1,318 research outputs found
A large displacement structural analysis of a pipeline subjected to gravity and bouyancy forces
p. 489-508A nonlinear analysis of an elastic tube subjected to gravity forces and buoyancy pressure is carried out. An update lagrangian formulation is used. The structural analysis efficiency in terms of computer time and accuracy, has been improved when load stiffness matrices have been introduced. In this way the follower forces characteristics such as their intensity and direction changes can be well represented. A sensitivity study of different involved variables on the final deformed pipeline shape is carried out.Mosquera, JC.; Garcia-Palacios, J.; Samartin, A. (2009). A large displacement structural analysis of a pipeline subjected to gravity and bouyancy forces. Editorial Universitat Politècnica de València. http://hdl.handle.net/10251/654
Determinación de los periodos propios de presas bóveda simétricas mediante fórmulas empíricas
El artículo presenta una formulación sencilla que permite obtener los seis primeros períodos propios de vibración de una presa bóveda simétrica diseñada según las recomendaciones del U.S. Bureau of Reclamation. Se indican las expresiones polinómicas aproximadas de estos períodos, tanto para embalse vacío como para embalse lleno. El efecto del embalse se modeliza mediante la técnica de Westergaard modificada. Asimismo se indica una expresión que intenta tener en cuenta, de modo tentativo, el efecto de la flexibilidad del terreno.Peer Reviewe
An origin for the main pulsation and overtones of SGR1900+14 during the August 27 (1998) superoutburst
The crucial observation on the occurrence of subpulses (overtones) in the
Power Spectral Density of the August 27 (1998) event from SGR1900+14, as
discovered by BeppoSAX (Feroci et al. 1999), has received no consistent
explanation in the context of the competing theories to explain the SGRs
phenomenology: the magnetar and accretion-driven models. Based on the
ultra-relativistic, ultracompact X-ray binary model introduced in the
accompanying paper (Mosquera Cuesta 2004a), I present here a self-consistent
explanation for such an striking feature. I suggest that both the fundamental
mode and the overtones observed in SGR1900+14 stem from pulsations of a massive
white dwarf (WD). The fundamental mode (and likely some of its harmonics) is
excited because of the mutual gravitational interaction with its orbital
companion (a NS, envisioned here as point mass object) whenever the binary
Keplerian orbital frequency is a multiple integer number () of that mode
frequency (Pons et al. 2002). Besides, a large part of the powerful irradiation
from the fireball-like explosion occurring on the NS (after partial accretion
of disk material) is absorbed in different regions of the star driving the
excitation of other multipoles (Podsiadlowski 1991,1995), i.e., the overtones
(fluid modes of higher frequency). Part of this energy is then reemitted into
space from the WD surface or atmosphere. This way, the WD lightcurve carries
with it the signature of these pulsations inasmuch the way as it happens with
the Sun pulsations in Helioseismology. It is shown that our theoretical
prediction on the pulsation spectrum agrees quite well with the one found by
BeppoSAX (Feroci et al. 1999). A feature confirmed by numerical simulations
(Montgomery & Winget 2000).Comment: This paper was submitted as a "Letter to the Editor" of MNRAS in July
17/2004. Since that time no answer or referee report was provided to the
Author [MNRAS publication policy limits reviewal process no longer than one
month (+/- half more) for the reviewal of this kind of submission]. I hope
this contribution is not receiving a similar "peer-reviewing" as given to the
A. Dar and A. De Rujula's "Cannonball model for gamma-ray bursts", or to the
R.K. Williams' "Penrose process for energy extraction from rotating black
holes". The author welcomes criticisms and suggestions on this pape
A Robust Determination of the size of quasar accretion disks using gravitational microlensing
Using microlensing measurements from a sample of 27 image-pairs of 19 lensed
quasars we determine a maximum likelihood estimate for the accretion disk size
of an {{\em}average} quasar of light days at rest
frame \AA\ for microlenses with a mean mass of
. This value, in good agreement with previous results from
smaller samples, is roughly a factor of 5 greater than the predictions of the
standard thin disk model. The individual size estimates for the 19 quasars in
our sample are also in excellent agreement with the results of the joint
maximum likelihood analysis.Comment: 6 pages, 3 figures, submitted to Ap
Hubble Diagram of Gamma-Rays Bursts calibrated with Gurzadyan-Xue Cosmology
Gamma-ray bursts (GRBs) being the most luminous among known cosmic objects
carry an essential potential for cosmological studies if properly used as
standard candles. In this paper we test with GRBs the cosmological predictions
of the Gurzadyan-Xue (GX) model of dark energy, a novel theory that predicts,
without any free parameters, the current vacuum fluctuation energy density
close to the value inferred from the SNIa observations. We also compare the GX
results with those predicted by the concordance scenario -CDM.
According to the statistical approach by Schaefer (2007), the use of several
empirical relations obtained from GRBs observables, after a consistent
calibration for a specific model, enables one to probe current cosmological
models. Based on this recently introduced method, we use the 69 GRBs sample
collected by Schaefer (2007); and the most recently released SWIFT satellite
data (Sakamoto et al. 2007) together with the 41 GRBs sample collected by
Rizzuto et al. (2007), which has the more firmly determined redshifts. Both
data samples span a distance scale up to redshift about 7. We show that the GX
models are compatible with the Hubble diagram of the Schaefer (2007) 69 GRBs
sample. Such adjustment is almost identical to the one for the concordance
-CDM.Comment: 9 pages, 17 figures, 11 tables; Astr. & Astrophys. (in press
Revealing the Structure of an Accretion Disk Through Energy Dependent X-ray Microlensing
We present results from monitoring observations of the gravitationally lensed
quasar RX J1131-1231 performed with the Chandra X-ray Observatory. The X-ray
observations were planned with relatively long exposures that allowed a search
for energy-dependent microlensing in the soft (0.2-2 keV) and hard (2-10 keV)
light curves of the images of RX J1131-1231. We detect significant microlensing
in the X-ray light-curves of images A and D, and energy-dependent microlensing
of image D. The magnification of the soft band appears to be larger than that
in the hard band by a factor of ~ 1.3 when image D becomes more magnified. This
can be explained by the difference between a compact, softer-spectrum corona
that is producing a more extended, harder spectrum reflection component off the
disk. This is supported by the evolution of the fluorescent iron line in image
D over three consecutive time-averaged phases of the light curve. In the first
period, a Fe line at E = 6.36(-0.16,+0.13) keV is detected (at > 99%
confidence). In the second period, two Fe lines are detected, one at E =
5.47(-0.08,+0.06) keV (detected at > 99% confidence) and another at E =
6.02(-0.07,+0.09) keV (marginally detected at > 90% confidence), and in the
third period, a broadened Fe line at 6.42(-0.15,+0.19) keV is detected (at >
99% confidence). This evolution of the Fe line profile during the microlensing
event is consistent with the line distortion expected when a caustic passes
over the inner disk where the shape of the fluorescent Fe line is distorted by
General Relativistic and Doppler effects.Comment: 20 pages, includes 10 figures, submitted to Ap
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