This page summarizes information about the selected resource and its origin based on SPASE metadata.
SPASE version 2.0.0
This data set has eight 6-hour fluxes (3.45-5.15, 30.55-56.47 and 120.7-227.3 MeV protons, 3.44-4.97, 10.03-21.7, 30.67-56.7 and 112.7-413 MeV/n alpha particles, and 2-6 MeV electrons), 28 count rates, and Poisson uncertainties in the fluxes and rates, as determined from the Cosmic Ray Telescope (CRT) on the Pioneer 11 spacecraft. Data are in annual files with consistent end-of-record marks. Spacecraft position data are not given in the data records but are accessible from Helioweb at http://cohoweb.gsfc.nasa.gov/helios/heli.html
the Principal Investigator, Frank B. McDonald
| Role | Person | |
|---|---|---|
| 1. | Principal investigator | Dr. Frank B. McDonald |
| 2. | General contact | Dr. Nand Lal |
For display and retrieval of parameter subsets
For ftp downloading of annual files
the Principal Investigator, Frank B. McDonald, and FTPBrowser at SPDF
This flux is obtained from LET-I and is derived from pulse height data using R11A for normalization
This flux is obtained from HET and is derived from pulse height data using R1 for normalization
This flux is obtained from HET and is derived from pulse height data using R2 for normalization
This flux is obtained from LET-1 and is derived from pulse height data using R11B for normalization
This flux is obtained from LET-1 and is derived from pulse height data using R11B for normalization
This flux is obtained from HET and is derived from pulse height data using R2B for normalization
This flux is obtained from HET and is derived from pulse height data using R3A for normalization
This flux is obtained from HET and is derived from pulse height data using R1 for normalization
These are the Poisson uncertainties in the eight fluxes named above as scalars. In the data records, each immediately follows the flux it refers to.
These are 28 6-hour-averaged count rates corresponding to various telescope sensors singly and in coincidence, and, for some, for various levels of energy deposition in sensors. The documentation cited above gives conditions for each rate: which sensors, which species (one or more), etc.
These are Poisson uncertainties in each of the above-identified 28 6-hour-averaged count rates corresponding to various telescope sensors singly and in coincidence, and, for some, for various levels of energy deposition in sensors. The documentation cited above gives conditions for each rate: which sensors, which species (one or more), etc. The uncertainty for each count rate immediately follows that count rate in the data records.
SPASE version 2.0.0
This experiment consisted of three 3-element telescopes, all looking normal to the spacecraft spin axis. A bidirectional telescope measured 20- to 800-MeV/nucleon particles with 5 to 10% energy resolution. Another telescope measured 3- to 22-MeV/nucleon particles with 5% resolution. These two telescopes measured particles with Z values between 1 and 8. The third telescope measured 50-keV to 1-MeV electrons and 50-keV to 20-MeV protons with 20% resolution. Data include the interplanetary region.
Information about the Cosmic-Ray Telescope experiment on the Pioneer 11 mission.
| Role | Person | |
|---|---|---|
| 1. | Principal investigator | Dr. Frank B. McDonald |
SPASE version 2.0.0
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 |
SPASE version 2.0.0
SPASE version 2.0.0
SPASE version 2.0.0
SPASE version 2.0.0
SPASE version 2.0.0
SPASE version 1.3.0
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 |