Stronger sexual desires only predict bold romantic intentions and reported infidelity when self-control is low

© 2014 The Australian Psychological Society. Objective: The present research examined whether people with lower self-control were more likely to act in accordance with their sexual desires in romantic situations. Specifically, we tested the hypothesis that sexual desires would be positively related to infidelity and courting intentions, but only when self-control was dispositionally low or temporarily impaired. Method: In Study 1, 331 participants who were recruited online completed survey measures of dispositional self-control, general sexual desire, and past infidelity. In Study 2, 120 undergraduate students were randomly allocated to either a depletion (low self-control) or control (high self-control) condition. Following the self-control manipulation, all participants completed implicit and explicit measures of courting intentions, and indicated the likelihood they would cheat on a long-term partner in an imagined scenario. Results: Study 1 found that sexual desire positively predicted reported infidelity frequency for people with low, but not high, dispositional self-control. Study 2 found that stronger sexual desires predicted increased infidelity intentions, sitting closer to an attractive stranger in an imagined scenario, and asking this person out in a hypothetical encounter, but only among people who had been depleted of their self-control resources. Sexual desires were unrelated to all constructs when participants' self-control was dispositionally high (Study 1) or not depleted (Study 2). Conclusions: Our findings suggest that when self-control is high, sexual behaviour may be largely divorced from desire, relying instead on analysis of situational or other cognitive factors. Sexual behaviour may reflect genuine sexual predispositions, however, when self-control is dispositionally low or temporarily depleted

Property and prejudice: How racial attitudes and social-evaluative concerns shape property appraisals

Property evaluations rarely occur in the absence of social context. However, no research has investigated how intergroup processes related to prejudice extend to concepts of property. In the present research, we propose that factors such as group status, prejudice and pressure to mask prejudiced attitudes affect how people value the property of racial ingroup and outgroup members. In Study 1, White American and Asian American participants were asked to appraise a hand-painted mug that was ostensibly created by either a White or an Asian person. Asian participants demonstrated an ingroup bias. White participants showed an outgroup bias, but this effect was qualified. Specifically, among White participants, higher racism towards Asian Americans predicted higher valuations of mugs created by Asian people. Study 2 revealed that White Americans' prejudice towards Asian Americans predicted higher valuations of the mug created by an Asian person only when participants were highly concerned about conveying a non-prejudiced personal image. Our results suggest that, ironically, prejudiced majority group members evaluate the property of minority group members whom they dislike more favourably. The current findings provide a foundation for melding intergroup relations research with research on property and ownership. © 2015 John Wile

High-Resolution Observations of Interstellar NA i and CA II Absorption Lines toward the Scorpius OB1 Association

Observations of Na I and Ca II in absorption toward 22 stars in the Sco OB1 region, obtained at resolution R = 100,000 with a coude echelle spectrograph and 3.3-m camera on the 1.9-m telescope at Mt. Stromlo Observatory during 1986, are reported. The data are presented in extensive tables and graphs and analyzed in detail. Features discussed include (1) strong absorption at heliocentric velocities between 0 and -20 km/sec, (2) sharp discrete components with blueshifted velocities of up to -50 km/sec, and (3) some absorption at positive heliocentric velocities up to +20 km/sec. The (Na I)/(Ca II) ratios are found to be 4-200 for component (1), near 1 for component (2), and 0.4 or less for component (3)

Optical observations of the ultrahigh-excitation Wolf-Rayet star Sanduleak 3

Recombination lines of O VII, O VIII, and C V have been identified in the optical spectrum of an O VI Wolf-Rayet star, representing the first non-X-ray detection of these ions in astronomical spectra and implying excitation energies in excess of 800 eV. Rapid variations on a time scale of about 150 s have been observed in the profile of one of the O VII lines

Self-Regulation and Power: How Self-Regulatory Failures Can Enhance Social Power

© 2016 John Wiley & Sons Ltd. Low self-control is often associated with poor life outcomes. Here, we propose that self-control failures may also provide social benefits by signaling and maintaining power. We identify several pathways by which reduced self-control can assist in ascending social hierarchies. First, the self-enhancing tendencies adopted by people with low self-control may contribute to making positive first impressions and advertising power to new acquaintances. The direct and disinhibited communication styles that stem from self-control failures may also enhance power and lubricate difficult social interactions. Disinhibited aggression can help people maintain and acquire material resources and establish dominance over rivals. Finally, the parallels between the behavior of people with low self-control and people with power (e.g., self-enhancement, disinhibition, approach-orientation, aggression) suggest that people with impaired self-control will be perceived as more powerful than people with intact self-control. Evidence for these propositions and directions for future research are discussed

