2.7.1 https://spdx.org/licenses/ SPDX CC0-1.0 https://spdx.org/licenses/CC0-1.0.html Creative Commons Zero v1.0 Universal CC0 1.0 Universal is the Creative Commons license applicable to all publicly available SPASE metadata descriptions spase://NASA/NumericalData/Weygand/Geotail/LEP/Propagated.LEP/GSE/PT60S NASA NumericalData Geotail Low Energy Particle (LEP) experiment data Weimer Propagated 60 s Resolution in GSE Coordinates Geotail LEP data https://doi.org/10.21978/p8fk8q 2025-12-04T13:32:44Z 2021-05-31T12:34:56.789 Updated to SPASE Version 2.3.2 if needed, Applied quality control for DOI usage, LFB 2025-08-05T13:12:56Z Added ObservedRegion(s). Changed http to https in top-level schemaLocation attribute. Fixed version number separator in top-level schemaLocation attribute. Matched version number in schemaLocation attribute to value in Version tag. ZCB 2025-12-04T13:32:44Z Added MetadataRightsList. Added ResourceType and NamingAuthority. Updated to 2.7.1. ZCB Geotail LEP Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution 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. Toshifumi Mukai;The Institute of Space and Astronautical Science Weygand, James M.; & McPherron, Robert L. 2006-01-01T00:00:00 University of California, Los Angeles spase://SMWG/Person/Toshifumi.Mukai PrincipalInvestigator spase://SMWG/Person/James.M.Weygand MetadataContact LEP experiment https://pwg.gsfc.nasa.gov/istp/geotail/geotail_inst.html LEP information LEP experiment https://www.stp.isas.jaxa.jp/geotail/QL/index.html LEP quicklook LEP experiment https://darts.isas.jaxa.jp/stp/geotail/caveats.html#lep LEP information Solar Wind Propagation Information http://www.igpp.ucla.edu/jweygand/htmls/Propagated_SW.html Solar wind archive at UCLA. This archive provides a list of available data resources and available time ranges. spase://VMO/NumericalData/Weygand/Geotail/LEP/Propagated.LEP/GSE/PT60S spase://VSPO/NumericalData/Geotail/CPI-MGF-LEP/PT1M spase://VSPO/NumericalData/Weygand/Geotail/LEP/Propagated.LEP/GSE/PT60S spase://SMWG/Repository/UCLA/VMO Online Open IGPP UCLA Geotail LEP Data JMW Processed Archive http://vmo.igpp.ucla.edu/data1/Weygand/PropagatedSolarWindGSE/weimer/Geotail/lep_lep/ Text ASCII Uncalibrated Geotail Low Energy Particle experiment Level-0 spase://SMWG/Instrument/Geotail/LEP ThermalPlasma 1993-10-01T00:00:00.000 -P1Y Time format in data files is: Day Month Year Hour Minute Second (DD MM YYYY HH MM SS.SSS) Earth.Magnetosheath Heliosphere.NearEarth 1 min solar wind magnetotail bow shock magnetopause plasma data LEP Propagated solar wind data Geotail Universal Time Time Universal Time AFTER Propagation columns from left to right are: day month year hour minute sec in the format of dd mm yyyy hh mm ss. PT60S 6 Universal Time expressed using a 6-column day, month, year, hour, minute, second representation Day 1 Day Month 2 Month Year 3 Year Hour 4 Hour Minute 5 Minute Second 6 Second Temporal Geotail LEP Thermal Speed Weimer Propagated 1 min Resolution Data in GSE Coordiates Thermal Speed Weimer propagated Geotail LEP thermal speed in GSE coordinates in units of km/s. Be sure you understand the instrument PT60S KM/S Ion ThermalSpeed Geotail LEP Density Weimer Propagated 1 min Resolution Data in GSE Coordiates Density Weimer propagated density data for Geotail LEP in GSE coordinates in units of number per cubic centimeter. PT60S #/cm^-3 Ion NumberDensity Geotail LEP Velocity Vector Weimer Propagated 1 min Resolution Data in GSE Coordiates Velocity Vectors Weimer propagated Flow vector for Geotail LEP in GSE coordinates in units of km/s. Be sure you understand the instrument PT60S KM/S Cartesian GSE 3 VX-GSE Component.I 1 pvxgse VY-GSE Component.J 2 pvygse VZ-GSE Component.K 3 pvzgse Ion Velocity Geotail Spacecraft Weimer Propagated Position Vector Interpolated to 1 min Resolution in GSE Coordiates Position Vectors Weimer propagated location of the spacecraft in GSE coordinates in units of Re. PT60S Re Cartesian GSE 3 X-GSE Component.I 1 pxgse Y-GSE Component.J 2 pygse Z-GSE Component.K 3 pzgse Positional