Pioneer 11 vector helium magnetometer observations of Saturn's planetary magnetic field, magnetosphere, magnetopause, and bow shock are presented. Models based on spherical harmonic analyses of measurements inside 8 Rs reveal that the planetary field has a high degree of symmetry about the rotation axis. The vector dipole moment of 0.2 G Rs³ has a tilt angle less than 1° and is offset along the polar axis 0.04±0.02 Rs. Equatorial offsets derived from the models show substantial variability and could be consistent with a very small offset. Beyond 10 Rs, near the noon meridian, the field topology is characteristic of a dipole field being compressed by high-speed solar wind. There is no evidence of plasma outflow, i.e., a planetary wind. Near the dawn meridian the field lines in the outer magnetosphere are stretched-out into a nearly equatorial orientation. Crossings of a thin current sheet are observed, apparently caused by motions driven from outside the magnetosphere. The field above and below the current sheet spirals out of the magnetic meridian plane at large distances to point tailward and parallel to the magnetopause. The location of the magnetopause is consistent with a shape that is similar to that of the earth but perhaps more blunt, as suggested by the attitude of the magnetopause near dawn. Near both the noon and dawn magnetopause the field in the magnetosheath equals or exceeds the field in the magnetosphere. The noon observations suggest a piling-up of magnetosheath field lines adjacent to the magnetopause. Large impulsive field compressions are observed in the magnetosheath near noon. Multiple crossings of the bow shock are observed, and the absence of significant changes in field direction shows that it is quasi-perpendicular. The speeds of motion of the shock toward and away from Saturn are estimated to be 150 and 50 km/s, respectively. A shock thickness of ∼2000 km is inferred.

The characteristics of the magnetic signature measured by Pioneer 11 during the several hour interval around the crossing of Titan's L shell have been found to be consistent with plausible models of the interaction of a 200 km/s corotating magnetized plasma with a conducting or magnetized object. The observed manner in which the magnetic fluctuations varied throughout the interval, the average magnetosheath/ambient field amplitude ratio, and the occurrence of a field minimum at the time of closest approach to the axis of the extended Titan tail are all consistent with the detection of a magnetic wake roughly 145 RT downstream from Titan. In addition, values of the plasma mass density derived from the interaction geometry are consistent with an upper limit inferred from in situ plasma measurements obtained during the outbound leg of Pioneer's trajectory at Saturn. Although two magnetic events of similar duration occurred within 10 hours and on either side of the Titan related event, they coincided closely with probable passage of the spacecraft through tail and/or ring current systems. In addition, the character of the Titan interval appears to differ from the other two in a number of other important aspects.

Pioneer 10 magnetic field measurements, supplemented by previously published plasma data, have been used to identify shocks at 2.2 AU associated with the large solar flares of early August 1972. The first three flares, which gave rise to three forward shocks at Pioneer 9 and at earth, led to only a single forward shock at Pioneer 10. The plasma driver accompanying the shock has been tentatively identified. A local shock velocity at Pioneer 10 of 717 km/s has been estimated by assuming that the shock was propagating radially across the interplanetary magnetic field. This velocity and the rise time of ≃2 s imply a shock thickness of ∼1400 km, which appears to be large in comparison with the characteristic plasma lengths customarily used to account for the thickness of the earth's bow shock. This Pioneer 10 shock is identified with the second forward shock observed at Pioneer 9, which was then at 0.8 AU and radially aligned with Pioneer 10, since it was apparently the only Pioneer 9 shock that was also driven. The local velocity of the Pioneer 9 shock of 670 km/s, previously inferred by other authors, compares reasonably well with the local velocity at Pioneer 10, but both values are significantly smaller than the average value computed from the time interval required for the shock to propagate from the sun to Pioneer 9 (2220 km/s). The velocity implied by the time required to propagate from Pioneer 9 to Pioneer 10 (770 km/s) is in reasonable agreement with the local velocities. The fourth solar flare also gave rise to a forward shock at Pioneer 10 as well as at Pioneer 9. The local velocity at Pioneer 10, estimated on the basis of quasi-perpendicularity, is 660 km/s, a value which again agrees well with previously derived velocities for the Pioneer 9 shock of 670 km/s. The local velocities for this shock and the velocity between Pioneer 9 and Pioneer 10 (635 km/s) are also significantly less than the average velocity of propagation from the sun to Pioneer 9 (830 km/s). The general finding that the local velocities of both shocks are approximately equal at 0.8 and 2.2 AU but significantly slower than the average speeds nearer the sun is interpreted as evidence of a major deceleration of the shocks as they propagate outward from the sun that is essentially completed when the shocks reach 0.8 AU, there being little, if any, subsequent deceleration. This conclusion is qualitatively inconsistent with previous inferences of a deceleration of the shocks as they propagate from 0.8 to 2.2 AU. A third, reverse shock is also identified in the Pioneer 10 data which was not seen either at Pioneer 9 or at earth. The estimated speed of this shock is 530 km/s, and its estimated thickness is ≲500 km, which compares well with an anticipated proton inertial length of 500 km.

A model for the night side Jovian magnetic field is derived partly on the basis of theoretical considerations and partly on the basis of the magnetic field data obtained during the outbound leg of the path of Pioneer 10. This model can explain the observed sawtooth modulation of energetic particle fluxes in terms of closed and open field lines that cannot contain the particles. The model is applicable only to the Jovian magnetotail.

Using the data from Veneras 4–8 and Mariners 5 and 10 related to the composition and structure of the atmosphere of Venus, the three scans obtained with the microwave radiometer on Mariner 2 at a wavelength of 1.9 cm have been reanalyzed. In the previous analysis of the microwave data, both the percentage of Co2 and the surface pressures were considerably lower than the in situ measurements and the assumed longitudinal temperature gradient was much larger than indicated by more recent measurements. Using these more recent data, it has not been possible to match the measured scan ratios with or without any spherically symmetric distribution of microwave cloud absorber. The scan ratios, therefore, require the existence of different average values of microwave cloud opacity for each scan. In addition, the anomalous temperature drop observed in the south polar region of the terminator scan has been found to require a very opaque microwave cloud in the local zenith angle range of 40°–70°. This type of distribution is consistent with the trend seen in the Mariner 2 infrared terminator scan suggesting some degree of coupling between the infrared and microwave clouds. It is suggested that some of the variability seen in the earth-based interferometer data may be a result of changes in the distribution of the microwave clouds over the disc of the planet.