Hubble Space Telescope Images of Magellanic Cloud Planetary Nebulae: Data and Correlations across Morphological Classes

The morphology of planetary nebulae (PNs) provides an essential tool for understanding their origin and evolution, since it reflects both the dynamics of the gas ejected at the tip of the asymptotic giant branch phase and the central-star energetics. Here we study the morphology of 27 Magellanic Cloud planetary nebulae (MCPNs) and present an analysis of their physical characteristics across morphological classes. Similar studies have been successfully carried out for Galactic PNs but were compromised by the uncertainty of individual PN distances. We present our own Hubble Space Telescope (HST) Faint Object Camera (FOC) images of 15 MCPNs acquired through a narrowband [O III] λ5007 filter. We use the Richardson-Lucy deconvolution technique on these pre-COSTAR images to achieve post-COSTAR quality. Three PNs imaged before and after COSTAR confirm the high reliability of our deconvolution procedure. We derive morphological classes, dimensions, and surface photometry for all of these PNs. We have combined this sample with HST/PC1 images of 15 MCPNs, three of which are in common with the FOC set acquired by Dopita et al., to obtain the largest MCPNs sample ever examined from the morphological viewpoint. By using the entire database, supplemented with published data from the literature, we have analyzed the properties of the MCPNs and compared them to a typical, complete Galactic sample. Morphology of the MCPNs is then correlated with PN density, chemistry, and evolution

Photoionization modelling based on HST images of Magellanic Cloud planetary nebulae – I. SMC N 2 and SMC N 5

We construct fully self-consistent, detailed photoionization models for two planetary nebulae (PNe) in the Small Magellanic Cloud (SMC), namely SMC N 2 and SMC N 5, to fit optical and UV spectrophotometric observations as well as HST Faint Object Camera (FOC) narrow-band images taken in the light of Hβ. The derived density structure shows that both PNe have a central cavity surrounded by a shell of decreasing density described by a parabolic curve. For both nebulae, our models fail to reproduce the HST images taken in the light of the [O III] λ 5007 line, in the sense that the observed [O III] λ 5007 surface brightness decreases more slowly outside the peak emission than predicted. An effective temperature of Teff = 111 500 K, a stellar surface gravity of log g = 5.45 and a luminosity of L* = 8430 Lʘ are derived for the central star of SMC N2; similarly Teff = 137 500 K, log g = 6.0 and L* = 5850 Lʘ are derived for SMC N 5. SMC N 2 is optically thin and has a total nebular mass (H plus He) of 0.180 Mʘ, while SMC N 5 is optically thick and has an ionized gas mass of 0.194 Mʘ. Using the H-burning SMC metal abundance (Z = 0.004) evolutionary tracks calculated by Vassiliadis & Wood, core masses of 0.674 Mʘ and 0.649Mʘ are derived for SMC N 2 and SMC N 5, respectively. Similarly, from the He-burning evolutionary tracks of Vassiliadis & Wood for progenitor stars of mean LMC heavy-element abundance (Z = 0.008), we find Mc = 0.695 and 0.675 Mʘ for SMC N 2 and SMC N 5, respectively. We find that Hβ images are needed if one is to derive accurate stellar luminosities directly from photoionization modelling. However, in the absence of an Hβ image, photoionization models based on [O III] images (and nebular line intensities) yield accurate values of Teff and log g, which in turn allow reliable stellar masses and luminosities to be derived from a comparison with theoretical evolutionary tracks. We show that the correct nebular ionized mass can be deduced from the nebular Hβ flux, provided the mean nebular density given by the C III] λ 1909/λ 1907 ratio is also known

Atomic and Molecular Interstellar Absorption Lines toward the High Galactic Latitude Stars HD 141569 and HD 157841 at Ultra-High Resolution

