopic Abundance Ratios | |||||||||||||||||
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Resource ID:spase://VEPO/NumericalData/ISEE3/IsotAbun | ||||||||||||||||||

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This data product consists of a single ASCII file containing values and their uncertainties for 32 abundance ratios of various pairs of isotopes of 13 chemical elements (C, O, Ne, Mg, Al, Si, Ti, V, Cr, Mn, Fe, Co, Ni). Between this data product and a companion catalog with isotopic fractions, isotopic composition information is given for 21 chemical elements. The ratios are based on 1978-1981 observations of ~50-500 MeV/n cosmic rays by the U. Chicago cosmic ray experiment on ISEE 3. Each of the ratios is linked in the ASCII file to the publication where its derivation is discussed. |

6) | ISEE 3 Isotopic Fractions | |||||||||||||||||
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Resource ID:spase://VEPO/NumericalData/ISEE3/IsotFrac | ||||||||||||||||||

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This data product consists of a single ASCII file containing values and their uncertainties for isotopic fractions of 56 specific isotopes relative to isotope-integrated elemental abundances, for 15 elements (Be, B, N, S, Cl, Ar, K, Ca, Ti, V, Cr, Mn, Fe, Co, Ni). Between this data product and a companion product with isotopic abundance ratios, isotopic composition information is given for 21 chemical elements. The fractions are based on 1978-1981 observations of ~50-500 MeV/n cosmic rays by the U. Chicago cosmic ray experiment on ISEE 3. Each of the ratios is linked in the ASCII file to the publication where its derivation is discussed. |

7) | ISEE 3 0.167-s magnetic field data | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/ISEE3/MAG/PT0.167S | ||||||||||||||||||

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ISEE 3 0.167-s magnetic field data, g-zipped ASCII, 6-hr files, deep tail through comet GZ encounter orbit phases |

8) | ISEE 3 (ICE) 1-m deep space magnetic field data | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/ISEE3/MAG/PT1M | ||||||||||||||||||

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ISEE 3 (ICE) 1-m magnetic field data, monthly ASCII files, deep space orbit phases 1984-1990 |

9) | ISEE 3 2-m merged magnetic field and plasma data | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/ISEE3/MAG/PT2M | ||||||||||||||||||

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ISEE 3 2-m merged magnetic field and plasma data, annual ASCII files, L1 orbit phase 1978-1982 (plasma data only to 1980.02.19) |

10) | ISEE 3 field and plasma data propagated to (17,0,0) Re | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/ISEE3/MAG_SWP/ISEE3/MAG/PT1M | ||||||||||||||||||

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This is a family of data sets containing 1-min resolution ISEE 3 magnetic field and plasma parameters, in GSE and GSM coordinates, both at the location of the ISEE 3 spacecraft and as propagated to the location (17,0,0) Re, GSE. Data taken when the spacecraft was inside the Spreiter et al (1966) model bow shock were excluded. Propagation was done by J. Weygand using software provided by D. Weimer. The software determines normal directions to assumed planar phase fronts using a modified minimum variance analysis of 1-min magnetic field data, and propagates data using these normals and the ISEE3-observed solar wind flow velocity. Magnetic field data consist of three Cartesian components, while plasma data consist of three Cartesian components of the flow velocity vector plus proton density and temperature. Different subdirectories hold data for unique combinations of field vs. plasma parameters, GSE vs. GSM coordinates, and unpropagated vs. propagated data. See the VMO interface for a more detailed breakout. |

11) | ISEE-3 Radio Mapping Experiment Demodulated - 1.5 sec resolution | |||||||||||||||||
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Resource ID:spase://VWO/NumericalData/ISEE3/RadioMapping/DEMOD.PT1.5S | ||||||||||||||||||

