Sample records for uit gecontamineerde oplossingen

  1. DOE Office of Scientific and Technical Information (OSTI.GOV)

    Sheaffer, P.; Lemar, P.; Honton, E. J.

    The Universal Interconnection Technology (UIT) Workshop - sponsored by the U.S. Department of Energy, Distributed Energy and Electric Reliability (DEER) Program, and Distribution and Interconnection R&D - was held July 25-26, 2002, in Chicago, Ill., to: (1) Examine the need for a modular universal interconnection technology; (2) Identify UIT functional and technical requirements; (3) Assess the feasibility of and potential roadblocks to UIT; (4) Create an action plan for UIT development. These proceedings begin with an overview of the workshop. The body of the proceedings provides a series of industry representative-prepared papers on UIT functions and features, present interconnection technology,more » approaches to modularization and expandability, and technical issues in UIT development as well as detailed summaries of group discussions. Presentations, a list of participants, a copy of the agenda, and contact information are provided in the appendices of this document.« less

  2. Wide-field direct CCD observations supporting the Astro-1 Space Shuttle mission's Ultraviolet Imaging Telescope

    NASA Technical Reports Server (NTRS)

    Hintzen, Paul; Angione, Ron; Talbert, Freddie; Cheng, K.-P.; Smith, Eric; Stecher, Theodore P.

    1993-01-01

    Wide field direct CCD observations are being obtained to support and complement the vacuum-ultraviolet (VUV) images provided by Astro's Ultraviolet Imaging Telescope (UIT) during a Space Shuttle flight in December 1990. Because of the wide variety of projects addressed by UIT, the fields observed include (1) galactic supernova remnants such as the Cygnus Loop and globular clusters such as Omega Cen and M79; (2) the Magellanic Clouds, M33, M81, and other galaxies in the Local Group; and (3) rich clusters of galaxies, principally the Perseus cluster and Abell 1367. Ground-based observations have been obtained for virtually all of the Astro-1 UIT fields. The optical images allow identification of individual UV sources in each field and provide the long baseline in wavelength necessary for accurate analysis of UV-bright sources. To facilitate use of our optical images for analysis of UIT data and other projects, we plan to archive them, with the UIT images, at the National Space Science Data Center (NSSDC), where they will be universally accessible via anonymous FTP. The UIT, one of three telescopes comprising the Astro spacecraft, is a 38-cm f/9 Ritchey-Chretien telescope on which high quantum efficiency, solar-blind image tubes are used to record VUV images on photographic film. Five filters with passbands centered between 1250A and 2500A provide both VUV colors and a measurement of extinction via the 2200A dust feature. The resulting calibrated VUV pictures are 40 arcminutes in diameter at 2.5 arcseconds resolution. The capabilities of UIT, therefore, complement HST's WFPC: the latter has 40 times greater collecting area, while UIT's usable field has 170 times WFPC's field area.

  3. The ultraviolet imaging telescope: Instrument and data characteristics

    NASA Astrophysics Data System (ADS)

    Stecher, Theodore P.; Ultraviolet Imaging Telescope Team

    1997-05-01

    The Ultraviolet Imaging Telescope (UIT) was flown as part of the Astro Observatory on the Space Shuttle Columbia in December 1990 (see Figure 1) and again on the Space Shuttle Endeavour in March 1995. Ultraviolet (1200-3300 Å) images of a wide variety of astronomical objects were detected with UV image intensifiers and recorded on photographic film. Typical angular resolutions were 2-3 arcsec over a 40 arcmin field of view. The reduced and calibrated images from the first flight are available to the astronomical community through the National Space Science Data Center (NSSDC); the data recorded during the second flight will soon be available as well. UIT's design, operation, data reduction, and calibration are described in detail in Stecher et al. (1997), including a comprehensive description of the data characteristics. This publication provides UIT data users with information for understanding and using the data, as well as guidelines for analyzing other astronomical imagery made with image intensifiers and photographic film. Further information on the Astro missions and the UIT science program is available at the following website http://fondue.gsfc.nasa.gov/UIT/UIT_HomePage.html and in an educational slideset that is available from the Astronomical Society of the Pacific (Waller & Offenberg 1994).

  4. Laser-Hardened and Ultrasonically Peened Surface Layers on Tool Steel AISI D2: Correlation of the Bearing Curves' Parameters, Hardness and Wear

    NASA Astrophysics Data System (ADS)

    Lesyk, D. A.; Martinez, S.; Mordyuk, B. N.; Dzhemelinskyi, V. V.; Lamikiz, A.; Prokopenko, G. I.; Grinkevych, K. E.; Tkachenko, I. V.

    2018-02-01

    This paper is focused on the effects of the separately applied laser heat treatment (LHT) and ultrasonic impact treatment (UIT) and the combined LHT + UIT process on the wear and friction behaviors of the hardened surface layers of the tool steel AISI D2. In comparison with the initial state, wear losses of the treated specimens after long-term wear tests were decreased by 68, 41, and 77% at the LHT, UIT, and combined LHT + UIT processes, respectively. The Abbott-Firestone bearing curves were used to analyze the material ratio and functional characterization (bearing capacity and oil capacitance) of the studied surface specimens. The wear losses registered after short (15 min) tests correlate well with the changes in experimental surface roughness Ra, and the predictive Rpk, and bearing capacity B C parameters, respectively, evaluated using the Abbott-Firestone curves and Kragelsky-Kombalov formula. The wear losses after the long-term (45 min) tests are in good correlation with the reciprocal surface microhardness HV and with the W L and W P wear parameters, respectively, estimated using Archard-Rabinowicz formula and complex roughness-and-strength approach. The observed HV increase is supported by nanotwins (LHT), by dense dislocation nets (UIT), and by dislocation cells/nanograins fixed with fine carbides (LHT + UIT) formed in the surface layers of the steel.

  5. VizieR Online Data Catalog: M33 GALEX catalogue of UV point sources (Mudd+, 2015)

    NASA Astrophysics Data System (ADS)

    Mudd, D.; Stanek, K. Z.

    2015-11-01

    This catalogue was made using the Ultraviolet Imaging Telescope (UIT), an instrument aboard the Astro-1 Mission. UIT used photographic plates with the B1 and A1 filters roughly corresponding to the FUV and NUV filters of GALEX, having central wavelengths of ~1500 and 2400Å, respectively. It should be noted, however, that the A1 filter is significantly broader than the NUV filter on GALEX, reaching several hundred angstroms to the red end of its GALEX counterpart. The field of view of UIT is also circular but has a smaller radius of 18 arcmin The FWHM of UIT is comparable to that of GALEX, at 4 and 5.2 arcsec in the NUV and FUV filters, respectively. (3 data files).

  6. Astro-1 ultraviolet imaging of the 30 Doradus and SN 1987A fields with the Ultraviolet Imaging Telescope

    NASA Technical Reports Server (NTRS)

    Cheng, Kwang-Ping; Michalitsianos, Andrew G.; Hintzen, Paul; Bohlin, Ralph C.; O'Connell, Robert W.; Cornett, Robert H.; Roberts, Morton S.; Smith, Andrew M.; Smith, Eric P.; Stecher, Theodore P.

    1992-01-01

    A preliminary analysis of Ultraviolet Imaging Telescope (UIT) images in the 30 Doradus region is reported. Photometry was obtained for the 30 Doradus cluster and its UV-bright core, R136, in various UIT bandpasses. It is found that about 14 percent of the total FUV light and about 16 percent of the total near-UV light of the 3-arcmin diameter 30 Doradus cluster originates from the region within 5 arcsec of R136. The UV magnitudes and colors of R136 and other known O and Wolf-Rayet WN stars in the same field were measured. The UIT data, combined with published observations at longer wavelengths, indicate that R136a1, the brightest component of R136, is not a supermassive stars. A qualitative comparison between the UIT images, Einstein X-ray data, IRAS HiRes images, and ground-based CCD images in forbidden O III 5007 A, H-alpha, B, R, U, and Stromgren u is performed. The extended diffuse UV feature detected in the UIT images is correlated with the IR structure seen in the IRAS 60-micron HiRes image, which suggests the existence of large amounts of widely distributed dust in this region.

  7. Astro-1 ultraviolet imaging of the 30 Doradus and SN 1987A fields with the Ultraviolet Imaging Telescope

    NASA Astrophysics Data System (ADS)

    Cheng, Kwang-Ping; Michalitsianos, Andrew G.; Hintzen, Paul; Bohlin, Ralph C.; O'Connell, Robert W.; Cornett, Robert H.; Roberts, Morton S.; Smith, Andrew M.; Smith, Eric P.; Stecher, Theodore P.

    1992-08-01

    A preliminary analysis of Ultraviolet Imaging Telescope (UIT) images in the 30 Doradus region is reported. Photometry was obtained for the 30 Doradus cluster and its UV-bright core, R136, in various UIT bandpasses. It is found that about 14 percent of the total FUV light and about 16 percent of the total near-UV light of the 3-arcmin diameter 30 Doradus cluster originates from the region within 5 arcsec of R136. The UV magnitudes and colors of R136 and other known O and Wolf-Rayet WN stars in the same field were measured. The UIT data, combined with published observations at longer wavelengths, indicate that R136a1, the brightest component of R136, is not a supermassive stars. A qualitative comparison between the UIT images, Einstein X-ray data, IRAS HiRes images, and ground-based CCD images in forbidden O III 5007 A, H-alpha, B, R, U, and Stromgren u is performed. The extended diffuse UV feature detected in the UIT images is correlated with the IR structure seen in the IRAS 60-micron HiRes image, which suggests the existence of large amounts of widely distributed dust in this region.

  8. A critical analysis of unplanned ICU transfer within 48 hours from ED admission as a quality measure.

    PubMed

    Dahn, Cassidy M; Manasco, A Travis; Breaud, Alan H; Kim, Samuel; Rumas, Natalia; Moin, Omer; Mitchell, Patricia M; Nelson, Kerrie P; Baker, William; Feldman, James A

    2016-08-01

    Unplanned intensive care unit (ICU) transfer (UIT) within 48 hours of emergency department (ED) admission increases morbidity and mortality. We hypothesized that a majority of UITs do not have critical interventions (CrIs) and that CrI is associated with worse outcomes. The objective of the study is to characterize all UITs (including patients who died before ICU transfer), the proportion with CrI, and the effect of having CrI on mortality. This is a single-center, retrospective cohort study of UITs within 48 hours from 2008 to 2013 at an urban academic medical center and included patients 18 years or older without advanced directives (ADs). Critical intervention was defined by modified Delphi process. Data included demographics, comorbidities, reasons for UIT, length of stay, CrIs, and mortality. We calculated descriptive statistics with 95% confidence intervals (CIs). A total of 837 (0.76%) of 108 732 floor admissions from the ED had a UIT within 48 hours; 86 admitted patients died before ICU. We excluded 23 ADs, 117 postoperative transfers, 177 planned ICU transfers, and 4 with missing data. Of the 516 remaining, 65% (95% CI, 61%-69%) received a CrI. Unplanned ICU transfer reasons are as follows: 33 medical errors, 90 disease processes not present on arrival, and 393 clinical deteriorations. Mortality was 10.5% (95% CI, 8%-14%), and mean length of stay was 258 hours (95% CI, 233-283) for those with CrI, whereas the mortality was 2.8% (95% CI, 1%-6%) and mean length of stay was 177 hours (95% CI, 157-197) for those without CrI. Unplanned ICU transfer is rare, and only 65% had a CrI. Those with CrI had increased morbidity and mortality. Copyright © 2016 Elsevier Inc. All rights reserved.

  9. UIT ultraviolet imaging of 30 Doradus

    NASA Technical Reports Server (NTRS)

    Hintzen, P.; Cheng, K.-P.; Michalitsianos, A.; Bohlin, R.; O'Connell, R.; Cornett, R.; Roberts, M.; Smith, A.; Smith, E.; Stecher, T.

    1992-01-01

    During the Astro-1 mission, near- and far-UV images of the 30 Doradus region were obtained using the Ultraviolet Imaging Telescope (UIT). These wide-field, 40 min in diameter, high spatial resolution, 2-3 sec, UIT UV images reveal a rich field of luminous UV-bright stars, clusters, and associations. There are 181 stars brighter than m(sub 2558A) = 16.5 and 197 stars brighter than m(sub 1615A) = 16.4 within 3 min diameter of the 30 Doradus central cluster. We have derived UV fluxes emitted from the 30 Doradus central cluster and from its UV bright core, R136. The region within 5 sec of R136 produces approximately 14% of the far-UV flux (lambda = 1892 A) and approximately 16% of the near-UV flux (lambda = 2558 A) emitted from the 3 min diameter central cluster. The derived UV luminosity of R136 at 1892 A is only 7.8 times that of the nearby O6-7 Iaf star, R139, and the m(sub 1892) - m(sub v) colors of R136 are similar to other O or Wolf-Rayet stars in the same region. These UIT data, combined with other published observations at longer wavelengths, indicate that there is no observational evidence for a supermassive star in R136.

  10. UIT ultraviolet imaging of 30 Doradus

    NASA Astrophysics Data System (ADS)

    Hintzen, P.; Cheng, K.-P.; Michalitsianos, A.; Bohlin, R.; O'Connell, R.; Cornett, R.; Roberts, M.; Smith, A.; Smith, E.; Stecher, T.

    During the Astro-1 mission, near- and far-UV images of the 30 Doradus region were obtained using the Ultraviolet Imaging Telescope (UIT). These wide-field, 40 min in diameter, high spatial resolution, 2-3 sec, UIT UV images reveal a rich field of luminous UV-bright stars, clusters, and associations. There are 181 stars brighter than m2558A = 16.5 and 197 stars brighter than m1615A = 16.4 within 3 min diameter of the 30 Doradus central cluster. We have derived UV fluxes emitted from the 30 Doradus central cluster and from its UV bright core, R136. The region within 5 sec of R136 produces approximately 14% of the far-UV flux (lambda = 1892 A) and approximately 16% of the near-UV flux (lambda = 2558 A) emitted from the 3 min diameter central cluster. The derived UV luminosity of R136 at 1892 A is only 7.8 times that of the nearby O6-7 Iaf star, R139, and the m1892 - mv colors of R136 are similar to other O or Wolf-Rayet stars in the same region. These UIT data, combined with other published observations at longer wavelengths, indicate that there is no observational evidence for a supermassive star in R136.

  11. Microstructural characterization of ultrasonic impact treated aluminum-magnesium alloy

    NASA Astrophysics Data System (ADS)

    Tran, Kim Ngoc Thi

    Aluminum 5456-H116 has high as-welded strength, is formable, and highly corrosion resistant, however, it can become sensitized when exposed to elevated temperatures for a prolonged time. Sensitization results in the formation of a continuous β phase at the grain boundaries that is anodic to the matrix. Thus the grain boundaries become susceptible to stress corrosion cracking (SCC) and intergranular corrosion cracking (IGC). Cracking issues on aluminum superstructures have prompted the use of a severe plastic deformation processes, such as ultrasonic impact treatment (UIT), to improve SCC resistance. This study correlated the effects of UIT on the properties of 5456-H116 alloy to the microstructural evolution of the alloy and helped develop a fundamental understanding of the mechanisms that cause the microstructural evolution. Ultrasonic impact treatment produces a deformed layer at the surface ˜ 10 to 18 µm thick that is characterized by micro-cracks, tears, and voids. Ultrasonic impact treatment results in grain refinement within the deformation layer and extending below the deformed layer. The microstructure exhibits weak crystallographic texture with larger fraction of high angle grain boundaries. Nanocrystalline grains within the deformation layer vary in size from 2 to 200 nm in diameter and exhibit curved or wavy grain boundaries. The nanocrystalline grains are thermally stable up to 300°C. Above 300°C, grain growth occurs with an activation energy of ˜ 32 kJ/mol. Below the deformation layer, the microstructure is characterized by submicron grains, complex structure of dislocations, sub-boundaries, and Moiré fringes depicting overlapping grains. The deformation layer does not exhibit the presence of a continuous β phase, however below the deformation layer; a continuous β phase along the grain boundaries is present. In general the highest hardness and yield strength is at the UIT surface which is attributed to the formation of nanocrystalline grains. Although the highest hardness and yield strength was observed at the UIT surface, the results were mixed with some lower values. The lower hardness and yield strength values at the UIT surface are attributed to the voids and micro cracking/micro voids observed in the deformation layer. The fracture mode was transgranular ductile fracture with micro void coalescence and dimples. Both UIT and untreated material exhibit similar levels of intergranular corrosion susceptibility. Corrosive attack was intergranular with slightly deeper attack in the untreated material. Numerical simulation modeling showed that the calculated residual stress under the tool, ˜80 MPa, is of the same order of magnitude as the compressive residual stresses measured by XRD measurements near the surface. Modeling also showed that high effective strains were induced almost immediately. The UIT process also resulted in rapid localized heating to a maximum temperature of ˜32°C during the first eleven pin tool cycles. The model also showed that during UIT processing, the material undulates as the pin tool impacts and retracts from the surface of the material. The undulations represent the elastic response of the surface to the compressive stresses built up during a pin tool cycle.

