Suchergebnisse

Are the traits preferred by voters also associated with success in political office? Drawing on the ascription-actuality trait theory of leadership the present study examines whether traits ascribed to politicians predict leadership outcomes differently to the actual traits they possess. We collected self-ratings of politicians' personality (N = 138) using the NEO-PI-R (actual traits) and observer ratings of politicians' facial appearance (ascribed traits) to examine their relationship with (a) leadership emergence, measured using share of vote in election, and (b) in-role leadership effectiveness, rated anonymously by political and local authority colleagues. Facial appearance predicted leadership emergence but not effectiveness. Personality had a more nuanced relationship with leadership outcomes. Conscientiousness predicted effectiveness but not emergence, and Agreeableness revealed a trait paradox, positively predicting emergence and negatively predicting effectiveness. These findings suggest a need to understand the contested nature of political leadership and qualities required for different aspects of political roles.

"Ouvrages de tapissier et de décorateur" has separate t.p. with imprint: Paris: Impr. et librairie administratives de Paul Dupont, 1867. ; At foot of t.p.: Collected and reprinted for private circulation only. ; Mode of access: Internet. ; Library's copy inscribed by the author to J.R. McClean on the front flyleaf.

The Astrophysical Journal 801.2 (2015): 143 reproduced by permission of the AAS ; The study of the planet-debris disk connection can shed light on the formation and evolution of planetary systemsand may help "predict" the presence of planets around stars with certain disk characteristics. In preliminary analyses of subsamples of the Herschel DEBRIS and DUNES surveys, Wyatt et al. and Marshall et al. identified a tentative correlation between debris and the presence of low-mass planets. Here we use the cleanest possible sample out of these Herschel surveys to assess the presence of such a correlation, discarding stars without known ages, with ages Gyr, and with binary companions AUto rule out possible correlations due to effects other than planet presence. In our resulting subsample of 204 FGK stars, we do not find evidence that debris disks are more common or more dusty around stars harboring high-mass or low-mass planets compared to a control sample without identified planets. There is no evidence either that the characteristic dust temperature of the debris disks around planet-bearing stars is any different from that in debris disks without identified planets, nor that debris disks are more or less common (or more or less dusty) around stars harboring multiple planets compared to single-planet systems. Diverse dynamical histories may account for the lack of correlations. The data show a correlation between the presence of high-mass planets and stellar metallicity, but no correlation between the presence of low-mass planets or debris and stellar metallicity. Comparing the observed cumulative distribution of fractional luminosity to those expected from a Gaussian distribution in logarithmic scale, we find that a distribution centered on the solar system's value fits the data well, while one centered at 10 times this value can be rejected. This is of interest in the context of future terrestrial planet detection and characterization because it indicates that there are good prospects for finding a large number of debris disk systems (i.e., with evidence of harboring planetesimals, the building blocks of planets) with exozodiacal emission low enough to be appropriate targets for an ATLAST-type mission to search for biosignatures ; A.M.-M. thanks Ewan Cameron for insightful comments and the STScI Directors Discretionary Research fund for support. J. P.M. is a UNSW Vice Chancellor's Postdoctoral Research Fellow. G.K. and M.C.W.'s work was supported by the European Union through ERC Grant 279973. C.E. and B.M. are partially supported by Spanish Ministry of Economy Grant AYA 2011-26202. D.R.R. acknowledges support from Chilean FONDECYT Grant 3130520. M.B. acknowledges support from a FONDECYT Postdoctoral Fellowship, Project 3140479