8,335 research outputs found
Critical velocity for superfluid flow across the BEC-BCS crossover
Critical velocities have been observed in an ultracold superfluid Fermi gas
throughout the BEC-BCS crossover. A pronounced peak of the critical velocity at
unitarity demonstrates that superfluidity is most robust for resonant atomic
interactions. Critical velocities were determined from the abrupt onset of
dissipation when the velocity of a moving one dimensional optical lattice was
varied. The dependence of the critical velocity on lattice depth and on the
inhomogeneous density profile was studied
Coupled valence and spin state transition in (Pr0.7Sm0.3)0.7Ca0.3CoO3
The coupled valence and spin state transition (VSST) taking place in
(Pr0.7Sm0.3)0.7Ca0.3CoO3 was investigated by soft x-ray absorption spectroscopy
(XAS) experiments carried out at the Pr-M4,5, Co-L2,3, and O-1s edges. This
VSST is found to be composed of a sharp Pr/Co valence and Co spin state
transition centered at T*=89.3 K, followed by a smoother Co spin-state
evolution at higher temperatures. At T < T*, we found that the praseodymium
displays a mixed valence Pr3+/Pr4+ with about 0.13 Pr4+/f.u., while all the
Co3+ is in the low-spin (LS) state. At T around T*, the sharp valence
transition converts all the Pr4+ to Pr3+ with a corresponding Co3+ to Co4+
compensation. This is accompanied by an equally sharp spin state transition of
the Co3+ from the low to an incoherent mixture of low and high spin (HS)
states. An involvement of the intermediate spin (IS) state can be discarded for
the Co3+. While above T* and at high temperatures the system shares rather
similar properties as Sr-doped LaCoO3, at low temperatures it behaves much more
like EuCoO3 with its highly stable LS configuration for the Co3+. Apparently,
the mechanism responsible for the formation of Pr4+ at low temperatures also
helps to stabilize the Co3+ in the LS configuration despite the presence of
Co4+ ions. We also found out that that the Co4+ is in an IS state over the
entire temperature range investigated in this study (10-290 K). The presence of
Co3+ HS and Co4+ IS at elevated temperatures facilitates the conductivity of
the material.Comment: 19 pages, 7 figures, Accepted in PR
The detection of extragalactic N: Consequences for nitrogen nucleosynthesis and chemical evolution
Detections of extragalactic N are reported from observations of the
rare hydrogen cyanide isotope HCN toward the Large Magellanic Cloud
(LMC) and the core of the (post-) starburst galaxy NGC 4945. Accounting for
optical depth effects, the LMC data from the massive star-forming region N113
infer a N ratio of 111 17, about twice the C
value. For the LMC star-forming region N159HW and for the central region of NGC
4945, N ratios are also 100. The N ratios
are smaller than all interstellar nitrogen isotope ratios measured in the disk
and center of the Milky Way, strongly supporting the idea that N is
predominantly of `primary' nature, with massive stars being its dominant
source. Although this appears to be in contradiction with standard stellar
evolution and nucleosynthesis calculations, it supports recent findings of
abundant N production due to rotationally induced mixing of protons into
the helium-burning shells of massive stars.Comment: 15 pages including one postscript figure, accepted for publication by
ApJ Letter, further comments: please contact Yi-nan Chi
Analytical and experimental study of stratification and liquid-ullage coupling, 1 June 1964 - 31 May 1965
Closed-form solution for stratification of subcooled fluids in containers subjected to heating, and for liquid-ullage vapor couplin
The 6-vertex model of hydrogen-bonded crystals with bond defects
It is shown that the percolation model of hydrogen-bonded crystals, which is
a 6-vertex model with bond defects, is completely equivalent with an 8-vertex
model in an external electric field. Using this equivalence we solve exactly a
particular 6-vertex model with bond defects. The general solution for the
Bethe-like lattice is also analyzed.Comment: 13 pages, 6 figures; added references for section
Anharmonicity Induced Resonances for Ultracold Atoms and their Detection
When two atoms interact in the presence of an anharmonic potential, such as
an optical lattice, the center of mass motion cannot be separated from the
relative motion. In addition to generating a confinement-induced resonance (or
shifting the position of an existing Feshbach resonance), the external
potential changes the resonance picture qualitatively by introducing new
resonances where molecular excited center of mass states cross the scattering
threshold. We demonstrate the existence of these resonances, give their
quantitative characterization in an optical superlattice, and propose an
experimental scheme to detect them through controlled sweeping of the magnetic
field.Comment: 6 pages, 5 figures; expanded presentatio
Abundances and Isotope Ratios in the Magellanic Clouds: The Star Forming Environment of N113
With the goal of deriving the physical and chemical conditions of star
forming regions in the Large Magellanic Cloud (LMC), a spectral line survey of
the prominent star forming region N113 is presented. The observations cover
parts of the frequency range from 85 GHz to 357 GHz and include 63 molecular
transitions from a total of 16 species, among them spectra of rare
isotopologues. Maps of selected molecular lines as well as the 1.2 mm continuum
distribution are also presented. Molecular abundances in the core of the
complex are found to be consistent with a photon dominated region (PDR) that is
nitrogen deficient, with the potential exception of N2H+. Densities range from
5x10^3 cm-3 for CO to almost 10^6 for CS and HCN, indicating that only the
densest regions provide sufficient shielding even for some of the most common
species. An ortho- to para-H_2CO ratio of ~3 hints at H_2CO formation in a warm
(>=40 K) environment. Isotope ratios are 12C/13C ~ 49+-5, 16O/18O ~ 2000+-250,
18O/17O ~ 1.7+-0.2 and 32S/34S ~ 15. Agreement with data from other star
forming clouds shows that the gas is well mixed in the LMC . The isotope ratios
do not only differ from those seen in the Galaxy. They also do not form a
continuation of the trends observed with decreasing metallicity from the inner
to the outer Galaxy. This implies that the outer Galaxy, is not providing a
transition zone between the inner Galaxy and the metal poor environment of the
Magellanic Clouds. A part of this discrepancy is likely caused by differences
in the age of the stellar populations in the outer Galaxy and the LMC.Comment: 50 pages, 13 figures, accepted for publication in Ap
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