2.0.1 spase://vspo/numericalData/P_CLUSTER_HDR_EFW_PP Cluster EFW Prime Parameter Data 2007-06-01T00:00:00 Cluster EFW 4-sec electric field spectral density at 0.3-10 and 10-180 Hz, duskward electric field spase://SMWG/Person/Mats.Andre GeneralContact spase://SMWG/Repository/NASA/NSSDC Online Open CDAWeb http://cdaweb.gsfc.nasa.gov CDF CALIBRATED spase://SMWG/Instrument/Cluster2-Rumba/EFW spase://SMWG/Instrument/Cluster2-Salsa/EFW spase://SMWG/Instrument/Cluster2-Samba/EFW spase://SMWG/Instrument/Cluster2-Tango/EFW ElectricField 2001-01-01T00:00:00 2004-10-31T00:00:00 Data extended through October, 2004, as of February, 2006. PT4S Earth.Magnetosphere spase://SMWG/Observatory/Cluster2-Rumba Cluster 2/FM5 (Rumba) 2000-045A FM5 Rumba Cluster-1 2009-05-20T20:00:12Z This Cluster II spacecraft, FM5 (Rumba), is also known as Phoenix, after a mythical Arabian bird which was burnt on a funeral pile and then rose from the ashes to live again. The original Cluster of four spacecraft experienced a launch failure in 1996. (NSSDC will carry the name "Cluster96" in its information files to designate the unsuccessful 1996 four-spacecraft Ariane 5 launch.) Phoenix was approved in July 1996 as a replacement for the lost four-spacecraft group. It was later (April 1997) agreed that the potential science return from a full Cluster reflight was so important that a further three near-replicas of the original spacecraft would also be built. This Cluster II spacecraft, FM5 (Rumba), was launched together with FM8 (Tango) by a Soyuz-Fregat rocket from Baikonur. The four similar spacecraft of the Cluster II mission are part of ESA's and NASA's Solar-Terrestrial Science Program (STSP). The purpose of the Cluster II mission is to study small-scale structures in three dimensions in the Earth's plasma environment, such as those involved in the interaction between the solar wind and the magnetospheric plasma, in global magnetotail dynamics, in cross-tail currents, and in the formation and dynamics of the neutral line and of plasmoids. The four Cluster II spacecraft will orbit in a tetrahedral formation in near-polar orbits of nominally 4 x 19.6 Earth radii, with period about 57 hours, and inclination about 90.7 degrees. Relative distances between the spacecraft will be adjusted in the course of the mission, depending on the spatial scales of the structures to be studied, varying from a few hundred km to a few Earth radii. The tetrahedral formation is essential for making three-dimensional measurements and for determining the curl of vectorial quantities such as the magnetic field. The orbits of all four spacecraft will be frequently maneuvered so as to achieve the targeted investigations. See http://jsoc1.bnsc.rl.ac.uk/pub/PlanningData.html for ongoing updates of orbital information and other status. Each spacecraft will be spin-stabilized, normally at around 15 rpm, and will be cylindrical in shape, with a 2.9-m diameter and 1.3-m length. It will have two rigid 5-m radial experiment booms, four 50-m experiment wire booms, and two axial telecommunications antenna booms. Telemetry downlink bit rate will be 2 to 262 kbit/s. Each spacecraft will have AC and DC magnetometers, an electric fields and waves sensor, an electron emitter/detector, an electron density sounder, electron and ion plasma analysers, an energetic particle detector, an ion emitter, and a data processing unit. Cluster operations will be performed by ESOC in Darmstadt, Germany, with support from NASA's Deep Space Network. Cluster is also an IACG mission. The scientific data are distributed by ESOC using CD-ROM as a medium to the Principal Investigators, Co-Investigators and the network of eight national data centres (6 in Europe, 1 in USA and 1 in China) that form the Cluster Science Data System (CSDS). There are approximately 80 recipients world-wide. Science operations are carried out by the Joint Science Operations Centre, co-located with the UK data centre at RAL, Didcot. A wide scientific community will have differing rights of access to the Cluster data. Scientists wishing to access Cluster data should contact their national Data Centres. The Cluster Summary Parameters are publicly available on CDAWeb at http://cdaweb.gsfc.nasa.gov/cdaweb/istp_public and the Prime Parameters are available on CDAWeb at http://cdaweb.gsfc.nasa.gov/cdaweb/ to project personnel (password-protected). See the Cluster II WWW site at http://sci.esa.int/cluster/ for more information, including spacecraft and exprient status. An article on 'The