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The following is extracted from "User Guide for ISEE-3 Radio Mapping Experiment CD-ROM Data" the original document is available via the Information URL below. The ISEE-3 Radio Mapping Experiment is designed to detect and measure radio bursts from the Sun, the interplanetary medium, and the Earth's magnetosphere, at frequencies from 30 kHz to 2 MHz. It is a collaboration of the Observatory of Paris-Meudon and the Goddard Space Flight Center; the Principal Investigator is Jean-Louis Steinberg. The experiment determines the direction of sources and estimates their apparent angular sizes using two dipole antennas. One dipole, the shorter of the two, is along the spin axis of the satellite, while the second dipole is perpendicular to the spin axis and is therefore carried around by the rotation of the satellite. Each of the monopoles making up the spin-axis dipole can be extended to 7m, whereas each monopole making up the dipole in the spin plane is 45m long. The signal received by the spinning dipole is modulated, being strongest when the dipole is perpendicular to the direction of the source. The phase of the spin modulation provides information on the direction of the source, projected onto the plane in which the dipole is spinning, and the amplitude of the modulation determines the angular size of the source as a function of its elevation above or below the spin plane. The additional information provided by the spin-axis dipole helps determine whether the source is above or below the spin plane, and its elevation. Detailed Description of the Data Acquisition The experiment is designed to make a series of measurements at each frequency (listed in Table 2-1), covering one-half spin. Such a series is called a step. The specifics of the data are described below. In this document, the spin-axis dipole is called the Z-dipole, because the spin axis is labeled the z-axis of the satellite-based coordinate system. The other dipole is called the S-dipole, because it is spinning. ISEE-3 has two spinning dipoles, called U and V. Only the V dipole was used to acquire radio data. Table 2-1. ISEE-3 Radio Mapping Experiment Frequencies +------------------------------------+ | Channel | Receiver Freq. (Khz) | | No. | Broad | Narrow | |===========|=========|==============| | 1 |1980 | 1000 | | 2 |1000 | 466 | | 3 | 513 | 290 | | 4 | 360 | 188 | | 5 | 233 | 145 | | 6 | 160 | 110 | | 7 | 123 | 80 | | 8 | 94 | 66 | | 9 | 72 | 56 | | 10 | 60 | 47 | | 11 | 50 | 36 | | 12 | 41 | 30 | +------------------------------------+ Demodulating the data The direction to the source and the source strength are determined from the spin-modulated S samples and the Z sample by the procedure described in the following section. The linear least-squares solution provides a despun source amplitude A, which is its maximum amplitude, observed when the S dipole is "broadside" to the source, the azimuth angle with respect to the Sun of the source center in the spin plane, and a measure of the modulation of the source due to the changing orientation of the S dipole, called alpha. The standard deviation of the least-squares fit and the uncertainties in the three parameters are also calculated. Comparison of the Z sample and A with the modulation index alpha permits to evaluate the source radius and its elevation from the spin plane. Data file contents There are 3 different sets of data files that are of potential interest to new users - 1.5 sec modulated data, 108 second averages, and 1.5 sec demodulated data. The 1.5 sec modulated data files contain individual data samples, calibrated in units of antenna temperature. The spin modulation has not been removed from these files. The 108 sec average files are simple averages of the 1.5 sec modulated data as a function of frequency. (Note that the average is done in log space, I.e., mean(log(antenna temperature)).) Finally, the 1.5 sec demodulated data file contains the parameters A, alpha, and azimuth. The demodulated data file is the file that most users will want to use. Contents of the ISEE-3 Radio 1.5 sec DEMOD Record +--------------------------------------------------------------------+ | VARIABLE | DIM| # | DESCRIPTION | |==========|====|=======|============================================| |MDATE | | |Julian date of record (YYDDD) | |MHMS | | |Time of midpoint of record in hhmmss | |MSEC | | |Time of midpoint or record in msecs | |NFREQ | | |Frequency channel 1-12 | |ADSP |4 |1 |Despun SB amplitude (or SN for Mode3) | | |2 | |Despun SN amplitude if mode 1 | | |3 | |Log of SB as log TA | | |4 | |Log SN if mode 1, else 0 | |ALPHA |2 |1 |Modulation Index for B(or N if mode3) | | | |2 |Modulation Index for N if mode 1, else 0 | |PHI |2 | |Source longitude(increasing to west of sun) | | | | |for B, N in degrees (-90 - 90) | |Z |4 | |Average Z amplitude - elements as for ADSP | |PHASE |2 | |Phase(volts) for the first input record used| | | | |in group for B, N(or both B for mode 2, both| | | | |N for mode 3) | |PHANG |2 | |Phase sun angle for B,N in radians | |ELEV |2 | |Calculated elevation angle for B,N | |RAD |2 | |Calculated source radius for B,N in degrees | |BW |4 |1 |Background value used for SB in calculating | | | | |ELEV and RAD | | | |2 |Background value used for SN (mode 1) | | | |3 |Background value used for ZB | | | |4 |Background value for ZN if mode 1 | |ST |2 | |Fractional standard deviations of least | | | | |squares fit for B,N | |SIGA |3x2 | |Uncertainties in parameters for least | | | | |squares fit | | | |1x |Uncertainty in mean SB, SN amplitude | | | |2x |Uncertainty in alpha for B,N | | | |3x |Uncertainty in PHI for B, N in degrees | |NSAMP | | |Number of S samples in fit | |IQUAL |2 | |Quality of analysis B, N | |KDATE | | |Julian date of processing | |MODE | | |Data mode | |SPINP | | |Spin period in msec | |GSE |3 | |XYZ coordinates Geocentric solar ecliptic | | | | |in meters | |SPARE |10 | |Spares | +--------------------------------------------------------------------+ |

