7,531 research outputs found
Changes in higher education and valuing the job: The views of accounting academics in Australia
In a previous article (Bellamy et al., 2003), the authors reported on survey research that investigated reasons why academics from business disciplines enter and remain in academia, and the conditions they deem necessary to creating ideal work satisfaction. For both entering and remaining, as well as in achieving ideal work satisfaction, the most important factors were found to be autonomy and flexibility, with teaching and research the next most important factors. In a subsequent analysis of the data, reported in this article, the authors identify and explore significant differences between accounting academics and other business academics in the relative importance placed on these key factors. The findings may be used to inform policy makers and university administrators of the importance of discipline differences when identifying key factors for recruitment and retention of accounting academics specifically, and business academics generally
Near-infrared Detection of WD 0806-661 B with the Hubble Space Telescope
WD 0806-661 B is one of the coldest known brown dwarfs (T=300-345 K) based on
previous mid-infrared photometry from the Spitzer Space Telescope. In addition,
it is a benchmark for testing theoretical models of brown dwarfs because its
age and distance are well-constrained via its primary star (2+/-0.5 Gyr,
19.2+/-0.6 pc). We present the first near-infrared detection of this object,
which has been achieved through F110W imaging (~Y+J) with the Wide Field Camera
3 on board the Hubble Space Telescope. We measure a Vega magnitude of
m110=25.70+/-0.08, which implies J~25.0. When combined with the Spitzer
photometry, our estimate of J helps to better define the empirical sequence of
the coldest brown dwarfs in M4.5 versus J-[4.5]. The positions of WD 0806-661 B
and other Y dwarfs in that diagram are best matched by the cloudy models of
Burrows et al. and the cloudless models of Saumon et al., both of which employ
chemical equilibrium. The calculations by Morley et al. for 50% cloud coverage
differ only modestly from the data. Spectroscopy would enable a more stringent
test of the models, but based on our F110W measurement, such observations are
currently possible only with Hubble, and would require at least ~10 orbits to
reach a signal-to-noise ratio of ~5
Resolved Spectroscopy of the T8.5 and Y0-0.5 Binary WISEPC J121756.91+162640.2AB
We present 0.9 - 2.5 um resolved spectra for the ultracool binary WISEPC
J121756.91+162640.2AB. The system consists of a pair of brown dwarfs that
straddles the currently defined T/Y spectral type boundary. We use synthetic
spectra generated by model atmospheres that include chloride and sulfide clouds
(Morley et al.), the distance to the system (Dupuy & Kraus), and the radius of
each component based on evolutionary models (Saumon & Marley) to determine a
probable range of physical properties for the binary. The effective temperature
of the T8.5 primary is 550 - 600 K, and that of the Y0 - Y0.5 secondary is 450
K. The atmospheres of both components are either free of clouds or have
extremely thin cloud layers. We find that the masses of the primary and
secondary are 30 and 22 M_Jup, respectively, and that the age of the system is
4 - 8 Gyr. This age is consistent with astrometric measurements (Dupuy & Kraus)
that show that the system has kinematics intermediate between those of the thin
and thick disks of the Galaxy. An older age is also consistent with an
indication by the H - K colors that the system is slightly metal-poor.Comment: 21 pages which include 6 Figures and 3 Tables. Accepted on November 8
2013 for publication in Ap
An L Band Spectrum of the Coldest Brown Dwarf
The coldest brown dwarf, WISE 0855, is the closest known planetary-mass,
free-floating object and has a temperature nearly as cold as the solar system
gas giants. Like Jupiter, it is predicted to have an atmosphere rich in
methane, water, and ammonia, with clouds of volatile ices. WISE 0855 is faint
at near-infrared wavelengths and emits almost all its energy in the
mid-infrared. Skemer et al. 2016 presented a spectrum of WISE 0855 from 4.5-5.1
micron (M band), revealing water vapor features. Here, we present a spectrum of
WISE 0855 in L band, from 3.4-4.14 micron. We present a set of atmosphere
models that include a range of compositions (metallicities and C/O ratios) and
water ice clouds. Methane absorption is clearly present in the spectrum. The
mid-infrared color can be better matched with a methane abundance that is
depleted relative to solar abundance. We find that there is evidence for water
ice clouds in the M band spectrum, and we find a lack of phosphine spectral
features in both the L and M band spectra. We suggest that a deep continuum
opacity source may be obscuring the near-infrared flux, possibly a deep
phosphorous-bearing cloud, ammonium dihyrogen phosphate. Observations of WISE
0855 provide critical constraints for cold planetary atmospheres, bridging the
temperature range between the long-studied solar system planets and accessible
exoplanets. JWST will soon revolutionize our understanding of cold brown dwarfs
with high-precision spectroscopy across the infrared, allowing us to study
their compositions and cloud properties, and to infer their atmospheric
dynamics and formation processes.Comment: 19 pages, 21 figures. Accepted for publication in Ap
Present-day stress orientations and tectonic provinces of the NW Borneo collisional margin
Extent: 15p.Borehole failure observed on image and dipmeter logs from 55 petroleum wells across the NW Borneo collisional margin were used to determine maximum horizontal stress (ÏH) orientations; combined with seismic and outcrop data, they define seven tectonic provinces. The Baram DeltaâDeepwater Fold-Thrust Belt exhibits three tectonic provinces: its inner shelf inverted province (ÏH is NW-SE, margin-normal), its outer shelf extension province (ÏH is NE-SW, margin-parallel), and its slope to basin floor compression province (ÏH is NW-SE, margin-normal). In the inverted province, ÏH reflects inversion of deltaic normal faults. The ÏH orientations in the extension and compression provinces reflect deltaic gravitational tectonics. The shale and minibasin provinces have been recognized in offshore Sabah. In the shale province, ÏH is N010°E, which aligns around the boundary of a massif of mobile shale. Currently, no data are available to determine ÏH in the minibasin province. In the Balingian province, ÏH is ESE-WNW, reflecting ESE absolute Sunda plate motions due to the absence of a thick detachment seen elsewhere in NW Borneo. The Central Luconia province demonstrates poorly constrained and variable ÏH orientations. These seven provinces result from the heterogeneous structural and stratigraphic development of the NW Borneo margin and formed due to complex collisional tectonics and the varied distribution and thicknesses of stratigraphic packages.Rosalind C. King, Mark R. P. Tingay, Richard R. Hillis, Christopher K. Morley, and James Clar
