79,172 research outputs found
The effect of timing noise on targeted and narrow-band coherent searches for continuous gravitational waves from pulsars
Most searches for continuous gravitational-waves from pulsars use Taylor
expansions in the phase to model the spin-down of neutron stars. Studies of
pulsars demonstrate that their electromagnetic (EM) emissions suffer from
\emph{timing noise}, small deviations in the phase from Taylor expansion
models. How the mechanism producing EM emission is related to any continuous
gravitational-wave (CW) emission is unknown; if they either interact or are
locked in phase then the CW will also experience timing noise. Any disparity
between the signal and the search template used in matched filtering methods
will result in a loss of signal-to-noise ratio (SNR), referred to as
`mismatch'. In this work we assume the CW suffers a similar level of timing
noise to its EM counterpart. We inject and recover fake CW signals, which
include timing noise generated from observational data on the Crab pulsar.
Measuring the mismatch over durations of order months, the effect is
for the most part found to be small. This suggests recent so-called
`narrow-band' searches which placed upper limits on the signals from the Crab
and Vela pulsars will not be significantly affected. At a fixed observation
time, we find the mismatch depends upon the observation epoch. Considering the
averaged mismatch as a function of observation time, we find that it increases
as a power law with time, and so may become relevant in long baseline searches.Comment: 9 pages, 5 figure
Comparing models of the periodic variations in spin-down and beam-width for PSR B1828-11
We build a framework using tools from Bayesian data analysis to evaluate
models explaining the periodic variations in spin-down and beam-width of PSR
B1828-11. The available data consists of the time averaged spin-down rate,
which displays a distinctive double-peaked modulation, and measurements of the
beam-width. Two concepts exist in the literature that are capable of explaining
these variations; we formulate predictive models from these and quantitatively
compare them. The first concept is phenomenological and stipulates that the
magnetosphere undergoes periodic switching between two meta-stable states as
first suggested by Lyne et al. The second concept, precession, was first
considered as a candidate for the modulation of B1828-11 by Stairs et al.. We
quantitatively compare models built from these concepts using a Bayesian
odds-ratio. Because the phenomenological switching model itself was informed by
this data in the first place, it is difficult to specify appropriate
parameter-space priors that can be trusted for an unbiased model comparison.
Therefore we first perform a parameter estimation using the spin-down data, and
then use the resulting posterior distributions as priors for model comparison
on the beam-width data. We find that a precession model with a simple circular
Gaussian beam geometry fails to appropriately describe the data, while allowing
for a more general beam geometry provides a good fit to the data. The resulting
odds between the precession model (with a general beam geometry) and the
switching model are estimated as in favour of the precession
model.Comment: 20 pages, 15 figures; removed incorrect factor of (2\pi) from
equation (15), allowed for arbitrary braking index, and revised prior ranges;
overall conclusions unchange
Implications of an r-mode in XTE J1751-305: Mass, radius and spin evolution
Recently Strohmayer and Mahmoodifar presented evidence for a coherent
oscillation in the X-ray light curve of the accreting millisecond pulsar XTE
J1751-305, using data taken by RXTE during the 2002 outburst of this source.
They noted that a possible explanation includes the excitation of a non-radial
oscillation mode of the neutron star, either in the form of a g-mode or an
r-mode. The r-mode interpretation has connections with proposed spin-evolution
scenarios for systems such as XTE J1751-305. Here we examine in detail this
interesting possible interpretation. Using the ratio of the observed
oscillation frequency to the star's spin frequency, we derive an approximate
neutron star mass-radius relation which yields reasonable values for the mass
over the range of expected stellar radius (as constrained by observations of
radius-expansion burst sources). However, we argue that the large mode
amplitude suggested by the Strohmayer and Mahmoodifar analysis would inevitably
lead to a large spin-down of the star, inconsistent with its observed spin
evolution, regardless of whether the r-mode itself is in a stable or unstable
regime. We therefore conclude that the r-mode interpretation of the observed
oscillation is not consistent with our current understanding of neutron star
dynamics and must be considered unlikely. Finally we note that, subject to the
availability of a sufficiently accurate timing model, a direct
gravitational-wave search may be able to confirm or reject an r-mode
interpretation unambiguously, should such an event, with a similar inferred
mode amplitude, recur during the Advanced detector era.Comment: 8 pages, 3 figures; submitted to MNRA
Using a fuzzy inference system to control a pumped storage hydro plant
The paper discusses the development of a fuzzy inference system (FIS) based governor control for a pumped storage hydroelectric plant. The First Hydro Company's plant at Dinorwig in North Wales is the largest of its kind in Europe and is mainly used for frequency control of the UK electrical grid. In previous investigations, a detailed model of the plant was developed using MATLAB(R)/SIMULINK(R) and this is now being used to compare FIS governor operation with the proportional-integral-derivative (PID) controller currently used. The paper describes the development of an FIS governor, and shows that its response to a step increase in load is superior to the PID under certain conditions of load. The paper proceeds to discuss the implications of these results in view of the possible practical application of an FIS governor at the Dinorwig plant
Propagation of Light Elements in the Galaxy
The origin and evolution of isotopes of the lightest elements H2, He3, Li,
Be, B in the universe is a key problem in such fields as astrophysics of CR,
Galactic evolution, non-thermal nucleosynthesis, and cosmological studies. One
of the major sources of these species is spallation by CR nuclei in the
interstellar medium. On the other hand, it is the B/C ratio in CR and Be10
abundance which are used to fix the propagation parameters and thus the
spallation rate. We study the production and Galactic propagation of isotopes
of elements Z<6 using the numerical propagation code GALPROP and updated
production cross sections.Comment: 4 pages, 6 ps-figures, tsukuba.sty, to appear in the Proc. 28th
International Cosmic Ray Conference (Tsukuba, Japan 2003). More details can
be found at http://www.gamma.mpe-garching.mpg.de/~aws/aws.htm
Recommended from our members
Refinement and preliminary evaluation of two tablet-based tests of real-world visual function
PURPOSE: To describe, refine, evaluate, and provide normative control data for two freely available tablet-based tests of real-world visual function, using a cohort of young, normally-sighted adults.