  12. Word Frequency Analysis. MOS: 75C. Skill Levels 1 & 2.

    DTIC Science & Technology

    1981-05-01

    A4Fi j, A REAS . I --- - ., ARISS 12 ARMY I A~K1h ’.-L ARRANGED 64 AS I ASCERTAIN 2 .L~u Ip ASSEMBLE 12 ASSEMBLED 1 ASSEMPLY I ASSI----------------2...GOVERNING .16 GRADE ’G.; S GRAA!TET I GRfATEST I GREEN I GFEP.I .4 ( AriSS I GROUPS s GUIDANCE I G lIn (;UItES V 1 E I GUIVIS/ 3 GWPM 1-’ 1 I.AO 1 HAE

  13. Clinical and Epidemiological Studies on Rickettsial Infections.

    DTIC Science & Technology

    1980-06-01

    investigations currently or fo Tly undertaken with the collaboration or spotof the following or n’iztiona- 1) In, Ethiopia : Naval Medical Research Uit-S.. 2) In B...data from the continuing studies in Burma ocanplement and extend our earlier investigati6ns in Ethiopia , we now sumarize those results frm the Ethiopian...TESTS COMPARING RATES IN RATTUS RATTUS A14D MUS MUSCULUS WITH OTHER RODENTS (INDOORS AND OUTDOORS) IN ETHIOPIA , WITH INDICATION OP THEIR MAJOR

  14. OMEGACAM and Gravitational Lensing

    NASA Astrophysics Data System (ADS)

    Christen, Fabrice Frédéric Thiébaut

    2007-04-01

    Het proefschrift van Fabrice Christen gaat over de ontwikkeling van nieuwe methoden voor het corrigeren van (digitale) foto's van melkwegstelsels. Met deze methoden kunnen de beelden uit het heelal beter worden geanalyseerd. Het eerste gedeelte is gewijd aan het werk dat bij ESO is uitgevoerd aan de CCD's van de OmegaCAM camera, het enige instrument van de VST. OmegaCAM is een optische groothoekcamera met een beeldveld van een vierkante graad, opgebouwd uit een mozaiek van 8 bij 4 CCD's. Van elk onderdeel moeten alle kenmerken volledig bekend zijn voordat het in het CCD mozaiek geplaatst kan worden. In het tweede deel van dit proefschrift wordt de ontwikkeling van een nieuwe methode voor het corrigeren van de ``point-spread function'' (PSF) en schatten van de ellipticiteit van de melkwegstelsels besproken. De nieuwe techniek wordt getest en vergeleken met een door sterrenkundigen algemeen gebruikte methode in het veld van zwaartekrachtslenzen, de Kaiser, Squire en Broadhurst (KSB) methode. De nieuwe methode, gebaseerd op shapelet ontleding (vergelijkbaar met wavelet ontleding), gaat verder, en is sneller en theoretisch preciezer dan de KSB methode. Door gebruik te maken van de gecorrigeerde ellipticiteit, kunnen we een statistische analyse uitvoeren om er een kosmisch vervormingssignaal uit te halen. De licht vervormde beelden van de melkwegstelsels bewij zen dat de niet-homogene massaverdeling op megaparsec-schaal voornamelijk bestaat uit grote hoeveelheden donkere materie. Verder vergelijken we de schattingen van de ellipticiteit van de shapelet en KSB methode. Bovendien voeren we ook nog een melkwegstelsel-melkwegstelsel lens analyse uit op de 50 VLT Fors1 afbeeldingen en slagen we erin de belangrijkste eigenschappen van de halo's van de stelsels, die zich op een afstand van een- tot tweeduizend megaparsec (1 parsec = 3,26 lichtjaar = 3,085 x 10^16 meter) bevinden, te bepalen door gebruik te maken van twee modellen van melkwegstelselhalo's. Vergeleken met andere overzichtsmetingen vinden we vergelijkbare resultaten.

  15. Spacelab

    NASA Image and Video Library

    1990-12-09

    This is a presentation of two comparison images of the Spiral Galaxy M81 in the constellation URA Major. The galaxy is about 12-million light years from Earth. The left image is the Spiral Galaxy M81 as photographed by the Ultraviolet Imaging Telescope (UIT) during the Astro-1 Mission (STS-35) on December 9, 1990. This UIT photograph, made with ultraviolet light, reveals regions where new stars are forming at a rapid rate. The right image is a photograph of the same galaxy in red light made with a 36-inch (0.9-meter) telescope at the Kitt Peak National Observatory near Tucson, Arizona. The Astro Observatory was designed to explore the universe by observing and measuring ultraviolet radiation from celestial objects. Three instruments made up the Astro Observatory: The Hopkins Ultraviolet Telescope (HUT), the Ultraviolet Imaging Telescope (UIT), and the Wisconsin Ultraviolet Photo-Polarimetry Experiment (WUPPE). The Marshall Space Flight Center had management responsibilities for the Astro-1 mission. The Astro-1 Observatory was launched aboard the Space Shuttle Orbiter Columbia (STS-35) on December 2, 1990.

  16. Waardering en Analyse van Simulatieresultaten (Valuation and Analysis of Simulation Results)

    DTIC Science & Technology

    1991-12-01

    is uit de tabel van de Students T-verdeling te halen . Deze wordt aangeduid met t,(v), waarin a de overschrijdingskans en v bet aantal vrijheidsgraden...2 vrijheidsgraden. Uit de tabol van de Student’s t-verdeling zija nu de kritieke waardon R, on R2 to halen zodanig dat P(t >R2 ) = i Wordt or eon...analyse van simnulatieresultaten - TDCnaK RAPPORTE1CENTRALE Frederikkazerne, Geb. 140 AD-A25 470van den Burchlaan 31AD-A25 470Telefoon: 070-3166394

  17. Astro-1 Image Taken by the Ultraviolet Imaging Telescope

    NASA Technical Reports Server (NTRS)

    1990-01-01

    This is a presentation of two comparison images of the Spiral Galaxy M81 in the constellation URA Major. The galaxy is about 12-million light years from Earth. The left image is the Spiral Galaxy M81 as photographed by the Ultraviolet Imaging Telescope (UIT) during the Astro-1 Mission (STS-35) on December 9, 1990. This UIT photograph, made with ultraviolet light, reveals regions where new stars are forming at a rapid rate. The right image is a photograph of the same galaxy in red light made with a 36-inch (0.9-meter) telescope at the Kitt Peak National Observatory near Tucson, Arizona. The Astro Observatory was designed to explore the universe by observing and measuring ultraviolet radiation from celestial objects. Three instruments made up the Astro Observatory: The Hopkins Ultraviolet Telescope (HUT), the Ultraviolet Imaging Telescope (UIT), and the Wisconsin Ultraviolet Photo-Polarimetry Experiment (WUPPE). The Marshall Space Flight Center had management responsibilities for the Astro-1 mission. The Astro-1 Observatory was launched aboard the Space Shuttle Orbiter Columbia (STS-35) on December 2, 1990.

  18. Correlated Equilibria in Continuous Games: Characterization and Computation

    DTIC Science & Technology

    2008-12-22

    there exist continuous functions gji : Ci → [0, 1] which sum to at most unity and equal the f ji except on a set of µi measure at most δ. Therefore∣∣∣∣∣ k...j=1 ∫ f ji (si) [ ui(t j i , s−i)− ui(s) ] dπ − k∑ j=1 ∫ gji (si) [ ui(t j i , s−i)− ui(s) ] dπ ∣∣∣∣∣ ≤ k∑ j=1 ∫ |f ji (si)− g j i (si)|dπ j i ≤ 2kδ

  19. Ultraviolet Imaging Telescope (UIT) observations of galaxies

    NASA Technical Reports Server (NTRS)

    Neff, S. G.

    1993-01-01

    Ultraviolet images of several galaxies were obtained during the ASTRO-1 shuttle mission in December, 1990. The images have a FWHM angular resolution of approximately 3 arcsecond and are of circular fields approximately 40 arcminutes in diameter. Most galaxies were observed in at least two and sometimes as many as four broad bands. A very few fields were observed with narrower band filters. The most basic result of these observations is that most systems look dramatically different in the UV from their well-known optical appearances. Preliminary results of these studies will be presented. Information will be available on fields observed by the UTI during the ASTRO 1 mission; when that data becomes public it can be obtained from the NSSDC. The ASTRO observatory is expected to fly again in 1994 with approximately half of the observing time from that mission devoted to guest observers. The Ultraviolet Imaging telescope is extremely well suited for galaxy studies, and the UIT term is interested in encouraging a wide range of scientific studies by guest observers. Ultraviolet Imaging telescope is extremely well suited for galaxy studies, and the UIT team is interested in encouraging a wide range of scientific studies by guest observers.

  20. A note on subtrees rooted along the primary path of a binary tree

    USGS Publications Warehouse

    Troutman, B.M.; Karlinger, M.R.

    1993-01-01

    Let Fn denote the set of rooted binary plane trees with n external nodes, for given T???Fn let ui(T) be the altitude i node along the primary path of T, and let ??i(T) denote the number of external nodes in the induced subtree rooted at ui(T). We set ??i(T) = 0 if i is greater than the length of the primary path of T. We prove limn?????? ???i???x/n En{??i}/???i

  1. GALEX Grism Spectroscopy of the Globular Cluster Omega Centauri

    NASA Astrophysics Data System (ADS)

    Sweigart, Allen

    We propose to obtain GALEX FUV-only grism spectroscopy of the hot stars in omega Centauri, the most massive globular cluster in our Galaxy. Previous UIT imagery of omega Cen showed that it contains about 2000 hot horizontal branch (HB) stars, and we estimate that GALEX spectra can be obtained for about 500 of these stars in the outer regions of the cluster, including about 50 of the hot ``blue hook'' stars discovered with UIT. The blue hook stars appear to be both hotter (35,000 K) and less luminous in the UIT color-magnitude diagram than predicted by canonical HB models and, indeed, are unexplained by standard evolutionary theory. Brown et al. (2001) have suggested that the blue hook stars are the progeny of stars which mixed their surface hydrogen into their hot He-burning interior during a delayed helium flash subsequent to leaving the red giant branch. This ``flash-mixing'' results in a hot hydrogen-deficient star with a typical surface abundance of 96% He and 4% C by mass. The GALEX spectral region includes the strong lines of C III 1426, 1578 A, C IV 1550 A, and He II 1640 A which will allow this predicted carbon and helium enrichment to be detected. These observations will therefore provide a crucial test of the Brown et al. flash-mixing hypothesis and will determine if flash mixing represents a new evolutionary channel for populating the hot HB. The GALEX spectra will also address other questions concerning the hot HB in omega Cen including (1) the metallicity distribution of HB stars with 9,000 K < Teff < 11,000 K, (2) the effect of radiative levitation on the UV spectra of stars with Teff > 11,000 K, and (3) the origin of the subluminous HB stars found in the UIT photometry with 15,000K < Teff < 30,000 K.

  2. The MAR databases: development and implementation of databases specific for marine metagenomics

    PubMed Central

    Klemetsen, Terje; Raknes, Inge A; Fu, Juan; Agafonov, Alexander; Balasundaram, Sudhagar V; Tartari, Giacomo; Robertsen, Espen

    2018-01-01

    Abstract We introduce the marine databases; MarRef, MarDB and MarCat (https://mmp.sfb.uit.no/databases/), which are publicly available resources that promote marine research and innovation. These data resources, which have been implemented in the Marine Metagenomics Portal (MMP) (https://mmp.sfb.uit.no/), are collections of richly annotated and manually curated contextual (metadata) and sequence databases representing three tiers of accuracy. While MarRef is a database for completely sequenced marine prokaryotic genomes, which represent a marine prokaryote reference genome database, MarDB includes all incomplete sequenced prokaryotic genomes regardless level of completeness. The last database, MarCat, represents a gene (protein) catalog of uncultivable (and cultivable) marine genes and proteins derived from marine metagenomics samples. The first versions of MarRef and MarDB contain 612 and 3726 records, respectively. Each record is built up of 106 metadata fields including attributes for sampling, sequencing, assembly and annotation in addition to the organism and taxonomic information. Currently, MarCat contains 1227 records with 55 metadata fields. Ontologies and controlled vocabularies are used in the contextual databases to enhance consistency. The user-friendly web interface lets the visitors browse, filter and search in the contextual databases and perform BLAST searches against the corresponding sequence databases. All contextual and sequence databases are freely accessible and downloadable from https://s1.sfb.uit.no/public/mar/. PMID:29106641

  3. PREFACE: 33rd UIT (Italian Union of Thermo-fluid dynamics) Heat Transfer Conference

    NASA Astrophysics Data System (ADS)

    Paoletti, Domenica; Ambrosini, Dario; Sfarra, Stefano

    2015-11-01

    The 33rd UIT (Italian Union of Thermo-Fluid Dynamics) Heat Transfer Conference was organized by the Dept. of Industrial and Information Engineering and Economics, University of L'Aquila (Italy) and was held at the Engineering Campus of Monteluco di Roio, L'Aquila, June 22-24, 2015. The annual UIT conference, which has grown over time, came back to L'Aquila after 21 years. The scope of the conference covers a range of major topics in theoretical, numerical and experimental heat transfer and related areas, ranging from energy efficiency to nuclear plants. This year, there was an emphasis on IR thermography, which is growing in importance both in scientific research and industrial applications. 2015 is also the International Year of Light. The Organizing Committee honored this event by introducing a new section, Technical Seminars, which in this edition was mainly devoted to optical flow visualization (also the subject of three different national workshops organized in L'Aquila by UIT in 2003, 2005 and 2008). The conference was held in the recently repaired Engineering buildings, six years after the 2009 earthquake and 50 years after the beginning of the Engineering courses in L'Aquila. Despite some logistical difficulties, 92 papers were submitted by about 270 authors, on eight different topics: heat transfer and efficiency in energy systems, environmental technologies and buildings (32 papers); micro and nano scale thermo-fluid dynamics (5 papers); multi-phase fluid dynamics, heat transfer and interface phenomena (16 papers); computational fluid dynamics and heat transfer (15 papers); heat transfer in nuclear plants (6 papers); natural, forced and mixed convection (6 papers); IR thermography (4 papers); conduction and radiation (3 papers). The conference program scheduled plenary, oral and poster sessions. The three invited plenary Keynote Lectures were given by Prof. Antonio Barletta (University of Bologna, Italy), Prof. Jean-Christophe Batsale (Arts et Metiers Paris Tech, Talence, France) and Prof. Walter Grassi (University of Pisa, Italy). The two invited Technical Seminars were given by Dr. Maurizio Santini (University of Bergamo, Italy) and Prof. Giovanni Tanda (University of Genova, Italy). There were also 13 oral sessions and three poster sessions. This special issue collects the five papers presented in the plenary sessions (keynote lectures and technical seminars) plus 60 papers selected from those presented and discussed during the congress. The UIT 2015 conference has been a useful occasion to stimulate discussion, further the understanding of heat transfer and related phenomena, present the state-of-the-art of some topics, discuss emerging trends and promote collaborations. We hope this issue will maintain and extend some of these features. A special thank you is due to the Organizing and Scientific Committees, to the sponsors and to all the participants.

