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Academics in an engineering school at an Australian university participated in peer observation of a teaching program using a partnership approach. The present case study explains and discusses program aims, design, process and outcomes. The success of the program was dependent on four critical elements: educational leadership; a staged, voluntary, opt-in/out-out process involving a hands-on preparatory workshop and trial observation; partnering early-career and experienced academic staff; and an "external to faculty" coordinator. The importance of these four elements, the stages of the program and the impact on the development of collegiality within the school and aspects of the teaching role are discussed. This case offers further insights into the complexities of peer observation of teaching and a tested framework for introducing peer observation of teaching programs within schools and departments. (Contains 2 tables and 2 figures.)

Discussion of role-play focuses on a case study of an asynchronous, anonymous online role-play at an Australian university within a WebCT bulletin board that was designed as an alternative to an existing face-to-face workshop to offer more flexible access for participants. Suggests further research needs. (Author/LRW)

To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2009.02.027 Byline: Beth Ellen Clark (a), Maureen E. Ockert-Bell (a), Ed A. Cloutis (b), David Nesvorny (c), Thais Mothe-Diniz (d), Schelte J. Bus (e) Keywords: Asteroids; Asteroids; composition; Asteroids; surfaces Abstract: This is the first focused study of non-Eos K asteroids. We have observed a total of 30 K-complex objects (12 K-2 Sk- and 13 Xk-type asteroids (from the Bus taxonomy), plus 3 K-candidates from previous work) and we present an analysis of their spectral properties from 0.4 to 2.5 [mu]m. We targeted these asteroids because their previous observations are spectrally similar enough to suggest a possible compositional relationship. All objects have exhibited spectral redness in the visible wavelengths and minor absorptions near 1 micron. If, as suggested, K-complex asteroids (including K, Xk, and Sk) are the parent bodies of carbonaceous meteorites, knowledge of K-asteroid properties and distribution is essential to our understanding of the cosmochemical importance of some of the most primitive meteorite materials in our collection. This paper presents initial results of our analysis of telescopic data, with supporting analysis of laboratory measurements of meteorite analogs. Our results indicate that K-complex asteroids are distinct from other main belt asteroid types (S, B, C, F, and G). They do not appear to be a subset of these other types. K asteroids nearly span the range of band center positions and geometric albedos exhibited by the carbonaceous chondrites (CO, CM, CV, CH, CK, CR, and CI). We find that B-, C-, F- and G-type asteroids tend to be darker than meteorites, and can have band centers longer than any of the chondrites measured here. This could indicate that K-complex asteroids are better spectral analogues for the majority of our carbonaceous meteorites than the traditional B-, C-, F- and G-matches suggested in the literature. This paper present first results of our ongoing survey to determine K-type mineralogy, meteorite linkages, and significance to the geology of the asteroid regions. Author Affiliation: (a) Department of Physics, Ithaca College, Ithaca, NY 14850, USA (b) Department of Geography, University of Winnipeg, Winnipeg, MB, R3B 2E9, Manitoba, Canada (c) Department of Space Sciences, Southwest Research Institute, 1050 Walnut Street 300, Boulder, CO 80302, USA (d) Universidade Federal do Rio de Janeiro, Observatorio do Valongo, Ladeira Pedro AntA[acute accent]nio, 43 CEP 20080-090, Rio de Janeiro, Brazil (e) University of Hawaii, Institute for Astronomy, 640 North A'ohoku Place, 209, Hilo, HI 96720-2700, USA Article History: Received 27 November 2007; Revised 23 January 2009; Accepted 3 February 2009

During the first six orbits of the Galileo spacecraft's prime mission, the Solid State Imaging (SSI) system acquired multispectral image mosaics of Jupiter's Great Red Spot, an equatorial belt/zone boundary, a '5-[[micro]meter] hot spot' similar to the Galileo Probe entry site, and two of the classic White Ovals. We present mosaics of each region, approximating their appearance at visible wavelengths and showing cloud height and opacity variations. The local wind field is derived by tracking cloud motions between multiple observations of each region with time separations of roughly 1 and 10 hr. Vertical cloud structure is derived in a companion paper by Banfield et al. (Icarus 135, 230-250). Galileo's brief, high-resolution observations complement Earth-based and Voyager studies and offer local meteorological context for the Galileo Probe results. Our results show that the dynamics of the zonal jets and large vortices have changed little since Voyager, with a few exceptions. We detect a cyclonic current within the center of the predominantly anticyclonic Great Red Spot. The zonal velocity difference between 0 [degrees] S and 6 [degrees] S has increased by 20 m [sec.sup.-1]. We measure a strong northeast flow approaching the hot spot. This flow indicates either massive horizontal convergence or the presence of a large anticyclonic vortex southeast of the hot spot. The current compact arrangement of two White Ovals and a cyclonic structure greatly perturbs the zonal jets in that region. Key Words: Jupiter atmosphere; atmospheric dynamics; image processing; spacecraft.

Galileo's Solid State Imaging camera recorded six images at wavelengths from 0.41 to 0.99 [[micro]meter] of Europa's trailing hemisphere ([approximately]1.6 km/pixel resolution) during the G1 orbit (1st orbit - target Ganymede) of the nominal mission. We have photometrically corrected these data and extracted spectra representing Europa's diverse geologic terrains. The goals of the analysis of these spectra are (1) to determine whether Europa's geologic units differ spectrally from one another, (2) to determine the number of color components necessary to explain Europa's dark material spectral behavior, and (3) to examine how europan dark materials may change in color with time. Our data indicate that europan dark spots, lineaments and triple band side materials represent a single 'dark' and reddish endmember component. We see no evidence for more than one dark endmember; however the dark endmember seen in these G1 data is probably not a 'pure' exposure of europan dark material. Mottled terrains, brighter lineaments, and aging triple bands can be modeled by a mixture of bright plains materials and the dark component. Exposures of europan dark materials may thus be brightening with time, eventually blending into the surrounding bright plains. Key Words: Europa; Galileo; multispectral imaging.