Letter from Food Commissioner E. F. Ladd to Attorney General Langer Regarding Malta Test Results, 1917

Letter dated July 19, 1917 from Food Commissioner and North Dakota Agricultural College president E. F. Ladd to Attorney General Langer regarding analysis of samples of malt beverage Malta. Ladd explains that earlier samples showed as high as 0.45% alchohol content, but that more recent samples have shown around 0.10%, leading him to believe that the manufacturer has been cutting down that alcohol in their manufacturing process. Ladd adds that he should be very glad to make analysis of any samples that you might submit because of the variations that have been found in the the samples [...] during the past three months.https://commons.und.edu/langer-papers/1279/thumbnail.jp

Letter from Food Commissioner E. F. Ladd to Attorney General Langer Regarding Beverage Analysis, 1917

Letter dated July 20, 1917 from Food Commissioner E. F. Ladd to Attorney General Langer replying to letter sent to W. C. Heath concerner various beverages. Ladd indicates he would be very glad to have an analysis made of the beverages, and encloses a copy of a recent analysis of various soft drink beverages currently on sale in the state, adding that there are a few that he has not been able to acquire, among them a product sold as Bevo.https://commons.und.edu/langer-papers/1284/thumbnail.jp

Luminous radio-quiet sources in the W3(MAIN) cloud core

We have resolved 450 micrometer and 800 micrometer emission from the W3(Main) star forming region into three major peaks, using 8 inch - 14 inch beams with the James Clerk Maxwell Telescope on the summit of Mauna Kea. One of the submillimeter sources is identified with W3 - IRS5, a well-known candidate protostar. However, to our surprise, we find that none of the submillimeter peaks coincides with any of the prominent compact HII regions in the area. We estimate that the three submillimeter sources together contribute 30-50 percent of the total bolometric luminosity of the region, and speculate that the contribution of luminous radio-quiet sources to the total luminosity of HII region/molecular cloud complexes may be larger than is often assumed

Winds in cataclysmic variable stars

Ultraviolet spectrophotometry of two dwarf novae, CN Ori and RX And, at various phases of their outburst cycles confirms that the far uv flux increases dramatically about 1-2 days after the optical outburst begins. At this time the uv spectral line profiles indicate the presence of a high velocity wind. The detectability of the wind depends more on the steepness of the spectrum, and thus on the flux in the extreme ultraviolet, than on the absolute value of the far uv luminosity. The uv continuum during outburst consists of (at least) two c

Sedimentation and Flow Through Porous Media: Simulating Dynamically Coupled Discrete and Continuum Phases

We describe a method to address efficiently problems of two-phase flow in the regime of low particle Reynolds number and negligible Brownian motion. One of the phases is an incompressible continuous fluid and the other a discrete particulate phase which we simulate by following the motion of single particles. Interactions between the phases are taken into account using locally defined drag forces. We apply our method to the problem of flow through random media at high porosity where we find good agreement to theoretical expectations for the functional dependence of the pressure drop on the solid volume fraction. We undertake further validations on systems undergoing gravity induced sedimentation.Comment: 22 pages REVTEX, figures separately in uudecoded, compressed postscript format - alternatively e-mail '[email protected]' for hardcopies

Star formation in Perseus

We present a complete survey of current star formation in the Perseus molecular cloud, made at 850 and 450 micron with SCUBA at the JCMT. Covering 3 deg^2, this submillimetre continuum survey for protostellar activity is second in size only to that of rho Ophiuchus (Johnstone et al. 2004). Complete above 0.4 msun (5 sigma detection in a 14'' beam), we detect a total of 91 protostars and prestellar cores. Of these, 80% lie in clusters, representative of star formation across the Galaxy. Two of the groups of cores are associated with the young stellar clusters IC348 and NGC1333, and are consistent with a steady or reduced star formation rate in the last 0.5 Myr, but not an increasing one. In Perseus, 40--60% of cores are in small clusters (< 50 msun) and isolated objects, much more than the 10% suggested from infrared studies. Complementing the dust continuum, we present a C^18O map of the whole cloud at 1' resolution. The gas and dust show filamentary structure of the dense gas on large and small scales, with the high column density filaments breaking up into clusters of cores. The filament mass per unit length is 5--11 msun per 0.1 pc. Given these filament masses, there is no requirement for substantial large scale flows along or onto the filaments in order to gather sufficient material for star formation. We find that the probability of finding a submillimetre core is a strongly increasing function of column density, as measured by C^18O integrated intensity, prob(core) proportional to I^3.0. This power law relation holds down to low column density, suggesting that there is no A_v threshold for star formation in Perseus, unless all the low-A_v submm cores can be demonstrated to be older protostars which have begun to lose their natal molecular cloud.Comment: 15 pages, 5 figures, bibtex file scubasf_astroph.bbl, included tex files SSA-clusters-sorted-tidy.te

KINEMATIC AND KINETIC ANALYSIS OF THE ELITE GOLF SWING

The purpose of this study was to determine the association between select biomechanical variables and clubhead speed at impact (CSI) in a sample of elite golfers. Power generation is thought to arise from a number of factors including body rotation and weight shift. CSI is often used to indicate power generation (Fradkin, et al., 2004). We hypothesized that CSI would be highly related to torque, relative hip-shoulder rotation (X-factor) and weight shift during the golf swing