  4. UIT Observations of Early-Type Galaxies and Analysis of the FUSE Spectrum of a Subdwarf B Star

    NASA Technical Reports Server (NTRS)

    Ohl, Raymond G.; Krebs, Carolyn (Technical Monitor)

    2001-01-01

    This work covers Ultraviolet Imaging Telescope (UIT) observations of early-type galaxies (155 nm) and Far Ultraviolet Spectroscopic Explorer (FUSE) spectra of a Galactic subdwarf B star (sdB). Early UV space astronomy missions revealed that early-type galaxies harbor a population of stars with effective temperatures greater than that of the main sequence turn-off (about 6,000 K) and UV emission that is very sensitive to characteristics of the stellar population. We present UV (155 nm) surface photometry and UV-B color profiles for 8 E and SO galaxies observed by UIT. Some objects have de Vaucouleurs surface brightness profiles, while others have disk-like profiles, but we find no other evidence for the presence of a disk or young, massive stars. There is a wide range of UV-B color gradients, but there is no correlation with metallicity gradients. SdB stars are the leading candidate UV emitters in old, high metallicity stellar populations (e.g., early-type galaxies). We observed the Galactic sdB star PG0749+658 with FUSE and derived abundances with the aim of constraining models of the heavy element distribution in sdB atmospheres. All of the elements measured are depleted with respect to solar, except for Cr and Mn, which are about solar, and Ni, which is enhanced. This work was supported in part by NASA grants NAG5-700 and NAG5-6403 to the University of Virginia and NAS5-32985 to Johns Hopkins University.

  5. The MAR databases: development and implementation of databases specific for marine metagenomics.

    PubMed

    Klemetsen, Terje; Raknes, Inge A; Fu, Juan; Agafonov, Alexander; Balasundaram, Sudhagar V; Tartari, Giacomo; Robertsen, Espen; Willassen, Nils P

    2018-01-04

    We introduce the marine databases; MarRef, MarDB and MarCat (https://mmp.sfb.uit.no/databases/), which are publicly available resources that promote marine research and innovation. These data resources, which have been implemented in the Marine Metagenomics Portal (MMP) (https://mmp.sfb.uit.no/), are collections of richly annotated and manually curated contextual (metadata) and sequence databases representing three tiers of accuracy. While MarRef is a database for completely sequenced marine prokaryotic genomes, which represent a marine prokaryote reference genome database, MarDB includes all incomplete sequenced prokaryotic genomes regardless level of completeness. The last database, MarCat, represents a gene (protein) catalog of uncultivable (and cultivable) marine genes and proteins derived from marine metagenomics samples. The first versions of MarRef and MarDB contain 612 and 3726 records, respectively. Each record is built up of 106 metadata fields including attributes for sampling, sequencing, assembly and annotation in addition to the organism and taxonomic information. Currently, MarCat contains 1227 records with 55 metadata fields. Ontologies and controlled vocabularies are used in the contextual databases to enhance consistency. The user-friendly web interface lets the visitors browse, filter and search in the contextual databases and perform BLAST searches against the corresponding sequence databases. All contextual and sequence databases are freely accessible and downloadable from https://s1.sfb.uit.no/public/mar/. © The Author(s) 2017. Published by Oxford University Press on behalf of Nucleic Acids Research.

  6. U.S. EPA, Pesticide Product Label, NALCO 7330, 12/22/2000

    EPA Pesticide Factsheets

    2011-04-14

    ... D.in!: pre.pllv • Ia." 'IntUit' ttt MUtu, ,thth sotu in or, if thtse iTt no ... il ..... it h." , .. tili ... f Nallt. Avoid Ilcoh.1. C.ll • ,.,.Iel .. I .... hhl'. N",. ,i" "Vlling bV ... ...

  7. U.S. EPA, Pesticide Product Label, CARBOFURAN TECHNICAL, 07/24/1989

    EPA Pesticide Factsheets

    2011-04-13

    ... on r,{~). Your rel! .. !" Lhp~~ condittons. "'·-cords. llUT IntUIt( CIPf ) "f'!"lf'!~~ u. ~"'w.:t:rr1~. Jr. Product r4ana

  8. 77 FR 27102 - Proposed Collection; Comment Request

    Federal Register 2010, 2011, 2012, 2013, 2014

    2012-05-08

    ..., Copies Available From: Securities and Exchange Commission, Office of Investor Education and Advocacy... the UIT. Absent the requirement to disclose all material information in reports, investors would be... the securities industry might be adversely affected. Requiring the submission of these reports to the...

  9. 76 FR 69301 - Submission for OMB Review; Comment Request

    Federal Register 2010, 2011, 2012, 2013, 2014

    2011-11-08

    ... management companies (``mutual funds''), unit investment trusts (``UITs'') or face-amount certificate companies (collectively, ``funds'') deemed to have registered an indefinite amount of securities to file... sold by funds that accompanies the payment of registration fees with respect to the securities sold...

  10. Urinary Concentrations and Antibacterial Activities of Nitroxoline at 250 Milligrams versus Trimethoprim at 200 Milligrams against Uropathogens in Healthy Volunteers

    PubMed Central

    Münch, Fabian; Pilatz, Adrian; Bärmann, Birte; Weidner, Wolfgang; Wagenlehner, Christine M.; Straubinger, Marion; Blenk, Holger; Pfister, Wolfgang; Kresken, Michael; Naber, Kurt G.

    2014-01-01

    Because of the increasing bacterial resistance of uropathogens against standard antibiotics, such as trimethoprim (TMP), older antimicrobial drugs, such as nitroxoline (NTX), should be reevaluated. This randomized crossover study investigated the urinary concentrations of parent drugs and their metabolites and their antibacterial activities (urinary inhibitory titers [UITs] and urinary bactericidal titers [UBTs]) against uropathogens at three different urinary pH values within 24 h in six healthy volunteers after a single oral dose of NTX at 250 mg versus TMP at 200 mg. In three additional volunteers, urinary bactericidal kinetics (UBK) were studied after oral administration of NTX at 250 mg three times a day. The mean urinary concentrations of NTX and NTX sulfate in 24 h were 0.012 to 0.507 mg/liter and 0.28 to 27.83 mg/liter, respectively. The mean urinary concentrations of TMP were 18.79 to 41.59 mg/liter. The antibacterial activity of NTX was higher in acidic urine than in alkaline urine, and that of TMP was higher in alkaline urine than in acidic urine. The UITs and UBTs of NTX were generally lower than those of TMP except for a TMP-resistant Escherichia coli strain, for which NTX showed higher UITs/UBTs than did TMP. UBK showed mainly bacteriostatic activity of NTX in urine. NTX exhibits mainly bacteriostatic activity and TMP also shows bactericidal activity in urine against susceptible strains. NTX is a more active antibacterial in acidic urine, and TMP is more active in alkaline urine. The cumulative effects of multiple doses or inhibition of bacterial adherence could not be evaluated. (This study has been registered at EudraCT under registration no. 2009-015631-32.) PMID:24217699

  11. 77 FR 41460 - Submission for OMB Review; Comment Request

    Federal Register 2010, 2011, 2012, 2013, 2014

    2012-07-13

    ..., Copies Available From: Securities and Exchange Commission, Office of Investor Education and Advocacy... of the UIT. Absent the requirement to disclose all material information in reports, investors would... confidence in the securities industry might be adversely affected. Requiring the submission of these reports...

  12. 75 FR 45179 - Virtus Opportunities Trust, et al.; Notice of Application

    Federal Register 2010, 2011, 2012, 2013, 2014

    2010-08-02

    ... Opportunities Trust, et al.; Notice of Application Date: July 27, 2010. AGENCY: Securities and Exchange... of other registered open-end management investment companies and unit investment trusts (``UITs... under common control with PVA. Applicants: (a) Virtus Opportunities Trust (the ``Trust''), including the...

  13. The ultraviolet-bright stars of Omega Centauri, M3, and M13

    NASA Technical Reports Server (NTRS)

    Landsman, Wayne B.; O'Connell, Robert W.; Whitney, Jonathan H.; Bohlin, Ralph C.; Hill, Robert S.; Maran, Stephen P.; Parise, Ronald A.; Roberts, Morton S.; Smith, Andrew A.; Stecher, Theodore P.

    1992-01-01

    Two new UV-bright stars detected within 2 arcmin of the center of Omega Cen are spectroscopically investigated with the short-wavelength spectrograph of the IUE. The IUE spectra of the UV-bright stars UIT-1 and UIT-2 in the core of Omega Cen superficially resemble those of Population I mid-B stars. The absorption lines of the core UV-bright stars are significantly weaker than in Population I stars, consistent with their membership in the cluster. Synthetic spectra calculated from low-metallicity Kurucz model stellar atmospheres are compared with the spectra. These objects are insufficiently luminous to be classical hydrogen-burning post-AGB stars. They may be evolved hot horizontal branch stars which have been brightened by more than 3 mag since leaving the zero-age horizontal branch. It is inferred from the spectra and luminosity of the core UV-bright stars that similar objects could provide the source of the UV light in elliptical galaxies.

  14. Hypoglycemic effects of cocoa (Theobroma cacao L.) autolysates.

    PubMed

    Sarmadi, Bahareh; Aminuddin, Farhana; Hamid, Muhajir; Saari, Nazamid; Abdul-Hamid, Azizah; Ismail, Amin

    2012-09-15

    Fat, alkaloid and polyphenol contents of two clones of cocoa (UIT1 and PBC 140) were removed and the remaining powder was autolyzed at pH 3.5 and 5.2. Based on the results, autolysates of UIT produced at pH 3.5 exhibited the highest ability to inhibit α-amylase activity. However, no α-glucosidase inhibition activity was observed under the conditions specified. Autolysates produced under pH 3.5 caused the highest amount of insulin secretion. In streptozotocin-diabetic rats, all cocoa autolysates significantly decreased blood glucose at 4h. To assure that the results from the assays were not due to the polyphenols of cocoa autolysates qualitative and quantitative tests were applied. According to their results cocoa autolysates were found to be free from polyphenols. Analysis of amino acid composition revealed that cocoa autolysates were abundant in hydrophobic amino acids. It can be suggested that besides other compounds of cocoa, its peptides and amino acids could contribute to its health benefits. Copyright © 2012 Elsevier Ltd. All rights reserved.

  15. 30 Doradus - Ultraviolet and optical stellar photometry

    NASA Technical Reports Server (NTRS)

    Hill, Jesse K.; Bohlin, Ralph C.; Cheng, Kwang-Ping; Fanelli, Michael N.; Hintzen, Paul; O'Connell, Robert W.; Roberts, Morton S.; Smith, Andrew M.; Smith, Eric P.; Stecher, Theodore P.

    1993-01-01

    Ultraviolet Imaging Telescope (UIT) UV magnitudes in four bands, together with optical B magnitudes, are presented for up to 314 early-type stars located in a 9.7 x 9.7 arcmin field centered on R136. The magnitudes have an rms uncertainty estimated at 0.10 mag from a comparison between the UIT magnitudes and the IUE spectra. Spectral types and E(B-V) color excesses are estimated. The mean color excesses following the two extinction curves agree well with the predictions of the two-component extinction model of Fitzpatrick and Savage (1984). However, the degree of nebular extinction is found to vary systematically by large amounts over the 30 Dor field. The minimum of nebular extinction in the central parts of the nebula suggests that dust has been expelled from this region by stellar winds. It is suggested that the form of the UV extinction curve can be understood as a consequence of the evolutionary state of the stellar population responsible for making the dust grains.

  16. Fatigue behavior of welded connections enhanced with ultrasonic impact treatment (UIT) and bolting.

    DOT National Transportation Integrated Search

    2008-11-01

    A common problem in bridges employing welded steel girders is development of fatigue cracks at the ends of girder coverplates. Fatigue cracks tend to form at the toes of the transverse welds connecting a coverplate to a girder flange since this detai...

  17. 76 FR 54819 - Proposed Collection; Comment Request

    Federal Register 2010, 2011, 2012, 2013, 2014

    2011-09-02

    ... (``mutual funds''), unit investment trusts (``UITs'') or face-amount certificate companies (collectively, ``funds'') deemed to have registered an indefinite amount of securities to file, not later than 90 days... 274.24) with the Commission. Form 24F-2 is the annual notice of securities sold by funds that...

  18. 75 FR 11585 - Lincoln Variable Insurance Products Trust, et al.; Notice of Application

    Federal Register 2010, 2011, 2012, 2013, 2014

    2010-03-11

    ...] Lincoln Variable Insurance Products Trust, et al.; Notice of Application March 5, 2010. AGENCY: Securities... registered open-end management investment companies and unit investment trusts (``UITs'') that are within and...: Lincoln Variable Insurance Products Trust (``Trust'') and Lincoln Investment Advisors Corporation...

  19. Scatterometry

    NASA Astrophysics Data System (ADS)

