456 research outputs found
Understanding light in lightweight fabric (ETFE foil) structures through field studies
This paper presents an experimental approach to investigate the luminous environment in lightweight fabric structures through field study. Buildings selected for the field study included the Engineering Science Learning Centre at the University of Nottingham and the Clarke Quay in Singapore.
By undertaking on site monitoring under different sky conditions in the chosen buildings with distinctively different site context, this research project explores how the typical homogeneously lit and rather dull luminous environment in lightweight fabric structure can be improved for enhanced visual interest, visual comfort, and three-dimensional modelling under both sunny and overcast sky conditions. Research data obtained from the subjective appreciation of the internal luminous environments and the quantitative spot measurement and mapping of light are compared and discussed.
This study concluded that selective use of transparent and translucent components in the ETFE envelope can offer architectural designers the opportunities to create well balanced, yet dynamic lit scenes. Also by combining single skin ETFE foil and the double or triple layered ETFE cushion and introducing ETFE cushions with different light transmittance to the building envelope can help improve the overall visual and luminous environment and enhance task illumination. The key findings from this research work are applicable to the design of light in lightweight fabric structure in general
Compatibility of a model for the QCD-Pomeron and chiral-symmetry breaking phenomenologies
The phenomenology of a QCD-Pomeron model based on the exchange of a pair of
non-perturbative gluons, i.e. gluon fields with a finite correlation length in
the vacuum, is studied in comparison with the phenomenology of QCD chiral
symmetry breaking, based on non-perturbative solutions of Schwinger-Dyson
equations for the quark propagator including these non-perturbative gluon
effects. We show that these models are incompatible, and point out some
possibles origins of this problem.Comment: 21 pages, uuencoded latex file, 3 postscript figures, uses epsf.sty
and epsf.tex. To be published in Phys. Lett.
Can We Improve the Preprocessing of Photospheric Vector Magnetograms by the Inclusion of Chromospheric Observations?
The solar magnetic field is key to understanding the physical processes in
the solar atmosphere. Nonlinear force-free codes have been shown to be useful
in extrapolating the coronal field upward from underlying vector boundary data.
However, we can only measure the magnetic field vector routinely with high
accuracy in the photosphere, and unfortunately these data do not fulfill the
force-free condition. We must therefore apply some transformations to these
data before nonlinear force-free extrapolation codes can be self-consistently
applied. To this end, we have developed a minimization procedure that yields a
more chromosphere-like field, using the measured photospheric field vectors as
input. The procedure includes force-free consistency integrals, spatial
smoothing, and -- newly included in the version presented here -- an improved
match to the field direction as inferred from fibrils as can be observed in,
e.g., chromospheric H images. We test the procedure using a model
active-region field that included buoyancy forces at the photospheric level.
The proposed preprocessing method allows us to approximate the chromospheric
vector field to within a few degrees and the free energy in the coronal field
to within one percent.Comment: 22 pages, 6 Figur
On the analysis of the pi -> e nu gamma experimental data
The most general amplitude for the radiative pion decay pi -> e nu gamma
including terms beyond V-A theory is considered. The experimental constraints
on the decay amplitude components are discussed. A model independent
presentation of the results of high statistics and high resolution experiments
is suggested.Comment: 5 pages, 2 figure
Aspects of radiative K^+_e3 decays
We re-investigate the radiative charged kaon decay K+- --> pi0 e+- nu_e gamma
in chiral perturbation theory, merging the chiral expansion with Low's theorem.
