1,580 research outputs found

    The motor fitness of primary school boys and girls

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    The purpose of this study was to assess the motor fitness level of boys and girls in the lower elementary grades and to differentiate the motor fitness level of boys and girls placed in a pre-first class with boys and girls placed in a regular first grade. [This is an excerpt from the abstract. For the complete abstract, please see the document.

    The Resuspension of Flocculent Solids in Sedimentation Basins

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    The phenomenon of resuspension has been considered to be an important factor in the imperfect behavior of sedimentation basins receiving suspensions containing flocculent solids. Resuspension is the entrainment into the flow of particles that have once settled to the floor of the basin. This investigation has been undertaken to study the resuspension phenomenon and to find ways in which its harmful effects can be reduced. Resuspension has been found extremely difficult to isolate and define scientifically because many other factors produce the same overall effect upon the settling tank. Furthermore it is practically necessary to identify individual particles in order to know whether a particular one found in suspension in the downstream portion of a settling tank had earlier been settled out and resting on the floor. Laboratory studies on settling tank behavior were conducted on a glass-walled "scour flume" 1.27 ft wide by 14 ft long with depth adjustable from 0.5 to 2.0 ft (see Fig. 1.1). In order to simulate certain aspects of the behavior of full-scale settling tanks the laboratory flume was fitted with moving flight scrapers similar to those installed in primary sewage settling tanks. For some of the later tests the flume was fitted with 14 probes that made it possible to sample the tank contents at practically any point of five cross sections along the length of the flume. Most of the studies on the laboratory flume utilized a discrete suspension of gilsonite {s. g. 1.04) particles or a flocculent suspension of ferric chloride and bentonite clay particles. Tests for critical velocity required for entrainment of particles from a smooth bed showed that fine light particles are more easily lifted from the bed than was previously supposed. With scrapers moving upstream, the critical velocity for two sizes of gilsonite tested was found to vary between 10.5 and 14.5 times the particle settling velocity. Field and laboratory studies on one scheme proposed to improve the performance of settling tanks - a series of transverse sloping baffles installed throughout the main body of a rectangular settling tank - both indicate that baffling a tank is not the answer. Tests on full-scale settling tanks of a sewage treatment plant showed that conventional measures of settling tank performance are meaningless when the suspension entering the tank is flocculent (as is sewage). Newer measures of performance are proposed, which show promise in evaluating the behavior of settling tanks receiving flocculent suspensions

    Experimentally Observed Instability of a Laminar Ekman Flow in a Rotating Basin

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    In studying the axi-symmetric flow induced by source-sink distributions in a rotating cylindrical basin in the absence of radial barriers, a highly organized pattern of instability has been observed in the laminar Ekman layer along the bottom of the basin. The instability manifests itself in the form of almost perfectly concentric cylindrical sheets or curtains of water which rise as sharply defined vertical jets from the Ekman layer and penetrate the entire depth of fluid. A less sharply defined downward motion between the curtains completes the circulation celis thus developed. At some maximum critical radius, the curtains usually disappear, and the flow at larger radii is a stable, laminar Ekman flow. Quantitative observations of ring spacing and critical radius are reported for experiments in which angular velocity, flow rate, viscosity and total depth of water were varied over experimentally available ranges

    The Mars observer camera

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    A camera designed to operate under the extreme constraints of the Mars Observer Mission was selected by NASA in April, 1986. Contingent upon final confirmation in mid-November, the Mars Observer Camera (MOC) will begin acquiring images of the surface and atmosphere of Mars in September-October 1991. The MOC incorporates both a wide angle system for low resolution global monitoring and intermediate resolution regional targeting, and a narrow angle system for high resolution selective surveys. Camera electronics provide control of image clocking and on-board, internal editing and buffering to match whatever spacecraft data system capabilities are allocated to the experiment. The objectives of the MOC experiment follow

    Sam Black gets a shot at Br\u27er Rabbit .

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    Color Black Americana stereographs. Set of 3. Features a black boy hunting with his dad. Entitled Sam Black gets a shot \u27Br\u27er Rabbit\u27, Lordy, Dad! Be Yous Kilt. and Oh! Golly, But Dat Ol\u27 Gun Done Kick .https://stars.library.ucf.edu/carolmundy-text/1008/thumbnail.jp

    Exploring Planets with Directed Aerial Robot Explorers

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    Global Aerospace Corporation (GAC) is developing a revolutionary system architecture for exploration of planetary atmospheres and surfaces from atmospheric altitudes. The work is supported by the NASA Institute for Advanced Concepts (NIAC). The innovative system architecture relies upon the use of Directed Aerial Robot Explorers (DAREs), which essentially are long-duration-flight autonomous balloons with trajectory control capabilities that can deploy swarms of miniature probes over multiple target areas. Balloon guidance capabilities will offer unprecedented opportunities in high-resolution, targeted observations of both atmospheric and surface phenomena. Multifunctional microprobes will be deployed from the balloons once over the target areas, and perform a multitude of functions, such as atmospheric profiling or surface exploration, relaying data back to the balloons or an orbiter. This architecture will enable low-cost, low-energy, long-term global exploration of planetary atmospheres and surfaces. This paper focuses on a conceptual analysis of the DARE architecture capabilities and science applications for Venus, Titan and Jupiter. Preliminary simulations with simplified atmospheric models show that a relatively small trajectory control wing can enable global coverage of the atmospheres of Venus and Titan by a single balloon over a 100-day mission. This presents unique opportunities for global in situ sampling of the atmospheric composition and dynamics, atmospheric profiling over multiple sites with small dropsondes and targeted deployment of surface microprobes. At Jupiter, path guidance capabilities of the DARE platforms permits targeting localized regions of interest, such as "hot spots" or the Great Red Spot. A single DARE platform at Jupiter can sample major types of the atmospheric flows (zones and belts) over a 100-day mission. Observations by deployable probes would reveal if the differences exist in radiative, dynamic and compositional environments at these sites

    One-pot silyl ketene acetal-formation-Mukaiyama–Mannich additions to imines mediated by trimethylsilyl trifluoromethanesulfonate

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    In the presence of trimethylsilyl trifluoromethanesulfonate and trialkylamine base, thioesters are readily converted to silyl ketene acetals in situ and undergo Mukaiyama–Mannich addition to N-phenylimines in one pot. The silyl triflates appears to play two roles, activating both the thioester and the imine. This process also works well when thioesters are replaced with amides, esters, or ketones. Products are isolated as desilylated anilines without the necessity of a deprotection step. Yields range from 65-99%

    Evolution of "51Peg b-like" Planets

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    About one-quarter of the extrasolar giant planets discovered so far have orbital distances smaller than 0.1 AU. These ``51Peg b-like'' planets can now be directly characterized, as shown by the planet transiting in front the star HD209458. We review the processes that affect their evolution. We apply our work to the case of HD209458b, whose radius has been recently measured. We argue that its radius can be reproduced only when the deep atmosphere is assumed to be unrealistically hot. When using more realistic atmospheric temperatures, an energy source appears to be missing in order to explain HD209458b's large size. The most likely source of energy available is not in the planet's spin or orbit, but in the intense radiation received from the parent star. We show that the radius of HD209458b can be reproduced if a small fraction (~1%) of the stellar flux is transformed into kinetic energy in the planetary atmosphere and subsequently converted to thermal energy by dynamical processes at pressures of tens of bars.Comment: 11 pages including 9 figures. A&A, in press. Also available at http://www.obs-nice.fr/guillot/pegasi-planets
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