    Stoffelen, Adrianus Cornelis Maria

    1996-10-01

    Een veelheid aan meteorologische metingen is dagelijks beschikbaar. De meeste van deze waarnemingen bevinden zich echter boven land, en met name windwaarnemingen boven de (Noord Atlantische) oceaan zijn schaars. Bij een westelijke luchtstroming is dit een duidelijke beperking voor de weers- en golfverwachtingen ten behoeve van Nederland. Juist dan is het gevaar voor bijvoorbeeld storm of overstroming het grootst. Ook in het aardse klimaatsysteem speelt de wind aan het oppervlak een grote rol en is de belangrijkste factor voor de aandrijving van de oceaancirculatie. De oceaancirculatie op zijn beurt is cruciaal voor de verschijnselen die samenhangen met bijvoorbeeld El Niño. Dit proefschift gaat over het scatterometer instrument dat vanuit de ruimte, zelfs onder een wolkendek, nauwkeurige en betrouwbare informatie geeft over de wind aan het oceaanoppervlak met een hoge mate van ruimtelijke consistentie. Tijdens de tweede wereldoorlog werden radars aan boord van schepen veelvuldig gebruikt voor de opsporing van vijandige vaartuigen. Hierbij werd vastgesteld dat de detectie slechter werd naarmate de wind aan het zeeoppervlak groter was. Proefondervindelijk was hiermee het principe van een wind scatterometer aangetoond. Al snel ontwikkelde zich dan ook de idee de wind aan het zeeoppervlak te meten met behulp van radar. Vanuit een vliegtuig of een satelliet word dan een microgolfbundel onder een schuine hoek naar het zeeoppervlak gestuurd. De microgolfstraling, met gewoonlijk een golflengte van enkele centimeters, wordt verstrooid aan het ruwe oppervlak, en een klein gedeelte van de uitgezonden puls keert terug naar het detectorgedeelte van de scatterometer. Het fysische fenomeen van belang voor de werking van de scatterometer is de aanwezigheid van zogeheten capillaire gavitatiegolven op het zeeoppervlak. Deze golven hebben een golflengte van enkele centimeters en reageren vrijwel instantaan op de sterkte van de wind. De verstrooiing van microgolven is op zijn beurt weer sterk afhankelijk van de amplitude van de capillaire golven. Bovendien blijken de capillaire golfjes over het algemeen gericht in lijn met de windrichting. Aldus bestaat er een verband tussen de hoeveelheid teruggestrooide energie en de windsterkte en -richting op enige hoogte. Een scatterometer instrument wordt zo ontworpen dat uit diverse metingen van het teruggestrooide vermogen, windsterkte en -richting afgeleid kunnen worden. Deze metingen kunnen dan eenvoudig vergeleken worden met bestaande windgegevens van boeien, schepen en weermodellen ter calibratie en validatie.?SAMENVATTING viii Overzicht In de loop der jaren zijn scatterometer instrumenten aan boord van verscheidene satellieten gelanceerd. De scatterometers op de ERS-1 en ERS-2 ("European Remote-sensing Satellite") hebben de langste staat van dienst en zijn sinds 1991 operationeel. Deze scatterometers (die identiek zijn) hebben ieder drie antennes, waarmee het oceaanoppervlak in drie verschillende richtingen bemeten wordt. Een punt op het aardoppervlak wordt eerst door de naar voren gerichte bundel belicht, dan door de naar opzij gerichte bundel, en als laatste door de naar achteren gerichte bundel. De drie metingen, verder kortweg aangeduid als trits, kunnen tegen elkaar worden uitgezet, hetgeen resulteert in een ruimtelijk (3D) plaatje. Door uitgekiende doorsneden te maken van deze ruimte kan de samenhang van de drie metingen kwalitatief worden bestudeerd. De drie metingen blijken dan inderdaad een sterke samenhang te vertonen die verklaard kan worden uit twee geofysische parameters. De drie metingen liggen namelijk in het algemeen dichtbij een hoornvormig (2D) oppervlak. De lengterichting van de hoorn blijkt voornamelijk te corresponderen met een variërende windsterkte (of ruwheid van de zee), en de kortste omtrek van de hoorn met een variërende windrichting (ofwel oriëntatie van de capillaire golfjes). De karakterisatie en modellering van dit oppervlak heeft geleid tot een aanzienlijke verbetering in de interpretatie van de scatterometer, zoals beschreven is in dit proefschrift. Hierboven is een uiterst simplistisch beeld gegeven van de fysica die van belang is bij de interpretatie van de scatterometer. Het eerste hoofdstuk van dit proefschrift beschrijft in meer detail de fysische modellering van belang bij de interpretatie van de scatterometer metingen. Ten eerste, de topografie van het zeeoppervlak is uitermate gecompliceerd en niet nauwkeurig te beschrijven met eenvoudige mathematische vergelijkingen. De capillaire golven hebben een andere fasesnelheid dan de langere golven en beide hebben hiermee een ingewikkelde dynamische interactie. Bij hogere windsnelheid breken de golven en ontstaan er schuimkoppen, hetgeen de fysische beschrijving verder compliceert. Ten tweede, de interactie van een schuin invallende microgolfbundel met dit gecompliceerde oppervlak is evenmin nauwkeurig te beschrijven. Zowel verstrooiing als reflectie kunnen een rol spelen. Ten derde, over de relatie tussen de amplitude van de capillaire golven en de wind op enige hoogte, laten we veronderstellen 10 m, is in de literatuur niet de overeenstemming tot in het gewenste detail. Bij lage windsnelheid zouden de oppervlaktespanning of variaties in de wind variabiliteit een rol kunnen spelen. Gezien de fysische complexiteit, is het niet verwonderlijk dat voor de interpretatie van scatterometer metingen statistische methoden hun opgang gevonden hebben. Dit proefschrift gaat met name in op deze methoden, en geeft, aan de hand van vijf wetenschappelijke publicaties, een tamelijk volledig beeld van de "state-of-the-art", zoals die bereikt is met de?SAMENVATTING ix ERS scatterometers (ERS-1 vanaf 17 juli 1991 en later ERS-2 vanaf 22 november 1995). Het derde hoofdstuk behandelt de visualisatie van de gemeten tritsen in de 3D meetruimte, de bepaling van de spreiding van de metingen rond het hoornvormige oppervlak, en de schatting van de meest waarschijnlijke "werkelijke" (of ruisvrije) trits bij het hoornvormige oppervlak gegeven de metingen en hun nauwkeurigheid (inversie). De perceptie dat de metingen met grote waarschijnlijkheid dichtbij een hoornvormig oppervlak liggen, vormt essentiële a priori informatie van belang voor de inversie. Een inversieprocedure gestoeld op waarschijnlijkheidstheorie is afgeleid. Verder worden aan de hand van de structuur van het hoornvormige oppervlak indicatoren bepaald, van belang voor de kwaliteitscontrole, instrumentbewaking, en de verdere verwerking van de gegevens. In de appendix wordt een methode besproken die beschrijft hoe, aan de hand van geselecteerde windgegevens en een goed wind-microgolf verband, ofwel transfer functie, de scatterometer verstrooiingsmetingen gecalibreerd kunnen worden boven de oceaan. Het blijkt dat deze calibratie, die per antenne wordt uitgevoerd, uiterst nauwkeurig is, en, wanneer toegepast, in de 3D meetruimte de verdeling van gemeten tritsen gemiddeld dichterbij de door de transfer functie gemodelleerde hoorn brengt. Dit levert een verbetert scatterometer wind product op. De methode was met name van groot belang voor de validatie en calibratie van de ERS-2 scatterometer, voordat de instrumentele calibratie was voltooid. Met behulp van een set windgegevens uit een weermodel en hun geschatte nauwkeurigheden, passend in locatie en tijd bij een set van scatterometer metingen en hun geschatte nauwkeurigheden, kan met quasi-lineaire schattingstheorie ("Maximum Likelihood Estimation") de meest waarschijnlijke wind-microgolf transfer functie worden afgeleid. De niet-lineariteit en onnauwkeurige formulering van de transfer functie, een niet-uniforme verdeling van invoergegevens, en een inaccurate formulering van de geschatte nauwkeurigheid kunnen hier een goed resultaat in de weg staan. Een nieuwe functie, genoemd CMOD4, wordt afgeleid in hoofdstuk IV. Een eerste eis die gesteld wordt aan een transfer functie, is dat het in de 3D meetruimte nauwkeurig bij de gemeten tritsen past. Wanneer de "fit" optimaal is zal het gecombineerde effect van meetonnauwkeurigheid en inversiefout kleiner zijn dan 0.5 m s -1 in de wind vector. CMOD4 blijkt binnen deze fout bij de metingen te passen. Een tweede eis is, dat voor een onafhankelijke gegevensset, het verschil tussen de geïnverteerde scatterometer wind en de bijpassende wind van bijvoorbeeld een weermodel zo klein mogelijk is. In de praktijk blijkt dat deze tweede eis impliciet volgt uit de eerste, maar ook dat de onnauwkeurigheid van de scatterometer wind met name wordt bepaald door de associatie van een locatie op de hoorn met een wind vector. De onnauwkeurigheid in de scatterometer wind kan dan ook goed beschreven worden in het wind domein.?SAMENVATTING x In hoofdstuk V wordt dit laatste verder uitgewerkt, en wordt gestreefd naar een gedetailleerde wind calibratie met behulp van in situ gegevens. Windgegevens bevatten doorgaans een relatief grote onnauwkeurigheid. Het wordt aangetoond dat ijking of regressie van zulke gegevens niet mogelijk is in een vergelijking van twee meetsystemen, tenzij de nauwkeurigheid van één van de twee meetsystemen bekend is. In de praktijk is dit meestal niet zo. Voor deze gevallen wordt een methode voorgesteld die uitgaat van de simultane vergelijking van drie meetsystemen. In dit geval kan zowel de ijking als een foutenmodel voor de drie meetsystemen worden opgelost. Toepassing van de methode laat zien dat de scatterometer wind afgeleid met behulp van CMOD4 ruwweg 5 % te laag is, en de oppervlaktewind van het gebruikte weermodel ongeveer 5 % te hoog. Het hoornvormige oppervlak blijkt te bestaan uit twee nauw samenvallende laagjes. Wanneer de wind een component heeft in de kijkrichting van de middelste microgolfbundel wordt de ene hoorn beschreven, en wanneer de wind een component heeft tegengesteld hieraan, de andere. Uit een trits metingen (met ruis) kan dus in het algemeen niet een unieke windvector worden bepaald. Twee ongeveer tegengestelde oplossingen resulteren. Deze dubbelzinnigheid in de windrichting kan in de praktijk worden opgelost door die oplossing te kiezen die het dichtst bij een korte termijn weervoorspelling ligt. Daarna kunnen eisen worden gesteld aan de ruimtelijke consistentie van het gevonden windvector veld. Zoals beschreven in hoofdstuk V levert zo'n methode de goede oplossing in meer dan 99 % van de gevallen. Zo kan een in het algemeen kwalitatief goed windproduct worden afgeleid uit de ERS scatterometermetingen. In het tweede gedeelte van hoofdstuk V wordt ingegaan op de assimilatie van scatterometergegevens in weermodellen. Voor variationele gegevensassimilatie wordt een methode voorgesteld, waarbij de dubbelzinnige scatterometerwinden worden geassimileerd, en niet direct de terugstrooiingsmetingen. Dit vanwege het feit dat de onzekerheid in de interpretatie van de scatterometer, het best is uit te drukken als een fout in de wind. De projectie van deze fout op de microgolfmetingen is niet-lineair, en daarmee tamelijk moeilijk te verwerken binnen de context van meteorologische variationele gegevensassimilatie. Assimilatie van de dubbelzinnige wind daarentegen is tamelijk recht toe recht aan. De scatterometermetingen leiden tot een duidelijk betere analyse en korte-termijn voorspelling van het windveld boven zee. De bedekking is echter zodanig dat andere windwaarnemingen nog lang een zeer welkome aanvulling zullen zijn. Nieuwe Amerikaanse scatterometers met een grotere bedekking zijn in ontwikkeling (met name QuikSCAT en SeaWinds). Vanwege hun andere geometrie en golflengte is echter eerst ontwikkelwerk nodig om tot een gedegen interpretatie te komen. De in dit proefschrift beschreven methodologie kan een belangrijke rol spelen in de interpretatie van de gegevens van deze scatterometers. De volgende generatie Europese scatterometers (ASCAT genoemd) heeft een?SAMENVATTING xi grote bedekking en de microgolflengte en meetgeometrie van de ERS scatterometers. Hiermee zijn we op termijn verzekerd van een goed scatterometer wind product.?SAMENVATTING xii

  20. 77 FR 57597 - Wells Fargo Funds Trust, et al.; Notice of Application

    Federal Register 2010, 2011, 2012, 2013, 2014

    2012-09-18

    ...] Wells Fargo Funds Trust, et al.; Notice of Application September 12, 2012. AGENCY: Securities and... companies and unit investment trusts (``UITs'') that are within and outside the same group of investment... the Act to invest in certain financial instruments. Applicants: Wells Fargo Funds Trust (``Trust...

  1. 75 FR 33369 - EQ Advisors Trust, et al.; Notice of Application

    Federal Register 2010, 2011, 2012, 2013, 2014

    2010-06-11

    ...] EQ Advisors Trust, et al.; Notice of Application June 4, 2010. AGENCY: Securities and Exchange... trusts (``UITs'') that are within or outside the same group of investment companies, and (b) permit... to invest in certain financial instruments. Applicants: EQ Advisors Trust, AXA Premier VIP Trust...

  2. 75 FR 47320 - Millington Securities, Inc., et al.; Notice of Application

    Federal Register 2010, 2011, 2012, 2013, 2014

    2010-08-05

    ... investment. At such time, the Series also will transmit to the Unaffiliated Underlying Fund a list of the... Unit Investment Trusts (the ``Trust''), on behalf of itself and any future series, and any future... by or under common control with the Depositor) and their respective series (the future UITs, together...

  3. Spacelab

    NASA Image and Video Library

    1990-12-05

    This image shows a part of the Cygnus loop supernova remnant, taken by the Ultraviolet Imaging Telescope (UIT) on the Astro Observatory during the Astro-1 mission (STS-35) on December 5, 1990. Pictured is a portion of the huge Cygnus loop, an array of interstellar gas clouds that have been blasted by a 900,000 mile per hour shock wave from a prehistoric stellar explosion, which occurred about 20,000 years ago, known as supernova. With ultraviolet and x-rays, astronomers can see emissions from extremely hot gases, intense magnetic fields, and other high-energy phenomena that more faintly appear in visible and infrared light or in radio waves that are crucial to deepening the understanding of the universe. The Astro Observatory was designed to explore the universe by observing and measuring the ultraviolet radiation from celestial objects. Three instruments make up the Astro Observatory: The Hopkins Ultraviolet Telescope (HUT), the Ultraviolet Imaging Telescope (UIT), and the Wisconsin Ultraviolet Photo-Polarimetry Experiment (WUPPE). The Marshall Space Flight Center had managment responsibilities for the Astro-1 mission. The Astro-1 Observatory was launched aboard the Space Shuttle Orbiter Columbia (STS-35) on December 2, 1990.

  4. PREFACE: 31st UIT (Italian Union of Thermo-fluid-dynamics) Heat Transfer Conference 2013

    NASA Astrophysics Data System (ADS)

    Vitali, Luigi; Niro, Alfonso; Colombo, Luigi; Sotgia, Giorgio

    2014-04-01

    The annual Conference of the ''Unione Italiana di Termofluidodinamica'' (UIT) aims at promoting cooperation in the field of heat transfer and thermal sciences, by bringing together scientists and engineers working in related areas. The 31st UIT Conference was held in Moltrasio (Como), Italy, 25-27 June, 2013 at the Grand Hotel Imperiale. The response has been enthusiastic, with more than 70 quality contributions from 224 authors on heat transfer related topics: natural, forced and mixed convection, conduction, radiation, multi-phase fluid dynamics and interface phenomena, computational fluid dynamics, micro- and nano-scales, efficiency in energy systems, environmental technologies and buildings. To encourage the debate, the Conference Program has scheduled ample poster sessions and invited lectures from the best experts in the field along with a few of the most talented researchers. Keynote Lectures were given by Professor Roberto Mauri (University of Pisa), Professor Lounés Tadrist (Polytech Marseille) and Professor Maurizio Quadrio (Politecnico di Milano). This special volume collects a selection of the scientific contributions discussed during this conference; these works give a good overview of the state-of-the art Italian research in the field of Heat Transfer related topics. I would like to thank sincerely the authors for presenting their works at the conference and in this special issue. I would also like to extend my thanks to the Scientific Committee and the authors for their accurate review process of each paper for this special issue. Special thanks go to the organizing committee and to our sponsors. As a professor of Politecnico di Milano, let me say I am very proud to have been the chair of this conference in the 150th anniversary of my university. Professor Alfonso Niro Details of organizers, sponsors and committees, as well as further information, are available in the PDF

  5. Theories of Notation and Polar Motion I,

    DTIC Science & Technology

    1980-12-01

    relative motions such as ocean currents and winds, as we shall do. For the consideration of such effects see (Munk and Macdonald, 1960, p. 123; Lambeck...n)e ,uite general and niot irestricted to a solid body. In Fact, we na~it also in toe Poi ncar model . The equation K 12-1:: no;s the exponencial

  6. 78 FR 21422 - TSC Distributors LLC and TSC UITS; Notice of Application

    Federal Register 2010, 2011, 2012, 2013, 2014

    2013-04-10

    ... purchase Units on the secondary market at the current public offering price plus a front-end sales charge... Units are offered to the public through the Depositor and dealers at a price which, during the initial... front'' (i.e., at the time an investor purchases the Units). The DSC would be collected subsequently in...

  7. 75 FR 64071 - Basis Reporting by Securities Brokers and Basis Determination for Stock

    Federal Register 2010, 2011, 2012, 2013, 2014

    2010-10-18

    ... Determination--Average Basis Method a. Definition of Dividend Reinvestment Plan i. Acquisition of Stock... this provision and allow all UITs that elect to be treated as RICs to use the average basis method. The... served to limit the average basis method to stock in a DRP, the final regulations provide that, for...

  8. Online Proctored versus Unproctored Low-Stakes Internet Test Administration: Is There Differential Test-Taking Behavior and Performance?

    ERIC Educational Resources Information Center

    Rios, Joseph A.; Liu, Ou Lydia

    2017-01-01

    Online higher education institutions are presented with the concern of how to obtain valid results when administering student learning outcomes (SLO) assessments remotely. Traditionally, there has been a great reliance on unproctored Internet test administration (UIT) due to increased flexibility and reduced costs; however, a number of validity…

  9. 75 FR 1090 - Submission for OMB Review; Comment Request

    Federal Register 2010, 2011, 2012, 2013, 2014

    2010-01-08

    ....C. 80a-8(b)). Form N-8B-2 requires disclosure about the organization of a UIT, its securities, the..., Washington, DC 20549-0213. Extension: Form N-8B-2; SEC File No. 270-186; OMB Control No. 3235-0186. Notice is... a request for extension of the previously approved collection of information discussed below. Form N...

  10. Experimental research on microhardness and wear resistances of pure Cu subjected to surface dynamic plastic deformation by ultrasonic impact

    NASA Astrophysics Data System (ADS)

    Chen, Zhaoxia; He, Yangming

    2018-04-01

    Dynamic plastic deformation (DPD) has been induced in the surface of pure Cu by ultrasonic impact treating (UIT) with the varied impact current and coverage percentage. The microstructures of the treated surface were analyzed by a scanning electron microscope (SEM). And the wear resistance of pure Cu was experimentally researched both with the treated and untreated specimens. The effect of DPD on the hardness was also investigated using microhardness tester. The results show that the grains on the top surfaces of pure Cu are highly refined. The maximum depth of the plastic deformation layer is approximately 1400 µm. The larger the current and coverage percentage, the greater of the microhardness and wear resistance the treated surface layer of pure Cu will be. When the impact current is 2 A and coverage percentage is 300%, the microhardness and wear resistance of the treated sample is about 276.1% and 68.8% higher than that of the untreated specimen, respectively. But the properties of the treated sample deteriorate when the UIT current is 3 A and the coverage percentage is 300% because of the formation of a new phase forms in the treated surface.