Resurrection of the Cluster Scientific Mission' was published in ESA Bulletin no. 91 (August 1997). A complete overview of the original mission, written before the loss with Ariane-5, was given in a series of articles in ESA Bulletin no. 84 (November 1995). ESA SP-1159, Paris, March 1993 is entitled "Cluster: Mission, Payload and Supporting Activities." spase://SMWG/Person/Melvyn.L.Goldstein ProjectScientist NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=2000-045A Information about the Cluster 2/FM5 (Rumba) mission CLUSTER Heliosphere.NearEarth spase://SMWG/Observatory/Cluster2-Salsa Cluster 2/FM6 (Salsa) 2000-041B FM6 Salsa Cluster-2 2009-05-20T20:00:12Z This Cluster II spacecraft, FM6 (Salsa), was launched together with FM7 (Samba) by a Soyuz-Fregat rocket from Baikonur. The four similar spacecraft of the Cluster II mission are part of ESA's and NASA's Solar-Terrestrial Science Program (STSP). The current Cluster II mission is a near-replica of the original four-spacecraft mission lost at launch in 1996. (NSSDC will carry the name "Cluster96" in its information files to designate the unsuccessful 1996 four-spacecraft Ariane 5 launch.) The purpose of the Cluster II mission is to study small-scale structures in three dimensions in the Earth's plasma environment, such as those involved in the interaction between the solar wind and the magnetospheric plasma, in global magnetotail dynamics, in cross-tail currents, and in the formation and dynamics of the neutral line and of plasmoids. The four Cluster II spacecraft will orbit in a tetrahedral formation in near-polar orbits of nominally 4 x 19.6 Earth radii, with period about 57 hours, and inclination about 90.7 degrees. Relative distances between the spacecraft will be adjusted in the course of the mission, depending on the spatial scales of the structures to be studied, varying from a few hundred km to a few Earth radii. The tetrahedral formation is essential for making three-dimensional measurements and for determining the curl of vectorial quantities such as the magnetic field. The orbits of all four spacecraft will be frequently maneuvered so as to achieve the targeted investigations. See http://jsoc1.bnsc.rl.ac.uk/pub/PlanningData.html for ongoing updates of orbital information and other status. Each spacecraft will be spin-stabilized, normally at around 15 rpm, and will be cylindrical in shape, with a 2.9-m diameter and 1.3-m length. It will have two rigid 5-m radial experiment booms, four 50-m experiment wire booms, and two axial telecommunications antenna booms. Telemetry downlink bit rate will be 2 to 262 kbit/s. Each spacecraft will have AC and DC magnetometers, an electric fields and waves sensor, an electron emitter/detector, an electron density sounder, electron and ion plasma analysers, an energetic particle detector, an ion emitter, and a data processing unit. Cluster operations will be performed by ESOC in Darmstadt, Germany, with support from NASA's Deep Space Network. Cluster is also an IACG mission. The scientific data are distributed by ESOC using CD-ROM as a medium to the Principal Investigators, Co-Investigators and the network of eight national data centres (6 in Europe, 1 in USA and 1 in China) that form the Cluster Science Data System (CSDS). There are approximately 80 recipients world-wide. Science operations are carried out by the Joint Science Operations Centre, co-located with the UK data centre at RAL, Didcot. A wide scientific community will have differing rights of access to the Cluster data. Scientists wishing to access Cluster data should contact their national Data Centres. The Cluster Summary Parameters are publicly available on CDAWeb at http://cdaweb.gsfc.nasa.gov/cdaweb/istp_public and the Prime Parameters are available on CDAWeb at http://cdaweb.gsfc.nasa.gov/cdaweb/ to project personnel (password-protected). See the Cluster II WWW site at http://sci.esa.int/cluster/ for more information, iincluding status of spacecraft and instruments. An article on 'The Resurrection of the Cluster Scientific Mission' was published in ESA Bulletin no. 91 (August 1997). A complete overview of the original mission, written before the loss with Ariane-5, was given in a series of articles in ESA Bulletin no. 84 (November 1995). ESA SP-1159, Paris, March 1993 is entitled "Cluster: Mission, Payload and Supporting Activities." spase://SMWG/Person/Melvyn.L.Goldstein ProjectScientist NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=2000-041B Information about the Cluster 2/FM6 (Salsa) mission