5,339 research outputs found
Geology of the Trial Harbour district
A Devonian (?) granite complex intrudes
Cambrian (?) volcanics, serpentinised dunite
(olivine Fo,), and siltstones and quartzites of the
Precambrian (?) Oonah Quartzite and Slate and
the Silurian Crotty Quartzite and Amber Slate
Formations. The general trends of these country
rocks are parallel to the granite margins.
The complex is composed of grey, pink and
white granites all with the same mineralogical
composition (quartz, orthoclase dominant, plagioclase
subordinate). The white granite commonly
contains tourmaline nodular segregations, Emplacement
began with the pink and grey granites,
followed closely by the white granite, and finally
the intrusion of minor bodies (porphyritic aplite,
micro-granite, aplite, pegmatite, quartz-tourmaline
dykes, pyroxene dyke) . Tourmaline is abundant
in the later intrusions and is sometimes accompanied
by cassiterite
Time-course of vascular adaptations during 8 weeks of exercise training in subjects with type 2 diabetes and middle-aged controls
CONCLUSION: Training leads to rapid improvement in brachial artery vascular function in diabetes patients and controls. In contrast to previous observations in healthy young subjects, the increase in function was preserved after 8 weeks of training in middle-aged diabetes patients and controls, suggesting a different time-course in vascular adaptations in subjects with endothelial dysfunction
A dearth of OH/IR stars in the Small Magellanic Cloud
We present the results of targeted observations and a survey of 1612-, 1665-,
and 1667-MHz circumstellar OH maser emission from asymptotic giant branch (AGB)
stars and red supergiants (RSGs) in the Small Magellanic Cloud (SMC), using the
Parkes and Australia Telescope Compact Array radio telescopes. No clear OH
maser emission has been detected in any of our observations targeting luminous,
long-period, large-amplitude variable stars, which have been confirmed
spectroscopically and photometrically to be mid- to late-M spectral type. These
observations have probed 3 - 4 times deeper than any OH maser survey in the
SMC. Using a bootstrapping method with LMC and Galactic OH/IR star samples and
our SMC observation upper limits, we have calculated the likelihood of not
detecting maser emission in any of the two sources considered to be the top
maser candidates to be less than 0.05%, assuming a similar pumping mechanism as
the LMC and Galactic OH/IR sources. We have performed a population comparison
of the Magellanic Clouds and used Spitzer IRAC and MIPS photometry to confirm
that we have observed all high luminosity SMC sources that are expected to
exhibit maser emission. We suspect that, compared to the OH/IR stars in the
Galaxy and LMC, the reduction in metallicity may curtail the dusty wind phase
at the end of the evolution of the most massive cool stars. We also suspect
that the conditions in the circumstellar envelope change beyond a simple
scaling of abundances and wind speed with metallicity
DIGIT survey of far-infrared lines from protoplanetary disks I
[abridged] We present far-infrared spectroscopic observations of PMS stars
taken with Herschel/PACS as part of the DIGIT key project. The sample includes
22 Herbig AeBe and 8 T Tauri sources. Multiple atomic fine structure and
molecular lines are detected at the source position: [OI], [CII], CO, OH, H_2O,
CH^+. The most common feature is the [OI] 63micron line detected in almost all
of the sources followed by OH. In contrast with CO, OH is detected toward both
Herbig AeBe groups (flared and non-flared sources). An isothermal LTE slab
model fit to the OH lines indicates column densities of 10^13 < N_OH < 10^16
cm^-2, emitting radii 15 < r < 100 AU and excitation temperatures 100 < T_ex <
400 K. The OH emission thus comes from a warm layer in the disk at intermediate
stellar distances. Warm H_2O emission is detected through multiple lines toward
the T Tauri systems AS 205, DG Tau, S CrA and RNO 90 and three Herbig AeBe
systems HD 104237, HD 142527, HD 163296 (through line stacking). Overall,
Herbig AeBe sources have higher OH/H_2O abundance ratios across the disk than
do T Tauri disks, from near- to far-infrared wavelengths. Far-infrared CH^+
emission is detected toward HD 100546 and HD 97048. The slab model suggests
moderate excitation (T_ex ~ 100 K) and compact (r ~ 60 AU) emission in the case
of HD 100546. The [CII] emission is spatially extended in all sources where the
line is detected. This suggests that not all [CII] emission is associated with
the disk and that there is a substantial contribution from diffuse material
around the young stars. The flux ratios of the atomic fine structure lines are
consistent with a disk origin for the oxygen lines for most of the sources.Comment: Accepted for publication in A&
Online social networking: Relationship marketing in UK hotels
The role and the existing and potential use of online social networking as a relationship marketing (RM) tool is evaluated in the context of luxury hotels. Semi-structured interviews were conducted with the persons responsible for the management of social networking in 10 luxury hotels. Constant comparative analysis, applied within a codebook framework, revealed online social networks (OSNs) provided RM opportunities and increased business value. It is acknowledged that the full potential of OSNs has yet to be realised in terms of hotel marketing. Opportunities for extending the utilisation of OSNs are identified alongside recommendations for hotel marketing practitioners with regard to addressing consumers' needs, and areas for further research are outlined. © 2013 Copyright 2013 Westburn Publishers Ltd
Differential geometry with a projection: Application to double field theory
In recent development of double field theory, as for the description of the
massless sector of closed strings, the spacetime dimension is formally doubled,
i.e. from D to D+D, and the T-duality is realized manifestly as a global O(D,D)
rotation. In this paper, we conceive a differential geometry characterized by a
O(D,D) symmetric projection, as the underlying mathematical structure of double
field theory. We introduce a differential operator compatible with the
projection, which, contracted with the projection, can be covariantized and may
replace the ordinary derivatives in the generalized Lie derivative that
generates the gauge symmetry of double field theory. We construct various gauge
covariant tensors which include a scalar and a tensor carrying two O(D,D)
vector indices.Comment: 1+22 pages, No figure; a previous result on 4-index tensor removed,
presentation improve
Finite Temperature and Density Effect on Symmetry Breaking by Wilson Loops
A finite temperature and density effect of Wilson loop elements on non-simply
connected space is investigated in the model suggested by Hosotani. Using
one-loop calculations it is shown that the value of an "order parameter" does
not shift as the temperature grows. We find that finite density effect is of
much importance for restoration of symmetry.Comment: 11pages, no figur
On chains in -closed topological pospaces
We study chains in an -closed topological partially ordered space. We give
sufficient conditions for a maximal chain in an -closed topological
partially ordered space such that contains a maximal (minimal) element.
