Personality and the effort-reward imbalance model of stress : individual differences in reward sensitivity

The Effort-Reward Imbalance (ERI) model comprises both situational components (i.e. effort and reward) and a person-specific component (overcommitment). The aims of this study were to investigate the role of theoretically and historically linked personality variables (i.e. overcommitment and Type A personality) within the ERI model and to expand and extend the ERI model by investigating the contribution of individual reward components to both psychological (i.e. psychological distress) and attitudinal (i.e. affective commitment) employee strain indicators. A total of 897 police officers from a large Australian police agency participated in the study. The results provided no evidence of an interaction effect of effort or reward with overcommitment. The Type A variables did, however, make significant contributions and were involved in a number of interactions, suggesting that the person-specific component of the ERI model could be extended with the Type A personality profile. The findings also suggest that the esteem component of reward has the greatest relevance to employee outcomes, although tangible aspects of reward are more likely to act as a buffer of perceived work demand.

Cinética da enzima alfa-galactosidase a e investigação de doença de fabry em pacientes hemodialisados

A Alfa-galactosidase A (α-Gal A) humana é uma enzima lisossômica que quando deficiente causa a doença de Fabry. A doença de Fabry é uma esfingolipidose cuja principal causa de morbi-mortalidade é a insuficiência renal crônica (IRC). O objetivo deste estudo foi a implantação de um protocolo laboratorial que permita o diagnóstico da doença de Fabry em plasma e leucócitos, além da análise das características cinéticas da enzima α-Gal A em plasma e busca ativa da doença em 25 indivíduos com IRC de causa desconhecida. Também foram avaliadas a reprodutibilidade e a estabilidade do método enzimático. A padronização dos ensaios foi realizada com o substrato fluorescente 4-metilumbeliferil-α-Dgalactopiranosídeo. A reprodutibilidade foi avaliada utilizando amostras de plasma aliquotadas a 4ºC, -20ºC e -70ºC, analisadas uma vez ao mês por 6 meses e a estabilidade da fluorescência por até 24 horas após o término do ensaio enzimático. A padronização permitiu a implantação de valores de referência da α-Gal A para o estado do Pará, de 4 a 28 nmoles/h/mL (plasma) e de 20 a 96 nmoles/h/mg proteína (leucócitos). A enzima α-Gal A se mostrou termolábil, visto que com apenas 1 minuto de pré-incubação das amostras a 60ºC, sua atividade decaiu 71,09%. Com relação ao tempo de incubação, a atividade enzimática apresentou uma disposição linear crescente entre 15 a 180 minutos de incubação. A α-Gal A apresentou maior atividade no pH 4,8, o Km encontrado para a α-Gal A foi de 1,007 mM e a Vmáx foi 30,9 nmoles/h/mL. A melhor temperatura de armazenamento de plasma até o ensaio enzimático é -20ºC, onde foi observada menor variação em um período máximo de 6 meses. O método enzimático utilizado é estável, mesmo após 24 horas do término do ensaio, em temperatura ambiente. Com relação aos pacientes com IRC de causa desconhecida, todos apresentaram valor de atividade da α-Gal A dentro dos parâmetros de referência e, portanto, nenhum foi diagnosticado com doença de Fabry. O entendimento da cinética da α-Gal A e do seu comportamento in vitro possibilita um melhor diagnóstico laboratorial da doença de Fabry gerando dados para futuras comparações com indivíduos afetados por mutações nesta enzima

Kinematic distances of pre-main-sequence stars in the Lupus star-forming region

To reliably determine the main physical parameters (masses and ages) of young stars, we must know their distances. While the average distance to nearby star-forming regions (<300 pc) is often known, the distances to individual stars are usually unknown. Individual distances to members of young moving groups can be derived from their radial velocities and proper motions using the convergent-point strategy. We investigate the kinematic properties of the Lupus moving group with the primary objective of deriving individual distances to all group members.

The Gaia-ESO Survey: The analysis of high-resolution UVES spectra of FGK-type stars

Context. The ongoing Gaia-ESO Public Spectroscopic Survey is using FLAMES at the VLT to obtain high-quality medium-resolution Giraffe spectra for about 105 stars and high-resolution UVES spectra for about 5000 stars. With UVES, the Survey has already observed 1447 FGK-type stars. Aims. These UVES spectra are analyzed in parallel by several state-of-the-art methodologies. Our aim is to present how these analyses were implemented, to discuss their results, and to describe how a final recommended parameter scale is defined. We also discuss the precision (method-to-method dispersion) and accuracy (biases with respect to the reference values) of the final parameters. These results are part of the Gaia-ESO second internal release and will be part of its first public release of advanced data products. Methods. The final parameter scale is tied to the scale defined by the Gaia benchmark stars, a set of stars with fundamental atmospheric parameters. In addition, a set of open and globular clusters is used to evaluate the physical soundness of the results. Each of the implemented methodologies is judged against the benchmark stars to define weights in three different regions of the parameter space. The final recommended results are the weighted medians of those from the individual methods. Results. The recommended results successfully reproduce the atmospheric parameters of the benchmark stars and the expected Teff-log  g relation of the calibrating clusters. Atmospheric parameters and abundances have been determined for 1301 FGK-type stars observed with UVES. The median of the method-to-method dispersion of the atmospheric parameters is 55 K for Teff, 0.13 dex for log  g and 0.07 dex for [Fe/H]. Systematic biases are estimated to be between 50−100 K for Teff, 0.10−0.25 dex for log  g and 0.05−0.10 dex for [Fe/H]. Abundances for 24 elements were derived: C, N, O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Zn, Y, Zr, Mo, Ba, Nd, and Eu. The typical method-to-method dispersion of the abundances varies between 0.10 and 0.20 dex. Conclusions. The Gaia-ESO sample of high-resolution spectra of FGK-type stars will be among the largest of its kind analyzed in a homogeneous way. The extensive list of elemental abundances derived in these stars will enable significant advances in the areas of stellar evolution and Milky Way formation and evolution.

Variable stars in Milton field 54,

Mode of access: Internet.

Variable stars,

"Corrections to index": slip laid in.

Catalogue of bright stars, containing all important data known in June, 1930, relating to all stars brighter than 6.5 visual magnitude, and to some fainter ones.

At head of title: Yale university observatory.

Three stars ... /

Mode of access: Internet.

The peak of the load; the waiting months on the hilltop from the entrance of the Stars and Stripes to the second victory of the Marne.

Mode of access: Internet.

Orbits of the double stars, A B of [Epsilon] Hydrae and ? 883, by the graphical method.

Type-written ms.

Trees, stars and birds : a book of outdoor science /

"List of books" at end of each part.

A catalogue of 1625 stars between 39o and 41o South declination for the equinox 1900-0 selected as reference points for the Astrographic catalogue,

T.p. missing.

Stars for navigators and polaris tables for the year 1910. (Appendix to the American nautical almanac for the year 1910)

Mode of access: Internet.

Generalized Ramsey numbers for stars /

"UIUCDCS-R-81-1050"--Cover.

A generalization of Ramsey theory for graphs, with stars and complete graphs as forbidden subgraphs /

Includes bibliographical references.