CLUSTER Earth.Magnetosheath Earth.Magnetosphere.Main Earth.Magnetosphere.Polar spase://SMWG/Observatory/Cluster2-Samba Cluster 2/FM7 (Samba) 2000-041A FM7 Samba Cluster-3 2009-05-20T20:00:12Z This Cluster II spacecraft, FM7 (Samba), was launched together with FM6 (Salsa) by a Soyuz-Fregat rocket from Baikonur. The four similar spacecraft of the Cluster II mission are part of ESA's and NASA's Solar-Terrestrial Science Program (STSP). The current Cluster II mission is a near-replica of the original four-spacecraft mission lost at launch in 1996. (NSSDC will carry the name "Cluster96" in its information files to designate the unsuccessful 1996 four-spacecraft Ariane 5 launch.) The purpose of the Cluster II mission is to study small-scale structures in three dimensions in the Earth's plasma environment, such as those involved in the interaction between the solar wind and the magnetospheric plasma, in global magnetotail dynamics, in cross-tail currents, and in the formation and dynamics of the neutral line and of plasmoids. The four Cluster II spacecraft will orbit in a tetrahedral formation in near-polar orbits of nominally 4 x 19.6 Earth radii, with period about 57 hours, and inclination about 90.7 degrees.. Relative distances between the spacecraft will be adjusted in the course of the mission, depending on the spatial scales of the structures to be studied, varying from a few hundred km to a few Earth radii. The tetrahedral formation is essential for making three-dimensional measurements and for determining the curl of vectorial quantities such as the magnetic field. The orbits of all four spacecraft will be frequently maneuvered so as to achieve the targeted investigations. See http://jsoc1.bnsc.rl.ac.uk/pub/PlanningData.html for ongoing updates of orbital information and other status. Each spacecraft will be spin-stabilized, normally at around 15 rpm, and will be cylindrical in shape, with a 2.9-m diameter and 1.3-m length. It will have two rigid 5-m radial experiment booms, four 50-m experiment wire booms, and two axial telecommunications antenna booms. Telemetry downlink bit rate will be 2 to 262 kbit/s. Each spacecraft will have AC and DC magnetometers, an electric fields and waves sensor, an electron emitter/detector, an electron density sounder, electron and ion plasma analysers, an energetic particle detector, an ion emitter, and a data processing unit. Cluster operations will be performed by ESOC in Darmstadt, Germany, with support from NASA's Deep Space Network. Cluster is also an IACG mission. The scientific data are distributed by ESOC using CD-ROM as a medium to the Principal Investigators, Co-Investigators and the network of eight national data centres (6 in Europe, 1 in USA and 1 in China) that form the Cluster Science Data System (CSDS). There are approximately 80 recipients world-wide. Science operations are carried out by the Joint Science Operations Centre, co-located with the UK data centre at RAL, Didcot. A wide scientific community will have differing rights of access to the Cluster data. Scientists wishing to access Cluster data should contact their national Data Centres. The Cluster Summary Parameters are publicly available on CDAWeb at http://cdaweb.gsfc.nasa.gov/cdaweb/istp_public and the Prime Parameters are available on CDAWeb at http://cdaweb.gsfc.nasa.gov/cdaweb/ to project personnel (password-protected). See the Cluster II WWW site at http://sci.esa.int/cluster/ for more information, including status of the spacecraft and instruments. An article on 'The Resurrection of the Cluster Scientific Mission' was published in ESA Bulletin no. 91 (August 1997). A complete overview of the original mission, written before the loss with Ariane-5, was given in a series of articles in ESA Bulletin no. 84 (November 1995). ESA SP-1159, Paris, March 1993 is entitled "Cluster: Mission, Payload and Supporting Activities." spase://SMWG/Person/Melvyn.L.Goldstein ProjectScientist NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=2000-041A Information about the Cluster 2/FM7 (Samba) mission CLUSTER Earth.Magnetosphere.Main Earth.Magnetosheath Earth.Magnetosphere.Polar spase://SMWG/Observatory/Cluster2-Tango Cluster 2/FM8 (Tango) 2000-045B Cluster-4 Tango FM8 2009-05-20T20:00:12Z This Cluster II spacecraft, FM8 (Tango), was launched together with FM5 (Rumba) by a Soyuz-Fregat rocket from Baikonur. The four similar spacecraft of the Cluster II mission are part of ESA's and NASA's Solar-Terrestrial Science Program (STSP). The current Cluster II mission