8- to 13-μm spectra of asteroids

We present 8- to 13-μm spectra of the main-belt asteroids 1, 2, 6, 7, 10, 16, 45, 51, 56, 65, 78, and 451. None of these exhibit pronounced emission features, and all can be fitted reasonably well using a standard thermal model. We also present wide- and narrowband photometry of 19 Fortuna, which has previously been reported to show an emission feature in this region.     

Linking large-parallax Spitzer–CFHT–VLT astrometry of asteroids

We show that the new ephemeris-space multiple-address-comparison (eMAC) method solves asteroid linking problems despite large parallaxes by applying the method to astrometric asteroid observation sets obtained nearly simultaneously with the Spitzer space telescope, the Canada–France–Hawaii Telescope (CFHT), and European Southern Observatory's Very Large Telescope (VLT). For main-belt asteroids, the parallax between Spitzer and the Earth-based telescopes is approximately one degree which is large as compared to a typical parallax for solely Earth-based telescopes in the arcseconds regime. In the eMAC method, we reduce the initially huge amount of possible linkages between observation sets by comparing samples of ephemerides that have been computed separately for all sets at, say, three common dates. If the non-zero ephemeris probability densities overlap at all common dates, we try to find an orbit solution for these so-called trial linkages. If there exists an orbit which reproduces all the astrometric observations assuming predefined observational errors, we call it a linkage. Known asteroids are independently identified among Spitzer, CFHT, and VLT astrometry, and comparing the identified observations to the linkages found shows that the method found all known correct linkages present in the data. In addition, we also found five previously unpublished linkages between Spitzer astrometry and Earth-based astrometry. Based on our simulations, we found virtually all Spitzer-related linkages between two single-night observation sets, and more than 99.4% of linkages between two single-night observation sets obtained by Earth-based observatories. Virtually all correct linkages consisting of at least three single-night sets were also detected. The results show that large-parallax discovery observations made from a spacecraft can be linked to Earth-based follow-up observations to ensure that the objects are not lost. Furthermore, we compute the heliocentric and Spitzer-centric distances as well as the corresponding solar phase angles at the dates of Spitzer observations. Based on comparisons to simulated geocentric observations, we also show that, for typical nearly-simultaneous observations, the parallax reduces the distance uncertainties by several orders of magnitude.     

Land degradation and climate change in South Africa

This paper considers the potential impact of future climate change on the nature and extent of land degradation in South Africa. The basis of the assessment is the comprehensive review published by the Department of Environmental Affairs and Tourism (DEA&T) as a contribution to the South African effort in respect of the United Nations Convention to Combat Desertification. The DEA&T report is founded on information collated from 34 workshops, one in each of the agricultural regions of South Africa, involving some 453 participants consisting mainly of agricultural extension officers and soil conservation technicians. This analysis reveals that land degradation is underpinned by poverty and its structural roots in colonial and apartheid political planning. Nevertheless, future climate change represents a key challenge to the developing economies of countries like South Africa. Regionally downscaled models predicting the nature and degree of rainfall changes in the future are used to assess the possible impact of future change on the South African land degradation situation. It is concluded that the most severely degraded areas of the country, including large areas of the former 'homeland' states, are likely to become even more susceptible under predicted climate change scenarios.     

Colour changes on Jupiter

An analysis of four-colour photographic images of Jupiter taken during 1970–1974 is presented. It is shown that major global and hemispheric changes in colour—mainly in the blue— occurred over this period.     

The detection of fast-moving asteroids and comets by IRAS

The Infrared Astronomical Satellite (IRAS) was used to search for fast-moving objects in the inner Solar System. The selection effects and limitations of the search are examined with particular reference to the objects which may be present in the moving-object data base at JPL. It is shown that the two new Apollo asteroid discoveries are in fair agreement with the discovery rate by ground-based telescopes. IRAS discovered six comets which is also consistent with the discovery rate for ground-based searches. It is estimated that there are 20–30 comets but no Apollo asteroids in the hours-confirmed moving-object data base established by the IRAS project.     

The origin and evolution of the atmospheres of the terrestrial planets

The chemical nature of the Earth's atmosphere is determined by its interaction with the biosphere, hydrosphere and lithosphere. Detailed balance is maintained over long time periods by a complex series of cyclical processes. The chemical differences between the atmosphere of the Earth, on the one hand, and the atmospheres of Venus and Mars, on the other, can be understood in terms of the greater complexity of the terrestrial interactions. When this has been taken into account, the origin of all three planetary atmospheres can be explained as resulting from degassing. Despite the similarity of the atmospheres of Venus and Mars, it seems necessary to invoke different mechanisms for the low amount of water vapour on each.     

Light and dark spots in the equatorial regions of Jupiter

The lifetimes and motions of dark and light spots in the equatorial regions of Jupiter have been studied for the 1972 apparition. The difference in lifetimes of the two types of spot is demonstrated, as are their differing modes of formation and disappearance. The way in which the spots interact is examined in detail, and it is pointed out that this may have implications for the fluid dynamics of the Jovian atmosphere,     

A simplified model for deriving planetary surface temperatures as a function of atmospheric chemical composition

The surface temperature of a planet with an atmosphere depends, amongst other factors, on the atmospheric chemical composition and surface pressure. However, the detailed calculation of surface temperature variations as a function of atmospheric composition is extremely complex. We therefore present in this paper a simplified model which can be used to follow surface temperature changes over periods up to the lifetime of the solar system. We apply this model to a number of chemical constituents of interest in studying the evolution of planetary atmospheres (with special reference to the Earth).     

The evolution of the surface temperature of Mars

Changes in the average surface temperature of Mars are studied as a function of the time that has elapsed since the origin of the planet. Time variations in the factors influencing the surface temperature are investigated: and approximate methods for computing the effect of such variations are discussed. Three possible degassing sequences are postulated, and their likely effects for the presence of liquid water on the Martian surface are assessed.     

Eddy current torques,air torques,and the spin decay of cylindrical rocket bodies in orbit

This paper considers the torques causing spin decay in cylindrical rocket bodies in orbit. Eddy current torques, due to the Earth's magnetic field, are estimated using Smith's (1962) model—a hollow cylindrical conducting shell, tumbling about a transverse axis. Air torques are estimated by numerical integration of aerodynamic moments over the rocket surface. It is shown that for Cosmos rockets, 7.4 m long and 2.4 m in diameter, eddy current torques outweigh air torques by several orders of magnitude at altitudes near 500 km, and that they are dominant at altitudes down to 160 km. Visual observations of several such rockets illustrate a variation of spin decay time with altitude which supports this conclusion. The same observations suggest that a few Cosmos rockets may be special cases, different from the rest in construction.