2,001 research outputs found

    Social studies references in six Rhode Island high schools

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    Thesis (Ed.M.)--Boston Universit

    Circuit Court Interpretations of Garcetti v. Ceballos and the Development of Public Employee Speech

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    The article presents an analysis on the advancement of public employee speech and interpretations of the U.S. Supreme Court on Garcetti v. Ceballos. It discusses the similarities and error that exists among the federal circuit courts. It overviews the factors shared by circuits different to certain courts. It reflects on the First Amendment jurisprudence related to public employee speech. It also put forwards the defenses and criticisms of Garcetti

    Exchange Reactions of the Transuranium Elements Section 1. Am(III)-Am(V)-Am(VI), Am(III)-Am(V), and Am(V)-Am(VI)

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    No exchange work prior to this dissertation has been reported on the Americium system. Neptunium exchange is presently being studied by J. C. Hindman and co-workers at the Argonne National Laboratory, but has not been completely reported. Study of uranium exchange, which is still in an unsatisfactory state, has been limited to the U(IV)-(VI) exchange

    The European War and Potash Supplies

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    SMOKE POINTS OF MICROGRAVITY AND NORMAL GRAVITY COFLOW DIFFUSION FLAMES

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    Smoke points were measured in microgravity aboard the International Space Station (ISS) as part of the Smoke Points in Coflow Experiment (SPICE), and in normal gravity conditions. In microgravity conditions increasing the coflow velocity or decreasing the burner diameter increased the smoke point flame length. A simplified prediction of centerline jet velocity did not yield residence-time-based criticalities or data collapse. Simulation of non-reacting flows showed that the simplified centerline velocity prediction was able to predict velocity decay for only relatively weak coflows. An improved model may yield different results. In normal earth gravity coflow velocity exhibited mixed effects. For burner diameters of 0.41, 0.76, and 1.6 mm, smoke points increased with increases of coflow velocity. For an unconfined coflow burner with a burner diameter of 13.7 mm smoke point length decreased with increasing coflow velocity for ethylene and propylene, while increasing for propane flames

    The Chelation of Praseodymium as a Function of pH Using Thenolytrifluoroacetone

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    The rare earth elements, including elements 57 through 71, provide many diverse series of studies through their chemical reactions. In as much as these elements are all in Group III of the periodic table, they are markedly similar in their properties. The separation, insulation and purification of the various rare earths from one another has long been a problem of great interest to the chemist

    Fe XIII emission lines in active region spectra obtained with the Solar Extreme-Ultraviolet Research Telescope and Spectrograph

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    Recent fully relativistic calculations of radiative rates and electron impact excitation cross sections for Fe {\sc xiii} are used to generate emission-line ratios involving 3s2^{2}3p2^{2}--3s3p3^{3} and 3s2^{2}3p2^{2}--3s2^{2}3p3d transitions in the 170--225 \AA and 235--450 \AA wavelength ranges covered by the Solar Extreme-Ultraviolet Research Telescope and Spectrograph (SERTS). A comparison of these line ratios with SERTS active region observations from rocket flights in 1989 and 1995 reveals generally very good agreement between theory and experiment. Several new Fe {\sc xiii} emission features are identified, at wavelengths of 203.79, 259.94, 288.56 and 290.81 \AA. However, major discrepancies between theory and observation remain for several Fe {\sc xiii} transitions, as previously found by Landi (2002) and others, which cannot be explained by blending. Errors in the adopted atomic data appear to be the most likely explanation, in particular for transitions which have 3s2^{2}3p3d 1^{1}D2_{2} as their upper level. The most useful Fe {\sc xiii} electron density diagnostics in the SERTS spectral regions are assessed, in terms of the line pairs involved being (i) apparently free of atomic physics problems and blends, (ii) close in wavelength to reduce the effects of possible errors in the instrumental intensity calibration, and (iii) very sensitive to changes in Ne_{e} over the range 108^{8}--1011^{11} cm‚ąí3^{-3}. It is concluded that the ratios which best satisfy these conditions are 200.03/202.04 and 203.17/202.04 for the 170--225 \AA wavelength region, and 348.18/320.80, 348.18/368.16, 359.64/348.18 and 359.83/368.16 for 235--450 \AA.Comment: 11 pages, 8 figures, 10 tables, MNRAS, in pres

    An Offense- Severity Model for Stop-and-Frisks

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    Emission lines of Fe XI in the 257--407 A wavelength region observed in solar spectra from EIS/Hinode and SERTS

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    Theoretical emission-line ratios involving Fe XI transitions in the 257-407 A wavelength range are derived using fully relativistic calculations of radiative rates and electron impact excitation cross sections. These are subsequently compared with both long wavelength channel Extreme-Ultraviolet Imaging Spectrometer (EIS) spectra from the Hinode satellite (covering 245-291 A), and first-order observations (235-449 A) obtained by the Solar Extreme-ultraviolet Research Telescope and Spectrograph (SERTS). The 266.39, 266.60 and 276.36 A lines of Fe XI are detected in two EIS spectra, confirming earlier identifications of these features, and 276.36 A is found to provide an electron density diagnostic when ratioed against the 257.55 A transition. Agreement between theory and observation is found to be generally good for the SERTS data sets, with discrepancies normally being due to known line blends, while the 257.55 A feature is detected for the first time in SERTS spectra. The most useful Fe XI electron density diagnostic is found to be the 308.54/352.67 intensity ratio, which varies by a factor of 8.4 between N_e = 10^8 and 10^11 cm^-3, while showing little temperature sensitivity. However, the 349.04/352.67 ratio potentially provides a superior diagnostic, as it involves lines which are closer in wavelength, and varies by a factor of 14.7 between N_e = 10^8 and 10^11 cm^-3. Unfortunately, the 349.04 A line is relatively weak, and also blended with the second-order Fe X 174.52 A feature, unless the first-order instrument response is enhanced.Comment: 9 pages, 5 figures, 13 tables; MNRAS in pres
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