Spreading of Antarctic Bottom Water in the Atlantic Ocean

This paper describes the transport of bottom water from its source region in the Weddell Sea through the abyssal channels of the Atlantic Ocean. The research brings together the recent observations and historical data. A strong flow of Antarctic Bottom Water through the Vema Channel is analyzed. The mean speed of the flow is 30 cm/s. A temperature increase was found in the deep Vema Channel, which has been observed for 30 years already. The flow of bottom water in the northern part of the Brazil Basin splits. Part of the water flows through the Romanche and Chain fracture zones. The other part flows to the North American Basin. Part of the latter flow propagates through the Vema Fracture Zone into the Northeast Atlantic. The properties of bottom water in the Kane Gap and Discovery Gap are also analyzed

Time-dependent Hartree-Fock studies of superheavy molecules

The time dependent Hartree-Fock approximation is used to study the dynamical formation of long-lived superheavy nuclear complexes. The effects of long-range Coulomb polarization are treated in terms of a classical quadrupole polarization model. Our calculations show the existence of "resonantlike" structures over a narrow range of bombarding energies near the Coulomb barrier. Calculations of 238U + 238U are presented and the consequences of these results for supercritical positron emission are discussed. NUCLEAR REACTIONS 238U + 238U collisions as a function of bombarding energy, in the time-dependent Hartree-Fock approximation. Superheavy molecules and strongly damped collisions

Business Improvement Recommendation

Presented to the Faculty of the University of Alaska Anchorage in Partial Fulfillment of the Requirements for the Degree of MASTER OF SCIENCEThe purpose of the ProBrainiac Project Management Plan (PMP) document is to provide the project stakeholders with an approved working guide for how the project will be managed during execution. The PMP outlines how the project work will be managed by the Project Manager (PM), project sponsor throughout the project phases ensuring efficient, timely, execution of the project and deliverable as outlined in the project charter.Introduction / Project Organization / Project Planning / Scope Management Plan / Schedule Management Plan / Cost Management Plan / Quality Management Plan / Human Resource Management Plan / Staffing Management Plan / Communications Management Plan / Risk Management Plan / Procurement Management Plan Stakeholder Management Plan / Change Management Plan / Project Execution / Phase Close-out and Lessons Learned / Appendice

Closed form solutions for the generalized extreme value distribution

This manuscript derives closed form solutions for conditional expectations of order statistics in models that are based on the extreme value and generalized extreme value distributions. Such conditional expectations are of interest in empirical anal-yses when the (identity of the) maximal statistic is observed, but the econometric model also relies on lower-rank order statistics which are unobserved. This is the case, for example, in some (sequential) bargaining models (e.g. Beckert, Smith and Takahashi (2015), for which this manuscript is a companion piece), or in empirical auctions models. The manuscript also provides an algorithm to derive the density of the GEV cumulative distribution function. This density is required to simulate nested logit models following the MCMC approach proposed by McFadden (1999)

Measuring 14 elemental abundances with R=1,800 LAMOST spectra

The LAMOST survey has acquired low-resolution spectra (R=1,800) for 5 million stars across the Milky Way, far more than any current stellar survey at a corresponding or higher spectral resolution. It is often assumed that only very few elemental abundances can be measured from such low-resolution spectra, limiting their utility for Galactic archaeology studies. However, Ting et al. (2017) used ab initio models to argue that low-resolution spectra should enable precision measurements of many elemental abundances, at least in theory. Here we verify this claim in practice by measuring the relative abundances of 14 elements from LAMOST spectra with a precision of $\lesssim$ 0.1 dex for objects with ${\rm S/N}_{\rm LAMOST}$ > 30 (per pixel). We employ a spectral modeling method in which a data-driven model is combined with priors that the model gradient spectra should resemble ab initio spectral models. This approach assures that the data-driven abundance determinations draw on physically sensible features in the spectrum in their predictions and do not just exploit astrophysical correlations among abundances. Our analysis is constrained to the number of elemental abundances measured in the APOGEE survey, which is the source of the training labels. Obtaining high quality/resolution spectra for a subset of LAMOST stars to measure more elemental abundances as training labels and then applying this method to the full LAMOST catalog will provide a sample with more than 20 elemental abundances that is an order of magnitude larger than current high-resolution surveys, substantially increasing the sample size for Galactic archaeology.Comment: 6 pages, 3 figures, ApJ (Accepted for publication- 2017 October 9