Cities of God? Medieval urban forms and their Christian Symbolism

Situated in the context of recent geographical engagements with 'landscape', this paper combines 'morphological' and 'iconographic' landscape interpretations to examine how urban forms were perceived in late medieval Europe. To date, morphological studies have mapped the medieval city either by classifying urban layouts according to particular types, or by analysing plan forms of particular towns and cities to reveal their spatial evolution. This paper outlines a third way, an 'iconographic' approach, which shows how urban forms in the Middle Ages conveyed Christian symbolism. Three such 'mappings' explore this thesis: the first uses textual and visual representations which show that the city was understood as a scaled-down world â?? a microcosm â?? linking city and cosmos in the medieval mind; the second 'mapping' develops this theme further and suggests that urban landscapes were inscribed with symbolic form through their layout on the ground; while the third looks at how Christian symbolism of urban forms was performed through the urban landscape in perennial religious processions. Each of these 'mappings' points to the symbolic, mystical significance urban form had in the Middle Ages, based on religious faith, and they thus offer a deepened appreciation of how urban landscapes were represented, constructed and experienced at the time.

Opacity in the upper atmospheres of active stars - II. AD Leonis

We present FUV and UV spectroscopic observations of AD Leonis, with the aim of investigating opacity effects in the transition regions of late-type stars. The C III lines in FUSE spectra show significant opacity during both the quiescent and flaring states of AD Leonis, with up to 30% of the expected flux being lost during the latter. Other FUSE emission lines tested for opacity include those of O VI, while C IV, Si IV and N V transitions observed with STIS are also investigated. These lines only reveal modest amounts of opacity with losses during flaring of up to 20%. Optical depths have been calculated for homogeneous and inhomogeneous geometries, giving path lengths of approximate to 20 - 60 km and approximate to 10 - 30 km, respectively, under quiescent conditions. However path lengths derived during flaring are approximate to 2 - 3 times larger. These values are in excellent agreement with both estimates of the small-scale structure observed in the solar transition region, and path lengths derived previously for several other active late-type stars.