{ "Spase": { "xmlns": "http://www.spase-group.org/data/schema", "xmlns:xsi": "http://www.w3.org/2001/XMLSchema-instance", "xsi:schemaLocation": "http://www.spase-group.org/data/schema http://www.spase-group.org/data/schema/spase-2_2_9.xsd", "Version": "2.2.9", "NumericalData": { "ResourceID": "spase://NASA/NumericalData/LANL/Avg/ESP/P1D", "ResourceHeader": { "ResourceName": "LANL-GEO ESP Differential Log-Flux Daily Avg.", "AlternateName": "Los Alamos National Laboratory (LANL)-GEOsynchronous (GEO) Energetic Spectrometer for Particles (ESP) Log (base 10) Differential Flux (Particles/(cm^2)/s/keV/steradian) Daily Avg. (of available satellite data)", "ReleaseDate": "2020-07-07T21:14:45Z", "Description": "Daily-averaged electron fluxes from the Los Alamos National Laboratory (LANL) Energetic Spectrometer for Particles (ESP) Daily averages from each geosynchronous satellite available on any given day were merged into a single, uniform daily average. Data span 22 September, 1989 through 31 December, 2009. Data are log(flux) with flux in units of electrons /(cm^2.s.sr.keV) [see t 2010JA015735 _LANL_Data_and_Processing for details]", "Acknowledgement": "Reeves, G. D., S. K. Morley, R. H. W. Friedel, M. G. Henderson, T. E. Cayton, G. Cunningham, J. B. Blake, R. A. Christensen, and D. Thomsen (2011), On the relationship between relativistic electron flux and solar wind velocity: Paulikas and Blake revisited, J. Geophys. Res., 116, A02213, doi:10.1029/2010JA015735.", "Contact": [ { "PersonID": "spase://SMWG/Person/Geoffrey.D.Reeves", "Role": "DataProducer" }, { "PersonID": "spase://SMWG/Person/Steven.Karl.Morley", "Role": "DataProducer" }, { "PersonID": "spase://SMWG/Person/Reiner.Friedel", "Role": "DataProducer" }, { "PersonID": "spase://SMWG/Person/Michael.G.Henderson", "Role": "DataProducer" }, { "PersonID": "spase://SMWG/Person/Thomas.E.Cayton", "Role": "DataProducer" }, { "PersonID": "spase://SMWG/Person/Glenn.F.Cunningham", "Role": "DataProducer" }, { "PersonID": "spase://SMWG/Person/J.Bernard.Blake", "Role": "DataProducer" } ], "InformationURL": [ { "Name": "On the relationship between relativistic electron flux and solar wind velocity: Paulikas and Blake revisited", "URL": "https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2010JA015735", "Description": "Describes the processing performed on the SOPA and ESP data that were included in Reeves et. al, 2011" }, { "Name": "Electronic supplement to \"On the relationship between relativistic electron flux and solar wind velocity: Paulikas and Blake Revisited” ", "URL": "https://agupubs.onlinelibrary.wiley.com/action/downloadSupplement?doi=10.1029%2F2010JA015735&attachmentId=69009962", "Description": "Detailed information concerning instruments used, algorithm, and the resulting caveats of usage for data set." }, { "Name": "2010ja015735-readme.txt", "URL": "https://agupubs.onlinelibrary.wiley.com/action/downloadSupplement?doi=10.1029%2F2010JA015735&attachmentId=69009961", "Description": "Readme file with basic information on processing performed." } ], "PriorID": [ "spase://ViRBO/NumericalData/LANL/ESP/P1D", "spase://VSPO/NumericalData/LANL/Avg/ESP/P1D" ] }, "AccessInformation": { "RepositoryID": "spase://SMWG/Repository/AGU/JGR", "Availability": "Online", "AccessURL": { "Name": "Download link for daily avg. of log LANL-GEO ESP Diff. Energy Flux", "URL": "https://agupubs.onlinelibrary.wiley.com/action/downloadSupplement?doi=10.1029%2F2010JA015735&attachmentId=69009963", "Description": "Daily-averaged electron fluxes from the Los Alamos National Laboratory (LANL) Energetic Spectrometer for Particles (ESP) Daily averages from each geosynchronous satellite available on any