7,830 research outputs found
On the thin-string limit of the 6d stringlike defect model
We show that in 6d models localizing gravity on stringlike defects and
satisfying the dominant energy condition, the metric exterior to the string
inevitably depends on the string's thickness. As a consequence, in the limit of
thin string either the gravity delocalizes, or the six-dimensional Planck scale
must be much larger that the four-dimensional one.Comment: 3 pages; v2: an alternative interpretation of our results, overlooked
in the first version, is adde
Identifying new physics contributions in the Higgs sector at linear e+e- colliders
Loop driven decay modes of the Higgs are sensitive to new physics
contributions because of new particles in the loops. To highlight this we look
at the dilepton-dijet signal in the dominant Higgs production channel at a
linear e+e- collider. We show that by taking a simple ratio between
cross-sections of two different final states such contributions can be very
easily identified.Comment: Latex 4 pages, 2 eps figures (style files included). Talk given at
the linear collider workshop LCWS06, Bangalore, March 200
X-ray Dust Scattering at Small Angles: The Complete Halo around GX13+1
The exquisite angular resolution available with Chandra should allow
precision measurements of faint diffuse emission surrounding bright sources,
such as the X-ray scattering halos created by interstellar dust. However, the
ACIS CCDs suffer from pileup when observing bright sources, and this creates
difficulties when trying to extract the scattered halo near the source. The
initial study of the X-ray halo around GX13+1 using only the ACIS-I detector
done by Smith, Edgar & Shafer (2002) suffered from a lack of sensitivity within
50'' of the source, limiting what conclusions could be drawn.
To address this problem, observations of GX13+1 were obtained with the
Chandra HRC-I and simultaneously with the RXTE PCA. Combined with the existing
ACIS-I data, this allowed measurements of the X-ray halo between 2-1000''.
After considering a range of dust models, each assumed to be smoothly
distributed with or without a dense cloud along the line of sight, the results
show that there is no evidence in this data for a dense cloud near the source,
as suggested by Xiang et al. (2005). Finally, although no model leads to
formally acceptable results, the Weingartner & Draine (2001) and nearly all of
the composite grain models from Zubko, Dwek & Arendt (2004) give poor fits.Comment: 8 pages, 6 figures, accepted for publication in Ap
SMP: A solid modeling program
A prototype solid modeling program, SMP, developed by CSC for Langley Research Center (LaRC) is documented in this paper. The SMP software is employed by the System and Experiments Branch (SEB) of the Space Systems Division (SSD) for preliminary space station design, but is intended as a general purpose tool. The SMP document provides details concerning: the basic geometric modeling primitives and associated operators, the data representation scheme utilized to structure the geometric model, the available commands for both editing and displaying the solid model, the interactive user interface and the input/output interfaces to external software, and the utility of the package in the LaRC computing environment. The document is sufficiently detailed to serve both as a user's guide and reference manual
Scalar field localization on a brane with cosmological constant
We address the localization of a scalar field, whose bulk-mass M is
considered in a wide range including the tachyonic region,on a three-brane. The
brane with non-zero cosmological constant is embedded in five
dimensional bulk space. We find in this case that the trapped scalar could have
mass which has an upper bound and expressed as with the calculable numbers . We point
out that this result would be important to study the stability of the brane and
cosmological problems based on the brane-world.Comment: 14 pages, 5 figure
Ionization Equilibrium Timescales in Collisional Plasmas
Astrophysical shocks or bursts from a photoionizing source can disturb the
typical collisional plasma found in galactic interstellar media or the
intergalactic medium. The spectrum emitted by this plasma contains diagnostics
that have been used to determine the time since the disturbing event, although
this determination becomes uncertain as the elements in the plasma return to
ionization equilibrium. A general solution for the equilibrium timescale for
each element arises from the elegant eigenvector method of solution to the
problem of a non-equilibrium plasma described by Masai (1984) and Hughes &
Helfand (1985). In general the ionization evolution of an element Z in a
constant electron temperature plasma is given by a coupled set of Z+1 first
order differential equations. However, they can be recast as Z uncoupled first
order differential equations using an eigenvector basis for the system. The
solution is then Z separate exponential functions, with the time constants
given by the eigenvalues of the rate matrix. The smallest of these eigenvalues
gives the scale of slowest return to equilibrium independent of the initial
conditions, while conversely the largest eigenvalue is the scale of the fastest
change in the ion population. These results hold for an ionizing plasma, a
recombining plasma, or even a plasma with random initial conditions, and will
allow users of these diagnostics to determine directly if their best-fit result
significantly limits the timescale since a disturbance or is so close to
equilibrium as to include an arbitrarily-long time.Comment: 4 pages, 2 figures. Accepted for publication by the Astrophysical
Journa
Growing Pains or Opportunities? A Customer Survey of Three Farmers\u27 Markets in One Rural Community
The continued growth of farmers\u27 markets is presenting new challenges to Extension. As the number of markets expands, how can Extension help those in the same community work together for mutual benefit? The study reported here examined similarities and differences among customers attending three different farmers\u27 markets within a single locality in Gettysburg, Pennsylvania. Based on 370 customer surveys, study results underscore the diversity of markets operating within the same community and provide insights into ways Extension might assist markets to work together to expand their shared customer base, increase revenues, and better serve local residents
Resiliently evolving supply-demand networks
Peer reviewedPublisher PD
Observations and asteroseismological analysis of the rapid subdwarf B pulsator EC 09582-1137
We made photometric and spectroscopic observations of the rapidly pulsating
subdwarf B star EC 09582-1137 with the aim of determining the target's
fundamental structural parameters from asteroseismology. The new data comprise
~ 30 hours of fast time-series photometry obtained with SUSI2 at the NTT on La
Silla, Chile, as well as 1 hour of low-resolution spectroscopy gathered with
EMMI, also mounted on the NTT. From the photometry we detected 5 independent
harmonic oscillations in the 135-170 s period range with amplitudes up to 0.5%
of the mean brightness of the star. In addition, we extracted two periodicities
interpreted as components of a rotationally split multiplet that indicate a
rotation period of the order of 2-5 days. We also recovered the first harmonic
of the dominant pulsation, albeit at an amplitude below the imposed 4-sigma
detection threshold. The spectroscopic observations led to the following
estimates of the atmospheric parameters of EC 09582-1137: Teff = 34,806+-233 K,
log g = 5.80+-0.04, and log[N(He)/N(H)] = - 1.68+-0.06.
Using the observed oscillations as input, we searched in model parameter
space for unique solutions that present a good fit to the data. Under the
assumption that the two dominant observed periodicities correspond to radial or
dipole modes, we were able to isolate a well-constrained optimal model that
agrees with the atmospheric parameters derived from spectroscopy. The inferred
structural parameters of EC 09582-1137 are Teff = 34,806 K (from spectroscopy),
log g = 5.788+-0.004, M = 0.485+-0.011 M_solar, log(M_env/M_star) = -
4.39+-0.10, R = 0.147+-0.002 R_solar, and L = 28.6+-1.7 L_solar. We
additionally derive the absolute magnitude M_V = 4.44+-0.05 and the distance d
= 1460+-66 pc.Comment: accepted for publication in Astronomy and Astrophysic
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