3,640 research outputs found
Mapping and historical reconstruction of the great Mexican 22 June 1932 tsunami
At 07:00 h (UTC-6) on 22 June 1932, a <i>M</i><sub>s</sub> = 6.9 earthquake shocked the coasts of Colima and Jalisco. Five minutes later a tsunami arrived at the coast. It almost completely destroyed the town of Cuyutlán, Colima, causing the deaths of 50 people and leaving about 1200 injured. In this study, newspaper reports and technical reports are reviewed, as well as survivors' testimonials. The physical characteristics (mean sea level at the time, time of arrival, sea retreat, and inundation distribution) and the tsunami effects (number of victims, injuries, affected buildings) have been reconstructed and mapped. The interpretation of historical data allowed us to determine the intensity of the tsunami and to reveal the tsunamigenic source. This study emphasizes the relevance of historical analysis, including survivor's testimonies, in the reconstruction of tsunamis that lack instrumental data. The results of this study are relevant to paleotsunami studies and tsunami related hazard planning
Chains of Viscoelastic Spheres
Given a chain of viscoelastic spheres with fixed masses of the first and last
particles. We raise the question: How to chose the masses of the other
particles of the chain to assure maximal energy transfer? The results are
compared with a chain of particles for which a constant coefficient of
restitution is assumed. Our simple example shows that the assumption of
viscoelastic particle properties has not only important consequences for very
large systems (see [1]) but leads also to qualitative changes in small systems
as compared with particles interacting via a constant restitution coefficient.Comment: 11 pages, 6 figure
The Frequency of Carbon Stars Among Extremely Metal-Poor Stars
We demonstrate that there are systematic scale errors in the [Fe/H] values
determined by the Hamburg/ESO Survey (and by inference by the HK Survey in the
past) for certain extremely metal poor highly C-enhanced giants. The
consequences of these scale errors are that a) the fraction of carbon stars at
extremely low metallicities has been overestimated in several papers in the
recent literature b) the number of extremely metal poor stars known is somewhat
lower than has been quoted in the recent literature c) the yield for extremely
metal poor stars by the HES Survey is somewhat lower than is stated in the
recent literature. A preliminary estimate for the frequency of Carbon stars
among the giants in the HES sample with -4 < [Fe/H] < -2.0 dex is 7.4 +-2.9%;
adding an estimate for the C-enhanced giants with [C/Fe] > 1.0 dex without
detectable C2 bands raises the fraction to 14 +-4$%.
We rely on the results of an extensive set of homogeneous detailed abundance
analyses of stars expected to have [Fe/H] < -3.0 dex selected from the HES to
establish these claims. We have found that the Fe-metallicity of the cooler
(Teff < 5200K) C-stars as derived from spectra taken with HIRES at Keck are a
factor of ~10 higher than those obtained via the algorithm used by the HES
project to analyze the moderate resolution follow-up spectra, which is
identical to that used until very recently by the HK Survey. This error in
Fe-abundance estimate for C-stars arises from a lowering of the emitted flux in
the continuum bandpasses of the KP (3933 A line of CaII) and particularly the
HP2 (Hdelta) indices used to estimate [Fe/H] due to absorption from strong
molecular bands.Comment: Accepted to the ApJL after a very lengthly duel with the 3
simultaneous referee
CLASSICAL SPLITTING OF FUNDAMENTAL STRINGS
We find exact solutions of the string equations of motion and constraints
describing the {\em classical}\ splitting of a string into two. We show that
for the same Cauchy data, the strings that split have {\bf smaller} action than
the string without splitting. This phenomenon is already present in flat
space-time. The mass, energy and momentum carried out by the strings are
computed. We show that the splitting solution describes a natural decay process
of one string of mass into two strings with a smaller total mass and some
kinetic energy. The standard non-splitting solution is contained as a
particular case. We also describe the splitting of a closed string in the
background of a singular gravitational plane wave, and show how the presence of
the strong gravitational field increases (and amplifies by an overall factor)
the negative difference between the action of the splitting and non-splitting
solutions.Comment: 27 pages, revtex
Simple mechanism for a positive exchange bias
We argue that the interface coupling, responsible for the positive exchange
bias (HE) observed in ferromagnetic/compensated antiferromagnetic (FM/AF)
bilayers, favors an antiferromagnetic alignment. At low cooling field this
coupling polarizes the AF spins close to the interface, which spin
configuration persists after the sample is cooled below the Neel temperature.
This pins the FM spins as in Bean's model and gives rise to a negative HE. When
the cooling field increases, it eventually dominates and polarizes the AF spins
in an opposite direction to the low field one. This results in a positive HE.
