Physical Modeling of the Atmospheric Boundary Layer in the University of New Hampshire’s Flow Physics Facility

The atmospheric boundary layer is the lowest part of the atmosphere, and is defined by a region from the surface of the earth to approximately 500-1000m altitude in which air velocity changes from zero at the surface to the velocity of the wind at a certain altitude. The type of atmospheric boundary layer is characterized by the terrain it encounters, varying from open sea and mud flats to suburban areas and city centers with high- and low-rise buildings. The goal of this project is to generate different types of atmospheric boundary layers for scale model testing in the UNH Flow Physics Facility (FPF).The project began with the analysis of smooth wall (baseline) data previously recorded in the FPF. Several arrays of roughness elements were designed to simulate varying roughness lengths experienced by atmospheric boundary layers and tested in the FPF. The resulting velocity profiles in the boundary layer were measured using hot wire anemometry and pitot static tubes. These measured velocity profiles (mean and turbulence) and velocity spectra were compared to atmospheric boundary layers using ASCE Standards (ASCE/SEI 49-12). This application can then be used in the future for wind engineering studies, such as the structural analysis of buildings

Young massive stars in the ISOGAL survey I. VLA observations of the ISOGAL l=+45 field

We present VLA radio continuum observations at 3.6 and 6 cm of a ~0.65 sq.deg. field in the galactic plane at l=+45deg . These observations are meant to be used in a comparison with ISO observations at 7 and 15 um of the same region. In this paper we compare the radio results with other radio surveys and with the IRAS-PSC. At 3.6 and/or 6 cm we detect a total of 34 discrete sources, 13 of which are found in five separate extended complexes. These are all multiple or single extended thermal ultra-compact HII (UCHII) regions. While for each of these complexes an IRAS counterpart could be reliably found, no IRAS counterpart could be reliably identified for any of the remaining 21 sources. Of these 21 compact sources, six are candidate UCHII regions, and the other 15 are most probably background extragalactic non-thermal sources. The five IRAS sources associated with the radio continuum complexes all satisfy the Wood & Churchwell (1989; WC89) color criteria for UCHII. None of the other 38 IRAS point sources present in our surveyed field show the same colors. This fraction of WC89 type to total IRAS sources is consistent with what is found over the entire galactic plane. The fact that, when observed with a compact VLA configuration, the IRAS sources with "UCHII colors" are found to be associated with arcminute-scale extended sources, rather than with compact or unresolved radio sources, may have important implications on the estimated lifetime of UCHII regions.Comment: 15 pages, 22 eps figures, A&A Supp. in press, higher resolution figures available at http://www.arcetri.astro.it/~lt/preprints/preprints.htm

SB13-20/21: Resolution Regarding ASUM\u27s Endorsement of the University of Montana COVID-19 Reporting System

SB13-20/21: Resolution Regarding ASUM\u27s Endorsement of the University of Montana COVID-19 Reporting System. This resolution was approved unanimously during the September 9, 2020 meeting of the Associated Students of the University of Montana (ASUM)