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A technique was devised for the Mariner Mars 1971 mission wherein both ground and in-flight calibrations were performed. A more analytical approach was used for ground calibration, and in-flight calibration was performed using narrow-angle television pictures of stars. The Mariner Mars 1971 calibration technique and results are summarized.
On the basis of data provided by the IR interferometer spectrometer on the Mariner 9 spacecraft, it is suggested that the composition of the Martian dust corresponds approximately to that of rocks of intermediate silicon dioxide content. The large dynamical pole flattening obtained from satellite observations has been confirmed by the Mariner 9 data.
Description of a self-contained portable data acquisition system for use in marine and ecological research. The compact lightweight data acquisition system is capable of recording 14 variables in its present configuration and is suitable for use in either a boat, pickup truck, or light aircraft. This system will provide the acquisition of reliable data on the structure of the environment and the effect of man-made and natural activities on the observed phenomenon. Utilizing both self-contained analog recording and a telemetry transmitter for real-time digital readout and recording, the prototype system has undergone extensive testing. Currently undergoing component performance upgrading, the prototype system has been utilized in several environmental science investigations associated with air pollution investigations and weather modification and is currently being used for marine data acquisition.
Satellite-star optical navigation, a new spacecraft navigation technique has been successfully demonstrated during Mariner 9's approach to Mars in mid-November. As Mariner 9 approached Mars, 21 TV pictures of its satellites, Phobos and Deimos, were taken and transmitted to earth. On earth, these pictures were carefully processed in order to locate the positions of the bright satellites against the relatively faint star background. The objectives and performance of the preflight and real time activities leading to the successful demonstration of satellite-star navigation data are described.
Results of an autocorrelation analysis of the Mariner 2 data concerning solar-wind speed obtained in late 1962. A statistically significant correlation associated with the solar rotation has been found near a lag of 27 days; however, the amplitude of the correlation is only about 0.4, in essential agreement with measurements of Vela 2 and 3 during the period from July 1964 to July 1967. The relatively modest correlation is interpreted to mean that a number of speed structures observed by Mariner 2 did not endure for more than one solar rotation; those structures that did endure evolved significantly in shape, amplitude, and solar longitude from one solar rotation to the next. The analysis also shows that typical solar-wind structures occupied about 30 to 45 deg in solar longitude near 1 AU.
Mariner 9 data analysis showed a good performance of the Mars probe planetary approach navigation systems and a good agreement between measured and predicted probe-approach characteristics. It was found that all operations were completed on time and that the calibration of the instruments and the observation of a greater-than-planned number of stars resulted in a higher-than-expected measurement accuracy. The key instruments of the Mariner were TV cameras taking pictures of Phobos and Deimos against a background of stars, calibrated sun and star sensors, and a scan platform. The error models used for optical navigation system elements, the calibration of the scan platform and of the TV cameras, and the image detection and location techniques are discussed in detail.
This paper describes the selection of launch and arrival conditions and Venus and Mercury encounter aiming zones to maximize the science return from the Mariner Venus-Mercury mission. A single Mariner spacecraft will be launched in November, 1973, fly by Venus in early February, 1974, and encounter Mercury (the primary target) in late March, 1974. Mercury aiming points will provide: (1) sun and earth occultation, (2) 1000 km periapsis altitude, and (3) return to Mercury after 176 days (two Mercury years). The selected Mercury arrival dates allow high-contrast television imaging. Aiming points at Venus allow gravity assist to Mercury and also permit earth occultation.
This paper presents the results of the applications of advanced filtering methods to the determination of the interplanetary orbit of the Mariner '71 spacecraft. The advanced techniques are specific extensions of the Kalman filter. The special problems associated with applying these techniques are discussed and the particular algorithmic implementations are outlined. The advanced methods are compared against the weighted least squares filters of conventional application. The results reveal that relatively simple advanced filter configurations yield solutions superior to those of the conventional methods when applied to the Mariner '71 radio measurements.
Current plans of NASA are to take advantage of the 1977 launch opportunity by sending a Mariner class spacecraft on a gravity assisted flyby of Jupiter which will then continue on to Saturn. The background of this Mariner Jupiter-Saturn 77 Project is reviewed and science objectives for this mission as currently adapted are given. This paper illustrates properties of the Jupiter-Saturn opportunities between 1976 and 1980 to give context to the 1977 opportunity. Details of the possibilities for the 1977 launch are shown along with constraints and example candidate trajectories. Options include close flybys and/or occultations of the satellites at Jupiter and Saturn, penetration of Saturn's rings, and various occultations of the planets. A short discussion of other factors, such as navigation and planetary quarantine (documented elsewhere) are included.
