5,728 research outputs found
Time delay of light signals in an energy-dependent spacetime metric
In this note we review the problem of time delay of photons propagating in a
spacetime with a metric that explicitly depends on the energy of the particles
(Gravity-Rainbow approach). We show that corrections due to this approach --
which is closely related to DSR proposal -- produce for small redshifts
() smaller time delays than in the generic Lorentz Invariance Violating
case.Comment: 5 pages. This version contains two new references with respect to the
published versio
String Thermodynamics in D-Brane Backgrounds
We discuss the thermal properties of string gases propagating in various
D-brane backgrounds in the weak-coupling limit, and at temperatures close to
the Hagedorn temperature. We determine, in the canonical ensemble, whether the
Hagedorn temperature is limiting or non-limiting. This depends on the
dimensionality of the D-brane, and the size of the compact dimensions. We find
that in many cases the non-limiting behaviour manifest in the canonical
ensemble is modified to a limiting behaviour in the microcanonical ensemble and
show that, when there are different systems in thermal contact, the energy
flows into open strings on the `limiting' D-branes of largest dimensionality.
Such energy densities may eventually exceed the D-brane intrinsic tension. We
discuss possible implications of this for the survival of Dp-branes with large
values of p in an early cosmological Hagedorn regime. We also discuss the
general phase diagram of the interacting theory, as implied by the holographic
and black-hole/string correspondence principles.Comment: 50 pages, LaTeX, 4 eps figures. Added discussion of random walk
picture. Corrected technical error in the treatment of ND strings (notice
some formulas are rewritten). Conclusions unchange
Random Antiferromagnetic SU(N) Spin Chains
We analyze random isotropic antiferromagnetic SU(N) spin chains using the
real space renormalization group. We find that they are governed at low
energies by a universal infinite randomness fixed point different from the one
of random spin-1/2 chains. We determine analytically the important exponents:
the energy-length scale relation is , where
, and the mean correlation function is given by
, where . Our analysis shows
that the infinite-N limit is unable to capture the behavior obtained at any
finite N.Comment: 4 pages, 3 figure
Some Thermodynamical Aspects of String Theory
Thermodynamical aspects of string theory are reviewed and discussed.Comment: 22 Pages plain latex; based on contributions to Golfand Memorial
Volume and Englertfest by E.Rabinovic
X-ray Scattering Study of the spin-Peierls transition and soft phonon behavior in TiOCl
We have studied the S=1/2 quasi-one-dimensional antiferromagnet TiOCl using
single crystal x-ray diffraction and inelastic x-ray scattering techniques. The
Ti ions form staggered spin chains which dimerize below Tc1 = 66 K and have an
incommensurate lattice distortion between Tc1 and Tc2 = 92 K. Based on our
measurements of the intensities, wave vectors, and harmonics of the
incommensurate superlattice peaks, we construct a model for the incommensurate
modulation. The results are in good agreement with a soliton lattice model,
though some quantitative discrepancies exist near Tc2. The behavior of the
phonons has been studied using inelastic x-ray scattering with ~2 meV energy
resolution. For the first time, a zone boundary phonon which softens at the
spin-Peierls temperature Tsp has been observed. Our results show reasonably
good quantitative agreement with the Cross-Fisher theory for the phonon
dynamics at wave vectors near the zone boundary and temperatures near Tsp.
However, not all aspects of the data can be described, such as the strong
overdamping of the soft mode above Tsp. Overall, our results show that TiOCl is
a good realization of a spin-Peierls system, where the phonon softening allows
us to identify the transition temperature as Tsp=Tc2=92 KComment: 14 pages, 14 figure
Fermion Masses and Mixing in Four and More Dimensions
We give an overview of recent progress in the study of fermion mass and
flavor mixing phenomena. Mass matrix ansatze are considered within the SM and
SUSY GUTs where some predictive frameworks based on SU(5) and SO(10) are
reviewed. We describe a variety of schemes to construct quark mass matrices in
extra dimensions focusing on four major classes: models with the SM residing on
3-brane, models with universal extra dimensions, models with split fermions and
models with warped extra dimensions. We outline how realistic patterns of quark
mass matrices could be derived from orbifold models in heterotic superstring
theory. Finally, we address the fermion mass problem in intersecting D-branes
scenarios, and present models with D6-branes able to give a good quantitatively
description of quark masses and mixing. The role of flavor/CP violation problem
as a probe of new physics is emphasized.Comment: a review based on seminars presented by S.K. in different places, 34
pages, late
Static and dynamic analysis of sandwich shells with viscoelastic damping
Static and dynamic elasticity, and viscous damping of laminated and sandwich plates, shells, and beam
Metallicity determination in gas-rich galaxies with semiempirical methods
A study of the precision of the semiempirical methods used in the
determination of the chemical abundances in gas-rich galaxies is carried out.
In order to do this the oxygen abundances of a total of 438 galaxies were
determined using the electronic temperature, the and the P methods.
The new calibration of the P method gives the smaller dispersion for the low
and high metallicity regions, while the best numbers in the turnaround region
are given by the method. We also found that the dispersion correlates
with the metallicity. Finally, it can be said that all the semiempirical
methods studied here are quite insensitive to metallicity with a value of
dex for more than 50% of the total sample.
\keywords{ISM: abundances; (ISM): H {\sc ii} regions}Comment: 26 pages, 9 figures and 2 tables. To appear at AJ, January 200
Physical conditions in the gas phases of the giant HII region LMC-N11 unveiled by Herschel - I. Diffuse [CII] and [OIII] emission in LMC-N11B
(Abridged) The Magellanic Clouds provide a nearby laboratory for metal-poor
dwarf galaxies. The low dust abundance enhances the penetration of UV photons
into the interstellar medium (ISM), resulting in a relatively larger filling
factor of the ionized gas. Furthermore, there is likely a hidden molecular gas
reservoir probed by the [CII]157um line. We present Herschel/PACS maps in
several tracers, [CII], [OI]63um,145um, [NII]122um, [NIII]57um, and [OIII]88um
in the HII region N11B in the Large Magellanic Cloud. Halpha and [OIII]5007A
images were used as complementary data to investigate the effect of dust
extinction. Observations were interpreted with photoionization models to infer
the gas conditions and estimate the ionized gas contribution to the [CII]
emission. Photodissociation regions (PDRs) are probed through polycyclic
aromatic hydrocarbons (PAHs). We first study the distribution and properties of
the ionized gas. We then constrain the origin of [CII]157um by comparing to
tracers of the low-excitation ionized gas and of PDRs. [OIII] is dominated by
extended emission from the high-excitation diffuse ionized gas; it is the
brightest far-infrared line, ~4 times brighter than [CII]. The extent of the
[OIII] emission suggests that the medium is rather fragmented, allowing far-UV
photons to permeate into the ISM to scales of >30pc. Furthermore, by comparing
[CII] with [NII], we find that 95% of [CII] arises in PDRs, except toward the
stellar cluster for which as much as 15% could arise in the ionized gas. We
find a remarkable correlation between [CII]+[OI] and PAH emission, with [CII]
dominating the cooling in diffuse PDRs and [OI] dominating in the densest PDRs.
The combination of [CII] and [OI] provides a proxy for the total gas cooling in
PDRs. Our results suggest that PAH emission describes better the PDR gas
heating as compared to the total infrared emission.Comment: Accepted for publication in Astronomy and Astrophysics. Fixed
inverted line ratio in Sect. 5.
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