Data Description

This page summarizes information about the selected resource and its origin based on SPASE metadata.

Table of Contents

  1. Product
  2. Repository
  3. Instruments
  4. ObservatoryObservatories
  5. Persons

SPASE version 2.2.0

Numerical Data Product: STEREO WAVES (SWAVES) Radio Intensity Spectra, both Ahead and Behind s/c

Resource ID
spase://VWO/NumericalData/STEREO/SWAVES/DS.Combined.PT1M Get XML
Name
STEREO WAVES (SWAVES) Radio Intensity Spectra, both Ahead and Behind s/c
Alternate name
STEREO_LEVEL2_SWAVES
Solar TErrestrial RElations Observatory (STEREO) Waves (SWAVES) STEREO-A and STEREO-B Level 2 CDFs at NASA's CDAWeb
Description

The CDF file contains 1 minute averaged radio intensity data from both the Ahead and Behind s/c.

A description of the STEREO/WAVES instrument is provided in: Bougeret, J.L, et al. (2008), S/WAVES: The Radio and Plasma Wave Investigation on the STEREO Mission, Space Science Reviews, 136, 487-528.

The STEREO / WAVES (SWAVES) instruments provide unique and critical observations for all primary science objectives of the STEREO mission, the generation of CMEs, their evolution, and their interaction with Earth's magnetosphere. SWAVES can probe a CME from lift-off to Earth by detecting the coronal and interplanetary (IP) shock of the most powerful CMEs, providing a radial profile through spectral imaging, determining the radial velocity from ~2 RS (from center of sun) to Earth, measuring the density of the volume of the heliosphere between the sun and Earth, and measuring important in situ properties of the IP shock, magnetic cloud, and density compression in the fast solar wind stream that follows.

SWAVES measures the fluctuation electric field present on three orthogonal monopole antennas mounted on the back (anti-sunward) surface of the spacecraft. Each monopole antenna unit is a 6 m long Beryllium-Copper (BeCu) “stacer” spring. The three units deploy from a common baseplate that also accommodates the preamplifier housing. The 6 m length was chosen to put the antenna quarter-wave resonance near the top of the SWAVES HFR2 frequency band.

These data consist of output from the SWAVES HFR and LFR receivers.

– the High Frequency Receivers (HFR) - for spectral analysis and direction finding of radio noise generated from a few solar radii (16 MHz) to about half an Astronomical Unit (125 kHz)

– the Low Frequency Receiver (LFR) - for spectral analysis and direction finding from about half an Astronomical Unit (160 kHz) to one AU (2.5 kHz).

Additional information
STEREO/WAVES Instrument Page

STEREO/WAVES instrument page maintained by NASA GSFC with science and instrument descriptions, data, personnel, publications, and related links sections

Language
en
STEREO Mission Page at NASA/GSFC

STEREO mission page with spacecraft and instrument descriptions, news, links to data (STEREO Science Center), and image gallerys

Language
en
Acknowledgement

Users please acknowledge the Coordinated Data Analysis Web (CDAWeb) at the NASA Goddard Space Flight Center and STEREO/WAVES Principal Investigator Jean-Louis Henry Bougeret.

Contact
Role Person
1. Principal investigator Dr. Jean-Louis Henry Bougeret Get XML
2. CoInvestigator

General contact 		Dr. Robert J. MacDowall Get XML
Release date
2012-02-24 17:41:06
Prior ID
spase://VWO/NumericalData/STEREO/SWAVES/CDF_DS_Combined_PT1M
Repository
Name
CDAWeb Data Repository FTP Interface Get XML
Availability
Online
Access rights
Open
URL
CDAWeb FTP access to STEREO/WAVES Level 2 CDFs

FTP access to repository of SWAVES Level 2 data in CDF format at NASA CDAWeb.

Language
en
CDAWeb web access portal to STEREO/WAVES CDF data

Repository of SWAVES data in CDF format at NASA CDAWeb, accessible via web interface. Name of the data resource: STEREO_LEVEL2_SWAVES.

Language
en
Format
CDF
Encoding
None
Acknowledgement

Users please acknowledge Coordinated Data Analysis Web (CDAWeb) at the NASA Goddard Space Flight Center and STEREO/WAVES Principal Investigator Jean-Louis Henry Bougeret

Processing level
Calibrated
Instruments
STEREO-A Waves (SWAVES) Get XML
STEREO-B Waves (SWAVES) Get XML
Measurement type
Spectrum
Passive waves
Temporal description
Start date
2006-10-27 20:24:42
Relative stop date
1 day ago
Cadence
1 minute
Spectral range
RadioFrequency
Observed regions
Heliosphere.Inner
Heliosphere.Remote1AU
Jupiter
Caveats
Keywords
Dynamic Spectrogram
Jovian Decametric Radiation
Jupiter DAM
Solar radio burst
Spectrogram
Type II Solar radio burst
Type III Solar radio burst
↑

Parameters

Parameter #1

Name
Epoch
Parameter key
Epoch
Description

Interval-centered time tag. Time since 0 AD.

