Increasing Clergy\u27s Knowledge of Mental Illness, Confidence, and Willingness to Refer

Over 43 million Americans suffer from mental illness annually with 40% seeking support from clergy (Polson & Rogers, 2007) who claim to be ineffectively prepared (Farrell & Goebert, 2008). This study investigated if mental health training administered to clergy would increase their knowledge of various mental disorders, alter their opinion regarding helpful resources, grow their self-confidence to help individuals experiencing mental health issues, and increase clergy\u27s willingness to refer out. The theoretical basis for this research was attribution theory that attempts to explain social perceptions (Mannarini & Boffo, 2013) and the struggle individuals (i.e. clergy) have regarding the causation of mental health concerns (Locke & Pennington, 1982) and identification of mental illness symptoms (Miller, Smith & Uleman, 1981). In the within-group study, clergy completed the Mental Health Effectiveness Questionnaire pre and post training to answer the following questions: Does participation in a training workshop affect clergy\u27s knowledge of mental disorders, opinion regarding helpful resources, self-confidence to assist an individual with mental health issues, and willingness to refer to a helpful resource? The majority of participants had experience with mental illness. Unexpected results showed mental health training positively influenced some opinions regarding helpful resources and confidence to assist someone with mental illness. The results of this research may influence positive social change by showing that faith based mental health training may do more than increase confidence to someone to assist and refer an individual experiencing mental health issues. It may also be a means of social support to family members already possessing knowledge of mental illness or indicate that family members are in search of more faith based mental health training

Widespread presence of shallow cusps in the surface-brightness profile of globular clusters

Surface brightness profiles of globular clusters with shallow central cusps (Sigma ~ R^v with -0.3<~ v <~ -0.05) have been associated by several recent studies with the presence of a central intermediate mass black hole (IMBH). Such shallow slopes are observed in several globular clusters thanks to the high angular resolution of Hubble Space Telescope imaging. In this Letter we evaluate whether shallow cusps are a unique signature of a central IMBH by analyzing a sample of direct N-body simulations of star clusters with and without a central IMBH. We ``observe'' the simulations as if they were HST images. Shallow cusps are common in our simulation sample: star clusters without an IMBH have v >~ -0.3 in the pre-core-collapse and core-collapse phases. Post-core-collapse clusters without an IMBH transition to steeper cusps, -0.7<~ v <~ -0.4, only if the primordial binary fraction is very small, f_{bin}< 3 per cent, and if there are few stellar-mass black holes remaining. Otherwise v values overlap the range usually ascribed to the presence of an IMBH throughout the entire duration of the simulations. In addition, measuring v is intrinsically prone to significant uncertainty, therefore typical measurement errors may lead to v > -0.3 even when <~ -0.4. Overall our analysis shows that a shallow cusp is not an unequivocal signature of a central IMBH and casts serious doubts on the usefulness of measuring v in the context of the hunt for IMBHs in globular clusters.Comment: 14 pages, 3 figures, Accepted for publication in The Astrophysical Journal, Letter

Trane Gas Test Stand Automation & Cycle Time Reduction

Mechatronic automation can eliminate many of the errors induced by manual, technician-operated controls, improving experiment quality. As such, automation of the Trane Gas Lab\u27s furnace testing devices will improve the quality of experiment data and reduce the time needed to complete a test, increasing productivity. To achieve this, the existing air shutters used in furnace testing were retrofitted using mechatronic equipment and computer controls to increase the efficiency of testing operations and remove the error introduced by human technicians. Compared to technician operated tests, the control devices developed have reduced the time required to perform the tests while significantly increasing data quality

Analysis Of Personality And Media Consumption

By drawing anonymous data from a thorough online survey, the link between a media consumer’s interest and personality type has been outlined. Using the internet as a host for the survey encouraged a sense of anonymity. This encourages truthfulness and participant willingness. This study explores the effects of personality types on media preferences. Trends within personality types and their collective likes and dislikes and correlational trends allow professionals to make assumptions pertaining to both individuals and the population. This allows science to create generalized profiles of the population and analyze how psychological types affect an individual’s overall perception of media.https://scholarworks.moreheadstate.edu/celebration_posters_2021/1053/thumbnail.jp

Some Effects of Thyroxine-Reserpine Treatment on Growth of Mice

Thyroxine, reserpine, and a combination of the two drugs were given to white mice over a ten-week period. Effects on growth rate were noted. Data are presented which indicate that a sequence of thyroxine for two days and reserpine for one day, with the sequence repeated over the experimental period, proved to have greatest effect on growth rate

Monte Carlo Simulations of Globular Cluster Evolution. V. Binary Stellar Evolution

