1,673 research outputs found
How rapidly do neutron stars spin at birth? Constaints from archival X-ray observations of extragalactic supernovae
Traditionally, studies aimed at inferring the distribution of birth periods of neutron stars are based on radio surveys. Here we propose an independent method to constrain the pulsar spin periods at birth based on their X-ray luminosities. In particular, the observed luminosity distribution of supernovae (SNe) poses a constraint on the initial rotational energy of the embedded pulsars, via the correlation found for radio pulsars, and under the assumption that this relation continues to hold beyond the observed range. We have extracted X-ray luminosities (or limits) for a large sample of historical SNe observed with Chandra, XMM and Swift, which have been firmly classified as core-collapse SNe. We have then compared these observational limits with the results of Monte Carlo simulations of the pulsar X-ray luminosity distribution for a range of values of the birth parameters. We find that a pulsar population dominated by millisecond periods at birth is ruled out by the data
A “Not Particularly Felicitous” Phrase: A History of the “Behavioral Sciences” Label
The article reconstructs the history of the "behavioral sciences" label, from scattered interwar use through to the decisive embrace of the newly prominent Ford Foundation in the early Cold War. The rapid uptake of the label, the article concludes, was the result of the Ford Foundation’s 1951 decision to name its social science unit the “Behavioral Sciences Program” (BSP). With Ford’s encouragement, the term was widely adopted by quantitative social scientists eager to tap the foundation’s social science funds. The label’s newness and its link to the gigantic foundation’s initiative generated much suspicion and resistance as well
Interface Width and Bulk Stability: requirements for the simulation of Deeply Quenched Liquid-Gas Systems
Simulations of liquid-gas systems with extended interfaces are observed to
fail to give accurate results for two reasons: the interface can get ``stuck''
on the lattice or a density overshoot develops around the interface. In the
first case the bulk densities can take a range of values, dependent on the
initial conditions. In the second case inaccurate bulk densities are found. In
this communication we derive the minimum interface width required for the
accurate simulation of liquid gas systems with a diffuse interface. We
demonstrate this criterion for lattice Boltzmann simulations of a van der Waals
gas. When combining this criterion with predictions for the bulk stability we
can predict the parameter range that leads to stable and accurate simulation
results. This allows us to identify parameter ranges leading to high density
ratios of over 1000. This is despite the fact that lattice Boltzmann
simulations of liquid-gas systems were believed to be restricted to modest
density ratios of less than 20.Comment: 5 pages, 3 figure
The psychological benefits of participating in group singing for members of the general public
The last decade has produced a growing number of studies examining the potential psychological benefits of singing in a choir. Studies have tended to focus on the benefits for groups that might be described as marginalized or criminal. In contrast, the current study focused on members of the general public who regularly participate in choral singing. An in-depth qualitative design was utilized to explore the meaning and importance of group singing for 10 participants. Thematic analysis based on an interpretive approach was utilized to analyse the data. Psychological benefits emerged as two themes: individual and group. A third theme, mediating factors, impacted upon both individual and group outcomes. Eight sub-themes were identified and labelled: psychological, musical, physical, ethos, group dynamic, past experiences, type of choir and musical director. Results illustrate that group singing is a joyful activity that promotes wellbeing and is life enhancing for those involved. Future research directions are briefly discussed
Limits on thermal variations in a dozen quiescent neutron stars over a decade
In quiescent low-mass X-ray binaries (qLMXBs) containing neutron stars, the
origin of the thermal X-ray component may be either release of heat from the
core of the neutron star, or continuing low-level accretion. In general, heat
from the core should be stable on timescales years, while continuing
accretion may produce variations on a range of timescales. While some quiescent
neutron stars (e.g. Cen X-4, Aql X-1) have shown variations in their thermal
components on a range of timescales, several others, particularly those in
globular clusters with no detectable nonthermal hard X-rays (fit with a
powerlaw), have shown no measurable variations. Here, we constrain the spectral
variations of 12 low mass X-ray binaries in 3 globular clusters over
years. We find no evidence of variations in 10 cases, with limits on
temperature variations below 11% for the 7 qLMXBs without powerlaw components,
and limits on variations below 20% for 3 other qLMXBs that do show non-thermal
emission. However, in 2 qLMXBs showing powerlaw components in their spectra
(NGC 6440 CX 1 & Terzan 5 CX 12) we find marginal evidence for a 10% decline in
temperature, suggesting the presence of continuing low-level accretion. This
work adds to the evidence that the thermal X-ray component in quiescent neutron
stars without powerlaw components can be explained by heat deposited in the
core during outbursts. Finally, we also investigate the correlation between
hydrogen column density (N) and optical extinction (A) using our sample
and current models of interstellar X-ray absorption, finding .Comment: 16 pages, 5 figures, MNRAS, in pres
- …