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Radio Plasma Imager (RPI)

ResourceID
spase://SMWG/Instrument/IMAGE/RPI

Description

The main science objective of the Radio Plasma Imager (RPI) was to characterize plasma in the Earth's magnetosphere utilizing imaging in the radio frequency range.

The RPI on the IMAGE spacecraft was a pioneering instrument designed as a low frequency (3 kHz to 3 MHz) long-range magnetospheric radio sounder, relaxation sounder, and a passive plasma wave instrument. RPI was a highly flexible instrument capable of being programmed to perform these types of measurements at times when IMAGE was located in key regions of the magnetosphere. For the remote sensing, RPI transmitted coded electromagnetic waves and used digital pulse compression and spectral integration to isolate the resulting echoes.

The RPI instrument consisted of an electronics unit, four 250-m wire antennas with antenna tuners, and a z-axis antenna with two 10-m lattice booms. RPI used the x axis antennas for all transmissions while echo reception was accomplished on all three. The x-axis dipole antenna was 500 m tip-to-tip at the beginning of the mission but was shortened to 370 m when it apparently collided with a micrometeoroid or orbital debris on 03 October 2000. The Y antenna suffered similar damage to its -Y segment 11 on August 2002 and complete loss of its +Y segment on 30 September 2004.

RPI was capable of detecting direct echoes from the plasmasphere from distances of 3 Earth radii or greater. RPI observed a large number of guided echoes in the plasmapause, plasmaspheric notches, in the plasma trough, and over the polar cap. These observations indicated that electromagnetic waves propagate along the magnetic field lines, often from one hemisphere to the other, possibly supported by field-aligned density structures. Inversion of RPI echo traces, guided or direct, provided a means of measuring evolving electron density distributions under a variety of geomagnetic conditions including plasmasphere depletion and refilling during a magnetic storm. RPI passive measurements also showed that AKR source locations move with season and local time and, when compared to Polar spacecraft observations, the overall intensity of AKR is less during solar maximum than solar minimum.

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Details

Version:2.0.0

Instrument

ResourceID
spase://SMWG/Instrument/IMAGE/RPI
ResourceHeader
ResourceName
Radio Plasma Imager (RPI)
AlternateName
RPI
ReleaseDate
2019-05-05 12:34:56Z
Description

The main science objective of the Radio Plasma Imager (RPI) was to characterize plasma in the Earth's magnetosphere utilizing imaging in the radio frequency range.

The RPI on the IMAGE spacecraft was a pioneering instrument designed as a low frequency (3 kHz to 3 MHz) long-range magnetospheric radio sounder, relaxation sounder, and a passive plasma wave instrument. RPI was a highly flexible instrument capable of being programmed to perform these types of measurements at times when IMAGE was located in key regions of the magnetosphere. For the remote sensing, RPI transmitted coded electromagnetic waves and used digital pulse compression and spectral integration to isolate the resulting echoes.

The RPI instrument consisted of an electronics unit, four 250-m wire antennas with antenna tuners, and a z-axis antenna with two 10-m lattice booms. RPI used the x axis antennas for all transmissions while echo reception was accomplished on all three. The x-axis dipole antenna was 500 m tip-to-tip at the beginning of the mission but was shortened to 370 m when it apparently collided with a micrometeoroid or orbital debris on 03 October 2000. The Y antenna suffered similar damage to its -Y segment 11 on August 2002 and complete loss of its +Y segment on 30 September 2004.

RPI was capable of detecting direct echoes from the plasmasphere from distances of 3 Earth radii or greater. RPI observed a large number of guided echoes in the plasmapause, plasmaspheric notches, in the plasma trough, and over the polar cap. These observations indicated that electromagnetic waves propagate along the magnetic field lines, often from one hemisphere to the other, possibly supported by field-aligned density structures. Inversion of RPI echo traces, guided or direct, provided a means of measuring evolving electron density distributions under a variety of geomagnetic conditions including plasmasphere depletion and refilling during a magnetic storm. RPI passive measurements also showed that AKR source locations move with season and local time and, when compared to Polar spacecraft observations, the overall intensity of AKR is less during solar maximum than solar minimum.

Contacts
RolePerson
1.PrincipalInvestigatorspase://SMWG/Person/Bodo.W.Reinisch
2.DataProducerspase://SMWG/Person/Ivan.A.Galkin
InformationURL
Name
NSSDC's Master Catalog
URL
https://nssdc.gsfc.nasa.gov/nmc/experiment/display.action?id=2000-017A-01
Description

Information about the Radio Plasma Imager (RPI) experiment on the IMAGE mission.

InformationURL
Name
IMAGE RPI Instrument Page
URL
https://image.gsfc.nasa.gov/rpi/
Description

IMAGE RPI Instrument page maintained by NASA GSFC with RPI facts, description, team, data, documents, discoveries, and related links sections

Language
en
InformationURL
Name
IMAGE RPI Instrument Page at UML
URL
https://ulcar.uml.edu/rpi.html
Description

IMAGE RPI Instrument page maintained by University of Massachusetts Lowell with RPI description, team, software downloads, software user guides, access to CORPRAL automated prospecting results, mission planning tools and commanding guide, data model descriptions for Level 0 and 1, sonification files of 2003 Halloween storm, and useful links

Language
en
InstrumentType
LongWire
InstrumentType
Sounder
InstrumentType
ResonanceSounder
InstrumentType
SpectralPowerReceiver
InvestigationName
Radio Plasma Imager (RPI) on IMAGE
ObservatoryID
spase://SMWG/Observatory/IMAGE