This page summarizes information about the selected resource and its origin based on SPASE metadata.
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This is an hourly resolution, merged magnetic field and plasma data set created at NSSDC for COHOWeb. Magnetic field vectors and plasma flow direction angles are given in RTN coordinates. Spacecraft position data are given in Heliographic inertial (HGI coordinates).
Please acknowledge the magnetic field and plasma Principal Investigators, Drs. E. Smith and P. Gazis, and NSSDC or GSFC-SPDF
| Role | Person | |
|---|---|---|
| 1. | Principal investigator | Dr. Edward J. Smith |
| 2. | Principal investigator | Dr. Paul R. Gazis |
| 3. | General contact | Dr. Natalia E. Papitashvili |
for annual files via ftp
Pioneer 11-specific page for plots and lists
Plots, lists, scatter plots, regressions, distributions, means, etc.
Please acknowledge the magnetic field and plasma Principal Investigators, Drs. E. Smith and P. Gazis, and NSSDC or GSFC-SPDF
Plasma data do not start until day 111 of 1973. Plasma data end on day 150 of 1992. Field and plasma data become increasingly sparse after the early 1980's.
Four digit Year
Decimal Day of Year
Hour
Heliocentric radial distance of Pioneer 11 in AU
Heliographic Inertial elevation angle of Pioneer 11 in deg
Heliographic Inertial azimuthal angle of Pioneer 11 in deg
Hourly averages of RTN components of fine time scale magnetic field vectors
R,T,N components
| Index | Name | Component | Parameter key |
|---|---|---|---|
| 1 | R component | I | Column07 |
| 2 | T component | J | Column08 |
| 3 | N component | K | Column09 |
Hourly average of fine time scale magnetic field magnitudes
Hourly averaged solar wind plasma flow speed
Hourly averaged solar wind plasma flow elevation angle
Hourly averaged solar wind plasma flow azimuthal angle
Hourly averaged solar wind plasma density
Hourly averaged solar wind plasma temperature
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The magnetometer on Pioneer 11 was a triaxial helium magnetometer with seven dynamic ranges, from plus or minus 2.5 nT to plus or minus 1.0E-3 T. The linearity was 0.1% and the noise threshold was 0.01 nT rms for 0-1 Hz. The accuracy was 0.5% of full scale range. The experimenter used RTN coordinates in the data analysis. In this system, R (or X) is radially outward from the sun, T (or Y) was parallel to the sun's equatorial plane and had its direction given by the cross product of the sun's spin vector into the radial direction (i.e., into R), and N (or Z) completed the right-handed orthogonal system (positive northward). A detailed instrument description may be found in Smith et al., IEEE Trans. On Magnetics, v. M-11, p. 962, July 1975. Data include the interplanetary region.
Information about the Magnetic Fields experiment on the Pioneer 11 mission.
| Role | Person | |
|---|---|---|
| 1. | Principal investigator | Dr. Edward J. Smith |
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The instrument consisted of dual 90-deg quadrispherical electrostatic analyzers, one with 26 individual particle detectors and the other with 5 current collectors. The system was capable of measuring incident plasma distribution parameters over the energy range 0.1 to 18 keV for protons and approximately 1 to 500 eV for electrons. The high-resolution analyzer with a constant of 9 keV/Q per kV applied to the plates, had a mean plate radius of 9 cm and separation of 0.5 cm. This analyzer was used to measure ions only, and had 26 channeltrons mounted on the semicircular exit to the analyzer. The aperture pointed through a wide slit in the back of the spacecraft high-gain antenna reflector and pointed along the spin axis toward the earth (and therefore the sun). The edges of the antenna reflector limited the viewing of the instrument to 73 deg with respect to the spin axis. The channeltrons covered a range of plus or minus 51 deg. Each channeltron near the center covered 3 deg and approximately 8 deg near the edges of the analyzer. The angular width perpendicular to the long angular width was about 2 deg. In half the spin period the whole cone of half-angle 51 deg centered on the sun was swept out. A medium-energy analyzer with a mean radius of 12 cm and a 1-cm plate separation (constant of 6 keV/Q per kV applied) was used to detect both ions and electrons. The detectors were five flat-surface current collectors. The three center collectors each covered 15 deg and covered the angular range of plus or minus 22.5 deg from the spin axis. The two outside collectors had an angular width of 47.5 deg and were located at plus or minus 46.25 deg from the center of the analyzer. There was a variety of possible operating modes for the experiment; however, the principal mode utilized during the encounter phase was one in which the analyzer plate potential was stepped through its range every one-half revolution of the spacecraft, and all current collectors or channeltrons were read out at the peak flux roll angle. The high and medium resolution analyzers operated independently, so a cross check between these analyzers was possible. The dynamic range for the particle fluxes was from 1.0E+2 to 3.0E+9/(sq cm-s) and the proton temperature down to 2.0E+3 deg K could be ascertained. Data include the interplanetary region. Detector A was turned off on September 16, 1987.
