13,496 research outputs found
Upgraded experiments with super neutrino beams: Reach versus Exposure
We introduce exposure as a means to making balanced comparisons of the
sensitivities of long-baseline neutrino experiments to a nonzero \theta_{13},
to CP violation and to the neutrino mass hierarchy. We illustrate its use by
comparing the sensitivities of possible upgrades of superbeam experiments,
namely NOvA*, T2KK and experiments with wide band beams. For the proposed
exposures, we find the best nominal CP violation performance for T2KK. For
equal exposures, a wide band beam experiment has the best mass hierarchy
performance. The physics concept on which NOvA* is based has the best potential
for discovering CP violation only for exposures above a threshold value.Comment: 4 pages, 2 figures, 1 table. Version to appear as a Rapid
Communication in PR
Particles held by springs in a linear shear flow exhibit oscillatory motion
The dynamics of small spheres, which are held by linear springs in a low
Reynolds number shear flow at neighboring locations is investigated. The flow
elongates the beads and the interplay of the shear gradient with the nonlinear
behavior of the hydrodynamic interaction among the spheres causes in a large
range of parameters a bifurcation to a surprising oscillatory bead motion. The
parameter ranges, wherein this bifurcation is either super- or subcritical, are
determined.Comment: 4 pages, 5 figure
Future of superheavy element research: Which nuclei could be synthesized within the next few years?
Low values of the fusion cross sections and very short half-lives of nuclei
with Z120 put obstacles in synthesis of new elements. Different nuclear
reactions (fusion of stable and radioactive nuclei, multi-nucleon transfers and
neutron capture), which could be used for the production of new isotopes of
superheavy (SH) elements, are discussed in the paper. The gap of unknown SH
nuclei, located between the isotopes which were produced earlier in the cold
and hot fusion reactions, can be filled in fusion reactions of Ca with
available lighter isotopes of Pu, Am, and Cm. Cross sections for the production
of these nuclei are predicted to be rather large, and the corresponding
experiments can be easily performed at existing facilities. For the first time,
a narrow pathway is found to the middle of the island of stability owing to
possible -decay of SH isotopes which can be formed in ordinary fusion
reactions of stable nuclei. Multi-nucleon transfer processes at near barrier
collisions of heavy (and very heavy, U-like) ions are shown to be quite
realistic reaction mechanism allowing us to produce new neutron enriched heavy
nuclei located in the unexplored upper part of the nuclear map. Neutron capture
reactions can be also used for the production of the long-living neutron rich
SH nuclei. Strong neutron fluxes might be provided by pulsed nuclear reactors
and by nuclear explosions in laboratory conditions and by supernova explosions
in nature. All these possibilities are discussed in the paper.Comment: An Invited Plenary Talk given by Valeriy I. Zagrebaev at the 11th
International Conference on Nucleus-Nucleus Collisions (NN2012), San Antonio,
Texas, USA, May 27-June 1, 2012. To appear in the NN2012 Proceedings in
Journal of Physics: Conference Series (JPCS
A Multi-Cloud Warm-Absorber Model for NGC 4051
A multi-cloud model is presented which explains the soft X-ray excess in NGC
4051 and, consistently, the optical line spectrum and the SED of the continuum.
The clouds are heated and ionized by the photoionizing flux from the active
center and by shocks. Diffuse radiation, partly absorbed throughout the clouds,
nicely fits the bump in the soft X-ray domain, while bremsstrahlung radiation
from the gaseous clouds contribute to the fit of the continuum SED. Debris of
high density fragmented clouds are necessary to explain the absorption oxygen
throats observed at 0.87 keV and 0.74 keV. The debris are heated by shocks of
about 200-300 km/s. Low velocity (100 km/s)-density (100 cm-3) clouds
contribute to the line and continuum spectra, as well as high velocity (1000
km/s)-density (8000 cm-3) clouds which are revealed by the FWHM of the line
profiles. The SED in the IR is explained by reradiation of dust, however, the
dust-to-gas ratio is not particularly high. Radio emission is well fitted by
synchrotron radiation created at the shock front by Fermi mechanism.Comment: 19 pages + 3 figures PostScrip
X-ray variability of AGNs in the soft and the hard X-ray bands
We investigate the X-ray variability characteristics of hard X-ray selected
AGNs (based on Swift/BAT data) in the soft X-ray band using the RXTE/ASM data.
The uncertainties involved in the individual dwell measurements of ASM are
critically examined and a method is developed to combine a large number of
dwells with appropriate error propagation to derive long duration flux
measurements (greater than 10 days). We also provide a general prescription to
estimate the errors in variability derived from rms values from unequally
spaced data. Though the derived variability for individual sources are not of
very high significance, we find that, in general, the soft X-ray variability is
higher than those in hard X-rays and the variability strengths decrease with
energy for the diverse classes of AGN. We also examine the strength of
variability as a function of the break time scale in the power density spectrum
(derived from the estimated mass and bolometric luminosity of the sources) and
find that the data are consistent with the idea of higher variability at time
scales longer than the break time scale.Comment: 17 pages, 15 Postscript figures, 3 tables, accepted for publication
in Ap
Chandra observations of the accretion-driven millisecond X-ray pulsars XTE J0929-314 and XTE J1751-305 in quiescence
(Abridge) We observed the accreting millisecond X-ray pulsars XTE J0929-314
and XTE J1751-305 in their quiescent states using Chandra. From XTE J0929-314
we detected 22 photons (0.3-8 keV) in 24.4 ksec, resulting in a count rate of 9
x 10^{-4} c/s. The small number of photons detected did not allow for a
detailed spectral analysis, but we can demonstrate that the spectrum is harder
than simple thermal emission which is what is usually presumed to arise from a
cooling neutron star that has been heated during the outbursts. Assuming a
power-law model for the spectrum, we obtain a power-law index of ~1.8 and an
unabsorbed flux of 6 x 10^{-15} ergs/s/cm^2 (0.5-10 keV), resulting in a
luminosity of 7 x 10^{31} (d/10 kpc)^2 ergs/s, with d in kpc. No thermal
component could be detected; such a component contributed at most 30% to the
0.5-10 keV flux. Variability in the count rate of XTE J0929-314 was observed at
the 95% confidence level. We did not conclusively detect XTE J1751-305 in our
43 ksec observation, with 0.5-10 keV flux upper limits between 0.2 and 2.7 x
10^{-14} ergs/s/cm^2 depending on assumed spectral shape, resulting in
luminosity upper limits of 0.2 - 2 x 10^{32} (d/8 kpc)^2 ergs/s. We compare our
results with those obtained for other neutron-star X-ray transients in their
quiescent state. Using simple accretion disk physics in combination with our
measured quiescent luminosity of XTE J0929-314 and the luminosity upper limits
of XTE J1751-305, and the known spin frequency of the neutron stars, we could
constrain the magnetic field of the neutron stars in XTE J0929-314 and XTE
J1751-305 to be less than 3 x 10^9 (d/10 kpc) and 3 - 7 x 10^8 (d/8 kpc) Gauss
(depending on assumed spectral shape of the quiescent spectrum), respectively.Comment: Accepted for publication in ApJ, 29 September 2004. Added spectral
variability search for the data of XTE J0929-314 and added the non-detection
with Chandra of XTE J1751-30
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