LFR Wiki¶

• Table of contents
• LFR Wiki
• Introduction
  • Context
  • Equipment Overview
  • Scientific Objectives and Performances
  • Instrument Description
    • Functional Description
    • Hardware Description
      • Figure 1 LFR Block Diagram
• Links
  • RPW
  • Solar Orbiter
  • RPW Contributors

Child pages:

• A3PEModulePinout
• Calibrations
  • PFM Calibrations
  • SPARE Calibrations
• Pictures
  • RTAX Prototyping
• Schematics

Introduction¶

Context¶

The Laboratory of Plasma Physics(LPP) is in charge of providing the Low Frequency Receiver(LFR) as a part of the Radio & Plasma Waves(RPW) instrument which will be embedded in Solar Orbiter probe. Solar Orbiter launch window is set to October 2018.

Equipment Overview¶

The LFR instrument is designed to produce and transmit waveforms (WF), averaged spectral matrices (ASM) and basic parameters (BP) from LF electromagnetic data (quasi DC-10kHz). The electric field data are provided by the electric antennas (ANT) and by the entity that controls their operation (BIAS). The magnetic field data are coming from the searchcoil magnetometer (SCM).
The LFR board will also have a special area reserved to the SCM Heater circuitry. LFR will monitor its own temperature and the temperature of the SCM. It will generate a calibration signal for the SCM.

Scientific Objectives and Performances¶

The science objective of LFR is the study of the electromagnetic wave activity in the extended corona and the solar wind, from a fraction of a Hertz to about 10 kHz, which should cover the electron gyrofrequency and most of the Doppler-shifted frequencies of the low frequency plasma waves. The main waves to be observed in this frequency range are thus kinetic or inertial Alfven waves, ion cyclotron waves, ion acoustic waves, and magnetosonic or whistler mode waves. Their characterization and the determination of their respective role in heating and accelerating the solar wind during its expansion is the main scientific issue addressed by LFR. Another important subject for LFR is the study of the low frequency plasma waves associated to solar wind disturbances, as for instance interplanetary shocks.
Characterizing the low frequency waves in the solar wind involves the capability of the LFR to distinguish solitary waves from broadband wave activity, to cover turbulence and plasma instabilities, to identify the wave modes at work. Performing a multi-component analysis of the data is thus mandatory, using either a classical Fourier analysis or another treatment of the waveforms more appropriate to turbulence analysis.
Given the limitations in the telemetry, it is necessary to implement specific techniques to take the maximum advantage of the data. The LFR is tailored to optimize the scientific return of the data. The LFR design gives the possibility of mixing different types of output data, from low-level processed data (waveform data) to high-level processed data (averaged spectral matrices and their derived parameters), with various data rate possibilities (continuous or cyclic transmission, adaptable frequency bandwidth as well as adaptable frequency and time resolutions). The scientific added value stems from the choice of the most relevant combination of the different data to be transmitted, according to the RPW Science Requirements Document (RD3). A number of predefined working modes will be defined, but it will also be possible to define other working modes in flight.

Instrument Description¶

Functional Description¶

The main functions of LFR are the following:

• Selection of 8 analog channels among 11 available.
• Sampling of 8 analog channels continuously at f0 = 24576 Hz (this includes analog anti-aliasing filtering, sampling at fs = 98304 Hz, digital anti-aliasing filtering and down-sampling at f0).
• Processing of the 8 data streams and transmission of the products to the DPU through a SpaceWire link.
• Monitoring of one SCM temperature and two LFR temperatures.
• Generation of a calibration signal for the SCM.
• Providing a reserved area on the LFR board for the SCM heater command system (design done by LPC2E, Orléans).

Hardware Description¶

LFR will be implemented on one PCB card inside the MEB. The block diagram is shown on Figure 1 . The LFR hardware can be divided into 3 main blocks: the analog part, the digital part and the SCM Heater part. This third part implements the means to command the SCM heating system. The design of this part is not under the responsibility of the LFR team which will only provide room for the SCM heating command board.
LFR has 11 analogue channels:

• 5 from BIAS (BIAS_1, BIAS_2, BIAS_3, BIAS_4 and BIAS_5)
• 3 from HF preamplifiers (VHF_1, VHF_2, VHF_3)
• 3 from SCM (SCM_1, SCM_2, SCM3)

LFR will digitize 8 signals among these 11 signals. The routing strategy is based on two main configurations named BIAS_WORKS and BIAS_FAILS. Whatever the configuration, the three channels coming from SCM are digitized.

The LFR analog part implements:

• The means to filter and route the 11 analog inputs. Several switches steered by the digital part allow the commutation between the BIAS_WORKS and BIAS_FAILS configurations. 8 ADCs sample continuously the selected analog channels and the data are sent to the digital part.
• The means to select and condition housekeeping data (1 temperature probe on the SCM and 2 temperature probes and the LFR).
• The means to generate a calibration signal for the SCM.
• The power supply regulation.
• The 3V voltage reference.

The digital part implements:

• An Actel RTAX4000D FPGA, more details here.
• LVDS interfaces for the SpaceWire link to the DPU.
• Memories for the FPGA.

Figure 1 LFR Block Diagram¶

All clock signals are derived by the FPGA logic using frequency division from two master clock frequencies generated by crystal oscillators at 50 MHz and 49.152 MHz (Figure 2). The following clock frequencies will be used on LFR:

• 25 MHz => Leon3, RAMs, AMBA bus, all other VHDL modules described in the next section
• 10 MHz => SpaceWire
• 98304 Hz => Sampling clock of the ADCs (8 main channels)

Links¶

RPW¶

LESIA's RPW website
CNES's RPW page

Solar Orbiter¶

CNES
ESA

RPW Contributors¶

RPW, LESIA
Search Coil Magnetometer(SCM), LPCEE
Time Domain Sampler(TDS), IAP
BIAS, IRF
Digital Processing Unit(RPW-DPU), IWF
Thermal Noise Receiver & High Frequency Receiver(TNR-HFR), LESIA
RPW-DPU onboard Software, LESIA