5,605 research outputs found
The challenges of risk management in diversified financial companies
In recent years, financial institutions and their supervisors have placed increased emphasis on the importance of measuring and managing risk on a firmwide basis—a coordinated process referred to as consolidated risk management. Although the benefits of this type of risk management are widely acknowledged, few if any financial firms have fully developed systems in place today, suggesting that significant obstacles have led them to manage risk in a more segmented fashion. In this article, the authors examine the economic rationale behind consolidated risk management. Their goal is to detail some of the key issues that supervisors and practitioners have confronted in assessing and developing consolidated risk management systems. In doing so, the authors clarify why implementing consolidated risk management involves significant conceptual and practical difficulties. They also suggest areas in which additional research could help resolve some of these difficulties.Risk management ; Financial institutions ; Bank supervision
Integrated ultrasonic particle positioning and low excitation light fluorescence imaging
A compact hybrid system has been developed to position and detect fluorescent micro-particles by combining a Single Photon Avalanche Diode (SPAD) imager with an acoustic manipulator. The detector comprises a SPAD array, light-emitting diode (LED), lenses, and optical filters. The acoustic device is formed of multiple transducers surrounding an octagonal cavity. By stimulating pairs of transducers simultaneously, an acoustic landscape is created causing fluorescent micro-particles to agglomerate into lines. The fluorescent pattern is excited by a low power LED and detected by the SPAD imager. Our technique combines particle manipulation and visualization in a compact, low power, portable setup
Long tails on thermonuclear X-ray bursts from neutron stars: a signature of inward heating?
We report the discovery of one-hour long tails on the few-minutes long X-ray
bursts from the `clocked burster' GS 1826-24. We propose that the tails are due
to enduring thermal radiation from the neutron star envelope. The enduring
emission can be explained by cooling of deeper NS layers which were heated up
through inward conduction of heat produced in the thermonuclear shell flash
responsible for the burst. Similar, though somewhat shorter, tails are seen in
bursts from EXO 0748-676 and 4U 1728-34. Only a small amount of cooling is
detected in all these tails. This is either due to compton up scattering of the
tail photons or, more likely, to a NS that is already fairly hot due to other,
stable, nuclear processes.Comment: Accepted for publication in Astronomy & Astrophysics, 12 pages, 14
figure
Novel thermal management of power electronic devices: high power high frequency planar gunn diodes
Thermal management of next generation of semiconductor devices is becoming more challenging, as the device power
increases and device dimensions decrease. The work is addressing novel thermal measurement and management for
planar heterostructure Gunn diodes, which will be of strategic importance for UK technology and industry
The Connection Between Low-Mass X-ray Binaries and (Millisecond) Pulsars: A Binary Evolution Perspective
I review the evolutionary connection between low-mass X-ray binaries (LMXBs)
and pulsars with binary companions (bPSRs) from a stellar binary evolution
perspective. I focus on the evolution of stellar binaries with end-states
consisting of a pulsar with a low-mass (<1.0 solar mass) companion, starting at
the point the companion's progenitor first initiates mass transfer onto the
neutron star. Whether this mass transfer is stable and the physics driving
ongoing mass transfer partitions the phase space of the companions's initial
mass and initial orbital period into five regions. The qualitative nature of
the mass-transfer process and the binary's final end-state differ between
systems in each region; four of these regions each produce a particular class
of LMXBs. I compare the theoretical expectations to the populations of galactic
field LMXBs with companion-mass constraints and field bPSRs. I show that the
population of accreting millisecond pulsars are all identified with only two of
the four LMXB classes and that these systems do not have readily identifiable
progeny in the bPSR population. I discuss which sub-populations of bPSRs can be
explained by binary evolution theory and those that currently are not. Finally
I discuss some outstanding questions in this field.Comment: 9 pages, 5 figures, to appear in the proceedings of the 40 Years of
Pulsars conference held at McGill University in August 200
Boosting clinical performance: The impact of enhanced final year placements.
BACKGROUND: This study follows on from a study that investigated how to develop effective final year medical student assistantship placements, using multidisciplinary clinical teams in planning and delivery. AIMS: This study assessed the effects on objective structured clinical examination (OSCE) performance of the in-course enhanced "super-assistantship" placement introduced to a randomly selected sample of 2013-14 final year medical students at Leeds medical school. METHODS: Quantitative data analysis was used to compare the global grades of OSCE stations between students who undertook this placement against those who did not. RESULTS: There was a small overall improvement in the "super-assistantship" student scores across the whole assessment (effect size = 0.085). "Pre-op Capacity", "Admissions Prescribing" and "Hip Pain" stations had small-medium effect sizes (0.226, 0.215, and 0.214) in favor of the intervention group. Other stations had small effect sizes (0.107-0.191), mostly in favor of the intervention group. CONCLUSIONS: The "super-assistantship" experience characterized by increasing student responsibility on placement can help to improve competence and confidence in clinical decision-making "in a simulated environment". The clinical environment and multidisciplinary team must be ready and supported to provide these opportunities effectively. Further in-course opportunities for increasing final year student responsibility should be developed
A change in the quiescent X-ray spectrum of the neutron star low-mass X-ray binary MXB 1659-29
The quasi-persistent neutron star low-mass X-ray binary MXB 1659-29 went into
quiescence in 2001, and we have followed its quiescent X-ray evolution since.
Observations over the first 4 years showed a rapid drop in flux and temperature
of the neutron star atmosphere, interpreted as cooling of the neutron star
crust which had been heated during the 2.5 year outburst. However, observations
taken approximately 1400 and 2400 days into quiescence were consistent with
each other, suggesting the crust had reached thermal equilibrium with the core.
Here we present a new Chandra observation of MXB 1659-29 taken 11 years into
quiescence and 4 years since the last Chandra observation. This new observation
shows an unexpected factor of ~3 drop in count rate and change in spectral
shape since the last observation, which cannot be explained simply by continued
cooling. Two possible scenarios are that either the neutron star temperature
has remained unchanged and there has been an increase in the column density,
or, alternatively the neutron star temperature has dropped precipitously and
the spectrum is now dominated by a power-law component. The first scenario may
be possible given that MXB 1659-29 is a near edge-on system, and an increase in
column density could be due to build-up of material in, and a thickening of, a
truncated accretion disk during quiescence. But, a large change in disk height
may not be plausible if standard accretion disk theory holds during quiescence.
Alternatively, the disk may be precessing, leading to a higher column density
during this latest observation.Comment: 6 pages, 4 figures, accepted for publication in Ap
Superbursts at near-Eddington mass accretion rates
Models for superbursts from neutron stars involving carbon shell flashes
predict that the mass accretion rate should be anywhere in excess of one tenth
of the Eddington limit. Yet, superbursts have so far only been detected in
systems for which the accretion rate is limited between 0.1 and 0.25 times that
limit. The question arises whether this is a selection effect or an intrinsic
property. Therefore, we have undertaken a systematic study of data from the
BeppoSAX Wide Field Cameras on the luminous source GX 17+2, comprising 10 Msec
of effective observing time on superbursts. GX 17+2 contains a neutron star
with regular Type-I X-ray bursts and accretes matter within a few tens of
percents of the Eddington limit. We find four hours-long flares which
reasonably match superburst characteristics. Two show a sudden rise (i.e.,
faster than 10 s), and two show a smooth decay combined with spectral
softening. The implied superburst recurrence time, carbon ignition column and
quenching time for ordinary bursts are close to the predicted values. However,
the flare decay time, fluence and the implied energy production of (2-4) x
10^17 erg/g are larger than expected from current theory.Comment: Accepted for publication in Astronomy & Astrophysic
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