A sound education: using podcasts to develop study skills

Coping with the demands of academic study at university level can be a challenging experience for many students, and effective study skills are crucial in achieving academic success. However, librarians and teachers in higher education will know that it is not always easy to engage students in developing their study skills. How can we find new ways of stimulating the interest of our students? An innovative approach to teaching and the exploitation of new technologies can provide solutions and ideas. Podcasting has been very popular in recent years for delivering entertainment, news and other information, but podcasts are also extensively used in education, enabling students to watch or listen at a time that suits them – at home, at work or while travelling. The Skills for learning website was established over ten years ago as part of the library service at Leeds Metropolitan University to support the teaching and learning of study skills. The website offers students a wide range of resources including topics such as academic writing, time management, group skills, reflection and how to do research. There is also a team of tutors who provide workshops and tutorials. We felt that a podcast series could provide an alternative and flexible way of delivering study skills support that might appeal to a new audience. The podcasts could also be used as a stimulus in classroom teaching. As they are usually released episodically, we hoped that subscribers or visitors to our podcast page would become ‘hooked’ on the series and want to tune in to future podcasts. All the podcasts were created in-house by members of the Skills for learning team

Crater morphology and morphometry on the Uranian satellites

Fresh craters on the icy Uranian satellites exhibit a range of morphologies similar to craters on the icy satellites of Jupiter and Saturn. The general structural features found in the craters are described. Estimates of transition diameters from simple to complex crater morphologies are given for the five large Uranian satellites and 1985U1, and plotted with transition diameters on other bodies against surface gravity. Possible large-scale impacts are discussed

Mechanical and thermal properties of planetologically important ices

Two squences of ice composition were proposed for the icy satellites: a dense nebula model and a solar nebula model. Careful modeling of the structure, composition, and thermal history of satellites composed of these various ices requires quantitative information on the density, compressibility, thermal expansion, heat capacity, and thermal conductivity. Equations of state were fitted to the density data of the molecular ices. The unusual thermal and mechanical properties of the molecular and binary ices suggest a larger range of phenomena than previously anticipated, sufficiently complex perhaps to account for many of the unusual geologic phenomena found on the icy satellites

Iapetus: Tectonic structure and geologic history

Many papers have been written about the surface of Iapetus, but most of these have discussed either the nature of the strongly contrasting light and dark materials or the cratering record. Little has been said about other geologic features on Iapetus, such as tectonic structures, which would provide constraints on Iapetus' thermal history. Most references have suggested that there is no conclusive evidence for any tectonic activity, even when thermal history studies indicate that there should be. However, a new study of Iapetus' surface involving the use of stereo pairs, an extensive tectonic network has been recognized. A few new observations concerning the craters and dark material were also made. Thus the geology and geologic history of Iapetus can be more fully outlined than before. The tectonic network is shown along with prominent craters and part of the dark material in the geologic/tectonic sketch map. The topology of crater rims and scarps are quite apparent and recognizable in the different image pairs. The heights and slopes of various features given are based on comparison with the depths of craters 50 to 100 km in diameter, which are assumed to have the same depths as craters of similar diameter on Rhea and Titania

Tectonic determinations of lithospheric thickness on Ganymede and Callisto

The concept of the Maxwell time of a viscoelastic material (4.5) is used in conjunction with calculated thermal profiles to evaluate the significance of tectonic estimates of lithospheric thickness. Thermal lithospheric thicknesses provide fundamental constraints on planetary thermal histories that complement the constraints provided by dateable surface deposits of endogenic origin. Lithospheric constraints are of particular value on the icy satellites where our understanding of both rheology and surface ages is considerably poorer than it is for the terrestrial planets. Certain extensional tectonic features can and have been used to estimate lithospheric thicknesses on Ganymede and Callisto. These estimates, however, refer to the depth of the elastic lithosphere defined by the zone of brittle failure. The relation between the elastic lithosphere and the thermal lithosphere (generally defined by the zone of conductive heat transport) is not straightforward, because the depth of brittle failure depends not only on the thermal profile, but also on rheology and strain rate (or the characteristic time over which stresses build towards failure). Characteristic time considerations are not trivial in this context because stresses generating brittle failure on the icy satellites may be produced by impacts, with characteristic times of seconds to days, or by geologic processes with time scales of hundreds of millions of years

The scaling of secondary craters

Secondary craters are common features around fresh planetary-scale primary impact craters throughout most of the Solar System. They derive from the ejection phase of crater formation, thus secondary scaling relations provide constraints on parameters affecting ejection processes. Secondary crater fields typically begin at the edge of the continuous ejecta blankets (CEB) and extend out several crater radii. Secondaries tend to have rounded rims and bilateral symmetry about an axis through the primary crater's center. Prominent secondary chains can extend inward across the CEB close to the rim. A simple method for comparing secondary crater fields was employed: averaging the diameters and ranges from the center of the primary crater of the five largest craters in a secondary crater field. While not as much information is obtained about individual crater fields by this method as in more complete secondary field mapping, it facilitates rapid comparison of many secondary fields. Also, by quantifying a few specific aspects of the secondary crater field, this method can be used to construct scaling relations for secondary craters

Equal Protection - Property Taxes as a Method of Funding Public Education; San Antonio Independent School District v. Rodriguez

Suit was brought in U.S. District Court for the Western District of Texas challenging the constitutionality of the Texas school financing system on the theory that it discriminated on a basis of wealth, permitting provision of a higher quality of education to be offered the children in property-rich school districts while residents pay a lower tax rate, thus denying equal protection of the law.\u27 The District Court found the laws forming this system unconstitutional on this basis. Appeal brought the case to the Supreme Court in October of 1972, where it was reversed