31,497 research outputs found
High Reynolds number tests of a NASA SC(3)-0712(B) airfoil in the Langley 0.3-meter transonic cryogenic tunnel
A wind tunnel investigation of a NASA 12-percent-thick, advanced-technology supercritical airfoil was conducted in the Langley 0.3-Meter Transonic Cryogenic Tunnel (TCT). This investigation represents another in the series of NASA/U.S. industry two-dimensional airfoil studies to be completed in the Advanced Technology Airfoil Tests program. Test temperature was varied from 220 K to 96 K at pressures ranging from 1.2 to 4.3 atm. Mach number was varied from 0.60 to 0.80. These variables provided a Reynolds number range from 4,400,000 to 40,000,000 based on a 15.24-cm (6.0-in.) airfoil chord. This investigation was designed to test a NASA advanced-technology airfoil from low to flight-equivalent Reynolds numbers, provide experience in cryogenic wind tunnel model design and testing techniques, and demonstrate the suitability of the 0.3-m TCT as an airfoil test facility. The aerodynamic results are presented as integrated force and moment coefficients and pressure distributions. Data are included which demonstrate the effects of fixed transition, Mach number, and Reynolds number on the aerodynamic characteristics. Also included are remarks on the model design, the model structural integrity, and the overall test experience
Pressure distribution from high Reynolds number tests of a NASA SC(3)-0712(B) airfoil in the Langley 0.3-meter transonic cryogenic tunnel
A wind tunnel investigation of a NASA 12-percent-thick, advanced-technology supercritical airfoil was conducted in the Langley 0.3-Meter Transonic Cryogenic Tunnel (TCT). This investigation represents another in the series of NASA/U.S. industry two-dimensional airfoil studies to be completed in the Advanced Technology Airfoil Tests program. Test temperature was varied from 220 K to 96 K at pressures ranging from 1.2 to 4.3 atm. Mach number was varied from 0.50 to 0.80. This investigation was designed to: (1) test a NASA advanced-technology airfoil from low to flight equivalent Reynolds numbers, (2) provide experience in cryogenic wind-tunnel model design and testing techniques, and (3) demonstrate the suitability of the 0.3-m TCT as an airfoil test facility. All the test objectives were met. The pressure data are presented without analysis in tabulated format and as plots of pressure coefficient versus position on the airfoil. This report was prepared for use in conjunction with the aerodynamic coefficient data published in NASA-TM-86371. Data are included which demonstrate the effects of fixed transition. Also included are remarks on the model design and fabrication
Li-rich RGB stars in the Galactic Bulge
We present Lithium abundance determination for a sample of K giant stars in
the galactic bulge. The stars presented here are the only 13 stars with
detectable Lithium line (6767.18 A) among ~400 stars for which we have spectra
in this wavelength range, half of them in Baade's Window (b=-4) and half in a
field at b=-6. The stars were observed with the GIRAFFE spectrograph of
FLAMES@VLT, with a spectral resolution of R~20,000. Abundances were derived via
spectral synthesis and the results are compared with those for stars with
similar parameters, but no detectable Li line. We find 13 stars with a
detectable Li line, among which 2 have abundances A(Li)>2.7. No clear
correlations were found between the Li abundance and those of other elements.
With the exception of the two most Li rich stars, the others follow a fairly
tight A(Li)-T_eff correlation. It would seems that there must be a Li
production phase during the red giant branch (RGB), acting either on a very
short timescale, or selectively only in some stars. The proposed Li production
phase associated with the RGB bump cannot be excluded, although our targets are
significantly brighter than the predicted RGB bump magnitude for a population
at 8 kpcComment: 8 pages, 9 figures, accepted for publication in A&
Electrodynamics of quasi-two-dimensional BEDT-TTF charge transfer salts
We consider the millimeter-wave electrodynamics specific to
quasi-two-dimensional conductors and superconductors based on the organic donor
molecule BEDT-TTF. Using realistic physical parameters, we examine the current
polarizations that result for different oscillating (GHz) electric and magnetic
field polarizations. We show that, in general, it is possible to discriminate
between effects (dissipation and dispersion) due to in-plane and interlayer ac
currents. However, we also show that it is not possible to selectively probe
any single component of the in-plane conductivity tensor, and that excitation
of interlayer currents is strongly influenced by the sample geometry and the
electromagnetic field polarization.Comment: 5 pages including 3 figures Minor correction to figure
The Calcium Triplet metallicity calibration for galactic bulge stars
We present a new calibration of the Calcium II Triplet equivalent widths
versus [Fe/H], constructed upon K giant stars in the Galactic bulge. This
calibration will be used to derive iron abundances for the targets of the GIBS
survey, and in general it is especially suited for solar and supersolar
metallicity giants, typical of external massive galaxies. About 150 bulge K
giants were observed with the GIRAFFE spectrograph at VLT, both at resolution
R~20,000 and at R~6,000. In the first case, the spectra allowed us to perform
direct determination of Fe abundances from several unblended Fe lines, deriving
what we call here high resolution [Fe/H] measurements. The low resolution
spectra allowed us to measure equivalent widths of the two strongest lines of
the near infrared Calcium II triplet at 8542 and 8662 A. By comparing the two
measurements we derived a relation between Calcium equivalent widths and [Fe/H]