We thoroughly analyze the precision of the predicted branching ratio relative
to the non-radiative decay channel. Structure dependent terms and their impact
on differential decay distributions are investigated in detail, and the
possibility to see effects of the chiral anomaly in this decay channel is
emphasized.Comment: 15 pages, 6 figure
Tunneling Violates Special Relativity
Experiments with evanescent modes and tunneling particles have shown that i)
their signal velocity may be faster than light, ii) they are described by
virtual particles, iii) they are nonlocal and act at a distance, iv)
experimental tunneling data of phonons, photons, and electrons display a
universal scattering time at the tunneling barrier front, and v) the properties
of evanescent, i.e. tunneling modes is not compatible with the special theory
of relativity
On the structure and evolution of a polar crown prominence/filament system
Polar crown prominences are made of chromospheric plasma partially circling
the Suns poles between 60 and 70 degree latitude. We aim to diagnose the 3D
dynamics of a polar crown prominence using high cadence EUV images from the
Solar Dynamics Observatory (SDO)/AIA at 304 and 171A and the Ahead spacecraft
of the Solar Terrestrial Relations Observatory (STEREO-A)/EUVI at 195A. Using
time series across specific structures we compare flows across the disk in 195A
with the prominence dynamics seen on the limb. The densest prominence material
forms vertical columns which are separated by many tens of Mm and connected by
dynamic bridges of plasma that are clearly visible in 304/171A two-color
images. We also observe intermittent but repetitious flows with velocity 15
km/s in the prominence that appear to be associated with EUV bright points on
the solar disk. The boundary between the prominence and the overlying cavity
appears as a sharp edge. We discuss the structure of the coronal cavity seen
both above and around the prominence. SDO/HMI and GONG magnetograms are used to
infer the underlying magnetic topology. The evolution and structure of the
prominence with respect to the magnetic field seems to agree with the filament
linkage model.Comment: 24 pages, 14 figures, Accepted for publication in Solar Physics
Journal, Movies can be found at http://www2.mps.mpg.de/data/outgoing/panesar
A spatio-temporal description of the abrupt changes in the photospheric magnetic and Lorentz-force vectors during the 2011 February 15 X2.2 flare
The active region NOAA 11158 produced the first X-class flare of Solar Cycle
24, an X2.2 flare at 01:44 UT on 2011 February 15. Here we analyze SDO/HMI
magnetograms covering a 12-hour interval centered at the time of this flare. We
describe the spatial distributions of the photospheric magnetic changes
associated with this flare, including the abrupt changes in the field vector,
vertical electric current and Lorentz force vector. We also trace these
parameters' temporal evolution. The abrupt magnetic changes were concentrated
near the neutral line and in two neighboring sunspots. Near the neutral line,
the field vectors became stronger and more horizontal during the flare and the
shear increased. This was due to an increase in strength of the horizontal
field components near the neutral line, most significant in the horizontal
component parallel to the neutral line but the perpendicular component also
increased in strength. The vertical component did not show a significant,
permanent overall change at the neutral line. The increase in total flux at the
neutral line was accompanied by a compensating flux decrease in the surrounding
volume. In the two sunspots near the neutral line the azimuthal flux abruptly
decreased during the flare but this change was permanent in only one of the
spots. There was a large, abrupt, downward vertical Lorentz force change during
the flare, consistent with results of past analyses and recent theoretical
work. The horizontal Lorentz force acted in opposite directions along each side
of neutral line, with the two sunspots at each end subject to abrupt torsional
forces. The shearing forces were consistent with field contraction and decrease
of shear near the neutral line, whereas the field itself became more sheared as
a result of the flux collapsing towards the neutral line from the surrounding
volume.Comment: DOI 10.1007/s11207-012-0071-0. Accepted for publication in Solar
Physics SDO3 Topical Issue. Some graphics missing due to 15MB limi
3D MHD Flux Emergence Experiments: Idealized models and coronal interactions
This paper reviews some of the many 3D numerical experiments of the emergence
of magnetic fields from the solar interior and the subsequent interaction with
the pre-existing coronal magnetic field. The models described here are
idealized, in the sense that the internal energy equation only involves the
adiabatic, Ohmic and viscous shock heating terms. However, provided the main
aim is to investigate the dynamical evolution, this is adequate. Many
interesting observational phenomena are explained by these models in a
self-consistent manner.Comment: Review article, accepted for publication in Solar Physic
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