Cadence
1 minute
Units
ms
Parameter type
Temporal

Parameter #2

Name
E-Avg Inten>Bgnd (Ahead)
Parameter key
avg_intens_ahead
Description

Ahead: Electric field avg intensity (dB above bgnd, 367 freqs 2.6 kHz - 16.025 MHz, inverted frequency order)

Units
dB>bgnd
Wave type
Plasma waves
Quantity
Intensity
Qualifier
Magnitude
Pseudo
Frequency range
Spectral range
RadioFrequency
Low frequency
2.6
High frequency
16025
Units
kHz

Parameter #3

Name
E-Avg Inten>Bgnd (Ahead)
Parameter key
avg_intens_ahead_noninvert
Description

Ahead: Electric field avg intensity (normal frequency order)

Units
dB>bgnd
Wave type
Plasma waves
Quantity
Intensity
Qualifier
Magnitude
Pseudo
Frequency range
Spectral range
RadioFrequency
Low frequency
2.6
High frequency
16025
Units
kHz

Parameter #4

Name
Bgnd Avg Inten (Ahead)
Parameter key
background_ahead
Description

Ahead: Background Intensity (normal frequency order)

Units
dB
Wave type
Plasma waves
Quantity
Intensity
Qualifier
Magnitude
Pseudo
Frequency range
Spectral range
RadioFrequency
Low frequency
2.6
High frequency
16025
Units
kHz

Parameter #5

Name
E-Avg Inten>Bgnd (Behind)
Parameter key
avg_intens_behind
Description

Behind: Electric field avg intensity (dB above bgnd, 367 log-spaced freqs 2.6 kHz - 16.025 MHz, normal frequency order)

Units
db>bgnd
Wave type
Plasma waves
Quantity
Intensity
Qualifier
Magnitude
Pseudo
Frequency range
Spectral range
RadioFrequency
Low frequency
2.6
High frequency
16025
Units
kHz

Parameter #6

Name
Bgnd Avg Inten (Behind)
Parameter key
background_behind
Description

Behind: Background Intensity (normal frequency order)

Units
dB
Wave type
Plasma waves
Quantity
Intensity
Qualifier
Magnitude
Pseudo
Frequency range
Spectral range
RadioFrequency
Low frequency
2.6
High frequency
16025
Units
kHz

Parameter #7

Name
Frequency
Parameter key
frequency
Description

Frequency

Units
kHz
Parameter type
Other
↑

SPASE version 2.0.3

Instrument: STEREO-A Waves (SWAVES)

Instrument ID
spase://SMWG/Instrument/STEREO-A/SWAVES Get XML
Name
STEREO-A Waves (SWAVES)
Alternate name
SWAVES
Description

This experiment is designed to measure remotely and in situ:

  • Type II radio bursts associated with electrons accelerated by CME-driven shocks;
  • Type III radio bursts associated with impulsively accelerated electrons streaming out from the sun;
  • in situ plasma waves and waveforms.

Two radio receivers measure wave intensity, source direction and angular size in the frequency range 16 MHz to 40 kHz, corresponding to heliocentric source distances of about 1 Rs to 1 AU. One 10-40 kHz receiver measures radio and plasma waves near the 1 AU electron plasma frequency. One receiver makes high time resolution measurements at 50 MHz. Time Domain Samplers make simultaneous wideband waveform measurements on three electric components. Antenna systems include three mutually orthogonal 6-meter monopoles.

Additional information
NSSDC's Master Catalog

Information about the Stereo/Waves (Swaves) experiment on the STEREO A mission.

Contact
Role Person
1. Principal investigator Dr. Jean-Louis Henry Bougeret Get XML
Release date
2010-03-10 21:08:40
Instrument type
Unspecified
Investigation name
Stereo/Waves (Swaves) on STEREO A
Observatory
STEREO A Get XML
↑

SPASE version 2.0.3

Instrument: STEREO-B Waves (SWAVES)

Instrument ID
spase://SMWG/Instrument/STEREO-B/SWAVES Get XML
Name
STEREO-B Waves (SWAVES)
Alternate name
SWAVES
Description

This experiment is designed to measure remotely and in situ:

  • Type II radio bursts associated with electrons accelerated by CME-driven shocks;
  • Type III radio bursts associated with impulsively accelerated electrons streaming out from the sun;
  • in situ plasma waves and waveforms.

