Merge Solar_Orbiter modifications

Benjamin Renard
1 parent 876462d7
Showing 6 changed files with 91 additions and 9 deletions Show diff stats
Instrument/CDPP-AMDA/Solar_Orbiter/MAG.xml
Instrument/CDPP-AMDA/Solar_Orbiter/PAS.xml
Instrument/CDPP-AMDA/Solar_Orbiter/RPW.xml
NumericalData/CDPP-AMDA/Solar_Orbiter/PAS/so-pas-l2.3d.xml
NumericalData/CDPP-AMDA/Solar_Orbiter/PAS/so-pas-l2.omni.xml
Person/Milan.Maksimovic.xml
@@ -7,8 +7,39 @@
       <ResourceName>MAG</ResourceName>
       <AlternateName>Magnetometer</AlternateName>
       <ReleaseDate>2018-10-27T18:45:12Z</ReleaseDate>
-      <Description>
-      </Description>
+      <Description>The magnetometer is a unique instrument on Solar Orbiter in that it provides essential 
+information about both the largest scale structures in space around the Sun, as well as the 
+smallest scale kinetic processes in the plasma. Indeed, the magnetic field plays a central role in 
+plasma dynamics since charged particles generally travel along the magnetic field, making it 
+the route from the Sun into space. The accurate measurement of the local magnetic field is 
+therefore central to the scientific success of Solar Orbiter. Magnetometer data are expected to 
+lead to significant advances in our understanding of how the Sun’s magnetic field links into 
+space and evolves over the solar cycle; how particles are accelerated and propagate around the 
+solar system, including to the Earth; and how the corona and solar wind are heated and 
+accelerated, among many others.
+
+The MAG team science objectives include:
+* How does the Sun’s magnetic field link into space?
+* How does the heliospheric magnetic field disconnect from the Sun?
+* How does the Sun’s magnetic field change over time?
+* How is the heliospheric current sheet related to coronal structure?
+* What is the role of ICMEs in the Sun’s magnetic cycle?
+* What is the origin of the slow speed solar wind?
+* What drives the evolution of the solar wind distribution?
+* What are the origins of waves, turbulence and small scale structures?
+* How is turbulent energy dissipated?
+* What are the properties of near-Sun shocks and the fluctuations around them?
+* What is the structure of plasma turbulence and how does it evolve?
+* How do large and small scale structures modulate particle fluxes?
+
+In order to achieve these objectives, the magnetometer will measure the magnetic field 
+continuously with sufficient cadence and precision to quantify fluid-scale phenomena 
+throughout the mission and, in burst mode, with sufficient cadence and precision to study ion 
+kinetic phenomena.
+
+Low latency data are generated at a very low cadence compared to normal magnetometer data 
+and are intended for rapid, broad characterisation of solar wind conditions at the spacecraft 
+location.</Description>
       <Acknowledgement></Acknowledgement>
       <Contact>
         <PersonID>spase://SMWG/Person/Tim.Horbury</PersonID>
@@ -7,8 +7,30 @@
       <ResourceName>PAS</ResourceName>
       <AlternateName>Proton-Alpha Sensor</AlternateName>
       <ReleaseDate>2018-10-27T18:45:12Z</ReleaseDate>
-      <Description>
-      </Description>
+      <Description>The Proton-Alpha Sensor (PAS) is designed to continuously determine the 3D 
+distribution functions of the dominant ions of the solar wind, from 200 eV to 20 KeV, 
+without mass and charge selection. In practice, this concerns mostly the proton and alfa 
+populations. These measurements are used to calculate the density, speed, pressure 
+and temperature tensors of the main component of the solar wind.
+
+At full resolution, PAS measures the 3D ion distribution function, in the form of arrays of 
+96 energies, 11  azimuth angles and 9 elevation angles, in about ~1 second. The 
+energy and the angle of elevation are selected by imposing different high voltages to 
+the electrodes of the deflection system and the electrostatic analyzer. The 11 azimuthal 
+angles correspond to the 11 detectors of the instrument (channeltron’).
+
+In ‘burst‘ mode, the measurement rate can reach up to 20 Hz. The phase space 
+sampling is then reduced, for example by 24 energies and 5 deflections, which allows 
+to increase the time cadence of distribution functions measurements. An algorithm 
+(peak tracking procedure) is used to select the peak of the distribution and to center 
+sampling around this peak.
+
+The different types of sampling are programmed in the form of cyclograms. They define 
+the operation of the instrument over periods of several days. In normal mode, the 
+functions are measured every 4 s with, every 300 s, a short burst mode of 9 s 
+(SnapShot). ‘Long’ burst mode is also acquired every day, consisting in 300 s of 
+continuous sampling at high cadence. The sampling frequency during burst or 
+snapshots is generally of 4 distributions / s (4 Hz analysis).</Description>
       <Acknowledgement></Acknowledgement>
       <Contact>
         <PersonID>spase://SMWG/Person/Philippe.Louarn</PersonID>
@@ -7,7 +7,35 @@
       <ResourceName>RPW</ResourceName>    
       <AlternateName>Plasma Wave Investigation</AlternateName>
       <ReleaseDate>2017-11-27T21:10:13Z</ReleaseDate>
-      <Description/>   
+      <Description>RPW will make key measurements in support of the first three, out of four top-level scientific questions, 
+which drive Solar Orbiter overall science objectives:
+* How and where do the solar wind plasma and magnetic field originate in the corona?
