Fix in Solar Orbiter MAG & RPW descriptions

Benjamin Renard
1 parent da96090a
Showing 2 changed files with 46 additions and 59 deletions Show diff stats
Instrument/CDPP-AMDA/Solar_Orbiter/MAG.xml
Instrument/CDPP-AMDA/Solar_Orbiter/RPW.xml
@@ -7,15 +7,15 @@
       <ResourceName>MAG</ResourceName>
       <AlternateName>Magnetometer</AlternateName>
       <ReleaseDate>2018-10-27T18:45:12Z</ReleaseDate>
-      <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
+      <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:
@@ -32,13 +32,13 @@ The MAG team science objectives include:
 * 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
+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
+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>
@@ -7,59 +7,46 @@
       <ResourceName>RPW</ResourceName>    
       <AlternateName>Plasma Wave Investigation</AlternateName>
       <ReleaseDate>2017-11-27T21:10:13Z</ReleaseDate>
-      <Description>RPW will make key measurements in support of the first three, out of four top-level scientific questions,
+      <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.
+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.
+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
+* 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