3,846 research outputs found
Epitaxial growth and the magnetic properties of orthorhombic YTiO3 thin films
High-quality YTiO3 thin films were grown on LaAlO3 (110) substrates at low
oxygen pressures (<10-8 Torr) using pulsed laser deposition. The in-plane
asymmetric atomic arrangements at the substrate surface allowed us to grow
epitaxial YTiO3 thin films, which have an orthorhombic crystal structure with
quite different a- and b-axes lattice constants. The YTiO3 film exhibited a
clear ferromagnetic transition at 30 K with a saturation magnetization of about
0.7 uB/Ti. The magnetic easy axis was found to be along the [1-10] direction of
the substrate, which differs from the single crystal easy axis direction, i.e.,
[001].Comment: 14 pages, 4 figure
A study of energy concentration and drain in incompressible fluids
In this paper we examine two opposite scenarios of energy behavior for
solutions of the Euler equation. We show that if is a regular solution on a
time interval and if for some , where is the dimension of the fluid, then the energy at the
time cannot concentrate on a set of Hausdorff dimension samller than . The same holds for solutions of the three-dimensional
Navier-Stokes equation in the range . Oppositely, if the energy
vanishes on a subregion of a fluid domain, it must vanish faster than
(T-t)^{1-\d}, for any \d>0. The results are applied to find new exclusions
of locally self-similar blow-up in cases not covered previously in the
literature.Comment: an update of the previous versio
The variation of relative magnetic helicity around major flares
We have investigated the variation of magnetic helicity over a span of
several days around the times of 11 X-class flares which occurred in seven
active regions (NOAA 9672, 10030, 10314, 10486, 10564, 10696, and 10720) using
the magnetograms taken by the Michelson Doppler Imager (MDI) on board the Solar
and Heliospheric Observatory (SOHO). As a major result we found that each of
these major flares was preceded by a significant helicity accumulation over a
long period (0.5 to a few days). Another finding is that the helicity
accumulates at a nearly constant rate and then becomes nearly constant before
the flares. This led us to distinguish the helicity variation into two phases:
a phase of monotonically increasing helicity and the following phase of
relatively constant helicity. As expected, the amount of helicity accumulated
shows a modest correlation with time-integrated soft X-ray flux during flares.
However, the average helicity change rate in the first phase shows even
stronger correlation with the time-integrated soft X-ray flux. We discuss the
physical implications of this result and the possibility that this
characteristic helicity variation pattern can be used as an early warning sign
for solar eruptions
Determination of Dynamic Shear Modulus of Soils from Static Strength
A correlation study between the dynamic shear modulus obtained from the resonant column technique and the static strength obtained from the undrained triaxial compression test is described. The materials studied were a uniform sand, a non-active fine silty clay and a highly-active bentonite clay treated with additives to increase the range for static and dynamic shear strength of the soils. It is noted that a linear relationship exists between the dynamic shear modulus, except for those soil specimens having very low strength, independent of test parameters. Using linear regression analysis, empirical equations for predicting the maximum dynamic shear modulus from the static strength have been obtained for the three different soils
Cosmological Parameters from the SDSS DR5 Velocity Dispersion Function of Early-Type Galaxies through Radio-Selected Lens Statistics
We improve strong lensing constraints on cosmological parameters in light of
the new measurement of the velocity dispersion function of early-type galaxies
based on the SDSS DR5 data and recent semi-analytical modeling of galaxy
formation. Using both the number statistics of the CLASS statistical sample and
the image separation distribution of the CLASS and the PANELS radio-selected
lenses, we find the cosmological matter density \Om = 0.25^{+0.12}_{-0.08}
(68% CL) assuming evolutions of galaxies predicted by a semi-analytical model
of galaxy formation and \Om = 0.26^{+0.12}_{-0.08} assuming no evolution of
galaxies for a flat cosmology with an Einstein cosmological constant. For a
flat cosmology with a generalized dark energy, we find the non-evolving dark
energy equation of state () at the 68% CL (95% CL).Comment: ApJL, accepted (results and presentations revised; conclusions
unchanged
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