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Bioorganic comparative analysis of desert soils, Precambrian shales and meteorites by automated pyrolysis-gas chromatography-mass spectrometry system for future Mars soil analysis
Mars photography from flybys and orbiters, communicating planetary scene information to eye- brain receiver of earth based interpreters
Review of the progress of Mariner series spacecraft with details on the Mariner 4, 6, 7, 8, and 9 missions and equipment. The systems of Mariner 9 are discussed in great detail. Mariner 9 photographs of Mars, Phobos, Diemos, Martian peaks, Nix Olympica, Martian equatorial region, and some other Martian surface details are included. Diagrams of Mariner 9 daily operating profile, of Mariner 9 TV coverage vs time in orbit, and of Mariner 9 in superior conjunction on Sept. 7, 1972 are also given. It is hoped that Martian landing missions as planned in 1975 by the Viking project will be more productive than Mariner 9 in answering the question of whether life did, or does, exist on that planet.
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Two cameras equipped with selenium sulfur slow scan vidicons were used in the orbital reconnaissance of Mars by the U.S. Spacecraft Mariner 9 and the performance characteristics of these devices are presented. Digital image processing techniques have been widely applied in the analysis of images of Mars and its satellites. Photometric and geometric distortion corrections, image detail enhancement and transformation to standard map projection have been routinely employed. More specializing applications included picture differencing, limb profiling, solar lighting corrections, noise removal, line plots and computer mosaics. Information on enhancements as well as important picture geometric information was stored in a master library. Display of the library data in graphic or numerical form was accomplished by a data management computer program.
The present work summarizes the principal results of the radio occultation experiments carried out to date for Mars. The early measurements, made at the time of the Martian dust storm of 1971, showed greatly reduced temperature gradients in the daytime troposphere, indicating the heating effect of the dust. The temperature gradients that were measured later when the atmosphere was apparently free of dust, were still much lower than expected under conditions of radiative-convective balance, indicating that dynamics may play a large part in determining the temperature structure of the Martian troposphere. The surface atmospheric pressure was observed to vary widely with topography ranging from about 1 mb at the summit of the Middle Spot volcano (Pavonis Mons) to over 10 mb in the North circumpolar region. The radius of the planet was measured with accuracies ranging from about 0.25 to about 2.1 km over latitudes ranging from 86 to -80 deg. These measurements have shown that Mars has pronounced equatorial and north-south asymmetries, which make it difficult to represent its shape by a simple triaxial figure. The daytime ionosphere measurements indicated that the main ionization peak was similar in behavior to a terrestrial F1 layer and is probably produced by photoionization of carbon dioxide by solar extreme ultraviolet.
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Data obtained from the Viking missions to Mars have lead to comparisons between characteristics of that planet and certain aspects of earth. Topics discussed include: thermal and compositional evolution of the planets' interiors, the origin of their atmospheres, the history of their fluid environments, the evolution of organic material, and climatic changes. Examples of convective and magmatic activity on the crusts of the two planets are contrasted; outgassing evidenced in the crustal zones is related to the evolution of atmosphere. Analysis of experimental degassing of meteorites provides further insight into the origin and composition of planetary atmospheres. Attributes of the Martian surface, which is apparently an oxidizing rather than reducing medium, are reviewed, and explanations proposed to account for its lack of an organic richness comparable to that found on earth. Data on long-range climatic changes on earth, related to precession, obliquity, and eccentricity of the planet, may contribute to understanding of the Martian polar caps, and vice versa.
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Scientific study of Mars after Viking will focus on the following areas: planetary formation from the solar nebula, internal development, interaction with its atmosphere and with the interplanetary medium, and biological history (if any). Four basic measurement modes are outlined to pursue these areas of investigation. They are: orbital, especially polar orbits with wide area surface, atmospheric, and magnetospheric studies; in situ, which include bio-, geo-, and meteorological surface ground stations; network, using separated ground stations and, possibly, RPV aircraft; and sample-return. Various vehicle concepts for the different study modes are described.
The Viking 1 and 2 spacecraft were launched in August and September, 1975 on a ten month journey to begin an in depth study of the nature, origin and evolution of Mars. Upon arrival at Mars, the previously selected Viking 1 landing site was found to be unsuitable and a new site was selected by means of cameras mounted on the Viking orbiter, which also revealed features suggesting a history of liquid water on the Martian surface. Once the new site in the Cryse basin was selected, the Viking 1 lander separated from the orbiter and landed on July 20, 1976, followed by the Viking 2 lander in August, 1976 at a site considerably to the north of the first site. At the two sites, scanning facsimile cameras allowed the panoramic imaging of the terrain and measurements were made of local atmospheric and soil compositions, temperatures, pressures, winds and seasonal changes. Soil analyzers have not detected the presence of organic materials at these sites, and although the results of the life detection experiments are ambiguous, the likelihood of life on Mars seems extremely remote.