  11. SBMLmod: a Python-based web application and web service for efficient data integration and model simulation.

    PubMed

    Schäuble, Sascha; Stavrum, Anne-Kristin; Bockwoldt, Mathias; Puntervoll, Pål; Heiland, Ines

    2017-06-24

    Systems Biology Markup Language (SBML) is the standard model representation and description language in systems biology. Enriching and analysing systems biology models by integrating the multitude of available data, increases the predictive power of these models. This may be a daunting task, which commonly requires bioinformatic competence and scripting. We present SBMLmod, a Python-based web application and service, that automates integration of high throughput data into SBML models. Subsequent steady state analysis is readily accessible via the web service COPASIWS. We illustrate the utility of SBMLmod by integrating gene expression data from different healthy tissues as well as from a cancer dataset into a previously published model of mammalian tryptophan metabolism. SBMLmod is a user-friendly platform for model modification and simulation. The web application is available at http://sbmlmod.uit.no , whereas the WSDL definition file for the web service is accessible via http://sbmlmod.uit.no/SBMLmod.wsdl . Furthermore, the entire package can be downloaded from https://github.com/MolecularBioinformatics/sbml-mod-ws . We envision that SBMLmod will make automated model modification and simulation available to a broader research community.

  12. Astro-1 Image Taken by Ultraviolet Imaging Telescope

    NASA Technical Reports Server (NTRS)

    1990-01-01

    This image shows a part of the Cygnus loop supernova remnant, taken by the Ultraviolet Imaging Telescope (UIT) on the Astro Observatory during the Astro-1 mission (STS-35) on December 5, 1990. Pictured is a portion of the huge Cygnus loop, an array of interstellar gas clouds that have been blasted by a 900,000 mile per hour shock wave from a prehistoric stellar explosion, which occurred about 20,000 years ago, known as supernova. With ultraviolet and x-rays, astronomers can see emissions from extremely hot gases, intense magnetic fields, and other high-energy phenomena that more faintly appear in visible and infrared light or in radio waves that are crucial to deepening the understanding of the universe. The Astro Observatory was designed to explore the universe by observing and measuring the ultraviolet radiation from celestial objects. Three instruments make up the Astro Observatory: The Hopkins Ultraviolet Telescope (HUT), the Ultraviolet Imaging Telescope (UIT), and the Wisconsin Ultraviolet Photo-Polarimetry Experiment (WUPPE). The Marshall Space Flight Center had managment responsibilities for the Astro-1 mission. The Astro-1 Observatory was launched aboard the Space Shuttle Orbiter Columbia (STS-35) on December 2, 1990.

  13. Shock and Vibration Bulletin No. 9

    DTIC Science & Technology

    1948-04-14

    nil liseomids S& P, THU󈧵’J, tM: Xaforrlng td the up to about 10 milliseconds anrd, An iiome error* onjondared by mm~lng tho resonaent exceptional...nfel ras 7tl 20 Comfide-stia - CAME".) 3RAXiM TOANSM $S104 It. /. MOl ,,,..,’t ."’ - P 7 04 OSCILLATOR UIT Flj . 5 MX 6-Trace CRO 7ývpe IB Layout of

  14. Unintentional Insider Threats: Social Engineering

    DTIC Science & Technology

    2014-01-01

    or business partner (2) who has or had authorized access to an organization’s network, system, or data and who, (3) through action or inaction...features. The accumulation and analysis of incident statistics will also ultimately help stakeholders prioritize different types of UIT threats and...is (1) a current or former employee, contractor, or business partner (2) who has or had authorized access to an organization’s network, system, or

  15. Results from the Ultraviolet Imaging Telescope on the Astro-2 Mission

    NASA Astrophysics Data System (ADS)

    Stecher, T. P.; Bohlin, R. C.; Neff, S. G.; O'Connell, R. W.; Roberts, M. R.; Smith, A. M.

    1995-03-01

    The solar-blind UIT camera with a CsI cathode obtained 722 frames with a cumulative exposure time of 260705 seconds during the March 1995 Astro-2 mission of Space Shuttle Endeavour. Filters were used to isolate selected bandpasses in the range 1200-1800 Angstroms, over the 40 arcmin field of view. Spatial resolution on most of the images is about 3 arcsec. Calibrated data, converted to machine-readable form, are under analysis and several posters on these investigations are presented in the Astro-2 poster session at this meeting (a first look at the UIT observations of Omega Cen, M31, and the Cygnus Loop is further elaborated here). UIT imagery of 20 spiral galaxies was obtained as part of a Guest Investigator program (Wendy Freedman et al.). UV imaging suppresses the red stellar population as expected and enhances the appearance of tracers of recent star formation. Known \\hii regions in these galaxies are made apparent through the scattering of stellar ultraviolet light by interstellar dust; typically their shapes differ from those seen in \\ha. A radial color gradient investigation will be delayed until ground observations can be made as the long-wavelength camera failed on launch and only the 1520 Angstroms and 1620 Angstroms images were made. The far-UV (1520 Angstroms) features are detected well beyond the Holmberg radius. UV/visible color-magnitude diagrams will be made as they were for the data from Astro-1. Our deepest images of the Magellanic Clouds reveal a rich field of luminous clusters and stars that are being searched for UV counterparts of the known x-ray sources in the photographed areas. The observed stars in the Clouds will be used to determine the current mass function. The respective contributions of nebular and stellar UV light in reflection nebulae are will be studied as several nebulae were observed with differing geometries and will provide interesting results on the far-UV albedo and phase function of nebular dust. A dozen globular and open clusters were imaged.

  16. ERDC MSRC Resource. High Performance Computing for the Warfighter. Fall 2006

    DTIC Science & Technology

    2006-01-01

    to as Aggregated Combat Modeling, putting us at the campaign level).” Incorporating UIT within DAC The DAC system is written in Python and uses...API calls with two Python classes, UITConnectionFactory and UITConnection. UITConnectionFactory supports Kerberos authentication and establishes a...API calls within these Python classes, we insulated the DAC code from the Python SOAP interface requirements and details of the ERDC MSRC Resource

  17. An Analysis of Recruit Training Attrition in the U.S. Marine Corps

    DTIC Science & Technology

    1978-02-01

    direct ir-licatimns for tt.e recruit-r..t. sel)(tion, arJ organizational entry process . To the extent potential recr-uits can :e given accurate...assimilation-socialization process (Graen, 1976) as it influences these and other variables and as this process relates to attrition. Summnarizing the...considers both individual and organizational variables; c) Combined with a longitudinal design, it permits assessment of the learning-socialization process

  18. Squad Weapons Analytical Trainer (SWAT) M-16 Version.

    DTIC Science & Technology

    1980-07-01

    TIERSSTRRT PROCEDURE EXTRL; /* STRT 8253 REGISTERS 8/ 1 2 END; 19 1 CLOCKSM ) PROCEDURE AD RESS EXTERNt /8 REIS CLOCK FOR TAWOE SHOTS S28 2 END; 21 1...589 OIL A, R5 ;CRENE EECTEt, RETUN CODE 02E2 AC 510 NOV R4,n ASTORE M 3 3459 511 COLL PtUIT ;GET FRON PAE I Af BYTE WICH WILL 5L2 AK THE M ( BIT SET

  19. Leadership Theory and Practice: Where East Meets West

    DTIC Science & Technology

    1989-06-01

    leadership concepts can be assimilated to good advantage by the Chinese. and what additional research ei’forts for the armed forces of the Republic... research ef- forts for the armed forces of the Republic of China should be undertaken. The this7s "su ,, L.,uitJ _ description of the eCHO sampiing...29 A. THE ECHO SAMPLING TECHNIQUE ....................... 29 B. THE MCBER SAMPLING METHOD .. ....................... 33 IV. CRITICAL

  20. Galaxy Morphology From the UV to the FIR: An Intercomparison of Recent Observations From Space With New Radiative Transfer Models

    NASA Technical Reports Server (NTRS)

    (CIT), Barry Madore

    1995-01-01

    We will present the latest multiwavelength observations of spiral galaxies made from space and from the ground covering the electromagnetic spectrum from the far ultraviolet (ASTRO-2 UIT observations) through the optical, and out to the far infrared (IRAS). Comparisons with recent theoretical models for the radiative transfer of stellar light through a three-dimensional dusty galaxy will be presented.

  1. Propagation of Sound Through the Atmosphere: Effects of Ground Cover

    DTIC Science & Technology

    1978-06-19

    Over Simulated Ground Cover", J. Acoust. Soc. Am. 49, 1069-1075 ( 1971 ). 8 J. . . Piercy, T. F. W. Embleton, and L. C. Sutherland, "A Review of Noise...FlPST., AM KALL C AND SUBMOUTINL NAIAE *𔃺’t.ATfl"v hISTTAD 0t "COPPIS?". C PANG4N IS Ali tUIT 01* IAANG4Kp [XCLUSVIfo UT NTt.14VENINC, Fj)ITSq C RANG

  2. DURIP: A Confocal Imaging System for Ultra-Fast Three-Dimensional Transport Studies in Thermal Management Applications

    DTIC Science & Technology

    2011-12-01

    Transport Phenomena and Thermal Management Applications,” Proceedings of the XXVIII UIT Heat Transfer Conference, Brescia, Italy, June 21-23, 2010...measurements in microscale systems. The integrated confocal microscope system is a critical component to obtain understanding of fluid- heat ...objective of this work was to develop a high speed three-dimensional (3D) confocal imaging system to study coupled fluidic and heat transport

  3. E-3A EMP Evaluation Program.

    DTIC Science & Technology

    1980-01-01

    34OGRAh~g"NT. PROJECT, TASI( AREA & YRIC UIT NUMBERS EG&G, Inc. 9733 Coors Road NW 67I/7Z~i Albuqueroue,_NM_87114 _____________ 11. CONTROLLING OFFICE...Report) III. SUPPLEMENTARY NOTES III. KCy WORDS (Centingnpo r. everse wooe Ii noeew ayE ~Eeatly by’ b1euk nuabr) E- 3A Airborne Warning and Control ... CONTROL PROCEDURE ANALYSIS . 73 1 L -.... TABLE OF CONTENTS (Continued) Page SECTION V TEST ACTIVITIES .... .............. . 81 1. PRE-PULSE

  4. SRA (Short Range Aids to Navigation) Resource Management: Measures of Effectiveness.

    DTIC Science & Technology

    1986-09-01

    invest ’ ’-" in R&D and technological innovation. uit Measures of effectiveness developed under the first task deal primarily with safety...illustratve example presented in Chapter 5. A project of this nature and complexity could not be carried out without the assistance and support of others. A...helping the project attain its goals. Foremost is Mr. Karl R. Schroeder, Short Range Aids to Navigation Section Chief in the USCG

  5. Development of Short Gate FET’s.

    DTIC Science & Technology

    1983-12-01

    Electrical Engineering AREA OK UIT NUMBERS S School of Engineering, Howard University 61102F 2300 Sixth St. N.W. Washington D.C. 20059 2305/Cl CITROLLING... Howard University Washington# D.C. 20059 64 04 24 021 RESEARCH OBJECTIVES The principal objective of this research is to try to under- stand the... Howard University Washington, D.C. 20059 (202)636-6684 James Comas Naval Research Laboratory, Code 6823 Washington, D.C. 20375 (202)767-3097

  6. On the Dynamics of Space Plasma

    DTIC Science & Technology

    1992-09-01

    proipagation characteristics uit lE6t propeittecs of wave-particle plasma interactions (Fejer. 19791. wcaves in nonuniform plasmas. If the incident frequency w...arlilauinei by solvinug lair thc Ilirirkct iuatti.ii t1 1), io!17 41) 4XlA~iis~a t alialictiiii ielaiolai (1Ideuaaaau 19611 We~ 111.1N cliaiii ilvC...Sileviteli ,iid E.. Villaloit. (enter lair lElectriuuutigneniic Goitiiiuui. V. L., rhra PrriPouguurnrn "Ii/ienugu- Waves ii Rcseat ch. Northeaster

  7. Study of Laser Created Metal Vapour Plasmas.

    DTIC Science & Technology

    1981-09-01

    ance saturation could lead to extensive ground Zcvei burnout of certain kinds of atoms or ions and that this could lead to the creation of a ground...level FORM DD I JAN ", 1473 UNCLASSIFIED SECURITY CLASSIFICATION OF THIS PACE ’l hen Dota Fnt ’UNCLASSIFIFD SS ~eUItTY CLASSIFICATION OF THIS PAqE(W"Sef...vapours. Preliminary calculations have suggested that laser resonance saturation could lead to extensive ground level burnout of certain kinds of

  8. Preparation and Analysis of Samples for the Third Round Robin Verification Exercise

    DTIC Science & Technology

    1992-07-01

    Hooge 34 Lid instituuts Advies Raad PML Prof. dr. U.A. Th. Brinkman 35 Directeur van het Medisch Biologisch Laboratorium TNO Proft dr. W.R.F. Notten 36...1991 werd uitgevoerd, heeft het Prins Maurits Laboratorium TNO de monsters aangemaakt die bestonden uit rubber, verf en beton. Deze materialen, die...Maurits Laboratorium TNO Chemische Research Prof. dr. G. Dijksrra 10 HBur. NBC-DMKIJOMATIKIO In. A.A.M. Slagveer 11 Lid van de Contact Cominissie NBC

  9. Geluidsexpositie bij gebruik van CEP door F-16 crewchiefs (Sound Exposure Level of F-16 Crew Chiefs Using Communications Earplugs)

    DTIC Science & Technology

    2008-03-01

    Communications Earplugs Auteur (s) dr. ir. M.M.J. Houben Programmanummer Projectnummer J.A. Verhave 032.13072 F.W.M. Geurtsen Rubricering rapport Program...de communicatie kiest men voor een geluidniveau dat luider is dan het waargenomen omgevingsgeluid. In theorie kan bet totale geluidsexpositieniveau...Afdelingshoofd Auteur TNO-rapport I TNO-DV 2008 A054 Bijlage A 1 1/3 A Simulatie Simulatie-omgeving Uit een opname gemaakt op Vhiegbasis Volkel hebben

  10. Applications of Known Quantitative Techniques for Developing Airborne ASW Crew Performance Criteria,

    DTIC Science & Technology

    1967-07-01

    environmental foot tunnel enable’s accurate tests to be conducted under specifications, controlled conditions, MA Ch I N E ( ‘OMI ’l ’F t T ION SERVICES C...ph~- 51 olo gical nioni tur ing equ ip— cc i dt’ a r t e ’t~ cci C ~~ii ’ ri iue ’nt s can hi’ ~‘onc1ui-ted u ndc r V a t t e s t s nie ’ni ; I

  11. Les objectifs des « réseaux futurs » vus par l'UIT

    NASA Astrophysics Data System (ADS)

    Mur, Jean-Michel

    2017-12-01

    Pour faire face à l'explosion de la demande en débits et la diversité des services souhaités, l'Union internationale des télécommunications a développé le concept de « Future Networks » (réseaux futurs) visant à remplacer les actuels « réseaux de prochaine génération » (Next Generation Networks). Panorama des principaux objectifs fixés à ces futurs réseaux de communication…

  12. Optimalisatie Draagsysteem (Optimization of the Load Carriage System)

    DTIC Science & Technology

    2008-06-01

    nadelige gevolgen beeft voor de beweeglijkheid. In bet prototype draagsysteem uit figuur 9 ’hangt’ bet scberfwerende vest met kogelwerende platen niet...Soesterberg TNO-rapport wwton T +31 346 35 62 11 TNO-DV 2008 A230 F +31 346 35 39 77Info-DenV@tno.nI Optimalisatie draagsysteem D)atun juni 2008 0 Autcur(s...de draagconstructie. Bij bet ILCS- 11 is gevarieerd met de hoeveelheid afsteuning op heupen en Beschrijving van de werkzaamhleden schouders, alsmede

  13. Modelling of the combustion velocity in UIT-85 on sustainable alternative gas fuel

    NASA Astrophysics Data System (ADS)

    Smolenskaya, N. M.; Korneev, N. V.

