1,460 research outputs found
Simulations of Mixed Morphology Supernova Remnants With Anisotropic Thermal Conduction
We explore the role of anisotropic thermal conduction on the evolution of
supernova remnants through interstellar media with a range of densities via
numerical simulations. We find that a remnant expanding in a dense environment
can produce centre-bright hard x-ray emission within 20 kyr, and centre-bright
soft x-ray emission within 60 kyr of the supernova event. In a more tenuous
environment, the appearance of a centre-bright structure in hard x-rays is
delayed until about 60 kyr. The soft x-ray emission from such a remnant may not
become centre bright during its observable lifetime. This can explain the
observations that show that mixed-morphology supernova remnants preferentially
occur close to denser, molecular environments. Remnants expanding into denser
environments tend to be smaller, making it easier for thermal conduction to
make larger changes in the temperatures of their hot gas bubbles. We show that
the lower temperatures make it very favorable to use high-stage ions as
diagnostics of the hot gas bubbles in SNRs. In particular, the distribution of
O VIII transitions from shell-bright at early epochs to centre-bright at later
epochs in the evolution of an SNR expanding in a dense ISM when the physics of
thermal conduction is included.Comment: 8 pages, 5 figures, submitted to Monthly Notice
The Formation of Self-Gravitating Cores in Turbulent Magnetized Clouds
We use ZEUS-MP to perform high resolution, three-dimensional, super-Alfvenic
turbulent simulations in order to investigate the role of magnetic fields in
self-gravitating core formation within turbulent molecular clouds. Statistical
properties of our super-Alfvenic model without gravity agree with previous
similar studies. Including self-gravity, our models give the following results.
They are consistent with the turbulent fragmentation prediction of the core
mass distribution of Padoan & Nordlund. They also confirm that local
gravitational collapse is not prevented by magnetohydrodynamic waves driven by
turbulent flows, even when the turbulent Jeans mass exceeds the mass in the
simulation volume. Comparison of results between 256^3 and 512^3 zone
simulations reveals convergence in the collapse rate. Analysis of
self-gravitating cores formed in the simulation shows that: (1) All cores
formed are magnetically supercritical by at least an order of magnitude. (2) A
power law relation between central magnetic field strength and density B_c
propto rho_c^{1/2} is observed despite the cores being strongly supercritical.
(3) Specific angular momentum j propto R^{3/2} for cores with radius R. (4)
Most cores are prolate and triaxial in shape, in agreement with the results of
Gammie et al.Comment: 49 pages, 22 figure
A comparison of laboratory and in situ methods to determine soil thermal conductivity for energy foundations and other ground heat exchanger applications
Soil thermal conductivity is an important factor in the design of energy foundations and other ground heat exchanger systems. It can be determined by a field thermal response test, which is both costly and time consuming, but tests a large volume of soil. Alternatively, cheaper and quicker laboratory test methods may be applied to smaller soil samples. This paper investigates two different laboratory methods: the steady-state thermal cell and the transient needle probe. U100 soil samples were taken during the site investigation for a small diameter test pile, for which a thermal response test was later conducted. The thermal conductivities of the samples were measured using the two laboratory methods. The results from the thermal cell and needle probe were significantly different, with the thermal cell consistently giving higher values for thermal conductivity. The main difficulty with the thermal cell was determining the rate of heat flow, as the apparatus experiences significant heat losses. The needle probe was found to have fewer significant sources of error, but tests a smaller soil sample than the thermal cell. However, both laboratory methods gave much lower values of thermal conductivity compared to the in situ thermal response test. Possible reasons for these discrepancies are discussed, including sample size, orientation and disturbance
Exploring the consequences of pairing algorithms for binary stars
Knowledge of the binary population in stellar groupings provides important
information about the outcome of the star forming process in different
environments (see, e.g., Blaauw 1991, and references therein). Binarity is also
a key ingredient in stellar population studies, and is a prerequisite to
calibrate the binary evolution channels. In this paper we present an overview
of several commonly used methods to pair individual stars into binary systems,
which we refer to as pairing functions. These pairing functions are frequently
used by observers and computational astronomers, either for their mathematical
convenience, or because they roughly describe the expected outcome of the star
forming process. We discuss the consequences of each pairing function for the
interpretation of observations and numerical simulations. The binary fraction
and mass ratio distribution generally depend strongly on the selection of the
range in primary spectral type in a sample. The mass ratio distribution and
binary fraction derived from a binarity survey among a mass-limited sample of
targets is thus not representative for the population as a whole. Neither
theory nor observations indicate that random pairing of binary components from
the mass distribution, the simplest pairing function, is realistic. It is more
likely that companion stars are formed in a disk around a star, or that a
pre-binary core fragments into two binary components. The results of our
analysis are important for (i) the interpretation of the observed mass ratio
distribution and binary fraction for a sample of stars, (ii) a range of
possible initial condition algorithms for star cluster simulations, and (iii)
how to discriminate between the different star formation scenarios.Comment: 43 pages, 18 figures, accepted for publication in A&
Evaluation of the current knowledge limitations in breast cancer research: a gap analysis
BACKGROUND
A gap analysis was conducted to determine which areas of breast cancer research, if targeted by researchers and funding bodies, could produce the greatest impact on patients.
METHODS
Fifty-six Breast Cancer Campaign grant holders and prominent UK breast cancer researchers participated in a gap analysis of current breast cancer research. Before, during and following the meeting, groups in seven key research areas participated in cycles of presentation, literature review and discussion. Summary papers were prepared by each group and collated into this position paper highlighting the research gaps, with recommendations for action.