A formal mission-planning process was developed for the Mariner Mars 1971 missions to allow large-scale mission-plan changes based upon flight experience. A modular approach was taken to the definition of requirements and constraints for elements of the mission. A set of rules for combining these modules was established. The concept of a standard mission day was developed in order to provide a consistent time framework for operations. The resulting process allowed for major mission revisions after the failure of Mariner 8 and again after a dust storm had obscured Mars. It allowed adaptive science planning on a short-term turnaround basis throughout the mission.
A combined data analysis and theoretical program aimed at interpreting and utilizing solar wind data obtained from Pioneer 6, Mariner 5, and Explorer 35 has been completed. A theoretical model of the radial dependence of large scale solar wind inhomogeneities was developed and used to map solar wind variations measured by Explorer 35 to various heliocentric distances and to the orbits of Mercury, Venus, and Mars. The model was also used to determine power spectra velocity, density and temperature variations of 20 R sub s from spectra obtained from the Mariner 5 data at an average heliocentric distance of 180 R sub s. Five stream-stream interaction events in the Pioneer 6 data were analyzed which confirmed the picture of a spiral compression ridge interfacing the two streams and the associated east-west deflections of the solar wind flow. Magnetopause crossings observed in Explorer 35 plasma data were used to develop statics on boundary motions at lunar distance. A study of the geomagnetic disturbance field asymmetry was performed and a model of disturbance field from a partial ring current was developed.
There are no author-identified significant results in this report. Progress in studies of the marine environment of the northern Gulf of California is described. A ship was chartered in Mexico, staffed with local seamen, equipped for oceanographic work, and is now conducting monthly cruises of 47 stations, collecting ground observations for correlation with ERTS-1 imagery in the Arizona Regional Ecological Test Site laboratory in Tucson. Progress is reported on fabrication of instrument buoys equipped with marine-adapted DCP's to transmit ground observations via satellite to Tucson. Data handling processes are described. Coordination of work with Mexican scientists is detailed.
This document describes the content and organization of the Mariner 9 Mission Test Computer/Mission Test Video System microfiche library. This 775 card library is intended to supply the user with a complete record of the images received from Mars orbit during the Mariner 9 mission operations, from 15 Nov. 1971 to 1 Nov. 1972.
The design and flight performance of the Mariner Mars 1971 power subsystem are presented. Mariner 9 was the first spacecraft to orbit another planet, and some of the power management techniques employed to support an orbital mission far from earth with marginal sunlight for its photovoltaic-battery power source are described. The performance of its nickel-cadmium battery during repetitive sun occultation phases of the mission, and the results of unique tests in flight to assess the performance capability of its solar array are reported.
A synopsis of significant results achieved within the marine resources and ocean surveys discipline of the overall ERTS program is provided. Summaries are provided of the following subdisciplines: (1) coastal processes; (2) bathymetry; (3) sea ice; (4) oceanic circulation and dynamics; and(5) living marine resources.
The author has identified the following significant results. While occupying standard oceanographic stations in the delta region of the Colorado River, two species of insects were collected which were of special interest. One of these is a single specimen of corixid bug, hitherto familiar to the investigators only as a freshwater insect, but taken swimming actively in high salinity water along with characteristic marine plankton. Further investigation showed that the species taken is well known from saline ponds but this is apparently the first record of its occurrence in a complete marine community. A small note on this collection record was prepared for publication and sent in manuscript form to NASA. The other record is of three specimens of a cicindelid beetle (normally a beach inhabitant) found at a night light for larval fish collection on station in the Colorado delta. The beetles were observed to light on and take off from water surface while actively moving around the night light. There is an interesting question of whether this species (Cicindela sinaloae schrammeli Cazier) may be especially adapted for a predatory life on the surface film, while the other two (larger) species sympatric with it are restricted to hunting on land.
It is possible to model the ultraviolet terminator observations of Mariner 9 either with a homogeneous atmosphere or with a scattering layer in addition to a homogeneous atmosphere. The characteristic shape of the twilight intensity variation is dependent on the latitude of observation. Observations north of 55N require a homogeneous model. Twilight measurements south of 55N indicate that a scattering layer may be a general Martian occurrence, at least in the evening. The day-to-day surveillance of the Martian terminator during the first 216 Mariner 9 revolutions indicates haze formation in the evening, and its continued presence until early morning is a daily occurrence in mid-latitudes up to 50N.
Selected results are presented for a considerable quantity of Mariner 9 1304-A data for the first 100 revolutions from both the bright limb and disk of Mars. The limb data suggest that the exospheric temperature is less than it was in 1969 when Mariners 6 and 7 encountered the planet. Similar (O) concentrations (0.5 to 1%) are derived for a temperature of about 300 K. Structure in the limb profiles below 200 km suggests the possibility that about 0.2 kR of the observed approximately 0.8 kR near 150 km is due to dissociative excitation of CO2. Significant differences in selected limb profiles suggest that local as well as random variations in (O) occur.