    2017-05-01

    The flame propagation velocity is one of the determining parameters characterizing the intensity of combustion process in the cylinder of an engine with spark ignition. Strengthening of requirements for toxicity and efficiency of the ICE contributes to gradual transition to sustainable alternative fuels, which include the mixture of natural gas with hydrogen. Currently, studies of conditions and regularities of combustion of this fuel to improve efficiency of its application are carried out in many countries. Therefore, the work is devoted to modeling the average propagation velocities of natural gas flame front laced with hydrogen to 15% by weight of the fuel, and determining the possibility of assessing the heat release characteristics on the average velocities of the flame front propagation in the primary and secondary phases of combustion. Experimental studies, conducted the on single cylinder universal installation UIT-85, showed the presence of relationship of the heat release characteristics with the parameters of the flame front propagation. Based on the analysis of experimental data, the empirical dependences for determination of average velocities of flame front propagation in the first and main phases of combustion, taking into account the change in various parameters of engine operation with spark ignition, were obtained. The obtained results allow to determine the characteristics of heat dissipation and to assess the impact of addition of hydrogen to the natural gas combustion process, that is needed to identify ways of improvement of the combustion process efficiency, including when you change the throttling parameters.

  14. PREFACE: 32nd UIT (Italian Union of Thermo-fluid-dynamics) Heat Transfer Conference

    NASA Astrophysics Data System (ADS)

    2014-11-01

    The annual Conference of the ''Unione Italiana di Termofluidodinamica'' (UIT) aims to promote cooperation in the field of heat transfer and thermal sciences by bringing together scientists and engineers working in related areas. The 32nd UIT Conference was held in Pisa, from the 23rd to the 25th of June, 2014 in the buildings of the School of Engineering, just a few months after the celebration of the 100th anniversary of the first Institution of the School of Engineering at the University of Pisa. The response was very good, with more than 100 participants and 80 high-quality contributions from 208 authors on seven different heat transfer related topics: Heat transfer and efficiency in energy systems, environmental technologies, and buildings (25 papers); Micro and nano scale thermo-fluid dynamics (9 papers); Multi-phase fluid dynamics, heat transfer and interface phenomena (14 papers); Computational fluid dynamics and heat transfer (10 papers); Heat transfer in nuclear plants (8 papers); Natural, forced and mixed convection (10 papers) and Conduction and radiation (4 papers). To encourage the debate, the Conference Program scheduled 16 oral sessions (44 papers), three ample poster sessions (36 papers) and four invited lectures given by experts in the various fields both from Industry and from University. Keynote Lectures were given by Dr. Roberto Parri (ENEL, Italy), Prof. Peter Stephan (TU Darmstadt, Germany), Prof. Bruno Panella (Politecnico di Torino), and Prof. Sara Rainieri (Universit;aacute; di Parma). This special volume collects a selection of the scientific contributions discussed during this conference. A total of 46 contributions, two keynote lectures and 44 papers both from oral and poster sessions, have been selected for publication in this special issue, after a second accurate revision process. These works give a good overview of the state of the art of Italian research in the field of Heat Transfer related topics at the date. The editors of the volume would like to sincerely thank the authors for presenting their works at the conference and in this special issue. Special thanks are also due to the Scientific Committee, to all the reviewers, and to all the authors for their accurate revision process of each paper for this special issue. Special thanks go to the Organizing Committee, chaired by Prof. Paolo Di Marco. Walter Grassi (Chairman of the Scientific Committee), Alessandro Franco, Nicola Forgione, Daniele Testi - Editors of the Special Issue

  15. Templehof Aprt, Berlin, Germany. Revised Uniform Summary of Surface Weather Observations (RUSSWO)

    DTIC Science & Technology

    1977-09-16

    SEP 16 ga j IS-DOCUMENT HAS BEEN APPROVED FEDERAL BUILDING RIBUTION IS UNLIMITED." SEILN.C OIR-PUBLIC RELEASE AND SALE ; ITS DIS. A H V L E . C R ’"I...ftFRLTI4 MA.7A 1A Y It~rm~ " lATM~ 10911 ITun 11401111 Al L W--ATHfI+ O000-0700 S cOI~iI@UIT SPEED MEAN (KNTS) 1.3 4-6 7*10 11•16 17 -21 22.27 26-33 34.40

  16. Vrouwen bij de Koninklijke Landmacht: Een Onderzoek naar de Maatregelen die het Behoud en de Doorstroom van Vrouwelijke Militairen Verbeteren (Women in the Royal Netherlands Army: Measures for Retention and Career Development)

    DTIC Science & Technology

    2007-02-01

    mannencultuur. Uit onderzoek blijkt dat vrouwelijke BBT-ers (Beroeps Bepaalde Tijd ) zicb goed tbuis voelen bij de (masculiene) organisatiecultuur van...de KL. Zij ervaren bovendien geen benadeling of negatieve bejegening. Vrouwelijke BOT-ers (Beroeps Onbepaalde Tijd ) geven daarentegen wel aan dat zij...arbeid en zorg. Meer tijd voor de thuissituatie, waarbij de werknemner zelf kan beslissen hoe zij deze fijd bet beste kan aanpassen aan de behoefte van

  17. Systematic Review of Uit Parameters on Residual Stresses of Sensitized AA5456 and Field Based Residual Stress Measurements for Predicting and Mitigating Stress Corrosion Cracking

    DTIC Science & Technology

    2014-03-01

    power, 4 mm pin size) at a position in or near the HAZ and a position in the base metal. The areas were electropolished using the “L1” solution as...quality of polish was assessed for each instance of electropolishing . 48 6 . Electrolytic Polishing The Proto Electrolytic Polisher Model 8818-V3...finish, followed by 0.05 μm colloidal silica. After metallography, the samples were electropolished using the Buehler Electromet 4 Electrolytic

  18. A Cold Temperature Evaluation of the Bonding Adhesives Used for the MUST Inflatable Shelters

    DTIC Science & Technology

    1975-04-01

    been known as the US Army Natick Laboratories (NLABS), and the US Army Natick Development Center ( NDC ). AMIN 1W 5Th Whit# WIN~ zD DI• ~kti u...section throughout the test period. The arctic climatic chamber is a closed ci;•uit wind tunnel in which the temperature can be lowered, controlled...and maintained at any level down to -54WC (-65°F). The shelter section was too large to fit in the test section of the tunnel . The shelter had to be

  19. Spotlight on GME/GHSE Supported Research

    DTIC Science & Technology

    2017-12-07

    REPORT TYPE 3. DATES COVERED (From- To) 12/07/2017 Poster 4. TITLE AND SUBTITLE Sa. CONTRACT NUMBER Spotlight on GME/GHSE-Supported Research Sb...Clinical Research Division ., 4t€t.>Jc~"-\\. ~[lJI~IT~&[L IT~W~~UIT@&lYIT©~~ ~~@@~[RJ ~[0@1J[LI1@ 1r (Q)~ @~ An example of a "Parent" 59 MDW/ST R&D Project...ORGANIZATION NAME(S) AND ADDRESS(ES) 8. PERFORMING ORGANIZATION 59th Clinical Research Division REPORT NUMBER 1100 Willford Hall Loop, Bldg 4430 JBSA

  20. Evaluatie Kennistechnologische Ondersteuning bij Diagnose van SEWACO systemen (Projectmanagementplan) (Evaluation of Knowledge Technological Support for Diagnosis of SEWACO Systems (Project Management Plan)

    DTIC Science & Technology

    1991-08-01

    diagnos van SE WACO systmnen/ AD-A245 424111 1fl1,l Niets uit deze uitgave mag warden vermenigvuldligd en/of oPenbaar gemaakt door middel van druk...fotakopie. microfilm of op welks andere whlze dan ook, zonder voorafgaande toeslemming van TNO. Hot ter inzage geven van het TNO-rapport aan direct...belanghebbenden is tegestaan. HYP. vanl OC dt Indian dit rapport in opdracht ward uitgebracht, wordt voor de, rechten en verpiichtingen van opdrachtgever en

  1. Training with Simulated Team Members (Trainen met Gesimuleerde Teamieden).

    DTIC Science & Technology

    1997-11-13

    TEAMTAKEN 9 2.1 Teams 9 2.2 Teamtaken 10 2.3 De individuele deeltaken 11 2.4 De teamcomponent 11 2.5 Motivatie en attitudes 14 3 HET TRAINEN VAN TEAMS 15... 11 Fax 0346 35 39 77 datum 13 november 1997 Alle rechten voorbehouden. A oe a jb Miets uit deze uitgave mag worden vermenigvuldigd en/of openbaar...13 November 1997 7. NUMBER OF PAGES 8. NUMBER OF REFERENCES 9 . TYPE OF REPORT AND DATES COVERED 35 64 Interim 10. TITLE AND SUBTITLE Trainen met

  2. Advanced On-The-Job Training System: User’s Handbook (Sections 10-11). Volume 3

    DTIC Science & Technology

    1990-05-01

    leWd 4. idsodity a ne bety position Quit This Plan Select Option: Z (i)d4L.-tti irman Ifrom List, ()nter Specific S, (q)uit ? I 10-2.-4 0 The AOTS...Print SUperviaima List q. Rit This Plans Select Option: S 10-44 STEP 6: SELECT THE SUPERVISION LIST OPTION. Enter 5 and press 3RETU 30 D RA FT AOTS...training is accomplished by the trainee completing an on-line CAI lesson , while for other tasks, knowledge training is accomplished off line by the trainee

  3. ASTRO-2 Spacelab Instrument Pointing System mission performance

    NASA Technical Reports Server (NTRS)

    Wessling, Francis C., III; Singh, S. P.

    1995-01-01

    This paper reports the performance of the Instrument Pointing System (IPS) that flew on the National Aeronautics and Space Administration (NASA) ASTRO-2 Spacelab mission aboard the Space Shuttle Endeavour in March 1995. The IPS provides a stabilizing platform for the ASTRO-2 instrument payload complement that consists of three main experiments (telescopes). The telescopes observe stellar targets in the universe within the ultraviolet portion of the electromagnetic spectrum that must be observed from beyond the earth's atmospheric filtering effects. The three main experiments for observation are the Hopkins Ultraviolet Telescope (HUT), the Ultraviolet Imaging Telescope (UIT), and the Wisconsin Ultraviolet Photo-Polarimetry Experiment (WUPPE). The HUT uses spectroscopy to obtain the structure and chemical makeup of ultraviolet targets. UIT is responsible for wide field photographing to capture the hidden view of the ultraviolet universe. The WUPPE gathers data on the polarization of the ultraviolet electromagnetic energy coming from the astronomical targets. The capability of IPS enables the experiments to 'see' faint celestial objects. A brief explanation of the IPS is given followed by a review of engineering efforts to improve IPS performance over the ASTRO-1 mission. The main focus of improvements was on enhancing the star acquisition capability through improved guide star selection, lab simulations, computer upgrades, data display systems improvements, and software modifications. A star simulator was developed in the lab to enable IPS to be simulated on the ground pre-mission with flight hardware and software in the loop. The paper concludes with results from the ASTRO-2 mission. The number of targets acquired and the IPS pointing accuracy/stability is reported along with recommendations for the future use of the Instrument Pointing System.

  4. Job Aid Manuals for Phase III-DEVELOP of the Instructional Systems Development Model

    DTIC Science & Technology

    1980-05-01

    well as " men ," are intended to include both the masculine and feminine gender. Any exceptions to this usage will be so noted. Iso 111.1 Specifying...avoid a repetitious use of the terminology, "he/she," the terms, "he," "him," and "his," as well as " men ," are intended to include both the masculine...sefu .11 tn d ui,t sWiuikig Yet pros , e fo pefo, e actte la t t I,, t’s m I tte, ’SO Btacks ste Sntlly. Infl trn men h- been abtlned e t a o -uld

  5. Onderzoek Naar de Bepaling van Wrijvingscoefficienten van een Voertuig uit Uitrolcurves (Research into the Determination of Friction Coefficients of a Vehicle from Deceleration Curves)

    DTIC Science & Technology

    1991-08-01

    en Aemne Vrwaarden Wo OndOrzoeks 8 FE 1 1 opdrchl aT00’ dn wet do bereflende F B 0 1 9 terzake tussen partilon geslOlen dw:Agsu overOerikomStf...Ongemlbric~~d 9 -028 14 :259 wwWmtmd.fl 59w IEEIIIIiiiarabIg𔃽 1 c~ Vrederikkazerle, Geb. InO 03 3.. ~ van den Burchlaal 312 03 173Telefoofl 070-3166394...1ILEIDING 6 2 HET FYSISCHE MODEL 8 3 ONDERZOEK AAN DE DIFFERENTIAALVERGELIJKING 11 3.1 Existentie en uniciteit van ccii oplossing 11 3.2 Continulleit en

  6. STS-35 Astronomy Laboratory 1 (ASTRO-1) in OV-102's payload bay at KSC

    NASA Image and Video Library

    1990-03-20

    STS-35 Astronomy Laboratory 1 (ASTRO-1) is installed in Columbia's, Orbiter Vehicle (OV) 102's, payload bay (PLB) at the Kennedy Space Center (KSC) Orbiter Processing Facility (OPF). On the left, in the aft PLB is the Broad Band X Ray Telescope (BBXRT) mounted on the two axis pointing system (TAPS). In the center, the three ultraviolet telescopes - Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE), the Hopkins Ultraviolet Telescope (HUT), and the Ultraviolet Imaging Telescope (UIT) - are mounted on the instrument pointing system (IPS) and are in stowed position. At the far right is the Spacelab Pallet System (SPS) igloo. View provided by KSC with alternate number KSSC-90PC-421.

  7. Military Assistance and Influence: Some Observations.

    DTIC Science & Technology

    1977-07-20

    I4 Non c ot iss unant I)c tent c anmd NAT O AD A 0 1 3 5 2 2 Deterrence and Detente AD A0 l3979 The Impact uit ( rises on the t v ol uti on of Strategy...24a-. .J “~ .1 .51 ACK T j 4 ~ 5 0 5 0 5 5 C R NuS! & A , ’ r ‘031.1’ .9 .’.., ~A. I, ~.fl tt KJ Of f ,R#I S S E C . ) , , Y R C L ASS,.4 t45. .nJ N...577 ARMY WAR COLL STRAT EGIC STUCIES INST CARLISLE BARRACKS PA FIG 5 /4 UNCLASSIFIED MILITARY ASSISTANCE AND INFLUENCE: SOME OBSERVATIONS.CtJ) JUL 77

  8. UIT: Ultraviolet surface photometry of the spiral galaxy M74 (NGC 628)

    NASA Technical Reports Server (NTRS)

    Cornett, Robert H.; O'Connell, Robert W.; Greason, Michael R.; Offenberg, Joel D.; Angione, Ronald J.; Bohlin, Ralph C.; Cheng, K. P.; Roberts, Morton S.; Smith, Andrew M.; Smith, Eric P.

    1994-01-01

    Ultraviolet photometry, obtained from Ultraviolet Imaging Telescope (UIT) images at 1520 A (far-UV; magnitudes m(152)) and 2490 A (near-UV; magnitudes m(249)), of the spiral galaxy M74 (NGC 628) is compared with H-alpha, R, V, and B surface photometry and with models. M74's surface brightness profiles have a central peak with an exponential falloff; the exponential scale lengths of the profiles increase with decreasing wavelength for the broad-band images. The slope of the continuum-subtracted H-alpha profile is intermediate between those of far-UV and near-UV profiles, consistent with the related origins of H-alpha and UV emission in extreme Population I material. M74's color profiles all become bluer with increasing radius. The (m(152) - m(249)) color as measured by UIT averages near 0.0 (the color of an A0 star) over the central 20 sec radius and decreases from approximately -0.2 to approximately -0.4 from 20 sec to 200 sec. The spiral arms are the dominant component of the surface photometry colors; interarm regions are slightly redder. In the UV, M74's nuclear region resembles its disk/spiral arm material in colors and morphology, unlike galaxies such as M81. No UV 'bulge' is apparent. The m(152) - m(249) colors and models of M74's central region clearly demonstrate that there is no significant population of O or B stars present in the central 10 sec. M74's UV morphology and (m(152) - m(249)) color profiles are similar to those of M33, although M74 is approximately 0.5 mag redder. M81 has a smooth UV bulge which is much redder than the nuclear regions of M74 and M33. M74 is approximately 0.4 mag bluer than M81 in its outer disk, although M81 has bright UV sources only in spiral arms more than 5 kpc from its center. We investigate possible explanations for the color profiles of the galaxies and the differences among the galaxies: abundances; reddening due to internal dust; interplanetary magnetic field (IMF) variations, and the history of formation of the dominant generations of stars. Abundance and IMF variations do not produce large enough m(152) - m(249) or UV - V color differences. Comparing model UV/optical colors with those of M74 shows that M74's disk has undergone significant star formation over the past 500 Myr, and that either the star-formation history or the extinction varies systematically across M74's disk. Comparison of M74, M33, and M81 (UV - V) colors shows that M74 colors range from the bluest of M33's colors to the bluest of M81's. The failure of reddening models to cover the range of colors, and the known abundance range in such material, leads to the conclusion that star-formation history varies significantly as a function of radius in these galaxies, and that such variation is required to explain the range of colors observed in M74, M33, and M81.