12) | ISEE 3 Electron Moments Noramlized Hourly Averages | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/ISEE3/SWIC/Normalized/PT1H | ||||||||||||||||||

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This data set contains ISEE 3 electron moments in the solar wind, normalized and in 1-hour resolution, from the LANL Solar Wind Plasma experiment. The data are electron-based and have been corrected and normalized to existing ion data. Each logical record contains the date (YYMMDD), the universal time (HRMIN), the spacecraft position in GSE coordinates in earth radii, the electron density (1/cm**3) normalized to the ion data, for dates 780816 - 821016, the bulk speed (km/s), and the electron temperature (K). Although the bulk parameters given are reliable, standard errors associated with them are higher for electrons than for ions. A few "bad" points remain on the tape. Densities less than .01/cm**3 and velocities less than 100 km/s should be considered erroneous. Each file contains data for a whole year. |

13) | ISEE 3 Electron Moments | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/ISEE3/SWIC/PT168.00S | ||||||||||||||||||

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ISEE 3 solar wind electron moments - density, bulk flow speed, bulk flow azimuth, minimum total temperature (Tper), maximum total temperature (Tpar,) azimuth of the maximum temperature, heat flux, and the heat flux azimuth - at 168-sec resolution from geocentric and deep-space orbit phases |

14) | ISEE 3 Electron Moments hourly averages | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/ISEE3/SWIC/PT1H | ||||||||||||||||||

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This data set was generated at NSSDC by making one-hour averages of the ISEE 3 Solar Wind Electron Moments in 168 second resolution. There were no time shifts used in creating these hourly averages. Each data file contains data for one year. Data coverage runs from 1982/02/01 through 1992/06/13. There is a data gap from 16 October 1982 to 23 December 1983, corresponding to the geotail phase of the mission. Data parameters (hourly averages) are: electron density, bulk flow speed, bulk flow azimuth, minimum total temperature (Tper), maximum total temperature (Tpar), azimuth of maximum temperature, heat flux, and the heat flux azimuth. There is no spacecraft position information in this data set. The normalized 1-hr data set, however, does include the spacecraft position. Hourly ephemeris data are available online for the time period from soon after launch through the end of the primary mission, i.e., from August 13, 1978 through February 7, 1987. See the data set "isee3_dp_ephem.asc" and its description "aareadme_isee3_dp_ephem" in the directory at ftp://nssdcftp.gsfc.nasa.gov/spacecraft_data/isee/isee3/traj/hourly_magnetospheric. There is also a trajectory data set with one point per day for the ICE phase of the mission: 1984 - 1997. Its documentation can be found at ftp://nssdcftp.gsfc.nasa.gov/spacecraft_data/isee/isee3/traj/daily/icetrjdy_fmt.txt and the data set itself is at ftp://nssdcftp.gsfc.nasa.gov/spacecraft_data/isee/isee3/traj/daily/icetrja.asc. |