Also we give sufficient conditions for a linearly ordered topological partially
ordered space to be -closed. We prove that any -closed topological
semilattice contains a zero. We show that a linearly ordered -closed
topological semilattice is an -closed topological pospace and show that in
the general case this is not true. We construct an example an -closed
topological pospace with a non--closed maximal chain and give sufficient
conditions that a maximal chain of an -closed topological pospace is an
-closed topological pospace.Comment: We have rewritten and substantially expanded the manuscrip
Casimir Energy of the Universe and New Regularization of Higher Dimensional Quantum Field Theories
Casimir energy is calculated for the 5D electromagnetism and 5D scalar theory
in the {\it warped} geometry. It is compared with the flat case. A new
regularization, called {\it sphere lattice regularization}, is taken. In the
integration over the 5D space, we introduce two boundary curves (IR-surface and
UV-surface) based on the {\it minimal area principle}. It is a {\it direct}
realization of the geometrical approach to the {\it renormalization group}. The
regularized configuration is {\it closed-string like}. We do {\it not} take the
KK-expansion approach. Instead, the position/momentum propagator is exploited,
combined with the {\it heat-kernel method}. All expressions are closed-form
(not KK-expanded form). The {\it generalized} P/M propagators are introduced.
We numerically evaluate \La(4D UV-cutoff), \om(5D bulk curvature, warp
parameter) and (extra space IR parameter) dependence of the Casimir energy.
We present two {\it new ideas} in order to define the 5D QFT: 1) the summation
(integral) region over the 5D space is {\it restricted} by two minimal surfaces
(IR-surface, UV-surface) ; or 2) we introduce a {\it weight function} and
require the dominant contribution, in the summation, is given by the {\it
minimal surface}. Based on these, 5D Casimir energy is {\it finitely} obtained
after the {\it proper renormalization procedure.} The {\it warp parameter}
\om suffers from the {\it renormalization effect}. The IR parameter does
not. We examine the meaning of the weight function and finally reach a {\it new
definition} of the Casimir energy where {\it the 4D momenta(or coordinates) are
quantized} with the extra coordinate as the Euclidean time (inverse
temperature). We examine the cosmological constant problem and present an
answer at the end. Dirac's large number naturally appears.Comment: 13 paes, 8 figures, proceedings of 1st Mediterranean Conf. on CQ
The First Detections of the Extragalactic Background Light at 3000, 5500, and 8000A (II): Measurement of Foreground Zodiacal Light
We present a measurement of the absolute surface brightness of the zodiacal
light (3900-5100A) toward a fixed extragalactic target at high ecliptic
latitude based on moderate resolution (~1.3A per pixel) spectrophotometry
obtained with the du Pont 2.5m telescope at Las Campanas Observatory in Chile.
This measurement and contemporaneous Hubble Space Telescope data from WFPC2 and
FOS comprise a coordinated program to measure the mean flux of the diffuse
extragalactic background light (EBL). The zodiacal light at optical wavelengths
results from scattering by interplanetary dust, so that the zodiacal light flux
toward any extragalactic target varies seasonally with the position of the
Earth. This measurement of zodiacal light is therefore relevant to the specific
observations (date and target field) under discussion. To obtain this result,
we have developed a technique that uses the strength of the zodiacal Fraunhofer
lines to identify the absolute flux of the zodiacal light in the
multiple-component night sky spectrum. Statistical uncertainties in the result
are 0.6% (1 sigma). However, the dominant source of uncertainty is systematic
errors, which we estimate to be 1.1% (1 sigma). We discuss the contributions
included in this estimate explicitly. The systematic errors in this result
contribute 25% in quadrature to the final error in our coordinated EBL
measurement, which is presented in the first paper of this series.Comment: Accepted for publication in ApJ, 22 pages using emulateapj.sty,
version with higher resolution figures available at
http://www.astro.lsa.umich.edu/~rab/publications.html or at
http://nedwww.ipac.caltech.edu/level5/Sep01/Bernstein2/frames.htm
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