The size of HE and the crossover cooling field are estimated. We explain why HE
is mostly positive for an AF single crystal, and discuss the role of interface
roughness on the magnitude of HE, and the quantum aspect of the interface
coupling.Comment: 10 pages, 2 figures, to be published on May 1 issue of PR
Self-diffusion in granular gases
The coefficient of self-diffusion for a homogeneously cooling granular gas
changes significantly if the impact-velocity dependence of the restitution
coefficient is taken into account. For the case of a constant
the particles spread logarithmically slow with time, whereas the
velocity dependent coefficient yields a power law time-dependence. The impact
of the difference in these time dependences on the properties of a freely
cooling granular gas is discussed.Comment: 6 pages, no figure
Gravitational Duality in MacDowell-Mansouri Gauge Theory
Strong-weak duality invariance can only be defined for particular sectors of
supersymmetric Yang-Mills theories. Nevertheless, for full non-Abelian
non-supersymmetric theories, dual theories with inverted couplings, have been
found. We show that an analogous procedure allows to find the dual action to
the gauge theory of gravity constructed by the MacDowell-Mansouri model plus
the superposition of a term.Comment: 9 pages, LaTeX, no figure
Signal processing and frequency-dependent associative memory based on nanoswitches
A signal processing concept based on nanoscale switches whose conductance can be tuned by an external stimulus between two (ON and OFF) states is proposed and analyzed theoretically. The building block of the system is formed by a metal nanoparticle linked to two electrodes by an organic ligand and a molecular switch. When we apply an alternating potential to the system of the same frequency as the periodic variation between the ON and OFF states induced on the switch, the net charge delivered by the system exhibits a sharp resonance. This resonance can be used to process an external signal by selectively extracting the weight of the different harmonics. In addition, a frequency-dependent associative memory that exploits the resonance property is also demonstrated. The general properties of the signal processing concept that are required for practical implementation are analyzed for different temperatures, times, conductance ratios, applied potentials, and noise [email protected] [email protected]
The VLT-FLAMES Tarantula Survey X: Evidence for a bimodal distribution of rotational velocities for the single early B-type stars
Aims: Projected rotational velocities (\vsini) have been estimated for 334
targets in the VLT-FLAMES Tarantula survey that do not manifest significant
radial velocity variations and are not supergiants. They have spectral types
from approximately O9.5 to B3. The estimates have been analysed to infer the
underlying rotational velocity distribution, which is critical for
understanding the evolution of massive stars.
Methods: Projected rotational velocities were deduced from the Fourier
transforms of spectral lines, with upper limits also being obtained from
profile fitting. For the narrower lined stars, metal and non-diffuse helium
lines were adopted, and for the broader lined stars, both non-diffuse and
diffuse helium lines; the estimates obtained using the different sets of lines
are in good agreement. The uncertainty in the mean estimates is typically 4%
for most targets. The iterative deconvolution procedure of Lucy has been used
to deduce the probability density distribution of the rotational velocities.
Results: Projected rotational velocities range up to approximately 450 \kms
and show a bi-modal structure. This is also present in the inferred rotational
velocity distribution with 25% of the sample having \ve100\,\kms
and the high velocity component having \ve\,\kms. There is no
evidence from the spatial and radial velocity distributions of the two
components that they represent either field and cluster populations or
different episodes of star formation. Be-type stars have also been identified.
Conclusions: The bi-modal rotational velocity distribution in our sample
resembles that found for late-B and early-A type stars. While magnetic braking
appears to be a possible mechanism for producing the low-velocity component, we
can not rule out alternative explanations.Comment: to be publisged in A&
Point Sources from a Spitzer IRAC Survey of the Galactic Center
We have obtained Spitzer/IRAC observations of the central 2.0 x 1.4 degrees
(~280 x 200 pc) of the Galaxy at 3.6-8.0 microns. A point source catalog of
1,065,565 objects is presented. The catalog includes magnitudes for the point
sources at 3.6, 4.5, 5.8, and 8.0 microns, as well as JHK photometry from
2MASS. The point source catalog is confusion limited with average limits of
12.4, 12.1, 11.7, and 11.2 magnitudes for [3.6], [4.5], [5.8], and [8.0],
respectively. We find that the confusion limits are spatially variable because
of stellar surface density, background surface brightness level, and extinction
variations across the survey region. The overall distribution of point source
density with Galactic latitude and longitude is essentially constant, but
structure does appear when sources of different magnitude ranges are selected.
Bright stars show a steep decreasing gradient with Galactic latitude, and a
slow decreasing gradient with Galactic longitude, with a peak at the position
of the Galactic center. From IRAC color-magnitude and color-color diagrams, we
conclude that most of the point sources in our catalog have IRAC magnitudes and
colors characteristic of red giant and AGB stars.Comment: 44 pages, 13 figures, ApJS in pres
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