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NumericalData/CDPP-AMDA/Solar_Orbiter/EPD/so-ept-e.north.xml 5.54 KB
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<?xml version="1.0" encoding="UTF-8"?>
<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_3_0.xsd">
   <Version>2.3.0</Version>
   <NumericalData>
      <ResourceID>spase://CNES/NumericalData/CDPP-AMDA/Solar_Orbiter/EPD/so-ept-e.north</ResourceID>
      <ResourceHeader>
          <ResourceName>southward flow</ResourceName>
          <AlternateName>Electron Flux From North Ecliptic Hemisphere Direction</AlternateName>      
          <ReleaseDate>2019-11-12T10:48:29Z</ReleaseDate>
          <Description>Solar Orbiter, Level 2 Data, Energetic Particle Detector, Electron and Proton Telescope, Rates. 
              
            EPT  measures electrons and ions in the lower part of the energetic particle spectrum. It 
effectuates measurements in 4 different fields of view :

* Anti-Sunward Flow. Detector looks in the direction of the mean Parker spiral towards the Sun.
* Sunward Flow. Detector looks opposite to the Sun direction.
* Northward Flow. Detector looks towards the south ecliptic hemisphere.
* Southward Flow. Detector looks towards the north ecliptic hemisphere.

Parameter ID uses Detector looking directon.

Additionally, EPT has 2 channels that separate electrons and ions:
* Magnet channel. Uses a permanent magnet to deflect electrons. It measures protons with energies between 25 keV and 6.5 MeV and alpha particles up to 25 MeV.
* Foil channel. Equipped with a foil that absorbs ions, it measures electrons in the energy range 25–500 keV. Ions with energies above 400 keV can penetrate the foil, contaminating the electron measurements. 
          </Description>
          <Acknowledgement>See http://espada.uah.es/epd/EPD_data.php</Acknowledgement>
         <Contact>
             <PersonID>spase://CDPP/Person/J.Rodrigues-Pacheco</PersonID>
           <Role>PrincipalInvestigator</Role>
         </Contact>         
          <InformationURL>
              <Name>SolO Archive Support Data</Name>
              <URL>https://issues.cosmos.esa.int/solarorbiterwiki/display/SOSP/Archive+Support+Data</URL>
              <Description></Description>
          </InformationURL> 
          <Association>
                <AssociationID>solo-epd-eptel</AssociationID>
                <AssociationType>PartOf</AssociationType>
                <Note>L2 : electron flux</Note>
            </Association>         
      </ResourceHeader>
      <AccessInformation>
         <RepositoryID>spase://SMWG/Repository/CNES/CDPP-AMDA</RepositoryID>
         <Availability>Online</Availability>
         <AccessRights>Open</AccessRights>
         <AccessURL>
            <Name>AMDA at CDPP</Name>
            <URL>http://amda.cdpp.eu</URL>
         </AccessURL>
         <Format>Text</Format>
         <Acknowledgement>
                AMDA is a science analysis system provided by the Centre de Donnees de la 
                Physique des Plasmas (CDPP) supported by CNRS, CNES, Observatoire de Paris and 
                Universite Paul Sabatier, Toulouse
         </Acknowledgement>
      </AccessInformation>
       <ProviderName>http://soar.esac.esa.int/soar</ProviderName> 
       <ProviderResourceName>EPD-EPT-SUN-RATES</ProviderResourceName>
       <ProviderAcknowlegment></ProviderAcknowlegment>
      <InstrumentID>spase://CNES/Instrument/CDPP-AMDA/Solar_Orbiter/EPD-EPT</InstrumentID>
      <MeasurementType>EnergeticParticles</MeasurementType>
      <TemporalDescription>
         <TimeSpan>
            <StartDate>2018-09-02T00:00:12Z</StartDate>
            <StopDate>2025-08-12T23:59:55Z</StopDate>
         </TimeSpan>
         <CadenceMin>PT60S</CadenceMin>
         <CadenceMax>PT300S</CadenceMax> 
      </TemporalDescription>      
      <ObservedRegion>Heliosphere.Inner</ObservedRegion>
      <ObservedRegion>Sun.Corona</ObservedRegion>
       <Caveats>Ions with energies around 500 keV can penetrate the foil and give a signal in the electron
           channel. In the presence of high ion flux, there could be a considerable contamination from ions in this product.</Caveats>
      <Parameter>
         <Name>el flux: southward</Name>
         <ParameterKey>solo_ept_north_eflux</ParameterKey>
         <Description>Particle flux in foil channel</Description>
         <Ucd/>
          <Units>1/(s cm^2 sr MeV)</Units>
         <UnitsConversion/>        
         <RenderingHints>
              <DisplayType>Spectrogram</DisplayType>
         </RenderingHints>
         <Structure>
            <Size>34</Size>
         </Structure>         
      </Parameter>
       <Parameter>
         <Name>el flux unc: southward</Name>
         <ParameterKey>solo_ept_north_eunc</ParameterKey>
         <Description>Uncertainty in electron flux</Description>
         <Ucd/>
          <Units>1/(s cm^2 sr MeV)</Units>
         <UnitsConversion/>        
         <RenderingHints>
              <DisplayType>Spectrogram</DisplayType>
         </RenderingHints>
         <Structure>
            <Size>34</Size>
         </Structure>         
      </Parameter>
       <Parameter>
           <Name>el cntrate: southward</Name>
           <ParameterKey>solo_ept_north_erate</ParameterKey>
           <Description>Particle count rate in foil channel</Description>
           <Ucd/>
           <Units>cnts/s</Units>
           <UnitsConversion/>        
           <RenderingHints>
               <DisplayType>Spectrogram</DisplayType>
           </RenderingHints>
           <Structure>
               <Size>34</Size>
           </Structure>         
       </Parameter>
</NumericalData>
</Spase>