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I acknowledge and agree with the comments made on Harkrider [1964] by A.D. Pierce.

A total of 201 complete television frames of Mars were returned by Mariners 6 and 7 in late July and early August of 1969. During the subsequent year over 3500 different versions of those frames were generated by computer processing involving the production of about 35,000 individual photographic prints and large amounts of computer printout as well. This extensive data processing and distribution required the significant participation of about fifteen scientists, engineers, and technicians, mainly at the Jet Propulsion Laboratory. During that same year, the processed data were analyzed and interpreted by approximately twenty-five scientists and technicians at six different institutions. The special supplement of which this is the introductory paper presents most of the scientific findings that have accrued during the first year following the Mariner 6 and 7 flybys of Mars. It constitutes a final report on the television experiment, although significant efforts are continuing. Preliminary results were presented in three papers published in August and October of 1969 [Leighton et al., 1969a, b, c]. Smith [1970] presented information about the size, shape, and surprisingly low albedo of the martian satellite Phobos. Information concerning various aspects of the camera and data systems has also been published recently [Danielson, 1970].

This is an analysis of the dispersive properties of transversely isotropic media. This kind of anisotropy is exhibited by hexagonal crystals, sediments, planar igneous bodies, ice sheets, and rolled metal sheets where the unique axis is perpendicular to the direction of surface wave propagation and the other axes are distributed randomly in the plane of the layers. Period equations are derived for waves of Rayleigh, Stoneley, and Love types, and comparisons are made, in certain cases, with ray theoretical and plane stress solutions. Anisotropy can have a pronounced effect on both the range of existence and the shape of the dispersion curves and can lead to an apparent discrepancy between Love and Rayleigh wave data. Attention is focused in this initial paper on a single solid layer in vacuo (i.e. a free plate) and a solid layer in contact with a fluid halfspace. The single layer solutions are generalized to n-layer media by the use of Haskell matrices.

The reconnaissance described in this paper was performed in 1964 and is an extension and refinement of the first observations (1962), in the 8- to 14-μ wavelength region, of the thermal emission from the lunar nighttime surface [Murray and Wildey, 1964]. The present investigation was intended to sample representatively enough of the lunar surface to determine the general character of the lunar nighttime emission and the relative abundance of nighttime infrared anomalies. More complete studies of the infrared emission with higher spatial resolution during eclipse were made at about the same time [Saari and Shorthill, 1965].

After the success of Surveyor 1 in meeting the objectives of the engineering flight series, selection from among candidate experiments led to the inclusion of the soil mechanics surface sampler (SMSS) on the Surveyor 3 payload. Although originally planned for later Surveyors, the SMSS was modified to fit the reduced telemetry and commanding capability of Surveyor 3. Specifically, the SMSS was adapted to the mounting location and the electronics interface of the approach television camera. This required a concentrated, short-term effort to modify, build, and test the SMSS to meet the demanding interface requirements. Modifications to the SMSS included removal of the strain-, acceleration-, and position-measuring systems originally planned and incorporation of a means for measuring current drawn by the motors during operation. A description of the modified device, its performance on Surveyor 3, and some conclusions about the lunar surface material are presented in this paper.