Information about the Quadrispherical Plasma Analyzer experiment on the Pioneer 11 mission.
| Role | Person | |
|---|---|---|
| 1. | Principal investigator | Dr. Aaron Barnes |
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Pioneer 11 was the second mission to investigate Jupiter and the outer solar system and the first to explore the planet Saturn and its main rings. Pioneer 11, like Pioneer 10, used Jupiter's gravitational field to alter its trajectory radically. It passed close to Saturn and then it followed an escape trajectory from the solar system.
The spacecraft was 2.9 m long and contained a 2.74-m diameter high-gain antenna of aluminum honeycomb sandwich material whose feed was topped with a medium-gain antenna. A low-gain, omnidirectional antenna was mounted below the high-gain dish. The spacecraft contained two nuclear electric-power generators, which generated 144 W at Jupiter, but decreased to 100 W at Saturn. There were three reference sensors: a star (Canopus) sensor, and two sun sensors. Attitude position could be calculated from the reference direction to the earth and the sun, with the known direction to Canopus as backup. Pioneer 11's star sensor gain and threshold settings were modified, based on experience gained from the settings used on Pioneer 10. Three pairs of rocket thrusters provided spin-axis control (maintained at 4.8 rpm) and change of the spacecraft velocity. The thrusters could be either fired steadily or pulsed, by command.
Communications were maintained via the omnidirectional and medium-gain antennas, which operated together, connected to one receiver, while the high-gain antenna was connected to the other receiver. The receivers could be interchanged by command. Two radio transmitters, coupled to two traveling-wave tube amplifiers, produced 8 W power each in S-band. Communication uplink (earth to spacecraft) operated at 2110 MHz, and downlink (spacecraft to earth) at 2292 MHz. At Jupiter's distance, round-trip communication time took 92 min. Data were received at the Deep Space Network (DSN). The spacecraft was temperature-controlled to between -23 and +38 deg C (-10 to +100 deg F). An additional experiment, a low-sensitivity fluxgate magnetometer, was added to the Pioneer 11 payload.
Instruments studied the interplanetary and planetary magnetic fields; solar wind properties; cosmic rays; transition region of the heliosphere; neutral hydrogen abundance; distribution, size, mass, flux, and velocity of dust particles; Jovian aurorae; Jovian radio waves; the atmospheres of planets and satellites; and the surfaces of Jupiter, Saturn, and some of their satellites. Instruments carried for these experiments were magnetometer, plasma analyzer (for solar wind), charged-particle detector, ionizing detector, non-imaging telescopes with overlapping fields of view to detect sunlight reflected from passing meteoroids, sealed pressurized cells of argon and nitrogen gas for measuring penetration of meteoroids, UV photometer, IR radiometer, and an imaging photopolarimeter, which produced photographs and measured the polarization. Further scientific information was obtained from celestial mechanics and occultation phenomena.
This spacecraft, like Pioneer 10, contains a plaque that has a drawing depicting man, woman, and the location of the sun and earth in the galaxy.
During its closest approach, December 4, 1974, Pioneer 11 passed to within 34,000 km of Jupiter's cloud tops. It passed by Saturn on September 1, 1979, at a distance of 21,000 km from Saturn's cloud tops. The spacecraft has operated on a backup transmitter since launch. Instrument power sharing began in February 1985 due to declining RTG power output. Science operations and daily telemetry ceased on September 30, 1995 when the RTG power level was insufficient to operate any experiments. As of the end of 1995 the spacecraft was located at 44.7 AU from the Sun at a nearly asymptotic latitude of 17.4 degrees above the solar equatorial plane and was heading outward at 2.5 AU/year.
Information about the Pioneer 11 mission
| Role | Person | |
|---|---|---|
| 1. | Project scientist | Dr. Palmer Dyal |
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Space Physics Data Facility
Space Physics Data Facility
| Role | Person | |
|---|---|---|
| 1. | General contact | Ms. Tamara J. Kovalick |
| 2. | Technical contact | Mr. Robert M. Candey |
| 3. | Project scientist | Dr. Robert E. McGuire |