5,025 research outputs found
Finding the right title for your article: Advice for academic author.
On reading the title of an article the reader can sometimes wonder what the author is trying to say, as the title seems so far removed from the research covered in the article. Do such authors forget that many readers of health and medical journals browse the list of contents (in a paper or electronic format) and use titles to select the article that attracts attention? Academic authors are often not clear enough in the titles of their articles, and hence may not attract as large a readership as possible.  Any author would want their article to be read and cited, and to stand out in a crowded Table of Contents or a list of papers found in a search on electronic databases.DOI: http://dx.doi.org/10.3126/nje.v4i1.10138 Nepal Journal of Epidemiology 2014;4 (1): 344-347</jats:p
The mid-infrared diameter of W Hydrae
Mid-infrared (8-13 microns) interferometric data of W Hya were obtained with
MIDI/VLTI between April 2007 and September 2009, covering nearly three
pulsation cycles. The spectrally dispersed visibility data of all 75
observations were analyzed by fitting a circular fully limb-darkened disk (FDD)
model to all data and individual pulsation phases. Asymmetries were studied
with an elliptical FDD. Modeling results in an apparent angular FDD diameter of
W Hya of about (80 +/- 1.2) mas (7.8 AU) between 8 and 10 microns, which
corresponds to an about 1.9 times larger diameter than the photospheric one.
The diameter gradually increases up to (105 +/- 1.2) mas (10.3 AU) at 12
microns. In contrast, the FDD relative flux fraction decreases from (0.85 +/-
0.02) to (0.77 +/- 0.02), reflecting the increased flux contribution from a
fully resolved surrounding silicate dust shell. The asymmetric character of the
extended structure could be confirmed. An elliptical FDD yields a position
angle of (11 +/- 20) deg and an axis ratio of (0.87 +/- 0.07). A weak pulsation
dependency is revealed with a diameter increase of (5.4 +/- 1.8) mas between
visual minimum and maximum, while detected cycle-to-cycle variations are
smaller. W Hya's diameter shows a behavior that is very similar to the Mira
stars RR Sco and S Ori and can be described by an analogous model. The constant
diameter part results from a partially resolved stellar disk, including a close
molecular layer of H2O, while the increase beyond 10 microns can most likely be
attributed to the contribution of a spatially resolved nearby Al2O3 dust shell.Comment: 18 pages, 16 figure
Entanglement of arbitrary superpositions of modes within two-dimensional orbital angular momentum state spaces
We use spatial light modulators (SLMs) to measure correlations between arbitrary superpositions of orbital angular momentum (OAM) states generated by spontaneous parametric down-conversion. Our technique allows us to fully access a two-dimensional OAM subspace described by a Bloch sphere, within the higher-dimensional OAM Hilbert space. We quantify the entanglement through violations of a Bell-type inequality for pairs of modal superpositions that lie on equatorial, polar, and arbitrary great circles of the Bloch sphere. Our work shows that SLMs can be used to measure arbitrary spatial states with a fidelity sufficient for appropriate quantum information processing systems
A close halo of large transparent grains around extreme red giant stars
Intermediate-mass stars end their lives by ejecting the bulk of their
envelope via a slow dense wind back into the interstellar medium, to form the
next generation of stars and planets. Stellar pulsations are thought to elevate
gas to an altitude cool enough for the condensation of dust, which is then
accelerated by radiation pressure from starlight, entraining the gas and
driving the wind. However accounting for the mass loss has been a problem due
to the difficulty in observing tenuous gas and dust tens of milliarcseconds
from the star, and there is accordingly no consensus on the way sufficient
momentum is transferred from the starlight to the outflow. Here, we present
spatially-resolved, multi-wavelength observations of circumstellar dust shells
of three stars on the asymptotic giant branch of the HR diagram. When imaged in
scattered light, dust shells were found at remarkably small radii (<~ 2 stellar
radii) and with unexpectedly large grains (~300 nm radius). This proximity to
the photosphere argues for dust species that are transparent to starlight and
therefore resistant to sublimation by the intense radiation field. While
transparency usually implies insufficient radiative pressure to drive a wind,
the radiation field can accelerate these large grains via photon scattering
rather than absorption - a plausible mass-loss mechanism for lower-amplitude
pulsating stars.Comment: 13 pages, 1 table, 6 figure
Properties of dense partially random graphs
We study the properties of random graphs where for each vertex a {\it
neighbourhood} has been previously defined. The probability of an edge joining
two vertices depends on whether the vertices are neighbours or not, as happens
in Small World Graphs (SWGs). But we consider the case where the average degree
of each node is of order of the size of the graph (unlike SWGs, which are
sparse). This allows us to calculate the mean distance and clustering, that are
qualitatively similar (although not in such a dramatic scale range) to the case
of SWGs. We also obtain analytically the distribution of eigenvalues of the
corresponding adjacency matrices. This distribution is discrete for large
eigenvalues and continuous for small eigenvalues. The continuous part of the
distribution follows a semicircle law, whose width is proportional to the
"disorder" of the graph, whereas the discrete part is simply a rescaling of the
spectrum of the substrate. We apply our results to the calculation of the
mixing rate and the synchronizability threshold.Comment: 14 pages. To be published in Physical Review
Discovery of spatial periodicities in a coronal loop using automated edge-tracking algorithms
A new method for automated coronal loop tracking, in both spatial and temporal domains, is presented. Applying this technique to TRACE data, obtained using the 171 Ã… filter on 1998 July 14, we detect a coronal loop undergoing a 270 s kink-mode oscillation, as previously found by Aschwanden et al. However, we also detect flare-induced, and previously unnoticed, spatial periodicities on a scale of 3500 km, which occur along the coronal loop edge. Furthermore, we establish a reduction in oscillatory power for these spatial periodicities of 45% over a 222 s interval. We relate the reduction in detected oscillatory power to the physical damping of these loop-top oscillations
On the origin of planets at very wide orbits from the re-capture of free floating planets
In recent years several planets have been discovered at wide orbits (>100 AU)
around their host stars. Theoretical studies encounter difficulties in
explaining their formation and origin. Here we propose a novel scenario for the
production of planetary systems at such orbits, through the dynamical recapture
of free floating planets (FFPs) in dispersing stellar clusters. This process is
a natural extension of the recently suggested scenario for the formation of
wide stellar binaries. We use N-body simulations of dispersing clusters with
10-1000 stars and comparable numbers of FFPs to study this process. We find
that planets are captured into wide orbits in the typical range ~100-10^6 AU,
and have a wide range of eccentricities (thermal distribution). Typically, 3-6
x (f_FFP/1) % of all stars capture a planetary companion with such properties
(where f_FFP is the number of FFP per star). The planetary capture efficiency
is comparable to that of capture-formed stellar-binaries, and shows a similar
dependence on the cluster size and structure. It is almost independent of the
specific planetary mass; planets as well as sub-stellar companions of any mass
can be captured. The capture efficiency decreases with increasing cluster size,
and for a given cluster size the it increases with the host/primary mass. More
than one planet can be captured around the same host and planets can be
captured into binary systems. Planets can also be captured into pre-existing
planetary and into orbits around black holes and massive white dwarfs, if these
formed early enough before the cluster dispersal. In particular, stellar black
holes have a high capture efficiency (>50 % and 5-10 x (f_FFP/1) % for capture
of stars and planetary companions, respectively) due to their large mass.
Finally, although rare, two FFPs or brown dwarfs can become bound and form a
FFP-binary system with no stellar host.Comment: ApJ, in press. Added two figure
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