  9. Modelling the average velocity of propagation of the flame front in a gasoline engine with hydrogen additives

    NASA Astrophysics Data System (ADS)

    Smolenskaya, N. M.; Smolenskii, V. V.

    2018-01-01

    The paper presents models for calculating the average velocity of propagation of the flame front, obtained from the results of experimental studies. Experimental studies were carried out on a single-cylinder gasoline engine UIT-85 with hydrogen additives up to 6% of the mass of fuel. The article shows the influence of hydrogen addition on the average velocity propagation of the flame front in the main combustion phase. The dependences of the turbulent propagation velocity of the flame front in the second combustion phase on the composition of the mixture and operating modes. The article shows the influence of the normal combustion rate on the average flame propagation velocity in the third combustion phase.

  10. STS-35 ASTRO-1 telescopes documented in OV-102's payload bay (PLB)

    NASA Image and Video Library

    1990-12-10

    STS035-13-008 (2-10 Dec. 1990) --- The various components of the Astro-1 payload are seen backdropped against the blue and white Earth in this 35mm scene photographed through Columbia's aft flight deck windows. Parts of the Hopkins Ultraviolet Telescope (HUT), Ultraviolet Imaging Telescope (UIT) and the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE) are visible on the Spacelab Pallet in the foreground. The Broad Band X-Ray Telescope (BBXRT) is behind this pallet and is not visible in this scene. The smaller cylinder in the foreground is the "Igloo," which is a pressurized container housing the Command and Data Management System, which interfaces with the in-cabin controllers to control the Instrument Pointing System (IPS) and the telescopes.

  11. Selected papers in the applied computer sciences 1992

    USGS Publications Warehouse

    Wiltshire, Denise A.

    1992-01-01

    This compilation of short papers reports on technical advances in the applied computer sciences. The papers describe computer applications in support of earth science investigations and research. This is the third volume in the series "Selected Papers in the Applied Computer Sciences." Listed below are the topics addressed in the compilation:Integration of geographic information systems and expert systems for resource management,Visualization of topography using digital image processing,Development of a ground-water data base for the southeastern Uited States using a geographic information system,Integration and aggregation of stream-drainage data using a geographic information system,Procedures used in production of digital geologic coverage using compact disc read-only memory (CD-ROM) technology, andAutomated methods for producing a technical publication on estimated water use in the United States.

  12. A 2dF survey of the Small Magellanic Cloud

    NASA Astrophysics Data System (ADS)

    Evans, Christopher J.; Howarth, Ian D.; Irwin, Michael J.; Burnley, Adam W.; Harries, Timothy J.

    2004-09-01

    We present a catalogue of new spectral types for hot, luminous stars in the Small Magellanic Cloud (SMC). The catalogue contains 4161 objects, giving an order-of-magnitude increase in the number of SMC stars with published spectroscopic classifications. The targets are primarily B- and A-type stars (2862 and 853 objects respectively), with one Wolf-Rayet, 139 O-type and 306 FG stars, sampling the main sequence to ~mid-B. The selection and classification criteria are described, and objects of particular interest are discussed, including UV-selected targets from the Ultraviolet Imaging Telescope (UIT) experiment, Be and B[e] stars, `anomalous A supergiants' and composite-spectrum systems. We examine the incidence of Balmer-line emission, and the relationship between Hγ equivalent width and absolute magnitude for BA stars.

  13. STS-35 ASTRO-1 telescopes documented in OV-102's payload bay (PLB)

    NASA Image and Video Library

    1990-12-10

    STS035-604-058 (2-10 Dec 1990) --- The various components of the Astro-1 payload are seen backdropped against the blue and white Earth in this scene photographed through Columbia's aft flight deck windows. Parts of the Hopkins Ultraviolet Telescope (HUT), Ultraviolet Imaging Telescope (UIT) and the Wisconsin Ultraviolet Photopolarimetry Experiment (WUPPE) are visible on the Spacelab pallet in the foreground. The Broad Band X-ray Telescope (BBXRT) is behind this pallet and is not visible in this scene. The smaller cylinder in the foreground is the "Igloo," which is a pressurized container housing the Command and Data Management System, which interfaces with the in-cabin controllers to control the Instrument Pointing System (IPS) and the telescopes. The photograph was made with a handheld Rolleiflex camera aimed through Columbia's aft flight deck windows.

  14. Unipolar Terminal-Attractor Based Neural Associative Memory with Adaptive Threshold

    NASA Technical Reports Server (NTRS)

    Liu, Hua-Kuang (Inventor); Barhen, Jacob (Inventor); Farhat, Nabil H. (Inventor); Wu, Chwan-Hwa (Inventor)

    1996-01-01

    A unipolar terminal-attractor based neural associative memory (TABAM) system with adaptive threshold for perfect convergence is presented. By adaptively setting the threshold values for the dynamic iteration for the unipolar binary neuron states with terminal-attractors for the purpose of reducing the spurious states in a Hopfield neural network for associative memory and using the inner-product approach, perfect convergence and correct retrieval is achieved. Simulation is completed with a small number of stored states (M) and a small number of neurons (N) but a large M/N ratio. An experiment with optical exclusive-OR logic operation using LCTV SLMs shows the feasibility of optoelectronic implementation of the models. A complete inner-product TABAM is implemented using a PC for calculation of adaptive threshold values to achieve a unipolar TABAM (UIT) in the case where there is no crosstalk, and a crosstalk model (CRIT) in the case where crosstalk corrupts the desired state.

  15. Unipolar terminal-attractor based neural associative memory with adaptive threshold

    NASA Technical Reports Server (NTRS)

    Liu, Hua-Kuang (Inventor); Barhen, Jacob (Inventor); Farhat, Nabil H. (Inventor); Wu, Chwan-Hwa (Inventor)

    1993-01-01

    A unipolar terminal-attractor based neural associative memory (TABAM) system with adaptive threshold for perfect convergence is presented. By adaptively setting the threshold values for the dynamic iteration for the unipolar binary neuron states with terminal-attractors for the purpose of reducing the spurious states in a Hopfield neural network for associative memory and using the inner product approach, perfect convergence and correct retrieval is achieved. Simulation is completed with a small number of stored states (M) and a small number of neurons (N) but a large M/N ratio. An experiment with optical exclusive-OR logic operation using LCTV SLMs shows the feasibility of optoelectronic implementation of the models. A complete inner-product TABAM is implemented using a PC for calculation of adaptive threshold values to achieve a unipolar TABAM (UIT) in the case where there is no crosstalk, and a crosstalk model (CRIT) in the case where crosstalk corrupts the desired state.

  16. STS-67 crew insignia

    NASA Technical Reports Server (NTRS)

    1995-01-01

    Observation and remote exploration of the Universe in the ultraviolet wavelengths of light are the focus of the STS-67/ASTRO-2 mission, as depicted in the crew patch designed by the crew members. The insignia shows the ASTRO-2 telescopes in the Space Shuttle Endeavour's payload bay, orbiting high above Earth's atmosphere. The three sets of rays, diverging from the telescope on the patch atop the Instrument Pointing System (IPS), correspond to the three ASTRO-2 telescopes - the Hopkins Ultraviolet Telescope (HUT), The Ultraviolet Imaging Telescope (UIT), and the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE). The telescopes are coaligned to simultaneously view the same astronomical object, as shown by the convergence of rays on the NASA symbol. This symbol also represents the excellence of the union of the NASA teams and the universality's in the exploration of the universe through astronomy. The celestial targets of ASTRO-2 include the observation of planets, stars and gala

  17. Space Science

    NASA Image and Video Library

    1990-12-02

    STS-35 lifted off December 2, 1990, at 1:19 am EST, aboard the Space Shuttle Orbiter Columbia. Her crew of eight included: Vance D. Brand, commander; Colonel Guy S. Gardner, pilot; mission specialists Dr. Robert A. R. Parker, John M. (Mike) Lounge, and Dr. Jeffery A. Hoffman; and payload specialists Dr. Kenneth H. Nordsieck, Dr. Samual T. Durrance, and Dr. Ronald A. Parise. The primary objective of the mission was round the clock observation of the celestial sphere in ultraviolet and X-Ray astronomy with the Astro-1 Observatory which consisted of four telescopes: the Hopkins Ultraviolet Telescope (HUT); the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE); the Ultraviolet Imaging Telescope (UIT); and the Broad Band X-Ray Telescope (BBXRT). Due to loss of data used for pointing and operating the ultraviolet telescopes, Marshall Space Flight Center ground teams were forced to aim the telescopes with fine tuning by the flight crew.

  18. Word Frequency Analysis. MOS: 62J. Skill Levels 1 & 2.

    DTIC Science & Technology

    1981-05-01

    WCRDI COUNT2 W OR u, CO UIT 3 WORD 3 COUNT’. kCRD4 I CELL 9 CLNTER I CERERLINE t CENTRALLY 2 C [JTP I FGAL 2 CZRT..IN I CESSIVE 46 LFI’ 14 C H%1% ~ 4...4 .4* 4 AD ,G4 ANGLI 4 fC S 0A 4 r. 5 54b d204 4 BE- J 4OCK4 ECAGNE 4 TTA .(.KFTS 4 B𔃻E.KER 4 44 CC!’PPCT 4 13FL*.~If 4 CCLC CTwV7CCC~L< EL4 CO 4 CE...t CI RE I CARTcUL I CAR7~ I 3 CARRY I CAL 7I C!! 11 E t C., TFPS I CA~TCH I C4TEO I co usIN Kr I CL TC1 I CELL 1CTNlERL!NEz I ’ENI P.LIY Ic3VEI

  19. Around Marshall

    NASA Image and Video Library

    1990-12-03

    The primary objective of the STS-35 mission was round the clock observation of the celestial sphere in ultraviolet and X-Ray astronomy with the Astro-1 observatory which consisted of four telescopes: the Hopkins Ultraviolet Telescope (HUT); the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE); the Ultraviolet Imaging Telescope (UIT); and the Broad Band X-Ray Telescope (BBXRT). The Huntsville Operations Support Center (HOSC) Spacelab Payload Operations Control Center (SL POCC) at the Marshall Space Flight Center (MSFC) was the air/ground communication channel used between the astronauts and ground control teams during the Spacelab missions. Teams of controllers and researchers directed on-orbit science operations, sent commands to the spacecraft, received data from experiments aboard the Space Shuttle, adjusted mission schedules to take advantage of unexpected science opportunities or unexpected results, and worked with crew members to resolve problems with their experiments. Pictured is Jack Jones in the Mission Manager Area.

  20. Mission Manager Area of the Spacelab Payload Operations Control Center (SL POCC)

    NASA Technical Reports Server (NTRS)

    1990-01-01

    The primary objective of the STS-35 mission was round the clock observation of the celestial sphere in ultraviolet and X-Ray astronomy with the Astro-1 observatory which consisted of four telescopes: the Hopkins Ultraviolet Telescope (HUT); the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE); the Ultraviolet Imaging Telescope (UIT); and the Broad Band X-Ray Telescope (BBXRT). The Huntsville Operations Support Center (HOSC) Spacelab Payload Operations Control Center (SL POCC) at the Marshall Space Flight Center (MSFC) was the air/ground communication channel used between the astronauts and ground control teams during the Spacelab missions. Teams of controllers and researchers directed on-orbit science operations, sent commands to the spacecraft, received data from experiments aboard the Space Shuttle, adjusted mission schedules to take advantage of unexpected science opportunities or unexpected results, and worked with crew members to resolve problems with their experiments. Pictured is Jack Jones in the Mission Manager Area.

  1. Around Marshall

    NASA Image and Video Library

    1990-12-07

    The primary objective of the STS-35 mission was round the clock observation of the celestial sphere in ultraviolet and X-Ray astronomy with the Astro-1 observatory which consisted of four telescopes: the Hopkins Ultraviolet Telescope (HUT); the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE); the Ultraviolet Imaging Telescope (UIT); and the Broad Band X-Ray Telescope (BBXRT). The Huntsville Operations Support Center (HOSC) Spacelab Payload Operations Control Center (SL POCC) at the Marshall Space Flight Center (MSFC) was the air/ground communication channel used between the astronauts and ground control teams during the Spacelab missions. Teams of controllers and researchers directed on-orbit science operations, sent commands to the spacecraft, received data from experiments aboard the Space Shuttle, adjusted mission schedules to take advantage of unexpected science opportunities or unexpected results, and worked with crew members to resolve problems with their experiments. This photo is of Space classroom students in the Discovery Optics Lab at MSFC during STS-35, ASTRO-1 mission payload operations.

  2. Space Shuttle Projects

    NASA Image and Video Library

    1989-11-27

    The primary payload for Space Shuttle Mission STS-35, launched December 2, 1990, was the ASTRO-1 Observatory. Designed for round the clock observation of the celestial sphere in ultraviolet and X-ray astronomy, ASTRO-1 featured a collection of four telescopes: the Hopkins Ultraviolet Telescope (HUT); the Wisconsin Ultraviolet Photo- Polarimeter Experiment (WUPPE); the Ultraviolet Imaging Telescope (UIT); and the Broad Band X-ray Telescope (BBXRT). Ultraviolet telescopes mounted on Spacelab elements in cargo bay were to be operated in shifts by flight crew. Loss of both data display units (used for pointing telescopes and operating experiments) during mission impacted crew-aiming procedures and forced ground teams at Marshall Space Flight Center to aim ultraviolet telescopes with fine-tuning by flight crew. BBXRT, also mounted in cargo bay, was directed from outset by ground-based operators at Goddard Space Flight Center. This is the logo or emblem that was designed to represent the ASTRO-1 payload.

  3. View of ASTRO-2 payload in cargo bay of STS-67 Endeavour

    NASA Image and Video Library

    1995-03-17

    STS067-713-072 (2-18 March 1995) --- This 70mm cargo bay scene, backdropped against a desert area of Namibia, typifies the view that daily greeted the Astro-2 crew members during their almost 17-days aboard the Space Shuttle Endeavour. Positioned on the Spacelab pallet amidst other hardware, the Astro-2 payload is in its operational mode. Visible here are the Instrument Pointing System (IPS), Hopkins Ultraviolet Telescope (HUT), Star Tracker (ST), Ultraviolet Imaging Telescope (UIT), Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE), and Integrated Radiator System (IRS). At this angle, the Optical Sensor Package (OPS) is not seen. The Igloo, which supports the package of experiments, is in center foreground. Two Get-Away Special (GAS) canisters are in lower left foreground. The Extended Duration Orbiter (EDO) pallet, located aft of the cargo bay, is obscured by the Astro-2 payload. The Endeavour was 190 nautical miles above Earth.

  4. Around Marshall

    NASA Image and Video Library

    1990-12-03

    The primary objective of the STS-35 mission was round the clock observation of the celestial sphere in ultraviolet and X-Ray astronomy with the Astro-1 observatory which consisted of four telescopes: the Hopkins Ultraviolet Telescope (HUT); the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE); the Ultraviolet Imaging Telescope (UIT); and the Broad Band X-Ray Telescope (BBXRT). The Huntsville Operations Support Center (HOSC) Spacelab Payload Operations Control Center (SL POCC) at the Marshall Space Flight Center (MSFC) was the air/ground communication channel used between the astronauts and ground control teams during the Spacelab missions. Teams of controllers and researchers directed on-orbit science operations, sent commands to the spacecraft, received data from experiments aboard the Space Shuttle, adjusted mission schedules to take advantage of unexpected science opportunities or unexpected results, and worked with crew members to resolve problems with their experiments. Pictured is the TV OPS area of the SL POCC.

