Can Parents Create Alcoholics?

Background: Research has shown a definitive genetic component to alcoholism, with children of alcoholic parents being much more likely to become alcoholics themselves when compared to children of non-alcoholics. Just because alcoholism runs in an individual\u27s family does not guarantee that said individual will become an alcoholic. This paper tries to discern if the way a parent raises their child can have an effect on the likelihood of the child being an alcoholic later in life. Results: A review of the literature suggests that there may be a correlation between a how a child is raised and the likelihood of the child becoming an alcoholic. Research shows authoritative parents to raise children who are better able to self-regulate and have higher self-esteem, both qualities that deter alcoholic tendencies. Research also shows that authoritative and neglectful parents raise children who have higher incidences of depression and low self-esteem, both potential risk factors for alcoholism. Conclusion: Reviewing the literature provides a theoretical framework for a study to be done to try and more fully and completely explore the relationship between parenting styles and alcoholism

Snow Cover in Alaska: Comprehensive Review

This report presents the results of a statistical analysis of snow cover in Alaska using historical data acquired from the Global Historical Climate Network. Measurements of snow depth and snow water equivalence were collected for Alaska stations between 1950 and 2017. Data cleaning and a distribution analysis were completed for all stations. Finally regression equations were developed to estimate snow water equivalence using recorded snow depth data from Alaska stations. The project is partially supported by ConocoPhillips Arctic Science and Engineering Foundation, UAA, and the Structural Engineers Association of Alaska (SEAAK).University of Alaska Anchorage ConocoPhillips Arctic Science and Engineering Foundation Structural Engineers Association of AlaskaAbstract / Introduction / Methodology / Discussion / Conclusion / References / Appendix 1 Predicted 50-year WESD Stations's snow laods / Appendix 2 Calcuated 50-Year SNWD Station's snow loads / Appendix 3 Distribution Assignment for WESD and SNWD Stations / Appendix 4 Station Plot

Localizing coalescing massive black hole binaries with gravitational waves

Massive black hole binary coalescences are prime targets for space-based gravitational wave (GW) observatories such as {\it LISA}. GW measurements can localize the position of a coalescing binary on the sky to an ellipse with a major axis of a few tens of arcminutes to a few degrees, depending on source redshift, and a minor axis which is $2 - 4$ times smaller. Neglecting weak gravitational lensing, the GWs would also determine the source's luminosity distance to better than percent accuracy for close sources, degrading to several percent for more distant sources. Weak lensing cannot, in fact, be neglected and is expected to limit the accuracy with which distances can be fixed to errors no less than a few percent. Assuming a well-measured cosmology, the source's redshift could be inferred with similar accuracy. GWs alone can thus pinpoint a binary to a three-dimensional ``pixel'' which can help guide searches for the hosts of these events. We examine the time evolution of this pixel, studying it at merger and at several intervals before merger. One day before merger, the major axis of the error ellipse is typically larger than its final value by a factor of $\sim 1.5-6$. The minor axis is larger by a factor of $\sim 2-9$, and, neglecting lensing, the error in the luminosity distance is larger by a factor of $\sim 1.5-7$. This large change over a short period of time is due to spin-induced precession, which is strongest in the final days before merger. The evolution is slower as we go back further in time. For $z = 1$, we find that GWs will localize a coalescing binary to within $\sim 10\ \mathrm{deg}^2$ as early as a month prior to merger and determine distance (and hence redshift) to several percent.Comment: 30 pages, 10 figures, 5 tables. Version published in Ap

Voter support for bond referenda: Does it matter if costs are presented as aggregate vs. personal costs?

We explore whether voters\u27 willingness to approve government spending in bond elections is affected by how costs are presented. Using an original survey experiment, we examine willingness to approve bonds, randomizing both the total cost of the bond and the framing of the cost as either a personal cost or an aggregate amount. We find that respondents are less supportive of bonds when the bond is framed as a personal expense and that respondents are more cost-responsive when they see personal costs. There is also substantial heterogeneity based on the respondent\u27s partisanship and the policy domain of the bond

Spectral variations of the X-ray binary pulsar LMC X-4 during its long period intensity variation and a comparison with Her X-1

We present spectral variations of the binary X-ray pulsar LMC X-4 using the RXTE/PCA observations at different phases of its 30.5 day long super-orbital period. Only out of eclipse data were used for this study. During the high state of the super-orbital period of LMC X-4, the spectrum is well described by a high energy cut-off power-law with a photon index in the range of 0.7-1.0 and an iron emission line. In the low state, the spectrum is found to be flatter with power-law photon index in the range 0.5-0.7. A direct correlation is detected between the continuum flux in 7-25 keV energy band and the iron emission line flux. The equivalent width of the iron emission line is found to be highly variable during low intensity state, whereas it remains almost constant during the high intensity state of the super-orbital period. It is observed that the spectral variations in LMC X-4 are similar to those of Her X-1 (using RXTE/PCA data). These results suggest that the geometry of the region where the iron line is produced and its visibility with respect to the phase of the super-orbital period is similar in LMC X-4 and Her X-1. A remarkable difference between these two systems is a highly variable absorption column density with phase of the super-orbital period that is observed in Her X-1 but not in LMC X-4.Comment: 7 pages, 5 figures, Accepted for publication in Astronomy and Astrophysic