406 research outputs found

    College Dating Violence: Evaluating an Online Intervention

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    The purpose of this study will be to replicate and extend a randomized controlled trial that tested the effectiveness of an online bystander intervention educational program (STOP Dating Violence; O'Brien, Sauber, Kearney, Venaglia, & Lemay, 2019). Specifically, the intervention was modified and converted into an engaging animated video and then tested for its effectiveness. College students will be randomly assigned to one of three conditions: (1) the STOP intervention, (2) a website containing information about dating violence, and (3) a control condition. Data collection is currently underway. Preliminary data analyses (N=39) suggest that there is a difference in post test scores on the knowledge of bystander interventions measure across conditions (F(2, 36) = 3.876, p <; .03, Ρ 2 = .18). This study will advance knowledge regarding how counseling psychologists might cost-effectively and successfully educate undergraduates about dating violence

    A Chandra HETGS observation of the Narrow-line Seyfert 1 galaxy Ark 564

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    We present results from a 50 ks observation of the narrow-line Seyfert 1 galaxy Ark 564 with the Chandra HETGS. The spectra above 2 keV are modeled by a power-law with a photon-index of 2.56+/-0.06. We confirm the presence of the soft excess below about 1.5 keV. If we fit the excess with blackbody model, the best-fit temperature is 0.124 keV. Ark 564 has been reported to show a peculiar emission line-like feature at 1 keV in various observations using lower resolution detectors, and the Chandra grating spectroscopy rules out an origin of blends of several narrow emission lines. We detect an edge-like feature at 0.712 keV in the source rest frame. The preferred interpretation of this feature is combination of the O VII K-edge and a number of L-absorption lines from slightly ionized iron, which suggests a warm absorber with ionization parameter xi~1 and N_H ~ 10^21 cm^-2. These properties are roughly consistent with those of the UV absorber. We also detect narrow absorption lines of O VII, O VIII, Ne IX, Ne X, and Mg XI at the systemic velocity. From these lines, a second warm absorber having log xi ~ 2 and N_H ~ 10^21 cm^-2 is required.Comment: 22 pages, including 5 figures and 2 tables. Accepted for publication in Ap
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