From ca6a51b77845d8d38c80c837cf1ef5acc8763a62 Mon Sep 17 00:00:00 2001
From: Benjamin Renard <benjamin.renard@akka.eu>
Date: Tue, 6 Apr 2021 09:18:08 +0200
Subject: [PATCH] Merge Solar_Orbiter modifications
---
Instrument/CDPP-AMDA/Solar_Orbiter/MAG.xml | 35 +++++++++++++++++++++++++++++++++--
Instrument/CDPP-AMDA/Solar_Orbiter/PAS.xml | 26 ++++++++++++++++++++++++--
Instrument/CDPP-AMDA/Solar_Orbiter/RPW.xml | 30 +++++++++++++++++++++++++++++-
NumericalData/CDPP-AMDA/Solar_Orbiter/PAS/so-pas-l2.3d.xml | 6 +++---
NumericalData/CDPP-AMDA/Solar_Orbiter/PAS/so-pas-l2.omni.xml | 2 +-
Person/Milan.Maksimovic.xml | 1 +
6 files changed, 91 insertions(+), 9 deletions(-)
diff --git a/Instrument/CDPP-AMDA/Solar_Orbiter/MAG.xml b/Instrument/CDPP-AMDA/Solar_Orbiter/MAG.xml
index f36b275..7b51b7a 100644
--- a/Instrument/CDPP-AMDA/Solar_Orbiter/MAG.xml
+++ b/Instrument/CDPP-AMDA/Solar_Orbiter/MAG.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>
diff --git a/Instrument/CDPP-AMDA/Solar_Orbiter/PAS.xml b/Instrument/CDPP-AMDA/Solar_Orbiter/PAS.xml
index d549b84..9d1fcfb 100644
--- a/Instrument/CDPP-AMDA/Solar_Orbiter/PAS.xml
+++ b/Instrument/CDPP-AMDA/Solar_Orbiter/PAS.xml
@@ -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>
diff --git a/Instrument/CDPP-AMDA/Solar_Orbiter/RPW.xml b/Instrument/CDPP-AMDA/Solar_Orbiter/RPW.xml
index 5d6c7de..b8243fb 100644
--- a/Instrument/CDPP-AMDA/Solar_Orbiter/RPW.xml
+++ b/Instrument/CDPP-AMDA/Solar_Orbiter/RPW.xml
@@ -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>
diff --git a/NumericalData/CDPP-AMDA/Solar_Orbiter/PAS/so-pas-l2.3d.xml b/NumericalData/CDPP-AMDA/Solar_Orbiter/PAS/so-pas-l2.3d.xml
index 2b2d273..098a59e 100644
--- a/NumericalData/CDPP-AMDA/Solar_Orbiter/PAS/so-pas-l2.3d.xml
+++ b/NumericalData/CDPP-AMDA/Solar_Orbiter/PAS/so-pas-l2.3d.xml
@@ -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>
diff --git a/NumericalData/CDPP-AMDA/Solar_Orbiter/PAS/so-pas-l2.omni.xml b/NumericalData/CDPP-AMDA/Solar_Orbiter/PAS/so-pas-l2.omni.xml
index acce66c..a86de5c 100644
--- a/NumericalData/CDPP-AMDA/Solar_Orbiter/PAS/so-pas-l2.omni.xml
+++ b/NumericalData/CDPP-AMDA/Solar_Orbiter/PAS/so-pas-l2.omni.xml
@@ -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>
diff --git a/Person/Milan.Maksimovic.xml b/Person/Milan.Maksimovic.xml
index d75290d..88b3fea 100644
--- a/Person/Milan.Maksimovic.xml
+++ b/Person/Milan.Maksimovic.xml
@@ -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>
--
libgit2 0.21.2