Pausing patterns: differences between L2 learners and native speakers

This paper reports on a comparative study of pauses made by L2 learners and native speakers of English while narrating picture stories. The comparison is based on the number of pauses and total amount of silence in themiddle and at the end of clauses in the performance of 40 native speakers and 40 L2 learners of English. The results of the quantitative analyses suggest that, although the L2 learners generally pausemore repeatedly and have longer periods of silence than the native speakers, the distinctive feature of their pausing pattern is that they pause frequently in the middle of clauses rather than at the end. The qualitative analysis of the data suggests that some of the L2 learners’mid-clause pauses are associated with processes such as replacement, reformulation, and online planning. Formulaic sequences, however, contain very few pauses and therefore appear to facilitate the learners’ fluency.

Spiral jetty, thirty seven years later: the cinematic time of James Benning

This article considers cinematic time in James Benning’s film, casting a glance (2007), in relation to its subject, Robert Smithson’s 1970 earthwork Spiral Jetty, and his film of the same name. The radicalism of Smithson’s thinking on time has been widely acknowledged, and his influence continues to pervade contemporary artistic practice. The relationship of Benning’s films with this legacy may appear somewhat oblique, given their apparent phenomenological rendition of ‘real time’. However, closer examination of Benning’s formal strategies reveals a more complex temporal construction, characterized by uncertain intervals that interrupt the folding of cinematic time into the flow of consciousness. Smithson’s film uses cinematic analogy to gesture towards vast reaches of geological time; Benning’s film creates a simulated timescale to evoke the short history of the earthwork itself. Smithson’s embrace of the entropic was a counter-cultural stance at the end of the1960s, but under the shadow of ecological disaster, this orientation has come to appear melancholy and romantic rather than radical. Benning’s film returns the jetty to anthropic time, but raises questions about the ways we inhabit time. His practice of working with ‘borrowed time’ is particularly suited to the cultural and historical moment of his later work.

Trace fossils and pseudofossils from the Wealden strata (non-marine Lower Cretaceous) of southern England

The trace fossils of the Wealden (non-marine Lower Cretaceous) of southern England are described. Sixteen invertebrate ichnotaxa include Agrichnium fimbriatus, Beaconites antarcticus, B. barretti, Cochlichnus anguineus, Diplichnites triassicus, Diplocraterion parallelum, Lockeia siliquaria, L. serialis, Monocraterion cf. tentaculum, Palaeophycus striatus, P. tubularis, Planolites montanus, Protovirgularia rugosa, Rhizocorallium isp., Scoyenia cf. gracilis, Unisulcus minutus, insect and root traces. Tetrapod tracks and trackways include tridactyl Iguanodontipus burreyi and other ornithopods, theropod, and tetradactyl sauropod (or possibly ankylosaur), together with extensive dinosaur tramplings. Coprolites are referred to two broad types: spiral, with or without included fish scales (attributable to sharks), and elongate and irregular (possibly produced by reptiles). A skinprint and two types of pseudofossil are also included. Five environmental associations are recognised: (1) lacustrine/lagoonal; (2) brackish incursions (flooding events) into the lacustrine/lagoonal environment; (3) a marginal lacustrine association with fluvial input; (4) a fluvial (lacustrine delta) association; (5) floodplain sediments (seasonal wetlands). These associations are assigned to the fluvial-lacustrine Scoyenia Ichnofacies and the incursions to Glossifungites lchnofacies. (c) 2005 Elsevier Ltd. All rights reserved.

What's in a name? Lexical knowledge drives infants' visual preferences in the absence of referential input

Seventeen-month-old infants were presented with pairs of images, in silence or with the non-directive auditory stimulus 'look!'. The images had been chosen so that one image depicted an item whose name was known to the infant, and the other image depicted an image whose name was not known to the infant. Infants looked longer at images for which they had names than at images for which they did not have names, despite the absence of any referential input. The experiment controlled for the familiarity of the objects depicted: in each trial, image pairs presented to infants had previously been judged by caregivers to be of roughly equal familiarity. From a theoretical perspective, the results indicate that objects with names are of intrinsic interest to the infant. The possible causal direction for this linkage is discussed and it is concluded that the results are consistent with Whorfian linguistic determinism, although other construals are possible. From a methodological perspective, the results have implications for the use of preferential looking as an index of early word comprehension.

Orographic Enhancement of Precipitation inside Hurricane Dean

On 17 August 2007, the center of Hurricane Dean passed within 92 km of the mountainous island of Dominica in the West Indies. Despite its distance from the island and its category 1–2 state, Dean brought significant total precipitation exceeding 500 mm and caused numerous landslides. Four rain gauges, a Moderate Resolution Imaging Spectroradiometer (MODIS) image, and 5-min radar scans from Guadeloupe and Martinique are used to determine the storm’s structure and the mountains’ effect on precipitation. The encounter is best described in three phases: (i) an east-northeast dry flow with three isolated drifting cells; (ii) a brief passage of the narrow outer rainband; and (iii) an extended period with south-southeast airflow in a nearly stationary spiral rainband. In this final phase, from 1100 to 2400 UTC, heavy rainfall from the stationary rainband was doubled by orographic enhancement. This enhancement pushed the sloping soils past the landslide threshold. The enhancement was caused by a modified seeder–feeder accretion mechanism that created a “dipole” pattern of precipitation, including a dry zone over the ocean in the lee. In contrast to normal trade-wind conditions, no terrain triggering of convection was identified in the hurricane environment.

