1,441 research outputs found
Structural Phase Transition in the Superconducting Pyrochlore Oxide Cd2Re2O7
We report a structural phase transition found at Ts = 200 K in a pyrochlore
oxide Cd2Re2O7 which shows superconductivity at Tc = 1.0 K. X-ray
diffractionexperiments indicate that the phase transition is of the second
order, from a high-temperature phase with the ideal cubic pyrochlore structure
(space group Fd-3m) to a low-temperature phase with another cubic structure
(space group F-43m). It is accompanied by a dramatic change in the resistivity
and magnetic susceptibility and thus must induce a significant change in the
electronic structure of Cd2Re2O7.Comment: 4 pages, 4figures, proceeding for ISSP
Product Origin and Reputation for Quality: the Case of Organic Foods
Replaced with revised version of paper 12/30/09.Agribusiness, Demand and Price Analysis, Industrial Organization,
Crustal Heating and Quiescent Emission from Transiently Accreting Neutron Stars
Nuclear reactions occurring deep in the crust of a transiently accreting
neutron star efficiently maintain the core at a temperature >5e7 K. When
accretion halts, the envelope relaxes to a thermal equilibrium set by the flux
from the hot core, as if the neutron star were newly born. For the
time-averaged accretion rates typical of low-mass X-ray transients, standard
neutrino cooling is unimportant and the core thermally re-radiates the
deposited heat. The resulting luminosity has the same magnitude as that
observed from several transient neutron stars in quiescence. Confirmation of
this mechanism would strongly constrain rapid neutrino cooling mechanisms for
neutron stars. Thermal emission had previously been dismissed as a predominant
source of quiescent emission since blackbody spectral fits implied an emitting
area much smaller than a neutron star's surface. However, as with thermal
emission from radio pulsars, fits with realistic emergent spectra will imply a
substantially larger emitting area. Other emission mechanisms, such as
accretion or a pulsar shock, can also operate in quiescence and generate
intensity and spectral variations over short timescales. Indeed, quiescent
accretion may produce gravitationally redshifted metal photoionization edges in
the quiescent spectra (detectable with AXAF and XMM). We discuss past
observations of Aql~X-1 and note that the low luminosity X-ray sources in
globular clusters and the Be star/X-ray transients are excellent candidates for
future study.Comment: 5 pages, 2 ps figures, uses AASTEX macros. To appear in ApJ letters,
10 September 1998. Revised to conform with journal; minor numerical
correction
Microscopic analysis of the chemical reaction between Fe(Te,Se) thin films and underlying CaF
To understand the chemical reaction at the interface of materials, we
performed a transmission electron microscopy (TEM) observation in four types of
Fe(Te,Se) superconducting thin films prepared on different types of substrates:
CaF2 substrate, CaF2 substrate with a CaF2 buffer layer, CaF2 substrate with a
FeSe buffer layer, and a LaAlO3 substrate with a CaF2 buffer layer. Based on
the energy-dispersive X-ray spectrometer (EDX) analysis, we found possible
interdiffusion between fluorine and selenium that has a strong influence on the
superconductivity in Fe(Te,Se) films. The chemical interdiffusion also plays a
significant role in the variation of the lattice parameters. The lattice
parameters of the Fe(Te,Se) thin films are primarily determined by the chemical
substitution of anions, and the lattice mismatch only plays a secondary role.Comment: 30 pages, 9 figur
A Comparative Study of the Parker Instability under Three Models of the Galactic Gravity
To examine how non-uniform nature of the Galactic gravity might affect length
and time scales of the Parker instability, we took three models of gravity,
uniform, linear and realistic ones. To make comparisons of the three gravity
models on a common basis, we first fixed the ratio of magnetic pressure to gas
pressure at = 0.25, that of cosmic-ray pressure at = 0.4, and
the rms velocity of interstellar clouds at = 6.4 km s, and then
adjusted parameters of the gravity models in such a way that the resulting
density scale heights for the three models may all have the same value of 160
pc. Performing linear stability analyses onto equilibrium states under the
three models with the typical ISM conditions, we calculate the maximum growth
rate and corresponding length scale for each of the gravity models. Under the
uniform gravity the Parker instability has the growth time of 1.2
years and the length scale of 1.6 kpc for symmetric mode. Under the realistic
