Explorer 32: Исследование верхней атмосферы Земли

NASA satellite of the Explorer program

Explorer 32, also known as Atmosphere Explorer B (AE B), as a successor to Explorer 17, which it strongly resembled, to directly measure the temperature, composition, density, and pressure of the upper atmosphere. Its main differences from the prior satellite were the addition of a tape recorder for data storage, solar cells to charge onboard batteries, a magnetic torquer to stabilize the satellite's spin, and a 3 axis fluxgate magnetometer for sensing the satellites aspect (facing) in orbit.

The objective of this experiment was to measure the distribution of electron temperature and densities from 10. E3 to 10. E6 electrons/cc using a swept voltage electron probe.

This experiment was designed to obtain a description of the concentrations of the ion species in the topside ionosphere (principally atomic hydrogen, helium, nitrogen, and oxygen), as a function of time, location, and solar and geomagnetic activity. The spectrometer sensor consisted of a 5 3 cycle ceramic tube with 5 mm grid spacing and an external guard ring assembly. Two RF frequencies, 3.7 and 9.0 MHz, were used with a trapezoidal shaped sweep voltage to cover the ion mass range 12 to 19, and 1 and 4 atomic mass units (u) assuring detection of the primary ionic constituents of the topside ionosphere. An experiment turn on consisted of one complete mass scan in 208 seconds followed by recycling of the sweep voltage and a second measurement of the high mass range. The stopping potential and the guard ring potential controlled the sensitivity of the spectrometer, and each voltage was commandable from the ground. The ion current reaching the spectrometer was measured by a series of five decade amplifiers with a particle sensitivity range of from about 10 x 1. E6 ions/cc. An automatic calibrator functioned once during each turn on to supply two known signals to the amplifier system and to the sweep monitor. Amplifier characteristics were calculated from the response to these pulses. The spectrometer tube was mounted on the equator of the almost spherically shaped spacecraft. The spacecraft spin period and attitude were magnetically controlled so that the spin axis remained essentially normal to the orbit plane and, consequently, the spectrometer orifice was aligned with the satellite velocity vector once each rotation. The spin rate was 29 ±1 rpm. Since the mass range was scanned slowly compared with the spin period, each peak in the ion spectrum was modulated at the spin frequency, with the ion current maxima occurring when the angle between the spectrometer axis and velocity vector was a minimum.

Two double focusing magnetic mass spectrometers were used to measure the composition of the neutral (uncharged) atmosphere between and One was mounted on the equator of the spherical satellite normal to the spin axis, and the other was mounted on the top of the satellite parallel to the spin axis. The neutral particles were ionized by electron bombardment and separated according to mass to charge ratio (M/Q) in the analyzer section of the instrument. There was one collector cup for each of seven different ion species. An electrometer amplifier, which had two sensitivity ranges differing by a factor of 100, sampled the seven collectors sequentially. The dwell time on a specific mass and sensitivity range was 2.4 seconds. The first four of the fifteen 2.4 seconds steps of a cycle were devoted to correcting any zero drift of the electrometer and to recording the low and high sensitivity zero levels. The ion currents were then measured in high sensitivity for M/Q equal to 2 (molecular hydrogen), 4 (helium), and 14 (atomic nitrogen) and in high and low sensitivity for M/Q equal to 28 (molecular nitrogen), 32 (molecular oxygen), 16 (atomic oxygen), and 18 (water vapor). The time for one complete cycle was 36 seconds. The experiment was designed to work in 4 minutes intervals, during which it would return real time data when in range of a ground station, or store the data on tape recorder until one was available.

Three cold cathode magnetron type density gauges (Redhead ionization gauges), each with its own high voltage supply and output electrometer, were flown to measure the density of the neutral atmosphere as a function of altitude, time, latitude, and solar and geomagnetic activity. One gauge was designated as NRC 528 and the other two as GCA R5 to reflect different origins. Mounted on the satellite equator was one gauge of each designation, with the third gauge mounted 55° above the equator. The metal ceramic GCA R5 gauges had an internal magnetic field of about 0.1 T and contained radioactive material deposited on the anode to permit operation at low atmospheric densities (less than 10. E 17 g/cc) with the anode potential fixed at 3500 volts. The GCA R5 equatorially mounted gauge had a linear range switchable electrometer output, and high resolution current measurements were obtained. The remaining two gauge outputs were through logarithmic electrometers. All electrometers were calibrated once each turn on. The time resolution of the measurements was 2 seconds, which was equal to the satellite spin period and corresponded to a spatial resolution of along the orbit path.

Because of its symmetrical shape, Explorer 32 was selected by the experimenters for use in determining upper atmospheric density as a function of altitude, latitude, season, and solar activity. This experiment was planned prior to launch. Density values near perigee were deduced from sequential observations of the spacecraft position, using optical (Baker Nunn camera network) and radio and/or radar tracking techniques. This experiment resulted in the successful determination of reasonable density values.

With all mission objectives achieved, Explorer 32 was declared a success in December 1966. Papers based on satellite data were first presented at the 17 20 April 1967 meeting of the American Geophysical Union in Washington D. C., additional results being reported at London's COSPAR meetings in July. When the satellite was near perigee, it was observed by networks of ground based Baker Nunn cameras, as well as being tracked by radio and radar. By measuring the change of the satellite's orbit due to atmospheric drag, it was determined that the models derived from Explorer 17 had been off by 35%, mostly due to calibration errors. Thus, Explorer 32 afforded a much improved map of air density at an altitude of around This information proved even more useful when combined with the data set of OV3 2, an U. S. Air Force satellite in orbit concurrently.