The Brown-dwarf Atmosphere Monitoring (BAM) Project II: Multi-epoch monitoring of extremely cool brown dwarfs
With the discovery of Y dwarfs by the WISE mission, the population of field
brown dwarfs now extends to objects with temperatures comparable to those of
Solar System planets. To investigate the atmospheres of these newly identified
brown dwarfs, we have conducted a pilot study monitoring an initial sample of
three late T-dwarfs (T6.5, T8 and T8.5) and one Y-dwarf (Y0) for infrared
photometric variability at multiple epochs. With J-band imaging, each target
was observed for a period of 1.0h to 4.5h per epoch, which covers a significant
fraction of the expected rotational period. These measurements represent the
first photometric monitoring for these targets. For three of the four targets
(2M1047, Ross 458C and WISE0458), multi-epoch monitoring was performed, with
the time span between epochs ranging from a few hours to ~2 years. During the
first epoch, the T8.5 target WISE0458 exhibited variations with a remarkable
min-to-max amplitude of 13%, while the second epoch light curve taken ~2 years
later did not note any variability to a 3% upper limit. With an effective
temperature of ~600 K, WISE0458 is the coldest variable brown dwarf published
to-date, and combined with its high and variable amplitude makes it a
fascinating target for detailed follow-up. The three remaining targets showed
no significant variations, with a photometric precision between 0.8% and 20.0%,
depending on the target brightness. Combining the new results with previous
multi-epoch observations of brown dwarfs with spectral types of T5 or later,
the currently identified variables have locations on the colour-colour diagram
better matched by theoretical models incorporating cloud opacities rather than
cloud-free atmospheres. This preliminary result requires further study to
determine if there is a definitive link between variability among late-T dwarfs
and their location on the colour-colour diagram.Comment: 9 pages, 6 figures, 3 tables, accepted for publication in MNRA
Cannabis and depression: A twin model approach to co-morbidity
Cannabis use disorder (CUD) co-occurs with major depressive disorder (MDD) more frequently than would be expected by chance. However, studies to date have not produced a clear understanding of the mechanisms underlying this co-morbidity. Genetically informative studies can add valuable insight to this problem, as they allow the evaluation of competing models of co-morbidity. This study uses data from the Australian Twin Registry to compare 13 co-morbidity twin models initially proposed by Neale and Kendler (Am J Hum Genet 57:935â953, 1995). The analysis sample comprised 2410 male and female monozygotic and dizygotic twins (average age 32) who were assessed on CUD and MDD using the SSAGA-OZ interview. Data were analyzed in OpenMx. Of the 13 different co-morbidity models, two fit equally well: CUD causes MDD and Random Multiformity of CUD. Both fit substantially better than the Correlated Liabilities model. Although the current study cannot differentiate between them statistically, these models, in combination, suggest that CUD risk factors may causally influence the risk to develop MDD, but only when risk for CUD is high
Effect of Longitude-Dependent Cloud Coverage on Exoplanet Visible Wavelength Reflected-Light Phase Curves
We use a planetary albedo model to investigate variations in visible wavelength phase curves of exoplanets. Thermal and cloud properties for these exoplanets are derived using one-dimensional radiative-convective and cloud simulations. The presence of clouds on these exoplanets significantly alters their planetary albedo spectra. We confirm that non-uniform cloud coverage on the dayside of tidally locked exoplanets will manifest as changes to the magnitude and shift of the phase curve. In this work, we first investigate a test case of our model using a Jupiter-like planet, at temperatures consistent to 2.0 AU insolation from a solar type star, to consider the effect of H2O clouds. We then extend our application of the model to the exoplanet Kepler-7b and consider the effect of varying cloud species, sedimentation efficiency, particle size, and cloud altitude. We show that, depending on the observational filter, the largest possible shift of the phase curve maximum will be similar to 2 degrees-10 degrees for a Jupiter-like planet, and up to similar to 30 degrees (similar to 0.08 in fractional orbital phase) for hot-Jupiter exoplanets at visible wavelengths as a function of dayside cloud distribution with a uniformly averaged thermal profile. The models presented in this work can be adapted for a variety of planetary cases at visible wavelengths to include variations in planet-star separation, gravity, metallicity, and source-observer geometry. Finally, we tailor our model for comparison with, and confirmation of, the recent optical phase-curve observations of Kepler-7b with the Kepler space telescope. The average planetary albedo can vary between 0.1 and 0.6 for the 1300 cloud scenarios that were compared to the observations. Many of these cases cannot produce a high enough albedo to match the observations. We observe that smaller particle size and increasing cloud altitude have a strong effect on increasing albedo. In particular, we show that a set of models where Kepler-7b has roughly half of its dayside covered in small-particle clouds high in the atmosphere, made of bright minerals like MgSiO3 and Mg2SiO4, provide the best fits to the observed offset and magnitude of the phase-curve, whereas Fe clouds are found to be too dark to fit the observations
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