15) | ISEE 3 24-s ion plasma data | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/ISEE3/SWP/PT24S | ||||||||||||||||||

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ISEE 3 24-s ion plasma data, L1 orbit phase 1978-1980 |

16) | ISEE-3 Linearly Interpolated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/ISEE3/MAG/Processed/GSE/PT60S | ||||||||||||||||||

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ISEE-3 linearly interpolated to have the measurements on the minute at 60 s resolution tri-axial fluxgate magnetometer data in GSE coordinates. This data set consists of processed solar wind data that has been linearly interpolated to 1 min resolution at the position of the spacecraft using the interp1.m function in MATLAB. 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 and cross correlation studies on solar wind. |

17) | ISEE-3 Linearly Interpolated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSM Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/ISEE3/MAG/Processed/GSM/PT60S | ||||||||||||||||||

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ISEE-3 linearly interpolated to have the measurements on the minute at 60 s resolution tri-axial fluxgate magnetometer data in GSM coordinates. This data set consists of processed solar wind data that has been linearly interpolated to 1 min resolution at the position of the spacecraft using the interp1.m function in MATLAB. 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 and cross correlation studies on solar wind. |

18) | ISEE-3 Weimer Propagated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/ISEE3/MAG/Propagated.SWP/GSE/PT60S | ||||||||||||||||||

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ISEE-3 Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution tri-axial fluxgate magnetometer data in GSE 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. |

19) | ISEE-3 Weimer Propagated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSM Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/ISEE3/MAG/Propagated.SWP/GSM/PT60S | ||||||||||||||||||

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ISEE-3 Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution tri-axial fluxgate magnetometer 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. |

20) | ISEE-3 Linearly Interpolated 60 s Resolution Solar Wind Plasma data in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/ISEE3/SWP/Processed/GSE/PT60S | ||||||||||||||||||

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ISEE-3 linearly interpolated to have the measurements on the minute at 60 s resolution solar wind plasma data in GSE coordinates. This data set consists of processed solar wind data that has been linearly interpolated to 1 min resolution at the position of the spacecraft using the interp1.m function in MATLAB. 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 and cross correlation studies on solar wind. |

21) | ISEE-3 Linearly Interpolated 60 s Resolution Solar Wind Plasma data in GSM Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/ISEE3/SWP/Processed/GSM/PT60S | ||||||||||||||||||

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ISEE-3 linearly interpolated to have the measurements on the minute at 60 s resolution solar wind plasma data in GSM coordinates. This data set consists of processed solar wind data that has been linearly interpolated to 1 min resolution at the position of the spacecraft using the interp1.m function in MATLAB. 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 and cross correlation studies on solar wind. |

22) | ISEE-3 Solar Wind Plasma Weimer Propagated 60 s Resolution in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/ISEE3/SWP/Propagated.SWP/GSE/PT60S | ||||||||||||||||||

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ISEE-3 Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution solar wind plasma data in GSE 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. |

23) | ISEE-3 Solar Wind Plasma Weimer Propagated 60 s Resolution in GSM Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/ISEE3/SWP/Propagated.SWP/GSM/PT60S | ||||||||||||||||||

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ISEE-3 Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution solar wind plasma 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. |

24) | ISEE-3 Solar Wind Weimer Propagation Details at 1 min Resolution | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/ISEE3/TAP/Propagated.SWP/GSE/PT60S | ||||||||||||||||||

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ISEE-3 Weimer propagated solar wind data and linearly interpolated time delay, cosine angle, and goodness information of propagated data at 1 min Resolution. 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. |

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