Two radio receivers measure wave intensity, source direction and angular size in the frequency range 16 MHz to 40 kHz, corresponding to heliocentric source distances of about 1 Rs to 1 AU. One 10-40 kHz receiver measures radio and plasma waves near the 1 AU electron plasma frequency. One receiver makes high time resolution measurements at 50 MHz. Time Domain Samplers make simultaneous wideband waveform measurements on three electric components. Antenna systems include three mutually orthogonal 6-meter monopoles.

Additional information
NSSDC's Master Catalog

Information about the Stereo/Waves (Swaves) experiment on the STEREO B mission.

Contact
Role Person
1. Principal investigator Dr. Jean-Louis Henry Bougeret Get XML
Release date
2010-03-10 21:08:40
Instrument type
Unspecified
Investigation name
Stereo/Waves (Swaves) on STEREO B
Observatory
STEREO B Get XML
↑

SPASE version 2.2.0

Observatory: STEREO A

Observatory ID
spase://SMWG/Observatory/STEREO-A Get XML
Name
STEREO A
Alternate name
STEREO Ahead
STEREO East
Solar Terrestrial Relations Observatory A
Description

The Solar-Terrestrial Relations Observatory (STEREO) mission includes two spacecraft respectively lagging (STEREO A) and leading (STEREO B) the Earth in heliocentric orbit around the Sun for remote 3-D imaging and radio observations of coronal mass ejections (CMEs). These events are responsible for large solar energetic particle events in interplanetary space and are the primary cause of major geomagnetic storms at Earth. The two spacecraft are launched to drift slowly away from the Earth in opposite directions at about 10 degrees per year for the lagging spacecraft and 20 degrees per year for the leading one. Optimal longitudinal separation of about sixty degrees is achieved after two years. Afterwards the separation gradually increases beyond the design lifetime of two years with the possibility of extended mission observations at larger angles. Science instruments selected for STEREO include the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) for extreme ultraviolet (EUV), white-light coronographic, and heliospheric imaging, the STEREO/WAVES (SWAVES) interplanetary radio burst tracker, the In situ Measurements of Particles and CME Transients (IMPACT) investigation for in-situ sampling the 3-D distribution and plasma characteristics of solar energetic particles and the interplanetary magnetic field, and the PLAsma and SupraThermal Ion and Composition (PLASTIC) experiment to measure elemental and charge composition of ambient and CME plasma ions. STEREO data recorded and stored onboard each spacecraft will be downlinked through the NASA Deep Space Network on a daily schedule. Real-time space weather data will be continuously transmitted through a separate beacon system to NASA and non-NASA receiving stations.

Additional information
STEREO Project Page

Project home page

NSSDC's Master Catalog

Information about the STEREO A mission

Contact
Role Person
1. Project scientist Mr. Michael L. Kaiser Get XML
Release date
2010-09-25 03:09:48
Prior ID
spase://vspo/observatory/139
Observatory group
STEREO Mission Get XML
Location
Region
Heliosphere.Remote1AU
↑

SPASE version 2.2.0

Observatory: STEREO B

Observatory ID
spase://SMWG/Observatory/STEREO-B Get XML
Name
STEREO B
Alternate name
STEREO Behind
STEREO West
Solar Terrestrial Relations Observatory B
Description

The Solar-Terrestrial Relations Observatory (STEREO) mission includes two spacecraft respectively lagging (STEREO A) and leading (STEREO B) the Earth in heliocentric orbit around the Sun for remote 3-D imaging and radio observations of coronal mass ejections (CMEs). These events are responsible for large solar energetic particle events in interplanetary space and are the primary cause of major geomagnetic storms at Earth. The two spacecraft are launched to drift slowly away from the Earth in opposite directions at about 10 degrees per year for the lagging spacecraft and 20 degrees per year for the leading one. Optimal longitudinal separation of about sixty degrees is achieved after two years. Afterwards the separation gradually increases beyond the design lifetime of two years with the possibility of extended mission observations at larger angles. Science instruments selected for STEREO include the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) for extreme ultraviolet (EUV), white-light coronographic, and heliospheric imaging, the STEREO/WAVES (SWAVES) interplanetary radio burst tracker, the In situ Measurements of Particles and CME Transients (IMPACT) investigation for in-situ sampling the 3-D distribution and plasma characteristics of solar energetic particles and the interplanetary magnetic field, and the PLAsma and SupraThermal Ion and Composition (PLASTIC) experiment to measure elemental and charge composition of ambient and CME plasma ions. STEREO data recorded and stored onboard each spacecraft will be downlinked through the NASA Deep Space Network on a daily schedule. Real-time space weather data will be continuously transmitted through a separate beacon system to NASA and non-NASA receiving stations.

