Junior Surface Warfare Officer retention

The purpose of this thesis is to identify factors that lead to resignation of Junior Surface Warfare Officers (SWO) and to develop an hedonic model of junior SWO turnover. The first source of data was a survey of active- duty, junior SWOs currently serving aboard ships. The second source of data was a survey of 0-3 SWOs who are currently drilling in the Naval Reserves. Results of the two surveys were compared to identify differing levels of satisfaction with the active-duty Navy. The reservists also compared their satisfaction between the active-duty Navy and their current civilian employment Civilian salary levels were obtained from the reservists and their spouses to determine the pay differential between the Navy and civilian jobs for former junior SWOs. A regression model found three factors to have significant power in explaining civilian pay: years since leaving active duty, employment status, and comparative work stress between civilian employment and the active-duty Navy. SWOs with full-time employment who experienced the greatest reductions in pay also experienced the greatest reduction in work Stress. Junior SWOs experienced, on average, a 20 percent pay cut after leaving active duty. Pay returned to its pre-departure level in 2 to three yearshttp://archive.org/details/juniorsurfacewar00dumoLieutenant, United States NavyApproved for public release; distribution is unlimited

Lick Northern Proper Motion Program. III. Lick NPM2 Catalog

The Lick Northern Proper Motion (NPM) program, a two-epoch (1947-1988) photographic survey of the northern two-thirds of the sky (Dec. > -23 deg), has measured absolute proper motions, on an inertial system defined by distant galaxies, for 380,000 stars from 8 <B < 18. The 1993 NPM1 Catalog contains 148,940 stars in 899 fields outside the Milky Way's zone of avoidance. The 2003 NPM2 Catalog contains 232,062 stars in the remaining 347 NPM fields near the plane of the Milky Way. This paper describes the NPM2 star selection, plate measurements, astrometric and photometric data reductions, and catalog compilation. The NPM2 Catalog contains 120,000 faint (B > 14) anonymous stars for astrometry and galactic studies, 92,000 bright (B < 14) positional reference stars, and 35,000 special stars chosen for astrophysical interest. The NPM2 proper motions are on the ICRS system, via Tycho-2 stars, to an accuracy of 0.5 mas/yr in each field. RMS proper motion precision is 6 mas/yr. Positional errors average 80 mas at the mean plate epoch 1968, and 200 mas at the NPM2 catalog epoch 2000. NPM2 photographic photometry errors average 0.18 mag in B, and 0.20 mag in B-V. The NPM2 Catalog and the updated (to J2000) NPM1 Catalog are available at the CDS Strasbourg data center and on the NPM WWW site (http://www.ucolick.org/~npm). The NPM2 Catalog completes the Lick Northern Proper Motion program after a half-century of work by three generations of Lick Observatory astronomers. The NPM Catalogs will serve as a database for research in galactic structure, stellar kinematics, and astrometry.Comment: 44 pages, 6 figures, accepted for publication in September 2004 Astronomical Journa

Kinematic Control of the Inertiality of the System of Tycho-2 and UCAC2 Stellar Proper Motions

Based on the Ogorodnikov-Milne model, we analyze the proper motions of Tycho-2 and UCAC2 stars. We have established that the model component that describes the rotation of all stars under consideration around the Galactic y axis differs significantly from zero at various magnitudes. We interpret this rotation found using the most distant stars as a residual rotation of the ICRS/Tycho-2 system relative to the inertial reference frame. For the most distant ($d\approx900$ pc) Tycho-2 and UCAC2 stars, the mean rotation around the Galactic y axis has been found to be $M_{13}=-0.37\pm0.04$ mas yr$^{-1}$. The proper motions of UCAC2 stars with magnitudes in the range $12-15^m$ are shown to be distorted appreciably by the magnitude equation in $\mu_\alpha\cos\delta$, which has the strongest effect for northern-sky stars with a coefficient of $-0.60\pm0.05$ mas yr$^{-1}$ mag$^{-1}$. We have detected no significant effect of the magnitude equation in the proper motions of UCAC2 stars brighter than $\approx11^m$.Comment: 15 pages, 6 figure