that is linear over the metallicity range probed here, -1<[Fe/H]<+0.7. By
adding a small second order correction, based on literature globular cluster
data, we derived the unique calibration equation [Fe/H], with a rms dispersion of 0.197 dex, valid across the
whole metallicity range -2.3<[Fe/H]<+0.7.Comment: Accepted for publication in A&
Sexual Attraction Toward Clients, Use of Supervision, and Prior Training: A Qualitative Study of Predoctoral Psychology Interns
Interviews were conducted with 13 predoctoral psychology interns about an experience of sexual attraction toward a client, use of supervision to address the sexual attraction, and prior training regarding sexual attraction. Results indicated that sexual attraction to clients consisted of physical and interpersonal aspects. Therapists believed they were more invested and attentive than usual to clients to whom they were sexually attracted, and they indicated that sexual attraction created distance, distraction, and loss of objectivity. In terms of supervision, only half of the participants disclosed their sexual attraction to supervisors, and supervisors seldom initiated the discussion. Furthermore, trainees found it helpful when supervisors normalized the sexual attraction and provided the opportunity to explore feelings in supervision. Finally, trainees believed their training programs did not adequately address therapist sexual attraction
Length Scales of Acceleration for Locally Isotropic Turbulence
Length scales are determined that govern the behavior at small separations of
the correlations of fluid-particle acceleration, viscous force, and pressure
gradient. The length scales and an associated universal constant are quantified
on the basis of published data. The length scale governing pressure spectra at
high wave numbers is discussed. Fluid-particle acceleration correlation is
governed by two length scales; one arises from the pressure gradient, the other
from the viscous force.Comment: 2 figures, 4 pages. Physical Review Letters, accepted August 200
Cyclotron Resonance in the Layered Perovskite Superconductor Sr2RuO4
We have measured the cyclotron masses in Sr2RuO4 through the observation of
periodic-orbit-resonances - a magnetic resonance technique closely related to
cyclotron resonance. We obtain values for the alpha, beta and gamma Fermi
surfaces of (4.33+/-0.05)me, (5.81+/-0.03)me and (9.71+/-0.11)me respectively.
The appreciable differences between these results and those obtained from de
Haas- van Alphen measurements are attributable to strong electron-electron
interactions in this system. Our findings appear to be consistent with
predictions for a strongly interacting Fermi liquid; indeed, semi-quantitative
agreement is obtained for the electron pockets beta and gamma.Comment: 4 pages + 3 figure
The Giraffe Inner Bulge Survey (GIBS) II. Metallicity distributions and alpha element abundances at fixed Galactic latitude
High resolution (R22,500) spectra for 400 red clump giants, in four
fields within and , were obtained within the GIRAFFE
Inner Bulge Survey (GIBS) project. To this sample we added another 400
stars in Baade's Window, observed with the identical instrumental
configuration. We constructed the metallicity distributions for the entire
sample, as well as for each field individually, in order to investigate the
presence of gradients or field-to-field variations in the shape of the
distributions. The metallicity distributions in the five fields are consistent
with being drawn from a single parent population, indicating the absence of a
gradient along the major axis of the Galactic bar. The global metallicity
distribution is well fitted by two Gaussians. The metal poor component is
rather broad, with a mean at dex and dex.
The metal-rich one is narrower, with mean and
dex. The [Mg/Fe] ratio follows a tight trend with [Fe/H], with enhancement with
respect to solar in the metal-poor regime, similar to the one observed for
giant stars in the local thick disc. [Ca/Fe] abundances follow a similar trend,
but with a considerably larger scatter than [Mg/Fe]. A decrease in [Mg/Fe] is
observed at dex. This \textit{knee} is in agreement with our
previous bulge study of K-giants along the minor axis, but is 0.1 dex lower in
metallicity than the one reported for the Bulge micro lensed dwarf and
sub-giant stars. We found no variation in -element abundance
distributions between different fields.Comment: Accepted for publication in A&
X-ray Doppler Imaging of 44i Boo with Chandra
Chandra High-Energy Transmission Grating observations of the bright eclipsing
contact binary 44i Boo show X-ray line profiles which are Doppler-shifted by
orbital motions. The X-ray emission spectrum contains a multitude of lines
superimposed on a weak continuum, with strong lines of O VIII, Ne X, Fe XVII,
and Mg XII. The profiles of these lines from the total observed spectrum show
Doppler-broadened widths of ~ 550 km s^{-1}. Line centroids vary with orbital
phase, indicating velocity changes of > 180 km s^{-1}. The first-order light
curve shows significant variability, but no clear evidence for either primary
or secondary eclipses. Flares are observed for all spectral ranges;
additionally, the light curve constructed near the peak of the emission measure
distribution (T_e = 5 to 8 X 10^6 K) shows quiescent variability as well as
flares. The phase-dependences of line profiles and light curves together imply
that at least half of the emission is localized at high latitude. A simple
model with two regions on the primary star at relatively high latitude
reproduces the observed line profile shifts and quiescent light curve. These
first clear X-ray Doppler shifts of stellar coronal material illustrate the
power of Chandra.Comment: 15 pages, 6 figures to be published in Astrophysical Journal Letter
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