The zonal asymmetry of the Southern Hemisphere storm-track

Atmospheric general circulation model experiments have been performed to investigate how the significant zonal asymmetry in the Southern Hemisphere (SH) winter storm track is forced by sea surface temperature (SST) and orography. An experiment with zonally symmetric tropical SSTs expands the SH upper-tropospheric storm track poleward and eastward and destroys its spiral structure. Diagnosis suggests that these aspects of the observed storm track result from Rossby wave propagation from a wave source in the Indian Ocean region associated with the monsoon there. The lower-tropospheric storm track is not sensitive to this forcing. However, an experiment with zonally symmetric midlatitude SSTs exhibits a marked reduction in the magnitude of the maximum intensity of the lower-tropospheric storm track associated with reduced SST gradients in the western Indian Ocean. Experiments without the elevation of the South African Plateau or the Andes show reductions in the intensity of the major storm track downstream of them due to reduced cyclogenesis associated with the topography. These results suggest that the zonal asymmetry of the SH winter storm track is mainly established by stationary waves excited by zonal asymmetry in tropical SST in the upper troposphere and by local SST gradients in the lower troposphere, and that it is modified through cyclogenesis associated with the topography of South Africa and South America.

Probing the large-scale topology of the heliospheric magnetic field using Jovian electrons

Jupiter’s magnetosphere acts as a point source of near-relativistic electrons within the heliosphere. In this study, three solar cycles of Jovian electron data in near-Earth space are examined. Jovian electron intensity is found to peak for an ideal Parker spiral connection, but with considerable spread about this point. Assuming the peak in Jovian electron counts indicates the best magnetic connection to Jupiter, we find a clear trend for fast and slow solar wind to be over- and under-wound with respect to the ideal Parker spiral, respectively. This is shown to be well explained in terms of solar wind stream interactions. Thus, modulation of Jovian electrons by corotating interaction regions (CIRs) may primarily be the result of changing magnetic connection, rather than CIRs acting as barriers to cross-field diffusion. By using Jovian electrons to remote sensing magnetic connectivity with Jupiter’s magnetosphere, we suggest that they provide a means to validate solar wind models between 1 and 5 AU, even when suitable in situ solar wind observations are not available. Furthermore, using Jovian electron observations as probes of heliospheric magnetic topology could provide insight into heliospheric magnetic field braiding and turbulence, as well as any systematic under-winding of the heliospheric magnetic field relative to the Parker spiral from footpoint motion of the magnetic field.

Suprathermal electron evolution in a Parker spiral magnetic field

Suprathermal electrons (>70 eV) form a small fraction of the total solar wind electron density but serve as valuable tracers of heliospheric magnetic field topology. Their usefulness as tracers of magnetic loops with both feet rooted on the Sun, however, most likely fades as the loops expand beyond some distance owing to scattering. As a first step toward quantifying that distance, we construct an observationally constrained model for the evolution of the suprathermal electron pitch-angle distributions on open field lines. We begin with a near-Sun isotropic distribution moving antisunward along a Parker spiral magnetic field while conserving magnetic moment, resulting in a field-aligned strahl within a few solar radii. Past this point, the distribution undergoes little evolution with heliocentric distance. We then add constant (with heliocentric distance, energy, and pitch angle) ad-hoc pitch-angle scattering. Close to the Sun, pitch-angle focusing still dominates, again resulting in a narrow strahl. Farther from the Sun, however, pitch-angle scattering dominates because focusing is effectively weakened by the increasing angle between the magnetic field direction and intensity gradient, a result of the spiral field. We determine the amount of scattering required to match Ulysses observations of strahl width in the fast solar wind, providing an important tool for inferring the large-scale properties and topologies of field lines in the interplanetary medium. Although the pitch-angle scattering term is independent of energy, time-of-flight effects in the spiral geometry result in an energy dependence of the strahl width that is in the observed sense although weaker in magnitude.

On the evolution of the solar wind between 1 and 5 AU at the time of the Cassini Jupiter flyby: Multispacecraft observations of interplanetary coronal mass ejections including the formation of a merged interaction region

The Cassini flyby of Jupiter occurred at a time near solar maximum. Consequently, the pre-Jupiter data set reveals clear and numerous transient perturbations to the Parker Spiral solar wind structure. Limited plasma data are available at Cassini for this period due to pointing restrictions imposed on the instrument. This renders the identification of the nature of such structures ambiguous, as determinations based on the magnetic field data alone are unreliable. However, a fortuitous alignment of the planets during this encounter allowed us to trace these structures back to those observed previously by the Wind spacecraft near the Earth. Of the phenomena that we are satisfactorily able to trace back to their manifestation at 1 AU, two are identified as being due to interplanetary coronal mass ejections. One event at Cassini is shown to be a merged interaction region, which is formed from the compression of a magnetic cloud by two anomalously fast solar wind streams. The flux-rope structure associated with this magnetic cloud is not as apparent at Cassini and has most likely been compressed and deformed. Confirmation of the validity of the ballistic projections used here is provided by results obtained from a one-dimensional magnetohydrodynamic projection of solar wind parameters measured upstream near the Earth. It is found that when the Earth and Cassini are within a few tens of degrees in heliospheric longitude, the results of this one-dimensional model predict the actual conditions measured at 5 AU to an impressive degree. Finally, the validity of the use of such one-dimensional projections in obtaining quasi-solar wind parameters at the outer planets is discussed.