‘Real business’? : gendered identities in accounting and management academia

This paper explores the gendered identities of women academics in accounting and management academia. Drawing upon autoethnographical detail, we reflect upon the complexities of identities as they are constructed, developed, experienced and understood both by ourselves and others. By presenting several short autobiographical vignettes, we examine perceptions of the gendered identity of women in academia as caring, ‘motherly’ and nurturing, and we demonstrate attempts to exploit so-called ‘natural’ feminine, mothering traits as a means of fulfilling the pastoral and administrative components of universities. In considering such stereotypes, we address examples of their selffulfilment, whilst considering how academic structures and practices also impose such distinctions. We consider negative implications for the career success of women academics in the ‘real business’ of academia, typified by research, publications and academic networking, arguing that until these stereotypes are challenged, women academics will continue to be disadvantaged within academic institutions

‘Real business’? : gendered identities in accounting and management academia

This paper explores the gendered identities of women academics in accounting and management academia. Drawing upon autoethnographical detail, we reflect upon the complexities of identities as they are constructed, developed, experienced and understood both by ourselves and others. By presenting several short autobiographical vignettes, we examine perceptions of the gendered identity of women in academia as caring, ‘motherly’ and nurturing, and we demonstrate attempts to exploit so-called ‘natural’ feminine, mothering traits as a means of fulfilling the pastoral and administrative components of universities. In considering such stereotypes, we address examples of their selffulfilment, whilst considering how academic structures and practices also impose such distinctions. We consider negative implications for the career success of women academics in the ‘real business’ of academia, typified by research, publications and academic networking, arguing that until these stereotypes are challenged, women academics will continue to be disadvantaged within academic institutions

The effect of the relative orientation between the coronal field and new emerging flux: I Global Properties

The emergence of magnetic flux from the convection zone into the corona is an important process for the dynamical evolution of the coronal magnetic field. In this paper we extend our previous numerical investigations, by looking at the process of flux interaction as an initially twisted flux tube emerges into a plane parallel, coronal magnetic field. Significant differences are found in the dynamical appearance and evolution of the emergence process depending on the relative orientation between the rising flux system and any preexisting coronal field. When the flux systems are nearly anti-parallel, the experiments show substantial reconnection and demonstrate clear signatures of a high temperature plasma located in the high velocity outflow regions extending from the reconnection region. However, the cases that have a more parallel orientation of the flux systems show very limited reconnection and none of the associated features. Despite the very different amount of reconnection between the two flux systems, it is found that the emerging flux that is still connected to the original tube, reaches the same height as a function of time. As a compensation for the loss of tube flux, a clear difference is found in the extent of the emerging loop in the direction perpendicular to the main axis of the initial flux tube. Increasing amounts of magnetic reconnection decrease the volume, which confines the remaining tube flux.Comment: 21 pages, 16 figures Accepted for Ap

Identifying galaxy candidates in WSRT HI imaging of ultra-compact high velocity clouds

Ultra-compact high velocity clouds (UCHVCs) were identified in the ALFALFA HI survey as potential gas-bearing dark matter halos. Here we present higher resolution neutral hydrogen (HI) observations of twelve UCHVCS with the Westerbork Synthesis Radio Telescope (WSRT). The UCHVCs were selected based on a combination of size, isolation, large recessional velocity and high column density as the best candidate dark matter halos. The WSRT data were tapered to image the UCHVCs at 210" (comparable to Arecibo) and 105" angular resolution. In a comparison of the single-dish to interferometer data, we find that the line flux recovered in the WSRT observations is comparable to that from the single-dish ALFALFA data. In addition, any structure seen in the ALFALFA data is reproduced in the WSRT maps at the same angular resolution. At 210'" resolution all the sources are generally compact with a smooth HI morphology, as expected from their identification as UCHVCs. At the higher angular resolution, a majority of the sources break into small clumps contained in a diffuse envelope. These UCHVCs also have no ordered velocity motion and are most likely Galactic halo clouds. We identify two UCHVCs, AGC 198606 and AGC 249525, as excellent galaxy candidates based on maintaining a smooth HI morphology at higher angular resolution and showing ordered velocity motion consistent with rotation. A third source, AGC 249565, lies between these two populations in properties and is a possible galaxy candidate. If interpreted as gas-bearing dark matter halos, the three candidate galaxies have rotation velocities of 8-15 km/s, HI masses of 0.6-50 x 10^5 Msun, HI radii of 0.3-2 kpc, and dynamical masses of 2-20 x 10^7 Msun for a range of plausible distances. These are the UCHVCs with the highest column density values in the ALFALFA HI data and we suggest this is the best way to identify further candidates.Comment: Accepted for publication in A&A. 26 pages, 19 figures, 5 table

