2,580 research outputs found
Design of Glass for High, Short Duration Wind Loads
This paper describes a case study for the design of structural glazed IGUs for theNew Concert Hall in Reykjavik, Iceland, which is subjected to high local windloads of approximately 10kN/m2, with a load duration of approximately 0.1s. Thepaper focuses on how to interpret the current available codes and research to obtaina glass thickness with adequate resistance for the high short duration loads. Thepaper also focuses on the wind loads to be applied when calculating the fixingsystem, the structural silicone, the embedded aluminium profiles and the toggleswhich fix the glass to the aluminium mullions. For short duration wind loads, thencurrently available codes and guidelines only provide the equivalent glass stress fora 3s load duration, equivalent to a kmod = 1. The paper explains how wind load fromwind tunnel tests should be used when sizing glass, and concludes how the IGUsfor the Reykjavik New Concert Hall were sized
Disorder mediated splitting of the cyclotron resonance in two-dimensional electron systems
We perform a direct study of the magnitude of the anomalous splitting in the
cyclotron resonance (CR) of a two-dimensional electron system (2DES) as a
function of sample disorder. In a series of AlGaAs/GaAs quantum wells,
identical except for a range of carbon doping in the well, we find the CR
splitting to vanish at high sample mobilities but to increase dramatically with
increasing impurity density and electron scattering rates. This observation
lends strong support to the conjecture that the non-zero wavevector, roton-like
minimum in the dispersion of 2D magnetoplasmons comes into resonance with the
CR, with the two modes being coupled via disorder.Comment: accepted to PRB Rapid Com
Physical activity and the risk of gestational diabetes mellitus: a systematic review and dose-response meta-analysis of epidemiological studies
Physical activity has been inconsistently associated with risk of gestational diabetes mellitus in epidemiological studies, and questions remain about the strength and shape of the dose-response relationship between the two. We therefore conducted a systematic review and meta-analysis of cohort studies and randomized trials on physical activity and gestational diabetes mellitus. PubMed, Embase and Ovid databases were searched for cohort studies, and randomized controlled trials of physical activity and risk of gestational diabetes mellitus, up to August 5th 2015. Summary relative risks (RRs) were estimated using a random effects model. Twenty-five studies (26 publications) were included. For total physical activity the summary RR for high versus low activity was 0.62 (95 % CI 0.41-0.94, I(2) = 0 %, n = 4) before pregnancy, and 0.66 (95 % CI 0.36-1.21, I(2) = 0 %, n = 3) during pregnancy. For leisure-time physical activity the respective summary RRs for high versus low activity was 0.78 (95 % CI 0.61-1.00, I(2) = 47 %, n = 8) before pregnancy, and it was 0.80 (95 % CI 0.64-1.00, I(2) = 17 %, n = 17) during pregnancy. The summary RR for pre-pregnancy activity was 0.70 (95 % CI 0.49-1.01, I(2) = 72.6 %, n = 3) per increment of 5 h/week and for activity during pregnancy was 0.98 (95 % CI 0.87-1.09, I(2) = 0 %, n = 3) per 5 h/week. There was evidence of a nonlinear association between physical activity before pregnancy and the risk of gestational diabetes mellitus, pnonlinearity = 0.005, with a slightly steeper association at lower levels of activity although further reductions in risk were observed up to 10 h/week. There was also evidence of nonlinearity for physical activity in early pregnancy, pnonlinearity = 0.008, with no further reduction in risk above 8 h/week. There was some indication of inverse associations between walking (before and during pregnancy) and vigorous activity (before pregnancy) and the risk of gestational diabetes mellitus. This meta-analysis suggests that there is a significant inverse association between physical activity before pregnancy and in early pregnancy and the risk of gestational diabetes mellitus. Further studies are needed to clarify the association between specific types and intensities of activity and gestational diabetes mellitus
A Spherical Model for "Starless" Cores of Magnetic Molecular Clouds and Dynamical Effects of Dust Grains
In the standard picture of isolated star formation, dense ``starless'' cores
are formed out of magnetic molecular clouds due to ambipolar diffusion. Under
the simplest spherical geometry, I demonstrate that ``starless'' cores formed
this way naturally exhibit a large scale inward motion, whose size and speed
are comparable to those detected recently by Taffala et al. and Williams et al.
in ``starless'' core L1544. My model clouds have a relatively low mass (of
order 10 ) and low field strength (of order 10 G) to begin with.
They evolve into a density profile with a central plateau surrounded by a
power-law envelope, as found previously. The density in the envelope decreases
with radius more steeply than those found by Mouschovias and collaborators for
the more strongly magnetized, disk-like clouds.