given day were merged into a single, uniform daily average. Data span 22 September, 1989 through 31 December, 2009. Data are log(flux) with flux in units of electrons /(cm^2.s.sr.keV) [see t 2010JA015735 _LANL_Data_and_Processing for details] \n\nNominal energy ranges for each ESP channel are \nE234: 1.8-3.5MeV; \nE56: 3.5-6.0MeV; \nE7: 6.0-7.8MeV;\n\n2.1 Column Date_YYYY-MM-DD Calendar date in YYYY-MM-DD format; \n2.2 Column log(E234), log(flux) ESP channel E234; \n2.3 Column log(E56), log(flux), ESP channel E56; \n2.4 Column log(E7), log(flux), ESP channel E7" }, "Format": "Text", "Encoding": "ASCII", "Acknowledgement": "Reeves, G. D., S. K. Morley, R. H. W. Friedel, M. G. Henderson, T. E. Cayton, G. Cunningham, J. B. Blake, R. A. Christensen, and D. Thomsen (2011), On the relationship between relativistic electron flux and solar wind velocity: Paulikas and Blake revisited, J. Geophys. Res., 116, A02213, doi:10.1029/2010JA015735." }, "ProcessingLevel": "Calibrated", "ProviderResourceName": "Daily-averaged electron fluxes from the Los Alamos National Laboratory (LANL) Energetic Spectrometer for Particles (ESP)", "InstrumentID": [ "spase://SMWG/Instrument/LANL/1989/ESP", "spase://SMWG/Instrument/LANL/1990/ESP", "spase://SMWG/Instrument/LANL/1991/ESP", "spase://SMWG/Instrument/LANL/1994/ESP", "spase://SMWG/Instrument/LANL/97A/ESP", "spase://SMWG/Instrument/LANL/01A/ESP", "spase://SMWG/Instrument/LANL/02A/ESP" ], "MeasurementType": "EnergeticParticles", "TemporalDescription": { "TimeSpan": { "StartDate": "1989-09-22T00:00:00", "StopDate": "2010-01-01T00:00:00" }, "Cadence": "PT24H" }, "ObservedRegion": "Earth.Magnetosphere", "Caveats": "\"There are a number of caveats associated with these data. Primary cosmic rays may account for a substantial fraction of the observed counts. A significant secondary contribution is also implied, however there is currently \nno modeling to suggest to what extent this contributes to the observed \ncounts. Some ESP channels appear to saturate at 4 x 10^4 counts/ s. The \nreported flux levels should not be used as absolute measures: It is known \nthat ESP yields lower fluxes and harder spectra than SOPA, in the region of \noverlap between the detectors. Calculation of spectra, for example, would \nnot be meaningful for this data set – especially as the data are daily averaged \nand merged from several satellites.\" (Electronic supplement to \"On the relationship between relativistic electron flux and solar wind velocity: Paulikas and Blake Revisited”) ", "Parameter": [ { "Name": "Date", "Description": "Date, YYYY-MM-DD", "Cadence": "PT24H", "Support": { "SupportQuantity": "Temporal" } }, { "Name": "log(E234)", "Description": "Base 10 logarithm of the total flux in channels 2, 3, and 4 of the LANL-GEO ESP measurements selected for a day", "Cadence": "PT24H", "Units": "#/cm^2/keV/s/sr", "Particle": { "ParticleType": "Electron", "ParticleQuantity": "NumberFlux", "EnergyRange": { "Low": "1.8", "High": "3.5", "Units": "MeV" } } }, { "Name": "log(E56)", "Description": "Base 10 logarithm of the total flux in channels 5 and 6 of the LANL-GEO ESP measurements selected for a day.", "Cadence": "PT24H", "Units": "#/cm^2/keV/s/sr", "Particle": { "ParticleType": "Electron", "ParticleQuantity": "NumberFlux", "EnergyRange": { "Low": "3.5", "High": "6.0", "Units": "MeV" } } }, { "Name": "log(E56)", "Description": "Base 10 logarithm of the total flux in channel 7 of the LANL-GEO ESP measurements selected for a day.", "Cadence": "PT24H", "Units": "#/cm^2/keV/s/sr", "Particle": { "ParticleType": "Electron", "ParticleQuantity": "NumberFlux", "EnergyRange": { "Low": "6.0", "High": "8.0", "Units": "MeV" } } } ] } } }