Kinematic Control of the Inertiality of ICRS Catalogs

We perform a kinematic analysis of the Hipparcos and TRC proper motions of stars by using a linear Ogorodnikov-Milne model. All of the distant (r more than 0.2 kpc) stars of the Hipparcos catalog have been found to rotate around the Galactic y axis with an angular velocity of -0.36 +/- 0.09 mas/year. One of the causes of this rotation may be an uncertainty in the lunisolar precession constant adopted when constructing the ICRS. In this case? the correction to the IAU (1976) lunisolar precession constant in longitude is shown to be -3.26 +/- 0.10 mas/yr. Based on the TRC catalog, we have determined the main Oort constants: A = 14.9 +/- 1.0 and B = -10.8 +/- 0.3 km/s/kpc. The component of the model that describes the rotation of all TRC stars around the Galactic y axis is nonzero for all magnitudes, My= -0.86 +/- 0.11 mas/yr.Comment: 10 pages, 4 figures, 2 table

Medico-Legal Findings, Legal Case Progression, and Outcomes in South African Rape Cases: Retrospective Review

Rachel Jewkes and colleagues examine the processing of rape cases by South African police and courts and show an association between documentation of ano-genital injuries, trials commencing, and convictions in rape cases

Kinematic Peculiarities of Gould Belt Stars

We analyzed the space velocities of Gould Belt stars younger than 125 Myr located at heliocentric distances <650 pc. We determined the rotation and expansion parameters of the Gould Belt by assuming the existence of a single kinematic center whose direction was found to be the following: $l_\circ=128^\circ$ and $R_\circ=150$ pc. The linear velocities reach their maximum at a distance of $\approx300$ pc from the center and are -6 km s$^{-1}$ for the rotation (whose direction coincides with the Galactic rotation) and +4 km s$^{-1}$ for the expansion. The stellar rotation model used here is shown to give a more faithful description of the observed velocity field than the linear model based on the Oort constants $A_G$ and $B_G$. We present evidence that the young clusters $\beta$ Pic, Tuc/HorA, and TWA belong to the Gould Belt structure.Comment: 17 pages, 5 figure

Application of Vector Spherical Harmonics and Kernel Regression to the computations of OMM Parameters

The high quality of Hipparcos data in position, proper motion, and parallax has allowed for studies about stellar kinematics with the aim of achieving a better physical understanding of our galaxy, based on accurate calculus of the Ogorodnikov-Milne model (OMM) parameters. The use of discrete least squares is the most common adjustment method, but it may lead to errors mainly because of the inhomogeneous spatial distribution of the data. We present an example of the instability of this method using the case of a function given by a linear combination of Legendre polynomials. These polynomials are basic in the use of vector spherical harmonics, which have been used to compute the OMM parameters by several authors, such as Makarov & Murphy, Mignard & Klioner, and Vityazev & Tsvetkov. To overcome the former problem, we propose the use of a mixed method (see Marco et al.) that includes the extension of the functions of residuals to any point on the celestial sphere. The goal is to be able to work with continuous variables in the calculation of the coefficients of the vector spherical harmonic developments with stability and efficiency. We apply this mixed procedure to the study of the kinematics of the stars in our Galaxy, employing the Hipparcos velocity field data to obtain the OMM parameters. Previously, we tested the method by perturbing the Vectorial Spherical Harmonics model as well as the velocity vector field.Part of this work was supported by a grant P1-1B2012-47 from UJI.Marco Castillo, FJ.; Martínez Uso, MJ.; Lopez, J. (2015). Application of Vector Spherical Harmonics and Kernel Regression to the computations of OMM Parameters. Astronomical Journal. 149(4):1-11. https://doi.org/10.1088/0004-6256/149/4/129S111149

The epidemiology and patterns of acute and chronic toxicity associated with recreational ketamine use

Ketamine was originally synthesised for use as a dissociative anaesthetic, and it remains widely used legitimately for this indication. However, there is increasing evidence of non-medical recreational use of ketamine, particularly in individuals who frequent the night-time economy. The population-level and sub-population (clubbers) prevalence of recreational use of ketamine is not known but is likely to be similar, or slightly lower than, that of other recreational drugs such as cocaine, MDMA, and amphetamine