50,488 research outputs found
Fluidic hydrogen detector production prototype development
A hydrogen gas sensor that can replace catalytic combustion sensors used to detect leaks in the liquid hydrogen transfer systems at Kennedy Space Center was developed. A fluidic sensor concept, based on the principle that the frequency of a fluidic oscillator is proportional to the square root of the molecular weight of its operating fluid, was utilized. To minimize sensitivity to pressure and temperature fluctuations, and to make the sensor specific for hydrogen, two oscillators are used. One oscillator operates on sample gas containing hydrogen, while the other operates on sample gas with the hydrogen converted to steam. The conversion is accomplished with a small catalytic converter. The frequency difference is taken, and the hydrogen concentration computed with a simple digital processing circuit. The output from the sensor is an analog signal proportional to hydrogen content. The sensor is shown to be accurate and insensitive to severe environmental disturbances. It is also specific for hydrogen, even with large helium concentrations in the sample gas
Constraints on Dark Energy from Supernovae, Gamma Ray Bursts, Acoustic Oscillations, Nucleosynthesis and Large Scale Structure and the Hubble constant
The luminosity distance vs. redshift law is now measured using supernovae and
gamma ray bursts, and the angular size distance is measured at the surface of
last scattering by the CMB and at z = 0.35 by baryon acoustic oscillations. In
this paper this data is fit to models for the equation of state with w = -1, w
= const, and w(z) = w_0+w_a(1-a). The last model is poorly constrained by the
distance data, leading to unphysical solutions where the dark energy dominates
at early times unless the large scale structure and acoustic scale constraints
are modified to allow for early time dark energy effects. A flat LambdaCDM
model is consistent with all the data.Comment: 19 pages Latex with 8 Postscript figure files. A new reference and
constraint, w vs w' contour plots updated. Version accepted by the the Ap
Attraction of Acorn-Infesting \u3ci\u3eCydia Latiferreana\u3c/i\u3e (Lepidoptera: Tortricidae) to Pheromone-Baited Traps
Males of acorn-infesting Cydia latiferreana are attracted to an equilibrium mixture of the four isomers of 8, 10-dodecadien-l-ol acetate, the virgin female-produced pheromone. Trap height relative to the height of trees in which traps are placed seems to be a significant factor influencing moth catches at attractant-baited traps. In an oak woodlot and in an oak nursery, catches of male moths were greater in traps placed near the upper periphery of the canopy than at traps deployed at lower levels in the tree. Practical application of pheromone-baited traps in a forest situation will require further study on lure formulation and on trap deployment under forest conditions
The limits of shelf water south of Cape Cod, 1941 to 1972
Some 19,000 batbythermograms and 1,600 oceanographic stations in the region 39° to 41°N, 69° to 72° W have been examined for evidence of changes in the character and position of the shelf water/slope water boundary. Results show a) the boundary, identified by the 10° isotherm, intersects the bottom within 16 km of the 100-m curve about 80 percent of the time, with a seasonal progression from the south in the winter to north in the foll;..
Refined Properties of the HD 130322 Planetary System
Exoplanetary systems closest to the Sun, with the brightest host stars,
provide the most favorable opportunities for characterization studies of the
host star and their planet(s). The Transit Ephemeris Refinement and Monitoring
Survey uses both new radial velocity measurements and photometry in order to
greatly improve planetary orbit uncertainties and the fundamental properties of
the star, in this case HD 130322. The only companion, HD 130322b, orbits in a
relatively circular orbit, e = 0.029 every ~10.7 days. Radial velocity
measurements from multiple sources, including 12 unpublished from the Keck I
telescope, over the course of ~14 years have reduced the uncertainty in the
transit midpoint to ~2 hours. The transit probability for the b-companion is
4.7%, where M_p sin i = 1.15 M_J and a = 0.0925 AU. In this paper, we compile
photometric data from the T11 0.8m Automated Photoelectric Telescope at
Fairborn Observatory taken over ~14 years, including the constrained transit
window, which results in a dispositive null result for both full transit
exclusion of HD 130322b to a depth of 0.017 mag and grazing transit exclusion
to a depth of ~0.001 mag. Our analysis of the starspot activity via the
photometric data reveals a highly accurate stellar rotation period: 26.53
+/-0.70 days. In addition, the brightness of the host with respect to the
comparison stars is anti-correlated with the Ca II H and K indices, typical for
a young solar-type star.Comment: 9 pages, 4 figures, 4 tables, accepted to Ap
The Panther Mountain circular structure, a possible buried meteorite crater
Panther Mountain, located near Phoenicia, New York, is part of the Catskill Mountains, which form the eastern end of the Allegheny Plateau in New York. It is a circular mass defined physiographically by an anomalous circular drainage pattern produced by Esopus Creek and its tributary Woodland Creek. The circular valley that rings the mountain is fracture-controlled; where bedrock is exposed, it shows a joint density 5 to 10 times greater than that on either side of the valley. Where obscured by alluvial valley fill, the bedrock's low seismic velocity suggests that this anomalous fracturing is continuous in the bedrock underlying the rim valley. North-south and east-west gravity and magnetic profiles were made across the structure. Terrane-corrected, residual gravity profiles show an 18-mgal negative anomaly, and very steep gradients indicate a near-surface source. Several possible explanations of the gravity data were modeled. We conclude that the Panther Mountain circular structure is probably a buried meteorite crater that formed contemporaneously with marine or fluvial sedimentation during Silurian or Devonian time. An examination of drill core and cuttings in the region is underway to search for ejecta deposits and possible seismic and tsunami effects in the sedimentary section. Success would result in both dating the impact and furnishing a chronostratigraphic marker horizon
Revised Orbit and Transit Exclusion for HD 114762b
Transiting planets around bright stars have allowed the detailed follow-up
and characterization of exoplanets, such as the study of exoplanetary
atmospheres. The Transit Ephemeris Refinement and Monitoring Survey (TERMS) is
refining the orbits of the known exoplanets to confirm or rule out both transit
signatures and the presence of additional companions. Here we present results
for the companion orbiting HD 114762 in an eccentric 84 day orbit. Radial
velocity analysis performed on 19 years of Lick Observatory data constrain the
uncertainty in the predicted time of mid-transit to ~5 hours, which is less
than the predicted one-half day transit duration. We find no evidence of
additional companions in this system. New photometric observations with one of
our Automated Photoelectric Telescopes (APTs) at Fairborn Observatory taken
during a revised transit time for companion b, along with 23 years of nightly
automated observations, allow us to rule out on-time central transits to a
limit of ~0.001 mag. Early or late central transits are ruled out to a limit of
~0.002 mag, and transits with half the duration of a central transit are ruled
out to a limit of ~0.003 mag.Comment: 5 pages, 2 figures, accepted for publication in ApJ
Is pulsar B0656+14 a very nearby RRAT source?
The recently discovered RRAT sources are characterized by very bright radio
bursts which, while being periodically related, occur infrequently. We find
bursts with the same characteristics for the known pulsar B0656+14. These
bursts represent pulses from the bright end of an extended smooth pulse-energy
distribution and are shown to be unlike giant pulses, giant micropulses or the
pulses of normal pulsars. The extreme peak-fluxes of the brightest of these
pulses indicates that PSR B0656+14, were it not so near, could only have been
discovered as an RRAT source. Longer observations of the RRATs may reveal that
they, like PSR B0656+14, emit weaker emission in addition to the bursts.Comment: 4 pages, 4 figures, accepted by ApJ
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