METHODS: Fifty young (18-40Â years), normally-sighted adults completed tablet-based assessments of (1) face discrimination and (2) visual search. Each test was performed twice, to assess test-retest repeatability. Post-hoc analyses were performed to determine the number of trials required to obtain stable estimates of performance. Distributions were fitted to the normative data to determine the 99% population-boundary for normally sighted observers. Participants were also asked to rate their comprehension of each test.
RESULTS: Both tests provided stable estimates in around 20 trials (~1-4Â min), with only a further reduction of 14%-17% in the 95% Coefficient of Repeatability (CoR95 ) when an additional 40 trials were included. When using only ~20 trials: median durations for the first run of each test were 191Â s (Faces) and 51Â s (Search); test-retest CoR95 were 0.27Â d (Faces) and 0.84Â s (Search); and normative 99% population-limits were 3.50Â d (Faces) and 3.1Â s (Search). No participants exhibited any difficulties completing either test (100% completion rate), and ratings of task-understanding were high (Faces: 9.6 out of 10; Search: 9.7 out of 10).
CONCLUSIONS: This preliminary assessment indicated that both tablet-based tests are able to provide simple, quick, and easy-to-administer measures of real-world visual function in normally-sighted young adults. Further work is required to assess their accuracy and utility in older people and individuals with visual impairment. Potential applications are discussed, including their use in clinic waiting rooms, and as an objective complement to Patient Reported Outcome Measures (PROMs)
Fano effect and Kondo effect in quantum dots formed in strongly coupled quantum wells
We present lateral transport measurements on strongly, vertically coupled
quantum dots formed in separate quantum wells in a GaAs/AlGaAs heterostructure.
Coulomb oscillations are observed forming a honeycomb lattice consistent with
two strongly coupled dots. When the tunnel barriers in the upper well are
reduced we observe the Fano effect due to the interfering paths through a
resonant state in the lower well and a continuum state in the upper well. In
both regimes an in plane magnetic field reduces the coupling between the wells
when the magnetic length is comparable to the center to center separation of
the wells. We also observe the Kondo effect which allows the spin states of the
double dot system to be probed.Comment: 4 pages, 5 figure
Modelling the alumina abundance of oxygen-rich evolved stars in the Large Magellanic Cloud
In order to determine the composition of the dust in the circumstellar
envelopes of oxygen-rich asymptotic giant branch (AGB) stars we have computed a
grid of modust radiative-transfer models for a range of dust compositions,
mass-loss rates, dust shell inner radii and stellar parameters. We compare the
resulting colours with the observed oxygen-rich AGB stars from the SAGE-Spec
Large Magellanic Cloud (LMC) sample, finding good overall agreement for stars
with a mid-infrared excess. We use these models to fit a sample of 37 O-rich
AGB stars in the LMC with optically thin circumstellar envelopes, for which
535-m Spitzer infrared spectrograph (IRS) spectra and broadband
photometry from the optical to the mid-infrared are available. From the
modelling, we find mass-loss rates in the range to
M, and we show that a grain
mixture consisting primarily of amorphous silicates, with contributions from
amorphous alumina and metallic iron provides a good fit to the observed
spectra. Furthermore, we show from dust models that the AKARI [11][15]
versus [3.2][7] colour-colour diagram, is able to determine the fractional
abundance of alumina in O-rich AGB stars.Comment: 22 pages, 17 figures, accepted MNRA
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