gravity it grows in 1.8 years for both symmetric and
antisymmetric modes, and develops density condensations at intervals of 400 pc
for the symmetric mode and 200 pc for the antisymmetric one. A simple change of
the gravity model has thus reduced the growth time by almost an order of
magnitude and its length scale by factors of four to eight. These results
suggest that an onset of the Parker instability in the ISM may not necessarily
be confined to the regions of high and .Comment: Accepted for publication in ApJ, using aaspp4.sty, 18 text pages with
9 figure
Convergence to a self-similar solution in general relativistic gravitational collapse
We study the spherical collapse of a perfect fluid with an equation of state
by full general relativistic numerical simulations. For 0, it has been known that there exists a general relativistic counterpart
of the Larson-Penston self-similar Newtonian solution. The numerical
simulations strongly suggest that, in the neighborhood of the center, generic
collapse converges to this solution in an approach to a singularity and that
self-similar solutions other than this solution, including a ``critical
solution'' in the black hole critical behavior, are relevant only when the
parameters which parametrize initial data are fine-tuned. This result is
supported by a mode analysis on the pertinent self-similar solutions. Since a
naked singularity forms in the general relativistic Larson-Penston solution for
0, this will be the most serious known counterexample against
cosmic censorship. It also provides strong evidence for the self-similarity
hypothesis in general relativistic gravitational collapse. The direct
consequence is that critical phenomena will be observed in the collapse of
isothermal gas in Newton gravity, and the critical exponent will be
given by , though the order parameter cannot be the black
hole mass.Comment: 22 pages, 15 figures, accepted for publication in Physical Review D,
reference added, typos correcte
Temperature Dependence of the Magnetic Penetration Depth in the Vortex State of the Pyrochlore Superconductor, Cd2Re2O7
We report transverse field and zero field muon spin rotation studies of the
superconducting rhenium oxide pyrochlore, Cd2Re2O7. Transverse field
measurements (H=0.007 T) show line broadening below Tc, which is characteristic
of a vortex state, demonstrating conclusively the type-II nature of this
superconductor. The penetration depth is seen to level off below about 400 mK
(T/Tc~0.4), with a rather large value of lambda (T=0)~7500A. The temperature
independent behavior below ~ 400 mK is consistent with a nodeless
superconducting energy gap. Zero-field measurements indicate no static magnetic
fields developing below the transition temperature.Comment: 4 pages, 4 figures, REVTEX 4, submitted to PR
Sedimentation and Type I X-ray Bursts at Low Accretion Rates
Neutron stars, with their strong surface gravity, have interestingly short
timescales for the sedimentation of heavy elements. Motivated by observations
of Type I X-ray bursts from sources with extremely low persistent accretion
luminosities, L_X < 10^{36}\usp\ergspersecond (\simeq
0.01\ensuremath{L_{\mathrm{Edd}}}), we study how sedimentation affects the
distribution of isotopes and the ignition of H and He in the envelope of an
accreting neutron star. For local mass accretion rates \mdot \lesssim
10^{-2}\medd (for which the ignition of H is unstable), where \medd =
8.8\times 10^{4}\nsp\gpscps, the helium and CNO elements sediment out of the
accreted fuel before reaching a temperature where H would ignite. Using
one-zone calculations of the thermonuclear burning, we find a range of
accretion rates for which the unstable H ignition does not trigger unstable He
burning. This range depends on the emergent flux from reactions in the deep
neutron star crust; for F = 0.1\nsp\MeV(\dot{m}/\mb), the range is 3\times
10^{-3}\medd\lesssim\mdot\lesssim 10^{-2}\medd. We speculate that sources
accreting in this range will build up a massive He layer that later produces an
energetic and long X-ray burst. At mass accretion rates lower than this range,
we find that the H flash leads to a strong mixed H/He flash. Surprisingly, even
at accretion rates \mdot \gtrsim 0.1\medd, although the H and He do not
completely segregate, the H abundance at the base of the accumulated layer is
still reduced. While following the evolution of the X-ray burst is beyond the
scope of this introductory paper, we note that the reduced proton-to-seed ratio
favors the production of \iso{12}{C}--an important ingredient for subsequent
superbursts.Comment: 15 pages, 14 figures, submitted to ApJ, revised versio
- …