We study the dynamical evolution of globular clusters containing primordial binaries, including full single and binary stellar evolution using our Monte Carlo cluster evolution code updated with an adaptation of the single and binary stellar evolution codes SSE/BSE from Hurley et. al (2000, 2002). We describe the modifications we have made to the code. We present several test calculations and comparisons with existing studies to illustrate the validity of the code. We show that our code finds very good agreement with direct N-body simulations including primordial binaries and stellar evolution. We find significant differences in the evolution of the global properties of the simulated clusters using stellar evolution compared to simulations without any stellar evolution. In particular, we find that the mass loss from stellar evolution acts as a significant energy production channel simply by reducing the total gravitational binding energy and can significantly prolong the initial core contraction phase before reaching the binary-burning quasi steady state of the cluster evolution as noticed in Paper IV. We simulate a large grid of clusters varying the initial cluster mass, binary fraction, and concentration and compare properties of the simulated clusters with those of the observed Galactic globular clusters (GGCs). We find that our simulated cluster properties agree well with the observed GGC properties. We explore in some detail qualitatively different clusters in different phases of their evolution, and construct synthetic Hertzprung-Russell diagrams for these clusters.Comment: 46 preprint pages, 18 figures, 3 tables, submitted to Ap

The fine-grained phase-space structure of Cold Dark Matter halos

We present a new and completely general technique for calculating the fine-grained phase-space structure of dark matter throughout the Galactic halo. Our goal is to understand this structure on the scales relevant for direct and indirect detection experiments. Our method is based on evaluating the geodesic deviation equation along the trajectories of individual DM particles. It requires no assumptions about the symmetry or stationarity of the halo formation process. In this paper we study general static potentials which exhibit more complex behaviour than the separable potentials studied previously. For ellipsoidal logarithmic potentials with a core, phase mixing is sensitive to the resonance structure, as indicated by the number of independent orbital frequencies. Regions of chaotic mixing can be identified by the very rapid decrease in the real space density of the associated dark matter streams. We also study the evolution of stream density in ellipsoidal NFW halos with radially varying isopotential shape, showing that if such a model is applied to the Galactic halo, at least $10^5$ streams are expected near the Sun. The most novel aspect of our approach is that general non-static systems can be studied through implementation in a cosmological N-body code. Such an implementation allows a robust and accurate evaluation of the enhancements in annihilation radiation due to fine-scale structure such as caustics. We embed the scheme in the current state-of-the-art code GADGET-3 and present tests which demonstrate that N-body discreteness effects can be kept under control in realistic configurations.Comment: 20 pages, 24 figures, submitted to MNRA

Tidal disruption, global mass function and structural parameters evolution in star clusters

[abridged] We present a unified picture for the evolution of star clusters on the two-body relaxation timescale. We use direct N-body simulations of star clusters in a galactic tidal field starting from different multi-mass King models, up to 10% of primordial binaries and up to Ntot=65536 particles. An additional run also includes a central Intermediate Mass Black Hole. We find that for the broad range of initial conditions we have studied the stellar mass function of these systems presents a universal evolution which depends only on the fractional mass loss. The structure of the system, as measured by the core to half mass radius ratio, also evolves toward a universal state, which is set by the efficiency of heating on the visible population of stars induced by dynamical interactions in the core of the system. Interactions with dark remnants are dominant over the heating induced by a moderate population of primordial binaries (3-5%), especially under the assumption that most of the neutron stars and black holes are retained in the system. All our models without primordial binaries undergo a deep gravothermal collapse in the radial mass profile. However their projected light distribution can be well fitted by medium concentration King models (with parameter W0 ~ 8), even though there tends to be an excess over the best fit for the innermost points of the surface brightness. This excess is consistent with a shallow cusp in the surface brightness (mu(R) ~ R^{-v} with v ~ 0.4-0.7), like it has been observed for many globular clusters from high-resolution HST imaging. Classification of core-collapsed globular clusters based on their surface brightness profile is likely to fail in systems that have already bounced back to lower concentrations.Comment: 33 pages, 11 figures, ApJ accepte

Historical changes in the phenology of British Odonata are related to climate

Responses of biota to climate change take a number of forms including distributional shifts, behavioural changes and life history changes. This study examined an extensive set of biological records to investigate changes in the timing of life history transitions (specifically emergence) in British Odonata between 1960 and 2004. The results show that there has been a significant, consistent advance in phenology in the taxon as a whole over the period of warming that is mediated by life history traits. British odonates significantly advanced the leading edge (first quartile date) of the flight period by a mean of 1.51 ±0.060 (SEM, n=17) days per decade or 3.08±1.16 (SEM, n=17) days per degree rise in temperature when phylogeny is controlled for. This study represents the first review of changes in odonate phenology in relation to climate change. The results suggest that the damped temperature oscillations experienced by aquatic organisms compared with terrestrial organisms are sufficient to evoke phenological responses similar to those of purely terrestrial taxa

Kinematics of the intermediate-mass black hole candidate HLX-1

We studied the optical spectrum of HLX-1 during its latest outburst, using the FORS2 spectrograph on the Very Large Telescope. We detect an Hα emission line centered at λ = 6718.9 ± 0.9 Å and find that its projected radial velocity with respect to the nucleus of ESO 243–49 is 424 ± 27 km s–1, while the maximum rotational velocity of the stars in that galaxy is 209 km s–1. This suggests that HLX-1 and its surrounding stars were not formed in situ, but came either from a disrupted dwarf galaxy or from a nuclear recoil. We also find that the Hα emission line is resolved with FWHM 400 km s–1, suggesting a nebular rather than disk origin for the emission. Its luminosity (L Hα = a few 1037 erg s–1, equivalent width = 70 Å) is also consistent with emission from a nebula photoionized by HLX-1