565 research outputs found
Testimony of John J. Lawler Before the Commission on the Future of Worker-Management Relations
Testimony_Lawler_022494.pdf: 224 downloads, before Oct. 1, 2020
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Improved Co I Log(gf) Values and Abundance Determinations in the Photospheres of the Sun and Metal-Poor Star HD 84937
New emission branching fraction measurements for 898 lines of the first spectrum of cobalt (Co I) are determined from hollow cathode lamp spectra recorded with the National Solar Observatory 1 m Fourier transform spectrometer on Kitt Peak, AZ and a high-resolution echelle spectrometer. Published radiative lifetimes from laser induced fluorescence measurements are combined with the branching fractions to determine accurate absolute atomic transition probabilities for the 898 lines. Hyperfine structure (hfs) constants for levels of neutral Co in the literature are surveyed and selected values are used to generate complete hfs component patterns for 195 transitions of Co I. These new laboratory data are applied to determine the Co abundance in the Sun and metal-poor star HD 84937, yielding log epsilon(Co) = 4.955 +/- 0.007 (sigma = 0.059) based on 82 Co I lines and log epsilon(Co) = 2.785 +/- 0.008 (sigma = 0.065) based on 66 Co I lines, respectively. A Saha or ionization balance test on the photosphere of HD 84937 is performed using 16 UV lines of Co II, and good agreement is found with the Co I result in this metal-poor ([Fe I/H] = -2.32, [Fe II/H] = -2.32) dwarf star. The resulting value of [Co/Fe]= +0.14 supports a rise of Co/Fe at low metallicity that has been suggested in other studies.NASA NNX10AN93GNSF AST-1211055, AST-1211585McDonald Observator
Visible Minorities under the Canadian Employment Equity Act, 1987-1999
This study focuses on the effectiveness of the federal Employment Equity Act (EEA). We assess the EEA with regard to visible minority (VM) employees using quantitative data from employer reports published under the provisions of the EEA and the Canadian Census. Data in this study cover the period 1987 to 1999. We find that large companies, and larger employment groups within companies, have higher levels of employment equity attainment. There are also considerable variations in employment equity attainment across industrial sectors, across provinces and across occupations. Overall, there has been general improvement in employment equity (EE) attainment over time. However, visible minorities continue to be disadvantaged in management, sales and service and technical positions. Several policy implications are drawn from these findings.Cette Ă©tude s’intĂ©resse Ă l’efficacitĂ© de la lĂ©gislation sur l’équitĂ© en emploi. Nous Ă©valuons cette loi visant les travailleurs de la minoritĂ© visible en faisant appel Ă des donnĂ©es quantitatives qu’on retrouve dans les rapports des employeurs publiĂ©s en application des dispositions de la lĂ©gislation et Ă celles tirĂ©es du recensement canadien. Ces donnĂ©es couvrent la pĂ©riode 1987-1999.Notre Ă©tude porte sur la relation entre le degrĂ© d’atteinte de l’équitĂ© en emploi eu Ă©gard aux minoritĂ©s visibles sous la lĂ©gislation et une gamme de facteurs contextuels. On y prĂ©sente des conclusions importantes et nombreuses.En premier lieu, tel que prĂ©vu, les plus grandes entreprises et les groupes occupationnels les plus importants prĂ©sentent des niveaux plus Ă©levĂ©s d’atteinte de l’équitĂ© en emploi. On peut attribuer ce fait Ă la taille en relation avec la visibilitĂ© des organisations et Ă la disponibilitĂ© de ressources plus abondantes pour rencontrer des objectifs d’équitĂ©.En deuxième lieu, il y a beaucoup de variation entre les secteurs industriels en termes d’atteinte de l’équitĂ©; le secteur bancaire prĂ©sentant des niveaux les plus Ă©levĂ©s, ce que nous avions anticipĂ©. Encore lĂ , on peut attribuer cela Ă la visibilitĂ© des banques et au fait que le secteur bancaire ne prĂ©sente pas les mĂŞmes pressions concurrentielles qu’on observe dans les secteurs des communications et des transports. Alors les banques ont plutĂ´t des ressources en surplus qu’elles peuvent allouer au support des efforts exigĂ©s par la loi et peut-ĂŞtre qu’elles sont, Ă cause de leur taille, plus sensibles Ă la surveillance des organismes de rĂ©gulation.En troisième lieu, on observe Ă©galement une variation importante d’une province Ă une autre en termes de degrĂ© d’atteinte de l’équitĂ©, avec