Additional information
STEREO Project Page

Project home page

NSSDC's Master Catalog

Information about the STEREO B mission

Contact
Role Person
1. Project scientist Mr. Michael L. Kaiser Get XML
Release date
2010-09-25 03:09:48
Prior ID
spase://vspo/observatory/140
Observatory group
STEREO Mission Get XML
Location
Region
Heliosphere.Remote1AU
↑

SPASE version 2.2.0

Observatory: STEREO Mission

Observatory ID
spase://SMWG/Observatory/STEREO Get XML
Name
STEREO Mission
Description

The Solar-Terrestrial Relations Observatory (STEREO) mission includes two spacecraft respectively lagging (STEREO A) and leading (STEREO B) the Earth in heliocentric orbit around the Sun for remote 3-D imaging and radio observations of coronal mass ejections (CMEs). These events are responsible for large solar energetic particle events in interplanetary space and are the primary cause of major geomagnetic storms at Earth. The two spacecraft are launched to drift slowly away from the Earth in opposite directions at about 10 degrees per year for the lagging spacecraft and 20 degrees per year for the leading one. Optimal longitudinal separation of about sixty degrees is achieved after two years. Afterwards the separation gradually increases beyond the design lifetime of two years with the possibility of extended mission observations at larger angles. Science instruments selected for STEREO include the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) for extreme ultraviolet (EUV), white-light coronographic, and heliospheric imaging, the STEREO/WAVES (SWAVES) interplanetary radio burst tracker, the In situ Measurements of Particles and CME Transients (IMPACT) investigation for in-situ sampling the 3-D distribution and plasma characteristics of solar energetic particles and the interplanetary magnetic field, and the PLAsma and SupraThermal Ion and Composition (PLASTIC) experiment to measure elemental and charge composition of ambient and CME plasma ions. STEREO data recorded and stored onboard each spacecraft will be downlinked through the NASA Deep Space Network on a daily schedule. Real-time space weather data will be continuously transmitted through a separate beacon system to NASA and non-NASA receiving stations.

Additional information
STEREO Project Page

Project home page

Contact
Role Person
1. Project scientist Mr. Michael L. Kaiser Get XML
Release date
2009-05-20 20:00:12
Location
Region
Heliosphere.Remote1AU
↑

SPASE version 2.2.0

Person: Dr. Jean-Louis Henry Bougeret

Name
Dr. Jean-Louis Henry Bougeret
Organization
Observatoire de Paris-Meudon
Person ID
spase://SMWG/Person/Jean-Louis.Henry.Bougeret Get XML
↑

SPASE version 2.2.0

Person: Dr. Robert J. MacDowall

Name
Dr. Robert J. MacDowall
Organization
GSFC-Code 695
Person ID
spase://SMWG/Person/Robert.J.MacDowall Get XML
↑

SPASE version 2.2.0

Person: Dr. Robert E. McGuire

Name
Dr. Robert E. McGuire
Organization
NASA Goddard Space Flight Center
Address
Code 672, Greenbelt, MD 20771, USA
Email
mcguire@mail630.gsfc.nasa.gov
Phone
+1 301 286 7794
Person ID
spase://SMWG/Person/Robert.E.McGuire Get XML
Release date
2010-08-05 17:35:47
↑

SPASE version 2.2.0

Person: Mr. Michael L. Kaiser

Name
Mr. Michael L. Kaiser
Organization
GSFC-Code 695
Person ID
spase://SMWG/Person/Michael.L.Kaiser Get XML
↑

SPASE version 2.2.0

Repository: CDAWeb Data Repository FTP Interface

Repository ID
spase://SMWG/Repository/NASA/GSFC/SPDF/CDAWeb Get XML
Name
CDAWeb Data Repository FTP Interface
Description

Coordinated Data Analysis Web (CDAWeb) supports not only interactive plotting of variables from multiple instruments on multiple investigations simultaneously on arbitrary, user-defined time-scales. It also supports data retrieval in various formats using its interactive web interface or ftp service.

Additional information
CDAWeb Home Page

Coordinated Data Analysis Web (CDAWeb) home page at Space Physics Data Facility of the NASA Goddard Space Flight Center.

Contact
Role Person
1. Project scientist Dr. Robert E. McGuire Get XML
Release date
2011-02-23 18:39:43
Prior ID
spase://VMO/Repository/CDAWeb
Access URL
FTP Access to CDAWeb Data
↑