Transient heat and mass transfer analysis of supercritical cryogenic storage systems with spherical static heaters Final report

Transient heat and mass transfer analysis of supercritical cryogenic storage systems with spherical static heaters by computer progra

Coolant pressure and flow distribution through an air-cooled vane for a high temperature gas turbine

Coolant pressure and flow distribution through air cooled vane for high temperature gas turbin

Soil survey of Vasse Research Station, Western Australia

This soil survey of the Vasse Research Station properties was carried out at the request of the Division of Plant Production of the Agriculture Western Australia. The survey followed a preliminary examination and mapping of soil series in the area by Mr T. Stoneman in 1982, after which it was concluded that more detailed survey work was required to assist farm management and research experimentation. The research station consists of two blocks, referred to here as the main block (Sussex Locations 1475, 1439, 2128, 2138, 2137, 2136, 2129, 2130, 2119, 2118, 2126 and 2125) and the hill block (Sussex Locations 3024, 3025 and part of 1864) approximately 12 km due south, and 15 km south-south-east respectively from Busselton. (Figure 1). The main (lowland) portion of the research station is approximately 610 ha in area and the hill block further south covers approximately 160 ha. The country is considered to be representative of much of the inland Swan Coastal Plain and its margin with the Whicher Range between Boyanup and Dunsborough. The work was conducted using a free survey technique where map unit boundaries and field observation sites were selected on the basis of air photo interpretation. Aerial photos enlarged to scales of 1:10,000 and 1:2000 respectively were used for the main and hill blocks. The final map presented in this report is at a uniform scale of 1:10,000. For those interested in the greater detail provided on the preliminary 1:2000 scale for the hill block map copies may be sought from the Division of Resource Management

The effect of parallel static and microwave electric fields on excited hydrogen atoms

Motivated by recent experiments we analyse the classical dynamics of a hydrogen atom in parallel static and microwave electric fields. Using an appropriate representation and averaging approximations we show that resonant ionisation is controlled by a separatrix, and provide necessary conditions for a dynamical resonance to affect the ionisation probability. The position of the dynamical resonance is computed using a high-order perturbation series, and estimate its radius of convergence. We show that the position of the dynamical resonance does not coincide precisely with the ionisation maxima, and that the field switch-on time can dramatically affect the ionisation signal which, for long switch times, reflects the shape of an incipient homoclinic. Similarly, the resonance ionisation time can reflect the time-scale of the separatrix motion, which is therefore longer than conventional static field Stark ionisation. We explain why these effects should be observed in the quantum dynamics. PACs: 32.80.Rm, 33.40.+f, 34.10.+x, 05.45.Ac, 05.45.MtComment: 47 pages, 20 figure

An unusual case of acute pulmonary embolism

Patiant with a history of hypertension presented to the emergency room with progressive dyspnoea over afew weeks. There was no relevant past history. Clinical examination revealed an elevated jugular venous pressure, pedal oedema and tenderness in the right hypochondrium

Elucidating the role of hyperfine interactions on organic magnetoresistance using deuterated aluminium tris(8-hydroxyquinoline)

Measurements of the effect of a magnetic field on the light output and current through an organic light emitting diode made with deuterated aluminium tris(8-hydroxyquinoline) have shown that hyperfine coupling with protons is not the cause of the intrinsic organic magnetoresistance. We suggest that interactions with unpaired electrons in the device may be responsible.Comment: Submitte

Step Position Distributions and the Pairwise Einstein Model for Steps on Crystal Surfaces

The Pairwise Einstein Model (PEM) of steps not only justifies the use of the Generalized Wigner Distribution (GWD) for Terrace Width Distributions (TWDs), it also predicts a specific form for the Step Position Distribution (SPD), i.e., the probability density function for the fluctuations of a step about its average position. The predicted form of the SPD is well approximated by a Gaussian with a finite variance. However, the variance of the SPD measured from either real surfaces or Monte Carlo simulations depends on $\Delta y$, the length of step over which it is calculated, with the measured variance diverging in the limit $\Delta y \to \infty$. As a result, a length scale $L_{\rm W}$ can be defined as the value of $\Delta y$ at which the measured and theoretical SPDs agree. Monte Carlo simulations of the terrace-step-kink model indicate that $L_{\rm W} \approx 14.2 \xi_Q$, where $\xi_Q$ is the correlation length in the direction parallel to the steps, independent of the strength of the step-step repulsion. $L_{\rm W}$ can also be understood as the length over which a {\em single} terrace must be sampled for the TWD to bear a "reasonable" resemblence to the GWD.Comment: 4 pages, 3 figure

AGN and starbursts at high redshift: High resolution EVN radio observations of the Hubble Deep Field

We present deep, wide-field European VLBI Network (EVN) 1.6 GHz observations of the Hubble Deep Field (HDF) region with a resolution of 0.025 arcseconds. Above the 210 microJy/beam (5sigma) detection level, the EVN clearly detects two radio sources in a field that encompasses the HDF and part of the Hubble Flanking Fields (HFF). The sources detected are: VLA J123644+621133 (a z=1.013, low-luminosity FR-I radio source located within the HDF itself) and VLA J123642+621331 (a dust enshrouded, optically faint, z=4.424 starburst system). A third radio source, J123646+621404, is detected at the 4sigma level. The VLBI detections of all three sources suggest that most of the radio emission of these particular sources (including the dusty starburst) is generated by an embedded AGN.Comment: 4 pages, 1 figure; Accepted by Astron. & Astrophys Letters ... See http://www.nfra.nl/~mag/hdf_evn.htm