des niveaux, Ă notre grande surprise, remarquablement faibles dans les provinces oĂą on retrouve les plus fortes concentrations de minoritĂ©s visibles (par exemple, l’Ontario et la Colombie-Britannique). Il s’agit lĂ d’un rĂ©sultat que nous n’avions pas anticipĂ©. Peut-ĂŞtre cela est-il dĂ» au grand nombre d’immigrants rĂ©sidant dans ces provinces au cours des dernières annĂ©es, de sorte qu’on a pu constater la prĂ©sence d’un nombre disproportionnĂ© de personnes ayant des aptitudes limitĂ©es au plan du langage et au plan de la crĂ©ation de liens avec la communautĂ© plus large. Des groupes de minoritĂ©s visibles dans les autres provinces ont pu s’intĂ©grer Ă des communautĂ©s mieux Ă©tablies et ainsi obtenir un accès plus grand aux entreprises en vertu d’une assimilation plus prononcĂ©e. De plus, le nombre de minoritĂ©s visibles de ces provinces est tout Ă fait minime, de sorte que les entreprises n’ont eu qu’à faire des efforts limitĂ©s pour atteindre des niveaux respectables d’équitĂ©.En quatrième lieu, nos donnĂ©es indiquent une amĂ©lioration gĂ©nĂ©rale avec le temps au plan de l’atteinte des objectifs de la lĂ©gislation, qui serait concordante avec l’efficacitĂ© de cette mĂŞme lĂ©gislation.En cinquième lieu, il n’y a pas d’indication claire Ă l’effet que les minoritĂ©s visibles sont surreprĂ©sentĂ©es dans le marchĂ© du travail secondaire. Enfin, nous avons constatĂ© que le degrĂ© de rĂ©alisation des objectifs de la loi varie considĂ©rablement d’une occupation Ă une autre. Les minoritĂ©s visibles sont particulièrement dĂ©savantagĂ©es dans les positions de gĂ©rance, de professionnels et de reprĂ©sentants commerciaux, tout comme dans les emplois manuels spĂ©cialisĂ©s.Plusieurs implications tant d’ordre politique que pratique dĂ©coulent de ces observations, ce qui inclut une intervention accrue de la part de la Commission canadienne des droits de la personne, une plus grande prĂ©occupation Ă l’égard des iniquitĂ©s occupationnelles et des disparitĂ©s sectorielles, de la taille des entreprises et du groupe d’emploi :Este estudio se concentra sobre la eficacia del Acta de Equidad en el Empleo (AEE) de nivel federal. Nosotros evaluamos el AEE respecto a los empleados del grupo de minorĂas visibles (MV) utilizando los datos cuantitativos de los informes de empleados publicados segĂşn las disposiciones del AEE y el Censo Canadiense. Los datos de este estudio cubren el periodo 1987-1999. Nuestros resultados indican que las grandes compañĂas, y los grupos mas grandes de empleo al interior de las compañĂas, han alcanzado altos niveles de equidad. Hay tambiĂ©n variaciones considerables en la realizaciĂłn de la equidad de empleo a travĂ©s los sectores industriales, a travĂ©s las provincias y a travĂ©s las ocupaciones. En el conjunto, ha habido una mejora general en la realizaciĂłn de la equidad del empleo en este periodo. Sin embargo, las minorĂas visibles siguen siendo desfavorecidos en los puestos de gestion, de ventas y servicos y en las ocupaciones tecnicas. Varias implicaciones polĂticas son diseñadas a partir de estos resultados
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Improved Log(gf) Values for Lines of Ti I and Abundance Determinations in the Photospheres of the Sun and Metal-Poor Star HD 84937 (Accurate Transition Probabilities for Ti I)
New atomic transition probability measurements for 948 lines of Ti I are reported. Branching fractions from Fourier transform spectra and from spectra recorded using a 3 m echelle spectrometer are combined with published radiative lifetimes from laser-induced fluorescence measurements to determine these transition probabilities. Generally good agreement is found in comparisons to the NIST Atomic Spectra Database. The new Ti I data are applied to re-determine the Ti abundance in the photospheres of the Sun and metal-poor star HD 84937 using many lines covering a range of wavelength and excitation potential to explore possible non-local thermal equilibrium effects. The variation of relative Ti/Fe abundance with metallicity in metal-poor stars observed in earlier studies is supported in this study.NSF AST-1211055, AST-0908978, AST-1211585NSF REU grant AST-1004881ESO Science Archive Facility 073.D-0024, 266.D-5655NASA NAS 5-26555Astronom
Nucleosynthesis: Stellar and Solar Abundances and Atomic Data
Abundance observations indicate the presence of often surprisingly large
amounts of neutron capture (i.e., s- and r-process) elements in old Galactic