Written medical discharge communication from an acute stroke service: a project to improve content through development of a structured stroke-specific template

Specific guidelines for the content of discharge summaries from acute stroke services do not currently exist. The aims of this project were to assess the strengths and weaknesses of stroke discharge communication from Imperial College Healthcare NHS Trust, to develop a structured template to guide completion, and to re-audit discharge communication following its implementation. The audit compared local performance against record standards from the Academy of Medical Royal Colleges (1), which was augmented by criteria generated from the British Association of Stroke Physicians (BASP) Stroke Service Standards (2). Discharge information was examined within the Trust’s Electronic Discharge Communication (EDC) system to determine the recording of selected items for consecutively discharged patients from the hyperacute and acute stroke units. The audit was repeated following implementation of a newly developed stroke-specific discharge summary template. Fifty-one EDC summaries were examined at baseline (July 2012) and 30 summaries at re-audit (January 2013). The criteria which showed low adherence initially and which showed the most significant improvement following the introduction of the template were the guidance on blood pressure and lipids targets (increased from 2% and 0% respectively at baseline, to 93% post intervention), and the driving and flying advice (from 3% to 79%). Documentation was also seen to improve for measures of physical and cognitive function, discharge arrangements, and follow up plans. This audit cycle has demonstrated improvement in the consistency of content within written discharge communication following the introduction of a structured stroke-specific template adhering to combined criteria from identified standards

PARAS program: Phased array radio astronomy from space

An orbiting radio telescope is proposed which, when operated in a Very Long Baseline Interferometry (VLBLI) scheme, would allow higher (than currently available) angular resolution and dynamic range in the maps, and the ability of observing rapidly changing astronomical sources. Using a passive phases array technology, the proposed design consists of 656 hexagonal modules forming a 150 meter diameter dish. Each observatory module is largely autonomous, having its own photovoltaic power supply and low-noise receiver and processor for phase shifting. The signals received by the modules are channeled via fiber optics to the central control computer in the central bus module. After processing and multiplexing, the data is transmitted to telemetry stations on the ground. The truss frame supporting each observatory pane is a hybrid structure consisting of a bottom graphite/epoxy tubular triangle and rigidized inflatable Kevlar tubes connecting the top observatory panel and bottom triangle. Attitude control and stationkeeping functions are performed by a system of momentum wheels in the bus and four propulsion modules located at the compass points on the periphery of the observatory dish. Each propulsion module has four monopropellant thrusters and six hydrazine arcjets, the latter supported by a nuclear reactor. The total mass of the spacecraft is 22,060 kg

AGC 226067: A possible interacting low-mass system

We present Arecibo, GBT, VLA and WIYN/pODI observations of the ALFALFA source AGC 226067. Originally identified as an ultra-compact high velocity cloud and candidate Local Group galaxy, AGC 226067 is spatially and kinematically coincident with the Virgo cluster, and the identification by multiple groups of an optical counterpart with no resolved stars supports the interpretation that this systems lies at the Virgo distance (D=17 Mpc). The combined observations reveal that the system consists of multiple components: a central HI source associated with the optical counterpart (AGC 226067), a smaller HI-only component (AGC 229490), a second optical component (AGC 229491), and extended low surface brightness HI. Only ~1/4 of the single-dish HI emission is associated with AGC 226067; as a result, we find M_HI/L_g ~ 6 Msun/Lsun, which is lower than previous work. At D=17 Mpc, AGC 226067 has an HI mass of 1.5 x 10^7 Msun and L_g = 2.4 x 10^6 Lsun, AGC 229490 (the HI-only component) has M_HI = 3.6 x 10^6 Msun, and AGC 229491 (the second optical component) has L_g = 3.6 x 10^5 Lsun. The nature of this system of three sources is uncertain: AGC 226067 and AGC 229490 may be connected by an HI bridge, and AGC 229490 and AGC 229491 are separated by only 0.5'. The current data do not resolve the HI in AGC 229490 and its origin is unclear. We discuss possible scenarios for this system of objects: an interacting system of dwarf galaxies, accretion of material onto AGC 226067, or stripping of material from AGC 226067.Comment: Accepted for publication in A&A. 6 pages, 4 figure