A model for the prediction of in-line vortex-induced vibrations of cylindrical elements in a non-uniform steady flow

The method presently adopted in the offshore industry for predicting the amplitude of vibration of circular cylinders undergoing in-line vortex-induced excitation is demonstrated to be valid only for structures in uniform flows at sub-critical Reynolds numbers.A model which predicts the response of structural elements experiencing this phenomenon where the diameter, mass, and velocity of flow varies along the length of the structure is presented. Comparison between the results of this method and available experimental measurements is made.The model is structured to be an easily applied design tool producing an upper-bound estimate.     

A review of three transform margins off eastern Canada

 The southwest Newfoundland transform margin has been studied by deep seismic reflection and refraction. Lower crustal reflectivity strengthens towards the margin, where there is a shear zone of thinned continental crust overplated with oceanic material. The reflectivity may be due to shear fabrics in the crust. Crustal thinning probably took place by flow in the lower crust. The Ungava transform margin has been less studied but has been explored and drilled. It appears more volcanic in character. The north Baffin region has undergone a complex tectonic history and provides an example of the transition from continent–ocean to continent–continent transform motion. Received: 9 March 1995 / Revision received: 25 July 1995     

On the total geostrophic circulation of the pacific ocean: flow patterns, tracers, and transports

The large-scale circulation of the Pacific Ocean consists of two great anticyclonic gyres that contract poleward at increasing depth, two high-latitude cyclonic gyres, two westward flows along 10° to 15° north and south that are found from the surface to abyssal depths, and an eastward flow that takes place just north of the equator at the surface and at about 500m, but lies along the equator at all other depths.This pattern is roughly symmetric about the equator except for the northward flow across the equator in the west and the southward flow in the east.As no water denser than about 26.8 in σ₀ is formed in the North Pacific, the denser waters of the North Pacific are dominated by the inflow from the South Pacific. Salinity and oxygen in the deeper water are higher in the South Pacific and the nutrients are lower. These characteristics define recognizable paths as they move northward across the equator in the west and circulate within the North Pacific. Return flow is seen across the equator in the east. Part of it turns westward and then southward with the southward limb of the extended cyclonic gyre, and part continues southward along the eastern boundary and through the Drake Passage.The important differences from earlier studies are that the equatorial crossings and the deep paths of flow are defined, and that there are strong cyclonic gyres in the tropics on either side of the equator.     

A note on albedo variations of the frozen surface of Lake Simcoe during march, 1978: Research note

Abstract

The relationships between monthly anomalies of sea surface temperature (SST) and monthly anomalies of several surface wind parameters are examined using ten years of data from the mid‐latitude North Pacific Ocean. The wind parameters involve both u³ _* and curl τ, where u_* is the atmospheric friction velocity and τ the surface stress. These quantities are calculated from surface wind components analysed on synoptic (6‐hourly) maps. In order to examine the effect of synoptic disturbances, the time series of surface wind components at each grid point is high‐pass filtered (passing periods less than 10 days) and the above wind parameters are calculated from both filtered and unfiltered wind components.

Two statistically significant relationships are found between monthly anomalies of SST and those of the various wind parameters. The first is a large coherent negative correlation between monthly anomalies of u³ _* calculated from the high‐pass filtered wind components and month‐to‐month changes in the SST anomalies in the Central Pacific. This relationship is attributed to the production of turbulent vertical mixing in the ocean by synoptic disturbances in the atmosphere. The second relationship is a large positive correlation between curl τ calculated from the unfiltered wind components and SST anomaly changes in the Eastern Pacific. This relationship, which is opposite to that expected from Ekman pumping, is attributed to a negative association between the wind stress curl and the meridional advection of heat by the eastern boundary current system. It is shown that these atmospheric forcing mechanisms explain up to 10 per cent of the variance of monthly SST anomalies in a large part of the mid‐latitude North Pacific Ocean. This amount is in addition to, but certainly less than, that which can be explained by anomalous horizontal advection through statistical relationships with sea‐level pressure anomalies (Davis, 1976).     

Metallicities and ages of stellar populations at a high Galactic latitude field

We present an analysis of UBVRI data from the selected area SA 141. By applying recalibrated methods of measuring ultraviolet excess (UVX), we approximate abundances and absolute magnitudes for 368 stars over 1.3 deg² out to distances over 10 kpc. With the density distribution constrained from our previous photometric parallax investigations and with sufficient accounting for the metallicity bias in the UVX method, we are able to compare the vertical abundance distribution to those measured in previous studies. We find that the abundance distribution has an underlying uniform component consistent with previous spectroscopic results that posit a monometallic thick disc and halo with abundances of  [Fe/H]=−0.8  and −1.4, respectively. However, there are a number of outlying data points that may indicate contamination by more metal-rich halo streams. The absence of vertical abundance gradients in the Galactic stellar populations and the possible presence of interloping halo streams would be consistent with expectations from merger models of Galaxy formation. We find that our UVX method has limited sensitivity in exploring the metallicity distribution of the distant Galactic halo, owing to the poor constraint on the UBV properties of very metal-poor stars. The derivation of metallicities from broad-band UBV photometry remains fundamentally sound for the exploration of the halo but is in need of both improved calibration and superior data.     

Radio planetary nebulae in the Magellanic Clouds

We report the extragalactic radio-continuum detection of 15 planetary nebulae (PNe) in the Magellanic Clouds (MCs) from recent Australia Telescope Compact Array+Parkes mosaic surveys. These detections were supplemented by new and high-resolution radio, optical and infrared observations which helped to resolve the true nature of the objects. Four of the PNe are located in the Small Magellanic Cloud (SMC) and 11 are located in the Large Magellanic Cloud (LMC). Based on Galactic PNe the expected radio flux densities at the distance of the LMC/SMC are up to ∼2.5 and ∼2.0 mJy at 1.4 GHz, respectively. We find that one of our new radio PNe in the SMC has a flux density of 5.1 mJy at 1.4 GHz, several times higher than expected. We suggest that the most luminous radio PN in the SMC (N S68) may represent the upper limit to radio-peak luminosity because it is approximately three times more luminous than NGC 7027, the most luminous known Galactic PN. We note that the optical diameters of these 15 Magellanic Clouds (MCs) PNe vary from very small (∼0.08 pc or 0.32 arcsec; SMP L47) to very large (∼1 pc or 4 arcsec; SMP L83). Their flux densities peak at different frequencies, suggesting that they may be in different stages of evolution. We briefly discuss mechanisms that may explain their unusually high radio-continuum flux densities. We argue that these detections may help solve the 'missing mass problem' in PNe whose central stars were originally  1–8 M_⊙  . We explore the possible link between ionized haloes ejected by the central stars in their late evolution and extended radio emission. Because of their higher than expected flux densities, we tentatively call this PNe (sub)sample –'Super PNe'.     

Ne vii emission lines in the solar EUV spectrum

Recent calculations of electron and proton impact excitation rates in Nevii are used to calculate theoretical emission line ratios involving both n=0 (2–2) and n=1 (2–3) transitions in the 97–895 Å wavelength range. A comparison of these with existing solar observations, obtained by instruments on rocket flights and on the Skylab mission, reveals generally good agreement between theory and observation. This provides experimental support for the accuracy of the atomic data adopted in the line ratio calculations, and implies that the latter may be applied with confidence to the analysis of solar and stellar spectra from current and future satellite missions.