Photographs of the planet Mars generated by the Viking Mars program are presented and discussed. The Martian surface and its volcanoes receive particular attention. In addition, the atmosphere, temperature, surface craters, polar regions, and composition of Mars are briefly reviewed. Planetary evolution is considered. The highlights of the Mariner program for Mars are given.
This paper describes methods of processing the Mars atmosphere to supply water, oxygen and buffer gas for a Mars base. Existing life support system technology is combined with innovative methods of water extraction, and buffer gas processing. The design may also be extended to incorporate an integrated greenhouse to supply food, oxygen and water recycling. It is found that the work required to supply one kilogram of an argon/nitrogen buffer gas is 9.4 kW-hr. To extract water from the dry Martian atmosphere can require up to 102.8 kW-hr per kilogram of water depending on the relative humidity of the air.
Mars has been an object of interest for the better part of this century. To a biologist, Mars assumes special importance because many aspects of the theory of chemical evolution for the origin of life can be tested there. The central idea of this theory is that life on a suitable planet arises through a process in which the so-called biogenic elements combine to form increasingly more complex molecules under the influence of naturally-occurring energy sources ultimately resulting in the formation of replicating organic molecules. The biogenic elements are present on Mars today. Furthermore, the available evidence also strongly suggests that Mars may have had an early history similar to that of the Earth, including a period in which large amounts of liquid water once flowed on its surface and a denser atmosphere and higher global temperatures prevailed. This is important since many lines of evidence indicate that living organisms were already present on the Earth within the first billion years after its formation at a time when the environment on Mars may have closely resembled that of Earth. Our current knowledge of the state of chemical evolution on Mars can best be described as paradoxical. Most of what we have learned has come from experiments performed on the Viking landers. The combination of planned investigations covered a broad range of techniques to detect signs of chemical evolution. The most surprising data from all of these was the absence of any detectable quantities of organic compounds at the two landing sites. On the other hand, the Viking experiments did indicate that the Martian surface samples contained unidentified strong oxidant(s) that could account for their absence.
Three major reasons for the continued study of the weather and climate of Mars are: (1) the engineering support of future unmanned and manned missions, including operations on the Martian surface, (2) the comparative study of the climates of earth and Mars, and (3) the perspective provided by understanding what Mars is really like now and how it got that way. Together, the suite of national and international missions to Mars currently in progress and in the advanced planning stages could provide a credible data base for addressing many outstanding climatic questions, as well as greatly improving current engineering models of the Mars atmosphere and surface.
Advanced chemical propulsion using Metallized Propellants (MP) can lead to significant reductions in launch mass for piloted Mars missions. MP allow the propellant density or the specific impulse I(sub sp) of the propulsion system, or both, to increase. It can reduce the propellant mass and the propulsion system dry mass. Detailed mass-scaling equations and estimates of the I(sub sp) for several MP combinations are presented. The most significant savings with MP are derived from increasing the payload delivered to Mars. For the mass in low Earth orbit (LEO), a metallized Mars transfer vehicle can deliver 20 to 22 percent additional payload. This 20-percent payload increase reduces the total number of Mars flights and therefore significantly reduces the number of Space Transportation System-Cargo launches for the entire Mars architecture. Using MP to reduce the mass in LEO per flight is not as effective as increasing the payload delivery capacity. The mass saving per flight, while delivering the same payload with a higher I(sub sp) system, is much smaller. Using MP in all of the Mars propulsion systems would produce a modest 3.3 percent LEO mass saving. This translates into a saving of 38,000 kg over the mass required with O2/H2 propulsion. A Mars excursion vehicle using Earth- or space-storable propellants for the ascent can be an alternative to storing cryogenic H2 on Mars. A space-storable system using oxygen/monomethyl hydrazine/aluminum (O2/MMH/Al) would deliver the lowest mass penalty over O2/H2. For lower-energy expedition missions the LEO mass penalty for using metallized O2/MMH/Al would be only 3 to 5 percent.
The results of a workshop on the feasibility and logic of a manned Mars mission and base are discussed. Criteria for evaluating the merit of proposed Mars expeditions are presented, and the precursor mission requirements of various proposed scenarios are considered. Science objectives and how various mission scenarios would serve them are addressed. Issues of launch, assembly, transportation, and Mars base infrastructure are examined. Advanced propulsion concepts for use in a Mars mission are discussed, and international cooperation in a Mars mission is addressed. The relevance of the workshop to the crisis of education in America is considered.
The Mars telecommunications system as currently conceived at JPL calls for the use of multifrequency bands in combination with advanced space and ground technologies. This paper reviews the architecture and technology requirements for the telecommunications system. It also presents an overview of the technology development plan.