We present ultra-high-resolution (0.32 km s-1) spectra obtained with the 3.9 m Anglo-Australian Telescope (AAT) and Ultra-High-Resolution Facility (UHRF) of interstellar Na I D1, Na I D2, Ca II K, K I, and CH absorption toward two high Galactic latitude stars HD 141569 and HD 157841. We have compared our data with 21 cm observations obtained from the Leiden/Dwingeloo H I survey. We derive the velocity structure and column densities of the clouds represented by the various components and identify the clouds with ISM structures seen in the region at other wavelengths. We further derive abundances, linear depletions, and H2 fractional abundances for these clouds wherever possible. Both stars are located in regions of IRAS 100 μm emission associated with high Galactic latitude molecular clouds (HLCs): HD 141569 lies, in projection, close to MBM 37 and the Lynds dark cloud L134N, whereas HD 157841 is in the vicinity of the MBM 151. Toward HD 141569 we detect two components in our UHRF spectra: a weak, broad b = 4.5 km s-1 component at -15 km s-1, seen only in Ca II K absorption, and another component at 0 km s-1, seen in Na I D1, Na I D2, Ca II K, K I, and CH absorption. The cloud represented by the -15 km s-1 component is warm and may be located in a region close to the star. The cloud represented by the 0 km s-1 component has a Ca linear depletion δ(Ca) = 1.4 × 10-4 and shows evidence for the presence of dust, consistent with strong 100 μm emission seen in this region. The H2 fractional abundance f(H2) derived for this cloud is 0.4, which is typically what is observed toward HLCs. We conclude that this 0 km s-1 cloud is associated with MBM 37 and L134N based on the presence of dust and molecular gas (CH) and good velocity agreement with CO emission from these two clouds. This places HD 141569 beyond MBM 37 and L134N, which are estimated to be at ≈ 110 pc. In the case of the HD 157841 sight line, a total of six components are seen on our UHRF spectra in Na I D1, Na I D2, Ca II K, K I, and CH absorption. Two of these six components are seen only in a single species. The cloud represented by the components at 1.85 km s-1 has a Ca linear depletion δ(Ca) = 2.8 × 10-4, indicating the presence of dust. The f(H2) derived for this cloud is 0.45, and there is good velocity agreement with CO emission from MBM 151. To the best of our knowledge, this 1.85 km s-1 component toward HD 157841 is the first one found to have relative line widths that are consistent with pure thermal broadening only. We associate the 1.85 km s-1 cloud seen in our UHRF spectra with MBM 151 and conclude that HD 157841 must lie beyond ~200 pc, the estimated distance to MBM 151

Turbulent flow at 190 m height above London during 2006-2008: A climatology and the applicability of similarity theory

Flow and turbulence above urban terrain is more complex than above rural terrain, due to the different momentum and heat transfer characteristics that are affected by the presence of buildings (e.g. pressure variations around buildings). The applicability of similarity theory (as developed over rural terrain) is tested using observations of flow from a sonic anemometer located at 190.3 m height in London, U.K. using about 6500 h of data. Turbulence statistics—dimensionless wind speed and temperature, standard deviations and correlation coefficients for momentum and heat transfer—were analysed in three ways. First, turbulence statistics were plotted as a function only of a local stability parameter z/Λ (where Λ is the local Obukhov length and z is the height above ground); the σ_i/u_* values (i = u, v, w) for neutral conditions are 2.3, 1.85 and 1.35 respectively, similar to canonical values. Second, analysis of urban mixed-layer formulations during daytime convective conditions over London was undertaken, showing that atmospheric turbulence at high altitude over large cities might not behave dissimilarly from that over rural terrain. Third, correlation coefficients for heat and momentum were analyzed with respect to local stability. The results give confidence in using the framework of local similarity for turbulence measured over London, and perhaps other cities. However, the following caveats for our data are worth noting: (i) the terrain is reasonably flat, (ii) building heights vary little over a large area, and (iii) the sensor height is above the mean roughness sublayer depth

Predicting participation in group parenting education in an Australian sample: The role of attitudes, norms, and control factors

We examined the theory of planned behavior (TPB) in predicting intentions to participate in group parenting education. One hundred and seventy-six parents (138 mothers and 38 fathers) with a child under 12 years completed TPB items assessing attitude, subjective norms, perceived behavioral control (PBC), and two additional social influence variables (self-identity and group norm). Regression analyses supported the TPB predictors of participation intentions with self-identity and group norm also significantly predicting intentions. These findings offer preliminary support for the TPB, along with additional sources of social influence, as a useful predictive model of participation in parenting education