At high enough densities, dust grains become dynamically important by greatly
enhancing the coupling between magnetic field and the neutral cloud matter. The
trapping of magnetic flux associated with the enhanced coupling leads, in the
spherical geometry, to a rapid assemblage of mass by the central protostar,
which exacerbates the so-called ``luminosity problem'' in star formation.Comment: 27 pages, 4 figures, accepted by Ap
Rotation and X-ray emission from protostars
The ASCA satellite has recently detected variable hard X-ray emission from
two Class I protostars in the rho Oph cloud, YLW15 (IRS43) and WL6, with a
characteristic time scale ~20h. In YLW15, the X-ray emission is in the form of
quasi-periodic energetic flares, which we explain in terms of strong magnetic
shearing and reconnection between the central star and the accretion disk. In
WL6, X-ray flaring is rotationally modulated, and appears to be more like the
solar-type magnetic activity ubiquitous on T Tauri stars. We find that YLW15 is
a fast rotator (near break-up), while WL6 rotates with a significantly longer
period. We derive a mass M_\star ~ 2 M_\odot and \simlt 0.4 M_\odot for the
central stars of YLW15 and WL6 respectively. On the long term, the interactions
between the star and the disk results in magnetic braking and angular momentum
loss of the star. On time scales t_{br} ~ a few 10^5 yrs, i.e., of the same
order as the estimated duration of the Class~I protostar stage. Close to the
birthline there must be a mass-rotation relation, t_{br} \simpropto M_\star,
such that stars with M_\star \simgt 1-2 M_\odot are fast rotators, while their
lower-mass counterparts have had the time to spin down. The rapid rotation and
strong star-disk magnetic interactions of YLW15 also naturally explain the
observation of X-ray ``superflares''. In the case of YLW15, and perhaps also of
other protostars, a hot coronal wind (T~10^6 K) may be responsible for the VLA
thermal radio emission. This paper thus proposes the first clues to the
rotation status and evolution of protostars.Comment: 13 pages with 6 figures. To be published in ApJ (April 10, 2000 Part
1 issue
Compact Resolved Ejecta in the Nearest Tidal Disruption Event
Tidal disruption events (TDEs) occur when a star or sub-stellar object passes
close enough to a galaxy's supermassive black hole to be disrupted by tidal
forces. NGC 4845 (d=17 Mpc) was host to a TDE, IGR J12580+0134, detected in
November 2010. Its proximity offers us a unique close-up of the TDE and its
aftermath. We discuss new Very Long Baseline Array (VLBA) and Karl G. Jansky
Very Large Array (JVLA) observations, which show that the radio flux from the
active nucleus created by the TDE has decayed in a manner consistent with
predictions from a jet-circumnuclear medium interaction model. This model
explains the source's broadband spectral evolution, which shows a spectral peak
that has moved from the submm (at the end of 2010) to GHz radio frequencies (in
2011-2013) to <1 GHz in 2015. The milliarcsecond-scale core is circularly
polarized at 1.5 GHz but not at 5 GHz, consistent with the model. The VLBA
images show a complex structure at 1.5 GHz that includes an east west extension
~40 milliarcsec (3 pc) long as well as a resolved component 52 milliarcsec (4.1
pc) northwest of the flat-spectrum core, which is all that can be seen at 5
GHz. If ejected in 2010, the NW component must have had v=0.96 c over five
years. However, this is unlikely, as our model suggests strong deceleration to
speeds < 0.5c within months and a much smaller, sub-parsec size. In this
interpretation, the northwest component could have either a non-nuclear origin
or be from an earlier event.Comment: 12 pages, 8 figures, ApJ, in press; v2 includes error corrections and
slight additions to the analysi
The final fate of spherical inhomogeneous dust collapse II: Initial data and causal structure of singularity
Further to results in [9], pointing out the role of initial density and
velocity distributions towards determining the final outcome of spherical dust
collapse, the causal structure of singularity is examined here in terms of
evolution of the apparent horizon. We also bring out several related features
which throw some useful light towards understanding the nature of this
singularity, including the behaviour of geodesic families coming out and some
aspects related to the stability of singularity.Comment: Latex file, uses epsf.sty, 15 pages and 3 eps figures. Paragraph on
role of smooth functions rewritten. Four references added. To appear in
Classical & Quantum Gravit
Constraints on the Formation and Evolution of Circumstellar Disks in Rotating Magnetized Cloud Cores
We use magnetic collapse models to place some constraints on the formation
and angular momentum evolution of circumstellar disks which are embedded in
magnetized cloud cores. Previous models have shown that the early evolution of
a magnetized cloud core is governed by ambipolar diffusion and magnetic
braking, and that the core takes the form of a nonequilibrium flattened
envelope which ultimately collapses dynamically to form a protostar. In this
paper, we focus on the inner centrifugally-supported disk, which is formed only
after a central protostar exists, and grows by dynamical accretion from the
flattened envelope. We estimate a centrifugal radius for the collapse of mass
shells within a rotating, magnetized cloud core. The centrifugal radius of the
inner disk is related to its mass through the two important parameters
characterizing the background medium: the background rotation rate \Omb and
the background magnetic field strength \Bref. We also revisit the issue of
how rapidly mass is deposited onto the disk (the mass accretion rate) and use
several recent models to comment upon the likely outcome in magnetized cores.
Our model predicts that a significant centrifugal disk (much larger than a
stellar radius) will be present in the very early (Class 0) stage of
protostellar evolution. Additionally, we derive an upper limit for the disk
radius as it evolves due to internal torques, under the assumption that the
star-disk system conserves its mass and angular momentum even while most of the
mass is transferred to a central star.Comment: 23 pages, 1 figure, aastex, to appear in the Astrophysical Journal
(10 Dec 1998
Quantum Radiation from Black Holes and Naked Singularities in Spherical Dust Collapse
A sufficiently massive collapsing star will end its life as a spacetime
singularity. The nature of the Hawking radiation emitted during collapse
depends critically on whether the star's boundary conditions are such as would
lead to the eventual formation of a black hole or, alternatively, to the
formation of a naked singularity. This latter possibility is not excluded by
the singularity theorems. We discuss the nature of the Hawking radiation
emitted in each case. We justify the use of Bogoliubov transforms in the
presence of a Cauchy horizon and show that if spacetime is assumed to terminate
at the Cauchy horizon, the resulting spectrum is thermal, but with a
temperature different from the Hawking temperature.Comment: PHYZZX macros, 27 pages, 3 figure
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