+* How do solar transients drive heliospheric variability?
+* How do solar eruptions produce energetic particle radiation that fills the heliosphere?
+* How does the solar dynamo work and drive connections between the Sun and the heliosphere?
+
+
+Here is the summary of the specific RPW Science Objectives:
+* Solar and Interplanetary Radio Burst: - What is the role of shocks and flares in accelerating particles near the Sun? - How is the Sun connected magnetically to the interplanetary medium? - What are the sources and the global dynamics of eruptive events? - What is the role of ambient medium conditions on particle acceleration and propagation? - How do variations and structure in the solar wind affect low frequency radio wave propagation? 
+* Electron density and temperature measurements with the Quasi-Thermal Noise spectroscopy: - Precise measurement of both the electron density and temperature, with accuracies respectively of a few % and around 10 %, at perihelion. - Study the non-thermal character of the electron distributions at perihelion. 
+* Radio emission processes from electron beams:  Langmuir waves and electromagnetic mode conversion: - Measurements for the first time in the Solar Wind of both the electric and magnetic field waveforms at high time resolution (up to 500 kSs). - Study of the mode conversion from Langmuir to electromagnetic waves. - Study of the energy balance between electron beams, Langmuir waves and e.m. radio waves at several radial distances 
+* Solar wind microphysics and turbulence: - Measure of the waves associated with the plasma instabilities that are generated by temperature anisotropies in the solar wind. - First DC/LF electric field measurements in the inner heliosphere and over a large radial distance in the solar. 
+* Shocks, Reconnection, Current Sheets, and Magnetic Holes: - Identification and study of the reconnection process in current sheets with thickness down to the ion scales and smaller. - Determination of the interplanetary shock structure down to the spatial and temporal scales comparable and smaller than the typical ion scales. - Determination of different particle energisation mechanisms within shocks and reconnection regions. - Distinguish different radio burst generation mechanisms. Interplanetary Dust - Determination, in combination with the EPD instrument, the spatial distribution, mass and dynamics of dust particles in the near-Sun heliosphere, in and out of the ecliptic. 
+
+
+To cover its specific Science Objectives, RPW will measure magnetic and electric fields at high time 
+resolution using a number of sensors, to determine the characteristics of electromagnetic and electrostatic 
+waves in the solar wind. More precisely, RPW will: 
+* Make the first-ever high accuracy, high-sensitivity and low noise measurements of electric fields at low frequencies (below ~1 kHz) in the inner Heliosphere.
+* Measure the magnetic and electric fields of the solar wind turbulence with high sensitivity and dynamic range along the spacecraft trajectory.
+* Store high-resolution data from scientifically interesting regions such as in-situ shock crossings, in-situ Type III events and others.
+* Measure the satellite potential with high temporal resolution permitting to estimate the density fluctuations in the solar wind and allowing higher accuracy particle instrument measurements.
+* Measure the quasi thermal noise and Langmuir waves around the local plasma frequency
+* Measure for the first type the high frequency magnetic counterpart of Langmuir waves associated with in-situ Type III bursts
+* Observe the solar and interplanetary radio burst
+* Observe the radio counterpart of dust particle impacts
+* Detect on-board in-situ shock crossings and store the corresponding data
+* Detect on-board in-situ Type III events and store the corresponding data</Description>  
       <Acknowledgement/>
       <Contact>
         <PersonID>spase://SMWG/Person/Milan.Maksimovic</PersonID>
@@ -83,7 +83,7 @@
             <ParameterKey>pas_l2_2d_elevation</ParameterKey>
             <Description/>
             <Ucd/>
-            <Units>cm^-6 s^-3</Units>
+            <Units>s3 m^-6</Units>
             <RenderingHints>
                 <DisplayType>Spectrogram</DisplayType>
             </RenderingHints>           
@@ -97,7 +97,7 @@
             <ParameterKey>pas_l2_2d_cem</ParameterKey>
             <Description/>
             <Ucd/>
-            <Units>cm^-6 s^-3</Units> 
+            <Units>s3 m^-6</Units> 
             <RenderingHints>
                 <DisplayType>Spectrogram</DisplayType>
             </RenderingHints>             
@@ -111,7 +111,7 @@
             <ParameterKey>pas_l2_2d_energy</ParameterKey>
             <Description/>
             <Ucd/>
-            <Units>cm^-6 s^-3</Units> 
+            <Units>s3 m^-6</Units> 
             <RenderingHints>
                 <DisplayType>Spectrogram</DisplayType>
             </RenderingHints>             
@@ -69,7 +69,7 @@
             <ParameterKey>pas_l2_omni</ParameterKey>
             <Description/>
             <Ucd/>
-            <Units>eV/cm^-2 s^-1 eV^-1</Units>
+            <Units>cm^-2 s^-1 eV/eV</Units>
             <RenderingHints>
                 <DisplayType>Spectrogram</DisplayType>
             </RenderingHints>           
@@ -5,5 +5,6 @@
     <ResourceID>spase://SMWG/Person/Milan.Maksimovic</ResourceID>
     <PersonName>Dr. Milan Maksimovic</PersonName>
     <OrganizationName>Observatoire de Paris-Meudon</OrganizationName>
+    <Email>milan.maksimovic@obspm.fr</Email>
   </Person>
 </Spase>