RESULTS
Gaps were identified in all seven themes. General barriers to progress were lack of financial and practical resources, and poor collaboration between disciplines. Critical gaps in each theme included: (1) genetics (knowledge of genetic changes, their effects and interactions); (2) initiation of breast cancer (how developmental signalling pathways cause ductal elongation and branching at the cellular level and influence stem cell dynamics, and how their disruption initiates tumour formation); (3) progression of breast cancer (deciphering the intracellular and extracellular regulators of early progression, tumour growth, angiogenesis and metastasis); (4) therapies and targets (understanding who develops advanced disease); (5) disease markers (incorporating intelligent trial design into all studies to ensure new treatments are tested in patient groups stratified using biomarkers); (6) prevention (strategies to prevent oestrogen-receptor negative tumours and the long-term effects of chemoprevention for oestrogen-receptor positive tumours); (7) psychosocial aspects of cancer (the use of appropriate psychosocial interventions, and the personal impact of all stages of the disease among patients from a range of ethnic and demographic backgrounds).
CONCLUSION
Through recommendations to address these gaps with future research, the long-term benefits to patients will include: better estimation of risk in families with breast cancer and strategies to reduce risk; better prediction of drug response and patient prognosis; improved tailoring of treatments to patient subgroups and development of new therapeutic approaches; earlier initiation of treatment; more effective use of resources for screening populations; and an enhanced experience for people with or at risk of breast cancer and their families. The challenge to funding bodies and researchers in all disciplines is to focus on these gaps and to drive advances in knowledge into improvements in patient care
Control of star formation by supersonic turbulence
Understanding the formation of stars in galaxies is central to much of modern
astrophysics. For several decades it has been thought that stellar birth is
primarily controlled by the interplay between gravity and magnetostatic
support, modulated by ambipolar diffusion. Recently, however, both
observational and numerical work has begun to suggest that support by
supersonic turbulence rather than magnetic fields controls star formation. In
this review we outline a new theory of star formation relying on the control by
turbulence. We demonstrate that although supersonic turbulence can provide
global support, it nevertheless produces density enhancements that allow local
collapse. Inefficient, isolated star formation is a hallmark of turbulent
support, while efficient, clustered star formation occurs in its absence. The
consequences of this theory are then explored for both local star formation and
galactic scale star formation. (ABSTRACT ABBREVIATED)Comment: Invited review for "Reviews of Modern Physics", 87 pages including 28
figures, in pres
Causal structures and causal boundaries
We give an up-to-date perspective with a general overview of the theory of
causal properties, the derived causal structures, their classification and
applications, and the definition and construction of causal boundaries and of
causal symmetries, mostly for Lorentzian manifolds but also in more abstract
settings.Comment: Final version. To appear in Classical and Quantum Gravit
Ageism and sexuality
Sexuality remains important throughout a person’s life, but sexual behavior does not receive the same levels of acceptance at all ages. Older people are challenged by ageist attitudes and perceptions that hinder their sexual expression. They are stereotyped as non-sexual beings who should not, cannot, and do not want to have sexual relationships. Expressing sexuality or engaging in sexual activity in later life is considered by many in society as immoral or perverted. False expectations for older people also stem from ideals of beauty, centralization of the biomedical perspective on sexuality of older adults, and the association of sex with reproduction. Unfortunately, older people internalize many ageist attitudes towards sexuality in later life and become less interested in sex and less sexually active. The following chapter explores attitudes towards sexuality in later life among the media, young people, older people themselves, and care providers. In order to enable older people to express their sexuality and sexual identity freely and fully, awareness of ageist perceptions must be raised and defeated
The stellar and sub-stellar IMF of simple and composite populations
The current knowledge on the stellar IMF is documented. It appears to become
top-heavy when the star-formation rate density surpasses about 0.1Msun/(yr
pc^3) on a pc scale and it may become increasingly bottom-heavy with increasing
metallicity and in increasingly massive early-type galaxies. It declines quite
steeply below about 0.07Msun with brown dwarfs (BDs) and very low mass stars
having their own IMF. The most massive star of mass mmax formed in an embedded
cluster with stellar mass Mecl correlates strongly with Mecl being a result of
gravitation-driven but resource-limited growth and fragmentation induced
starvation. There is no convincing evidence whatsoever that massive stars do
form in isolation. Various methods of discretising a stellar population are
introduced: optimal sampling leads to a mass distribution that perfectly
represents the exact form of the desired IMF and the mmax-to-Mecl relation,
while random sampling results in statistical variations of the shape of the
IMF. The observed mmax-to-Mecl correlation and the small spread of IMF
power-law indices together suggest that optimally sampling the IMF may be the
more realistic description of star formation than random sampling from a
universal IMF with a constant upper mass limit. Composite populations on galaxy
scales, which are formed from many pc scale star formation events, need to be
described by the integrated galactic IMF. This IGIMF varies systematically from
top-light to top-heavy in dependence of galaxy type and star formation rate,
with dramatic implications for theories of galaxy formation and evolution.Comment: 167 pages, 37 figures, 3 tables, published in Stellar Systems and
Galactic Structure, Vol.5, Springer. This revised version is consistent with
the published version and includes additional references and minor additions
to the text as well as a recomputed Table 1. ISBN 978-90-481-8817-
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