is a near-replica of the original four-spacecraft mission lost at launch in 1996. (NSSDC will carry the name "Cluster96" in its information files to designate the unsuccessful 1996 four-spacecraft Ariane 5 launch.) The purpose of the Cluster II mission is to study small-scale structures in three dimensions in the Earth's plasma environment, such as those involved in the interaction between the solar wind and the magnetospheric plasma, in global magnetotail dynamics, in cross-tail currents, and in the formation and dynamics of the neutral line and of plasmoids. The four Cluster II spacecraft will orbit in a tetrahedral formation in near-polar orbits of nominally 4 x 19.6 Earth radii, with period about 57 hours, and inclination about 90.7 degrees. Relative distances between the spacecraft will be adjusted in the course of the mission, depending on the spatial scales of the structures to be studied, varying from a few hundred km to a few Earth radii. The tetrahedral formation is essential for making three-dimensional measurements and for determining the curl of vectorial quantities such as the magnetic field. The orbits of all four spacecraft will be frequently maneuvered so as to achieve the targeted investigations. See http://jsoc1.bnsc.rl.ac.uk/pub/PlanningData.html for ongoing updates of orbital information and other status. Each spacecraft will be spin-stabilized, normally at around 15 rpm, and will be cylindrical in shape, with a 2.9-m diameter and 1.3-m length. It will have two rigid 5-m radial experiment booms, four 50-m experiment wire booms, and two axial telecommunications antenna booms. Telemetry downlink bit rate will be 2 to 262 kbit/s. Each spacecraft will have AC and DC magnetometers, an electric fields and waves sensor, an electron emitter/detector, an electron density sounder, electron and ion plasma analysers, an energetic particle detector, an ion emitter, and a data processing unit. Cluster operations will be performed by ESOC in Darmstadt, Germany, with support from NASA's Deep Space Network. Cluster is also an IACG mission. The scientific data are distributed by ESOC using CD-ROM as a medium to the Principal Investigators, Co-Investigators and the network of eight national data centres (6 in Europe, 1 in USA and 1 in China) that form the Cluster Science Data System (CSDS). There are approximately 80 recipients world-wide. Science operations are carried out by the Joint Science Operations Centre, co-located with the UK data centre at RAL, Didcot. A wide scientific community will have differing rights of access to the Cluster data. Scientists wishing to access Cluster data should contact their national Data Centres. The Cluster Summary Parameters are publicly available on CDAWeb at http://cdaweb.gsfc.nasa.gov/cdaweb/istp_public/ and the Prime Parameters are available on CDAWeb at http://cdaweb.gsfc.nasa.gov/cdaweb/ to project personnel (password-protected). See the Cluster II WWW site at http://sci.esa.int/cluster/ for more information. An article on 'The Resurrection of the Cluster Scientific Mission' was published in ESA Bulletin no. 91 (August 1997). A complete overview of the original mission, written before the loss with Ariane-5, was given in a series of articles in ESA Bulletin no. 84 (November 1995). ESA SP-1159, Paris, March 1993 is entitled "Cluster: Mission, Payload and Supporting Activities." spase://SMWG/Person/Melvyn.L.Goldstein ProjectScientist NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=2000-045B Information about the Cluster 2/FM8 (Tango) mission CLUSTER Earth.Magnetosheath Earth.Magnetosphere.Main Earth.Magnetosphere.Polar spase://SMWG/Instrument/Cluster2-Salsa/EFW Electric Field and Waves (EFW) EFW 2009-05-20T21:10:16Z The EFW (Electric Field and Waves) instrument consists of four orthogonal spherical sensors deployed from 50 m cable booms in the spin plane of the spacecraft, plus four deployment units and a main electronics unit. Each deployment unit deploys a multiconductor cable and tip-mounted spherical sensor. Each opposing pair of cables will be symmetrically deployed to a tip-to-tip distance of approximately 100 m, except for about a week at the beginning of the mission when 70 m will be used for one boom pair (the Z-booms) and 100 m for the other pair. The potentials of the spherical sensor and nearby conductors are controlled by the microprocessor to minimize errors associated with photoelectron fluxes to and from the spheres. Output signals from the sensor preamplifiers are provided to the wave