Louisville / Jefferson County Hazardous Material Commodity Flow Analysis

This report presents the results of a Hazardous Material Commodity Flow Analysis for the Louisville Metro area and Jefferson County. Study components were conducted by Western Kentucky University in partnership with Louisville / Jefferson County Emergency Management Agency. The study area was focused in Louisville and Jefferson County, Louisville Metro area, and included monitoring in Bullet County and Oldham County, as shown in Figure 1.1. As part of the study, hazardous material transport was monitored at the following sites: Interstate-64 (I-64), East and West bound lanes at The Belvedere; I-64, East and West bound lanes at Blankenbaker exit location; Interstate-65 (I-65, North and South bound lanes at the Jewish Hospital; I-65, North and South bound lanes at Brooks, KY exit location; Interstate-71 (I-71), North and South bound lanes at Oldham County rest areas; Hwy 841, North and South bound Lanes at Westport Road. The purpose of this report is to present information on patterns of hazardous material commodity flow along I-64, I-65, I-71 and Highway 841, as observed from June 11, 2012 to August 2, 2012. This report also summarizes incidents involving hazardous materials over the previous 3 years, August 2008 to June 2011, in the Louisville Metro area. Finally, this report assesses survey information collected from fixed facilities that ship and receive hazardous materials in the Louisville Metro Area

Characterizing the Cool KOIs. V. KOI-256: A Mutually Eclipsing Post-common Envelope Binary

We report that Kepler Object of Interest 256 (KOI-256) is a mutually eclipsing post-common envelope binary (ePCEB), consisting of a cool white dwarf (M_★ = 0.592 ± 0.089 M_☉, R_★ = 0.01345 ± 0.00091 R_☉, T_(eff) = 7100 ± 700 K) and an active M3 dwarf (M_★ = 0.51 ± 0.16 M_☉, R_★ = 0.540 ± 0.014 R_☉, T_(eff) = 3450 ± 50 K) with an orbital period of 1.37865 ± 0.00001 days. KOI-256 is listed as hosting a transiting planet-candidate by Borucki et al. and Batalha et al.; here we report that the planet-candidate transit signal is in fact the occultation of a white dwarf as it passes behind the M dwarf. We combine publicly-available long- and short-cadence Kepler light curves with ground-based measurements to robustly determine the system parameters. The occultation events are readily apparent in the Kepler light curve, as is spin-orbit synchronization of the M dwarf, and we detect the transit of the white dwarf in front of the M dwarf halfway between the occultation events. The size of the white dwarf with respect to the Einstein ring during transit (R_(Ein) = 0.00473 ± 0.00055 R ☉) causes the transit depth to be shallower than expected from pure geometry due to gravitational lensing. KOI-256 is an old, long-period ePCEB and serves as a benchmark object for studying the evolution of binary star systems as well as white dwarfs themselves, thanks largely to the availability of near-continuous, ultra-precise Kepler photometry

Characterizing the cool kois. V. koi-256: A mutually eclipsing post-common envelope binary

We report that Kepler Object of Interest 256 (KOI-256) is a mutually eclipsing post-common envelope binary (ePCEB), consisting of a cool white dwarf (M* = 0.592 ± 0.089 M, R = 0.01345 ± 0.00091 R , T eff = 7100 ± 700 K) and an active M3 dwarf (M* = 0.51 ± 0.16 M , R* = 0.540 ± 0.014 R , T eff = 3450 ± 50 K) with an orbital period of 1.37865 ± 0.00001 days. KOI-256 is listed as hosting a transiting planet-candidate by Borucki et al. and Batalha et al.; here we report that the planet-candidate transit signal is in fact the occultation of a white dwarf as it passes behind the M dwarf. We combine publicly-available long- and short-cadence Kepler light curves with ground-based measurements to robustly determine the system parameters. The occultation events are readily apparent in the Kepler light curve, as is spin-orbit synchronization of the M dwarf, and we detect the transit of the white dwarf in front of the M dwarf halfway between the occultation events. The size of the white dwarf with respect to the Einstein ring during transit (R Ein = 0.00473 ± 0.00055 R ) causes the transit depth to be shallower than expected from pure geometry due to gravitational lensing. KOI-256 is an old, long-period ePCEB and serves as a benchmark object for studying the evolution of binary star systems as well as white dwarfs themselves, thanks largely to the availability of near-continuous, ultra-precise Kepler photometry. © 2013. The American Astronomical Society. All rights reserved.

New hope for old Dobbbin's broken leg

"Dr. Hickcox, who holds both a DVM and MD degree from the University, has applied both disciplines to his work here as assistant professor of veterinary medicine and surgery and resident in orthopedica surgery. Specifically, he is using a technique that he learned at the University Medical Center for setting and healing fractures on his animal patients."--Page 3

Dynamic traffic assignment: A primer (Transportation Research Circular E-C153)

Dynamic Traffic Assignment: A Primer is designed to help explain the basic concepts and definitions of dynamic traffic assignment (DTA) models and addresses the application, selection, planning, and execution of a DTA model. The report also describes the general DTA modeling procedure and modeling issues that may concern a model user

Keck Adaptive Optics Current and Future Roles as an ELT Pathfinder

International audienceKeck Adaptive Optics Current and Future Roles as an ELT Pathfinde

Keck Adaptive Optics Current and Future Roles as an ELT Pathfinder

International audienceKeck Adaptive Optics Current and Future Roles as an ELT Pathfinde

CHARACTERIZING THE COOL KOIs. V. KOI-256: A MUTUALLY ECLIPSING POST-COMMON ENVELOPE BINARY

We report that Kepler Object of Interest 256 (KOI-256) is a mutually eclipsing post-common envelope binary (ePCEB), consisting of a cool white dwarf (M = 0.592 +/- 0.089 MSun, R = 0.01345 +/- 0.00091 RSun, Teff = 7100 +/- 700 K) and an active M3 dwarf (M = 0.51 +/- 0.16 MSun, R = 0.540 +/- 0.014 RSun, Teff = 3450 +/- 50 K) with an orbital period of 1.37865 +/- 0.00001 days. KOI-256 is listed as hosting a transiting planet-candidate by Borucki et al. and Batalha et al.; here we report that the planet-candidate transit signal is in fact the occultation of a white dwarf as it passes behind the M dwarf. We combine publicly-available long- and short-cadence Kepler light curves with ground-based measurements to robustly determine the system parameters. The occultation events are readily apparent in the Kepler light curve, as is spin-orbit synchronization of the M dwarf, and we detect the transit of the white dwarf in front of the M dwarf halfway between the occultation events. The size of the white dwarf with respect to the Einstein ring during transit (REin = 0.00473 +/- 0.00055 RSun) causes the transit depth to be shallower than expected from pure geometry due to gravitational lensing. KOI-256 is an old, long-period ePCEB and serves as a benchmark object for studying the evolution of binary star systems as well as white dwarfs themselves, thanks largely to the availability of near-continuous, ultra-precise Kepler photometry.Comment: To be published in the Astrophysical Journa