Ultraviolet HST Observations of the Jet in M87

We present new ultraviolet photometry of the jet in M87 obtained from HST WFPC2 imaging. We combine these ultraviolet data with previously published photometry for the knots of the jet in radio, optical, and X-ray, and fit three theoretical synchrotron models to the full data set. The synchrotron models consistently overpredict the flux in the ultraviolet when fit over the entire dataset. We show that if the fit is restricted to the radio through ultraviolet data, the synchrotron models can provide a good match to the data. The break frequencies of these fits are much lower than previous estimates. The implied synchrotron lifetimes for the bulk of the emitting population are longer than earlier work, but still much shorter than the estimated kinematic lifetimes of the knots. The observed X-ray flux cannot be successfully explained by the simple synchrotron models that fit the ultraviolet and optical fluxes. We discuss the possible implications of these results for the physical properties of the M87 jet. We also observe increased flux for the HST-1 knot that is consistent with previous results for flaring. This observation fills in a significant gap in the time coverage early in the history of the flare, and therefore sets constraints on the initial brightening of the flare.Comment: 14 pages, 2 figures, Accepted for publication in ApJ, changed lightcurve and caption in Figure

Infrared High-Resolution Spectroscopy of Post-AGB Circumstellar Disks. I. HR 4049 - The Winnowing Flow Observed?

High-resolution infrared spectroscopy in the 2.3-4.6 micron region is reported for the peculiar A supergiant, single-lined spectroscopic binary HR 4049. Lines from the CO fundamental and first overtone, OH fundamental, and several H2O vibration-rotation transitions have been observed in the near-infrared spectrum. The spectrum of HR 4049 appears principally in emission through the 3 and 4.6 micron region and in absorption in the 2 micron region. The 4.6 micron spectrum shows a rich 'forest' of emission lines. All the spectral lines observed in the 2.3-4.6 micron spectrum are shown to be circumbinary in origin. The presence of OH and H2O lines confirm the oxygen-rich nature of the circumbinary gas which is in contrast to the previously detected carbon-rich material. The emission and absorption line profiles show that the circumbinary gas is located in a thin, rotating layer near the dust disk. The properties of the dust and gas circumbinary disk and the spectroscopic orbit yield masses for the individual stars, M_AI~0.58 Msolar and M_MV~0.34 Msolar. Gas in the disk also has an outward flow with a velocity of $\gtrsim$ 1 km/s. The severe depletion of refractory elements but near-solar abundances of volatile elements observed in HR 4049 results from abundance winnowing. The separation of the volatiles from the grains in the disk and the subsequent accretion by the star are discussed. Contrary to prior reports, the HR 4049 carbon and oxygen isotopic abundances are typical AGB values: 12C/13C=6^{+9}_{-4} and 16O/17O>200.Comment: 42 pages, 14 figures, Accepted by Ap

Flow in a slowly-tapering channel with oscillating walls

The flow of a fluid in a channel with walls inclined at an angle to each other is investigated at arbitrary Reynolds number. The flow is driven by an oscillatory motion of the wall incorporating a time-periodic displacement perpendicular to the channel centreline. The gap between the walls varies linearly with distance along the channel and is a prescribed periodic function of time. An approximate solution is constructed assuming that the angle of inclination of the walls is small. At leading order the flow corresponds to that in a channel with parallel, vertically oscillating walls examined by Hall and Papageorgiou \cite{HP}. A careful study of the governing partial differential system for the first order approximation controlling the tapering flow due to the wall inclination is conducted. It is found that as the Reynolds number is increased from zero the tapering flow loses symmetry and undergoes exponential growth in time. The loss of symmetry occurs at a lower Reynolds number than the symmetry-breaking for the parallel-wall flow. A window of asymmetric, time-periodic solutions is found at higher Reynolds number, and these are reached via a quasiperiodic transient from a given set of initial conditions. Beyond this window stability is again lost to exponentially growing solutions as the Reynolds number is increased

Building research capacity: An exploratory model of GPs' training needs and barriers to research involvement

Copyright © 2003 Royal Australian College of General Practitioners Copyright to Australian Family Physician. Reproduced with permission. Permission to reproduce must be sought from the publisher, The Royal Australian College of General Practitioners.AIMS: To determine general practitioners' research training needs, and the barriers to involvement in research. METHOD: Semi-structured interviews with 11 GPs in rural and metropolitan South Australia, analysed using a grounded theory approach. RESULTS: General practitioners' perceptions about their research needs were limited by their own experience and focussed at an individual level. Overlapping needs and barriers emerged, categorised as: 'individual issues' (a lack of research training or experience, concepts and attitudes to research, and research interest) and 'systems issues' (funding arrangements for general practice, access to resources, opportunity for publication and the role of The Royal Australian College of General Practitioners [RACGP]). DISCUSSION: Our data provide an exploratory model that may assist in developing suitable strategies for research capacity building programs. General practitioners perceived both individual and systems solutions to building research capacity, including multifaceted interventions.A. Jones, T.A. Burgess , E.A. Farmer, J. Fuller, N.P. Stocks, J.E. Taylor and R.L. Water

Infrared Excess in the Be Star Delta Scorpii

We present infrared photometric observations of the Be binary system delta Scorpii obtained in 2006. The J,H and K magnitudes are the same within the errors compared to observations taken 10 months earlier. We derive the infrared excess from the observation and compare this to the color excess predicted by a radiative equilibrium model of the primary star and its circumstellar disk. We use a non-LTE computational code to model the gaseous envelope concentrated in the star's equatorial plane and calculate the expected spectral energy distribution and Halpha emission profile of the star with its circumstellar disk. Using the observed infrared excess of delta Sco, as well as Halpha spectroscopy bracketing the IR observations in time, we place constraints on the radial density distribution in the circumstellar disk. Because the disk exhibits variability in its density distribution, this work will be helpful in understanding its dynamics.Comment: 12 pages, 14 figures, to be published in PASP May 200

Wave propagation and scattering in reinforced concrete beams

Steel reinforcement bars (rebars) are vital to the strength of reinforced concrete (RC) structures, but can become damaged due to corrosion. Such damage is generally invisible and non-destructive testing methods are needed to assess their integrity. Guided wave methods are popular because they are capable of detecting damage using sensors placed remotely from the damage site, which is often unknown. This paper predicts free wave propagation in RC beams from which the concept of a guided wave based damage detection method emerges. The wave solutions are obtained using the wave finite element framework where a short section of a beam's cross section is modeled in conventional finite element (FE) and periodic boundary conditions are subsequently applied. Reinforcement elements are used in the FE model of the cross section as a neat and efficient means of coupling the concrete to the rebars and imposing prestress. The results show that prestress, important for static behavior, has a negligible effect on wave dispersion. A RC beam with a damaged section is modeled by coupling three waveguides, the center waveguide being identical to the outer ones except for a thickness loss in one rebar. Only small differences in cut-on frequencies are observed between the damaged and undamaged sections. However, these small differences give rise to strong reflection of some waves at frequencies close to cut-on. Below cut-on, most incident power is transmitted but experiences wave mode conversion, whereas above cut-on most power is transmitted to the same wave type. These observations form the basis for ongoing work to develop a damage detection technique premised on wave reflection near cut-on