instruments for analysis of high frequency wave phenomena. There is a 1 MB burst memory and tow fast A/D conversion circuits for recording electric field wave forms for time resolutions of up to 36,000 samples/s. Data gathered in the burst memory will be played back through the telemetry stream allocated to the instrument by pre-empting a portion of the real-time data. Incoming data are continuously monitored by algorithms in the software to determine whether to trigger the burst-playback mode. A large number of sampling modes is possible, yielding four possible telemetry rates from 1.440--29.440 Kbps. This data stream is transferred via the DWP instrument. The main measured quantities will be, in various modes: (1) the instantaneous spin-plane components of the electric field vector, from 0.1--700 V/Km, with time resolution down to 0.1 ms, in four frequency ranges from DC to upper limits of 10 Hz, 180 Hz, 4 KHz, or 32 KHz; (2) the AC electric field components from 10 Hz to 8 KHz, within the dynamic range of ~3 mV/Km to 10 V/Km; (3) plasma density fluctuations within the range of 1--100/cm and in three frequency ranges from 0 Hz to upper limits of 10 Hz, 180 Hz, or 4 KHz; and, (4) density and temperature (in Langmuir sweeps) in the eV range, with a dynamic range of 1--100/cm. There is also a frequency counter covering the range 10--200 KHz. On-board calculations of least-square fits to the electric field data over one spacecraft spin period (4 s) will provide a baseline of high-quality two-dimensional electric field components that are present in the telemetry stream, except for periods when three or four sensors are in current mode. The spacecraft potential is calculated and transmitted via DWP to other instruments on board. The three components from the search coil instrument (WHISPER) are also available in EFW with a bandwidth of 4 KHz. For more details of the Cluster mission, the spacecraft, and its instruments, see the report ``Cluster: mission, payload and supporting activities,'' March 1993, ESA SP-1159, and the included article ``The Spherical Probe Electric Field and Wave Experiment for the Cluster Mission,'' by G. Gustafsson et al., from which this information was obtained. spase://SMWG/Person/Georg.Gustafsson PrincipalInvestigator NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=2000-041B&ex=8 Information about the Electric Field and Waves (EFW) experiment on the Cluster 2/FM6 (Salsa) mission. LongWire Electric Field and Waves (EFW) on Cluster 2/FM6 (Salsa) spase://SMWG/Observatory/Cluster2-Salsa spase://SMWG/Instrument/Cluster2-Rumba/EFW Electric Field and Waves (EFW) EFW 2009-05-20T21:10:10Z The EFW (Electric Field and Waves) instrument consists of four orthogonal spherical sensors deployed from 50 m cable booms in the spin plane of the spacecraft, plus four deployment units and a main electronics unit. Each deployment unit deploys a multiconductor cable and tip-mounted spherical sensor. Each opposing pair of cables will be symmetrically deployed to a tip-to-tip distance of approximately 100 m, except for about a week at the beginning of the mission when 70 m will be used for one boom pair (the Z-booms) and 100 m for the other pair. The potentials of the spherical sensor and nearby conductors are controlled by the microprocessor to minimize errors associated with photoelectron fluxes to and from the spheres. Output signals from the sensor preamplifiers are provided to the wave instruments for analysis of high frequency wave phenomena. There is a 1 MB burst memory and tow fast A/D conversion circuits for recording electric field wave forms for time resolutions of up to 36,000 samples/s. Data gathered in the burst memory will be played back through the telemetry stream allocated to the instrument by pre-empting a portion of the real-time data. Incoming data are continuously monitored by algorithms in the software to determine whether to trigger the burst-playback mode. A large number of sampling modes is possible, yielding four possible telemetry rates from 1.440--29.440 Kbps. This data stream is transferred via the DWP instrument. The main measured quantities will be, in various modes: (1) the instantaneous spin-plane components of the electric field vector, from 0.1--700 V/Km, with time resolution down to 0.1 ms, in four frequency ranges from DC to upper limits of 10 Hz, 180 Hz, 4 KHz, or 32 KHz; (2) the AC electric field components from 10 Hz to 8 KHz, within the dynamic range of ~3 mV/Km to 10 V/Km; (3) plasma density fluctuations within the range