halo and globular cluster stars. These observations provide insight into the
nature of the earliest generations of stars in the Galaxy -- the progenitors of
the halo stars -- responsible for neutron-capture synthesis. Comparisons of
abundance trends can be used to understand the chemical evolution of the Galaxy
and the nature of heavy element nucleosynthesis. In addition age
determinations, based upon long-lived radioactive nuclei abundances, can now be
obtained. These stellar abundance determinations depend critically upon atomic
data. Improved laboratory transition probabilities have been recently obtained
for a number of elements. These new gf values have been used to greatly refine
the abundances of neutron-capture elemental abundances in the solar photosphere
and in very metal-poor Galactic halo stars. The newly determined stellar
abundances are surprisingly consistent with a (relative) Solar System r-process
pattern, and are also consistent with abundance predictions expected from such
neutron-capture nucleosynthesis.Comment: 8 pages, 2 figures, 1 table. To appear in the Proceedings of the NASA
Laboratory Astrophysics Workshop in Las Vegas, NV (February 2006
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Improved V I Log(gf) Values and Abundance Determinations in the Photospheres of the Sun and Metal-Poor Star HD 84937
New emission branching fraction measurements for 836 lines of the first spectrum of vanadium (V I) are determined from hollow cathode lamp spectra recorded with the National Solar Observatory 1 m Fourier transform spectrometer (FTS) and a high-resolution echelle spectrometer. The branching fractions are combined with recently published radiative lifetimes from laser-induced fluorescence measurements to determine accurate absolute atomic transition probabilities for the 836 lines. The FTS data are also used to extract new hyperfine structure A coefficients for 26 levels of neutral vanadium. These new laboratory data are applied to determine the V abundance in the Sun and metal-poor star HD 84937, yielding log epsilon(V) = 3.956 +/- 0.004 (sigma = 0.037) based on 93 V I lines and log epsilon(V) = 1.89 +/- 0.03 (sigma = 0.07) based on nine Vi lines, respectively, using the Holweger-Muller 1D model. These new V I abundance values for the Sun and HD 84937 agree well with our earlier determinations based upon V II.NASA NNX10AN93GNSF AST-1211055, AST-1211585Astronom
Europium, Samarium, and Neodymium Isotopic Fractions in Metal-Poor Stars
We have derived isotopic fractions of europium, samarium, and neodymium in
two metal-poor giants with differing neutron-capture nucleosynthetic histories.
These isotopic fractions were measured from new high resolution (R ~ 120,000),
high signal-to-noise (S/N ~ 160-1000) spectra obtained with the 2dCoude
spectrograph of McDonald Observatory's 2.7m Smith telescope. Synthetic spectra
were generated using recent high-precision laboratory measurements of hyperfine
and isotopic subcomponents of several transitions of these elements and matched
quantitatively to the observed spectra. We interpret our isotopic fractions by
the nucleosynthesis predictions of the stellar model, which reproduces
s-process nucleosynthesis from the physical conditions expected in low-mass,
thermally-pulsing stars on the AGB, and the classical method, which
approximates s-process nucleosynthesis by a steady neutron flux impinging upon
Fe-peak seed nuclei. Our Eu isotopic fraction in HD 175305 is consistent with
an r-process origin by the classical method and is consistent with either an r-
or an s-process origin by the stellar model. Our Sm isotopic fraction in HD
175305 suggests a predominantly r-process origin, and our Sm isotopic fraction
in HD 196944 is consistent with an s-process origin. The Nd isotopic fractions,
while consistent with either r-process or s-process origins, have very little
ability to distinguish between any physical values for the isotopic fraction in
either star. This study for the first time extends the n-capture origin of
multiple rare earths in metal-poor stars from elemental abundances to the
isotopic level, strengthening the r-process interpretation for HD 175305 and
the s-process interpretation for HD196944.Comment: 40 pages, 16 figures. Accepted for publication in ApJ. Full versions
of tables 4 and 5 are available from the first author upon reques
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