of 1--100/cm and in three frequency ranges from 0 Hz to upper limits of 10 Hz, 180 Hz, or 4 KHz; and, (4) density and temperature (in Langmuir sweeps) in the eV range, with a dynamic range of 1--100/cm. There is also a frequency counter covering the range 10--200 KHz. On-board calculations of least-square fits to the electric field data over one spacecraft spin period (4 s) will provide a baseline of high-quality two-dimensional electric field components that are present in the telemetry stream, except for periods when three or four sensors are in current mode. The spacecraft potential is calculated and transmitted via DWP to other instruments on board. The three components from the search coil instrument (WHISPER) are also available in EFW with a bandwidth of 4 KHz. For more details of the Cluster mission, the spacecraft, and its instruments, see the report ``Cluster: mission, payload and supporting activities,'' March 1993, ESA SP-1159, and the included article ``The Spherical Probe Electric Field and Wave Experiment for the Cluster Mission,'' by G. Gustafsson et al., from which this information was obtained. spase://SMWG/Person/Georg.Gustafsson PrincipalInvestigator NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=2000-045A&ex=8 Information about the Electric Field and Waves (EFW) experiment on the Cluster 2/FM5 (Rumba) mission. LongWire Electric Field and Waves (EFW) on Cluster 2/FM5 (Rumba) spase://SMWG/Observatory/Cluster2-Rumba spase://SMWG/Instrument/Cluster2-Samba/EFW Electric Field and Waves (EFW) EFW 2009-05-20T21:10:15Z The EFW (Electric Field and Waves) instrument consists of four orthogonal spherical sensors deployed from 50 m cable booms in the spin plane of the spacecraft, plus four deployment units and a main electronics unit. Each deployment unit deploys a multiconductor cable and tip-mounted spherical sensor. Each opposing pair of cables will be symmetrically deployed to a tip-to-tip distance of approximately 100 m, except for about a week at the beginning of the mission when 70 m will be used for one boom pair (the Z-booms) and 100 m for the other pair. The potentials of the spherical sensor and nearby conductors are controlled by the microprocessor to minimize errors associated with photoelectron fluxes to and from the spheres. Output signals from the sensor preamplifiers are provided to the wave instruments for analysis of high frequency wave phenomena. There is a 1 MB burst memory and tow fast A/D conversion circuits for recording electric field wave forms for time resolutions of up to 36,000 samples/s. Data gathered in the burst memory will be played back through the telemetry stream allocated to the instrument by pre-empting a portion of the real-time data. Incoming data are continuously monitored by algorithms in the software to determine whether to trigger the burst-playback mode. A large number of sampling modes is possible, yielding four possible telemetry rates from 1.440--29.440 Kbps. This data stream is transferred via the DWP instrument. The main measured quantities will be, in various modes: (1) the instantaneous spin-plane components of the electric field vector, from 0.1--700 V/Km, with time resolution down to 0.1 ms, in four frequency ranges from DC to upper limits of 10 Hz, 180 Hz, 4 KHz, or 32 KHz; (2) the AC electric field components from 10 Hz to 8 KHz, within the dynamic range of ~3 mV/Km to 10 V/Km; (3) plasma density fluctuations within the range of 1--100/cm and in three frequency ranges from 0 Hz to upper limits of 10 Hz, 180 Hz, or 4 KHz; and, (4) density and temperature (in Langmuir sweeps) in the eV range, with a dynamic range of 1--100/cm. There is also a frequency counter covering the range 10--200 KHz. On-board calculations of least-square fits to the electric field data over one spacecraft spin period (4 s) will provide a baseline of high-quality two-dimensional electric field components that are present in the telemetry stream, except for periods when three or four sensors are in current mode. The spacecraft potential is calculated and transmitted via DWP to other instruments on board. The three components from the search coil instrument (WHISPER) are also available in EFW with a bandwidth of 4 KHz. For more details of the Cluster mission, the spacecraft, and its instruments, see the report ``Cluster: mission, payload and supporting activities,'' March 1993, ESA SP-1159, and the included article ``The Spherical Probe Electric Field and Wave Experiment for the Cluster Mission,'' by G. Gustafsson et al., from which this information was obtained. spase://SMWG/Person/Georg.Gustafsson PrincipalInvestigator NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=2000-041A&ex=8 Information about the Electric Field and Waves (EFW) experiment on the Cluster 2/FM7 (Samba) mission. LongWire Electric Field and Waves (EFW) on Cluster 2/FM7 (Samba) spase://SMWG/Observatory/Cluster2-Samba spase://SMWG/Instrument/Cluster2-Tango/EFW Electric Field and Waves (EFW) EFW 2009-05-20T21:10:13Z The EFW (Electric Field and Waves) instrument consists of four orthogonal spherical sensors deployed from 50 m cable booms in the spin plane of the spacecraft, plus four deployment units and a main electronics unit. Each deployment unit deploys a multiconductor cable and tip-mounted spherical sensor. Each opposing pair of cables will be symmetrically deployed to a tip-to-tip distance of approximately 100 m, except for about a week at the beginning of the mission when 70 m will be used for one boom pair (the Z-booms) and 100 m for the other pair. The potentials of the spherical sensor and nearby conductors are controlled by the microprocessor to minimize errors associated with photoelectron fluxes to and from the spheres. Output signals from the sensor preamplifiers are provided to the wave instruments for analysis of high frequency wave phenomena. There is a 1 MB burst memory and tow fast A/D conversion circuits for recording electric field wave forms for time resolutions of up to 36,000 samples/s. Data gathered in the burst memory will be played back through the telemetry stream allocated to the instrument by pre-empting a portion of the real-time data. Incoming data are continuously monitored by algorithms in the software to determine whether to trigger the burst-playback mode. A large number of sampling modes is possible, yielding four possible telemetry rates from 1.440--29.440 Kbps. This data stream is transferred via the DWP instrument. The main measured quantities will be, in various modes: (1) the instantaneous spin-plane components of the electric field vector, from 0.1--700 V/Km, with time resolution down to 0.1 ms, in four frequency ranges from DC to upper limits of 10 Hz, 180 Hz, 4 KHz, or 32 KHz; (2) the AC electric field components from 10 Hz to 8 KHz, within the dynamic range of ~3 mV/Km to 10 V/Km; (3) plasma density fluctuations within the range of 1--100/cm and in three frequency ranges from 0 Hz to upper limits of 10 Hz, 180 Hz, or 4 KHz; and, (4) density and temperature (in Langmuir sweeps) in the eV range, with a dynamic range of 1--100/cm. There is also a frequency counter covering the range 10--200 KHz. On-board calculations of least-square fits to the electric field data over one spacecraft spin period (4 s) will provide a baseline of high-quality two-dimensional electric field components that are present in the telemetry stream, except for periods when three or four sensors are in current mode. The spacecraft potential is calculated and transmitted via DWP to other instruments on board. The three components from the search coil instrument (WHISPER) are also available in EFW with a bandwidth of 4 KHz. For more details of the Cluster mission, the spacecraft, and its instruments, see the report ``Cluster: mission, payload and supporting activities,'' March 1993, ESA SP-1159, and the included article ``The Spherical Probe Electric Field and Wave Experiment for the Cluster Mission,'' by G. Gustafsson et al., from which this information was obtained. spase://SMWG/Person/Georg.Gustafsson PrincipalInvestigator NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=2000-045B&ex=8 Information about the Electric Field and Waves (EFW) experiment on the Cluster 2/FM8 (Tango) mission. LongWire Electric Field and Waves (EFW) on Cluster 2/FM8 (Tango) spase://SMWG/Observatory/Cluster2-Tango spase://SMWG/Repository/NASA/NSSDC NSSDC 2008-08-26T21:02:30Z National Space Science Data Center spase://SMWG/Person/Edwin.J.Grayzeck.Jr GeneralContact spase://SMWG/Person/Edwin.V.Bell.II GeneralContact spase://SMWG/Repository/NSSDC spase://SMWG/Person/Melvyn.L.Goldstein 1999-08-18T00:00:00Z Dr. Melvyn L. Goldstein GSFC-Code 692 melvyn.l.goldstein@nasa.gov +1-301-286-7828 spase://SMWG/Person/Mats.Andre Mr. Mats Andre Swedish Institute of Space Physics spase://SMWG/Person/Edwin.V.Bell.II Dr. Edwin V. Bell, II GSFC-Code 690.1 spase://SMWG/Person/Edwin.J.Grayzeck.Jr Dr. Edwin J. Grayzeck, Jr. GSFC-Code 690.1 spase://SMWG/Person/Georg.Gustafsson Dr. Georg Gustafsson Swedish Institute of Space Physics