  5. Obituary: Ronald A. Parise, 1951-2008

    NASA Astrophysics Data System (ADS)

    Gull, Theodore R.

    2009-01-01

    Ronald A. Parise, astronomer and astronaut, passed away at his home in Burtonsville, Maryland, in the presence of his family on 9 May 2008. He died of a brain tumor at age 56 after several years of valiant struggle. He was an inspiration to many students, ham operators, astronomers, and friends the world over. His enthusiasm for astronomy and space exploration was infectious. We, colleagues at Goddard Space Flight Center and Computer Sciences Corporation, treasured his contributions to space astronomy and human spaceflight. Ron, along with Samuel Durrance, flew as Payload Specialist on Astro-1 and Astro-2. They were selected by peers from the instrument teams of the Hopkins Ultraviolet Telescope (HUT provided by Hopkins University), the Ultraviolet Imaging Telescope (UIT, Goddard Space Flight Center) and the Wisconsin Ultraviolet Photo-Polarimetry Experiment (WUPPE, University of Wisconsin). Astro-1 flew 2-10 December 1990 on the Columbia. Astro-2 flew 2-18 March 1995. Ron carried along amateur radio equipment and operated on the air during his free time during the missions. Ron was born 24 May 1951 in Warren, Ohio, to Henry and Catherine Parise. His interests first were in amateur radio, becoming a licensed operator by age eleven. He later was attracted to both astronomy and aviation, becoming a pilot in his teens. Ron graduated from Western Reserve High School in 1969 and attended Youngstown State University where he received a bachelor of science degree in physics with minors in mathematics, astronomy. and geology. His graduate work was at University of Florida where he obtained a masters degree in 1977 and a doctorate in 1979 in astronomy. Ron joined Operations Research, Inc. upon graduation, working at Goddard Space Flight Center where he supported studies of several NASA missions. In 1980 he joined Computer Sciences Corporation supporting the International Ultraviolet Explorer [IUE], first as a data-management scientist and later as the section manager of the IUE hardcopy facility. By 1981 he joined a team of engineers and scientists beginning the development of the newly selected the Ultraviolet Imaging Telescope (UIT), selected by NASA to fly on board the space shuttles as an attached Spacelab experiment. The UIT project, headed by Ted Stecher as Principal Investigator, was one of three ultraviolet experimental telescopes selected to fly together as an Office of Space Sciences [OSS] payload. Initial plans were for multiple flights with emphasis of observing Halley's Comet in three missions from November 1985 to summer 1986. Ron's responsibilities involved flight hardware and software development, electronic system design, and mission planning activities for UIT. His proficiency led to his selection by the Principal Investigators of the three instruments as a Payload Specialist candidate and acceptance by NASA as one of three payload specialists in support of the series of missions. He, Samuel Durrance, and Kenneth Nordsieck shouldered the responsibilities of training as payload specialists for the instruments integrated on a common pointer, the Spacelab Instrument Pointing System, IPS. As a team they represented the operational needs of the instrument teams and trained to fly with the shuttle team. Preparations moved forward to the March 1986 launch date of Astro-1 to observe Comet Halley and well over a hundred astronomical sources. Unfortunately, the Challenger accident occurred 28 January 1986, thirty-five days before the intended launch date of Astro-1. Ron and Sam, as prime Payload Specialists, and Ken as backup/ ground communicator, took the delay well, staying focused on training to ensure that Astro-1, delayed until December 1990, would be an outstanding success. With at least thirteen launch delays, and on-orbit operational problems, they, the professional astronaut crew, the science teams, and the multitude of engineers and mission support staff managed to accomplish a very successful astronomy mission. Even though Comet Halley was not observed by Astro-1, well over a hundred papers on multiple astronomical sources resulted from Astro-1 and Astro-2. Ron participated in a number of observational astronomy projects using data from ground-based observatories, Copernicus, IUE, and the Astro observatory. His interests were primarily in circumstellar matter within binary star systems and globular- cluster evolution. He bridged the gaps between science, engineering, and spaceflight operations. After the completion of the two Astro missions, Ron supported NASA studies in advanced communications for spaceflight missions and was involved in projects in the Advanced Architectures and Automation Branch developing standard Internet Protocols [IP] in space-data transmission applications. Throughout his career, Ron supported education both by appearances at schools and through his amateur radio interests. Indeed, he had a large following of ham radio operators as he, along with Frank Bauer, brought about the Shuttle Amateur Radio Experiment [SAREX] payload that enabled many schools to talk to Shuttle crew members in space. Ron's love for amateur radio and for inspiring students came to focus through the Amateur Radio on the International Space STation [ARISS] program. His volunteer help was key in the development of those systems now on board the ISS. As Frank Bauer, a ham colleague, put it in his tribute to Ron Parise, WA4SIR SK: may your exploration spirit live on in us all! Ron leaves behind his wife, Cecilia; son, Nicholas; daughter, Katharine; his parents Henry and Kathryn Parise; and sister, Rita Parise.

  6. Space Students Visit MSFC During STS-35 Astro-1 Mission

    NASA Technical Reports Server (NTRS)

    1990-01-01

    The primary objective of the STS-35 mission was round the clock observation of the celestial sphere in ultraviolet and X-Ray astronomy with the Astro-1 observatory which consisted of four telescopes: the Hopkins Ultraviolet Telescope (HUT); the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE); the Ultraviolet Imaging Telescope (UIT); and the Broad Band X-Ray Telescope (BBXRT). The Huntsville Operations Support Center (HOSC) Spacelab Payload Operations Control Center (SL POCC) at the Marshall Space Flight Center (MSFC) was the air/ground communication channel used between the astronauts and ground control teams during the Spacelab missions. Teams of controllers and researchers directed on-orbit science operations, sent commands to the spacecraft, received data from experiments aboard the Space Shuttle, adjusted mission schedules to take advantage of unexpected science opportunities or unexpected results, and worked with crew members to resolve problems with their experiments. This photo is of Space classroom students in the Discovery Optics Lab at MSFC during STS-35, ASTRO-1 mission payload operations.

  7. Space Science

    NASA Image and Video Library

    1990-01-16

    This montage consists of 8 individual STS-35 crew member portraits surrounding the mission’s insignia. Starting from top center, clockwise, are Vance D. Brand, commander; mission specialists Dr. Robert A. R. Parker, John M. (Mike) Lounge, and Dr. Jeffery A. Hoffman; Colonel Guy S. Gardner, pilot; and payload specialists Dr. Kenneth H. Nordsieck, Dr. Samual T. Durrance, and Dr. Ronald A. Parise. The crew of 8 launched aboard the Space Shuttle Orbiter Columbia on December 2, 1990 at 1:19:01am (EST). The primary objective of the mission was round the clock observation of the celestial sphere in ultrviolet and X-Ray astronomy with the Astro-1 observatory which consisted of four telescopes: the Hopkins Ultraviolet Telescope (HUT); the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE); the Ultraviolet Imaging Telescope (UIT); and the Broad Band X-Ray Telescope (BBXRT). Due to loss of data used for pointing and operating the ultraviolet telescopes, Marshall Space Flight Center ground teams were forced to aim the telescopes with fine tuning by the flight crew.

  8. Atmospheric Conditions at the High Energy Laser Systems Test Facility (HELSTF), White Sands Missile Range (WSMR), New Mexico 24 March to 8 April 1977

    DTIC Science & Technology

    1978-01-01

    En 1 S - G)) cc E LS-3CS -L I m L 3 cc0 0 W) in w 3 33c v 3c do - I. ILL. ccL ts0.lIL 00 lC ) C) C LI C> C C.) C12 C.) C\\ 3 C...8217IVW(’) C’Jý9;o ) r uitN U) En QE0LD . P" ý 0 0 0282 4~ x D ,qRRKY 07 RPR 1977 o -’ !1.06 U!( 1.65-J.00501=- 1.,j " 3 3 8 0 L• [ ! . 17- J .0 C 5...004 C3 $ 𔃺 - %5.4 .- 4’ -- 4 $404 - - o 41 Z0.0 0ɘ U4- $4 - $ 1. 4’ . $41 U 0.00-40-00-4 01*034 4 0 r- 0 0 -- .0 .00 0 En 0 0 U 0 U E . 3 -

  9. Spacelab

    NASA Image and Video Library

    1990-12-02

    Onboard the Space Shuttle Orbiter Columbia (STS-35), the various components of the Astro-1 payload are seen backdropped against dark space. Parts of the Hopkins Ultraviolet Telescope (HUT), Ultraviolet Imaging Telescope (UIT), and the Wisconsin Ultraviolet Photo-Polarimetry Experiment (WUPPE) are visible on the Spacelab pallet. The Broad-Band X-Ray Telescope (BBXRT) is behind the pallet and is not visible in this scene. The smaller cylinder in the foreground is the igloo. The igloo was a pressurized container housing the Command Data Management System, that interfaced with the in-cabin controllers to control the Instrument Pointing System (IPS) and the telescopes. The Astro Observatory was designed to explore the universe by observing and measuring the ultraviolet radiation from celestial objects. Astronomical targets of observation selected for Astro missions included planets, stars, star clusters, galaxies, clusters of galaxies, quasars, remnants of exploded stars (supernovae), clouds of gas and dust (nebulae), and the interstellar medium. Managed by the Marshall Space Flight Center, the Astro-1 was launched aboard the Space Shuttle Orbiter Columbia (STS-35) on December 2, 1990.

  10. Increase in the thermodynamic efficiency of the working process of spark-ignited engines on natural gas with the addition of hydrogen

    NASA Astrophysics Data System (ADS)

    Mikhailovna Smolenskaya, Natalia; Vladimirovich Smolenskii, Victor; Vladimirovich Korneev, Nicholas

    2018-02-01

    The work is devoted to the substantiation and practical implementation of a new approach for estimating the change in internal energy by pressure and volume. The pressure is measured with a calibrated sensor. The change in volume inside the cylinder is determined by changing the position of the piston. The position of the piston is precisely determined by the angle of rotation of the crankshaft. On the basis of the proposed approach, the thermodynamic efficiency of the working process of spark ignition engines on natural gas with the addition of hydrogen was estimated. Experimental studies were carried out on a single-cylinder unit UIT-85. Their analysis showed an increase in the thermodynamic efficiency of the working process with the addition of hydrogen in a compressed natural gas (CNG).The results obtained make it possible to determine the characteristic of heat release from the analysis of experimental data. The effect of hydrogen addition on the CNG combustion process is estimated.

  11. An Ultraviolet and Near-Infrared View of NGC 4214: A Starbursting Core Embedded in a Low Surface Brightness Disk

    NASA Astrophysics Data System (ADS)

    Fanelli, Michael N.; Waller, William W.; Smith, Denise A.; Freedman, Wendy L.; Madore, Barry; Neff, Susan G.; O'Connell, Robert W.; Roberts, Morton S.; Bohlin, Ralph; Smith, Andrew M.; Stecher, Theodore P.

    1997-05-01

    During the Astro-2 Spacelab mission in 1995 March, the Ultraviolet Imaging Telescope (UIT) obtained far-UV (λ = 1500 Å) imagery of the nearby Sm/Im galaxy NGC 4214. The UIT images have a spatial resolution of ~3" and a limiting surface brightness, μ1500 > 25 mag arcsec-2, permitting detailed investigation of the intensity and spatial distribution of the young, high-mass stellar component. These data provide the first far-UV imagery covering the full spatial extent of NGC 4214. Comparison with a corresponding I-band image reveals the presence of a starbursting core embedded in an extensive low surface brightness disk. In the far-UV (FUV), NGC 4214 is resolved into several components: a luminous, central knot; an inner region (r <~ 2.5 kpc) with ~15 resolved sources embedded in bright, diffuse emission; and a population of fainter knots extending to the edge of the optically defined disk (r ~ 5 kpc). The FUV light, which traces recent massive star formation, is observed to be more centrally concentrated than the I-band light, which traces the global stellar population. The FUV radial light profile is remarkably well represented by an R1/4 law, providing evidence that the centrally concentrated massive star formation in NGC 4214 is the result of an interaction, possibly a tidal encounter, with a dwarf companion(s). The brightest FUV source produces ~8% of the global FUV luminosity. This unresolved source, corresponding to the Wolf-Rayet knot described by Sargent & Filippenko, is located at the center of the FUV light distribution, giving NGC 4214 an active galactic nucleus-like morphology. Another strong source is present in the I band, located 19" west, 10" north of the central starburst knot, with no FUV counterpart. The I-band source may be the previously unrecognized nucleus of NGC 4214 or an evolved star cluster with an age greater than ~200 Myr. The global star formation rate derived from the total FUV flux is consistent with rates derived using data at other wavelengths and lends support to the scenario of roughly constant star formation during the last few hundred million years at a level significantly enhanced relative to the lifetime averaged star formation rate. The hybrid disk/starburst-irregular morphology evident in NGC 4214 emphasizes the danger of classifying galaxies based on their high surface brightness components at any particular wavelength.

  12. Onboard photo:Astro-1 in Cargo Bay

    NASA Technical Reports Server (NTRS)

    1990-01-01

    Onboard the Space Shuttle Orbiter Columbia (STS-35), the various components of the Astro-1 payload are seen backdropped against dark space. Parts of the Hopkins Ultraviolet Telescope (HUT), Ultraviolet Imaging Telescope (UIT), and the Wisconsin Ultraviolet Photo-Polarimetry Experiment (WUPPE) are visible on the Spacelab pallet. The Broad-Band X-Ray Telescope (BBXRT) is behind the pallet and is not visible in this scene. The smaller cylinder in the foreground is the igloo. The igloo was a pressurized container housing the Command Data Management System, that interfaced with the in-cabin controllers to control the Instrument Pointing System (IPS) and the telescopes. The Astro Observatory was designed to explore the universe by observing and measuring the ultraviolet radiation from celestial objects. Astronomical targets of observation selected for Astro missions included planets, stars, star clusters, galaxies, clusters of galaxies, quasars, remnants of exploded stars (supernovae), clouds of gas and dust (nebulae), and the interstellar medium. Managed by the Marshall Space Flight Center, the Astro-1 was launched aboard the Space Shuttle Orbiter Columbia (STS-35) on December 2, 1990.

  13. Onboard Photo:Astro-1 Ultraviolet Telescope in Cargo Bay

    NASA Technical Reports Server (NTRS)

    1990-01-01

    Onboard the Space Shuttle Orbiter Columbia (STS-35), the various components of the Astro-1 payload are seen backdropped against a blue and white Earth. Parts of the Hopkins Ultraviolet Telescope (HUT), the Ultraviolet Imaging Telescope (UIT), and the Wisconsin Ultraviolet Photo-Polarimetry Experiment (WUPPE) are visible on the Spacelab pallet. The Broad-Band X-Ray Telescope (BBXRT) is behind the pallet and is not visible in this scene. The smaller cylinder in the foreground is the igloo. The igloo was a pressurized container housing the Command Data Management System, that interfaced with the in-cabin controllers to control the Instrument Pointing System (IPS) and the telescopes. The Astro Observatory was designed to explore the universe by observing and measuring the ultraviolet radiation from celestial objects. Astronomical targets of observation selected for Astro missions included planets, stars, star clusters, galaxies, clusters of galaxies, quasars, remnants of exploded stars (supernovae), clouds of gas and dust (nebulae), and the interstellar medium. Managed by the Marshall Space Flight Center, the Astro-1 was launched aboard the Space Shuttle Orbiter Columbia (STS-35) on December 2, 1990.

  14. Ultraviolet Imaging Telescope ultraviolet images - Large-scale structure, H II regions, and extinction in M81

    NASA Technical Reports Server (NTRS)

    Hill, Jesse K.; Bohlin, Ralph C.; Cheng, Kwang-Ping; Hintzen, Paul M. N.; Landsman, Wayne B.; Neff, Susan G.; O'Connell, Robert W.; Roberts, Morton S.; Smith, Andrew M.; Smith, Eric P.

    1992-01-01

    The study employs UV images of M81 obtained by the Ultraviolet Imaging Telescope (UIT) during the December 1990 Astro-1 spacelab mission to determine 2490- and 1520-A fluxes from 46 H II regions and global surface brightness profiles. Comparison photometry in the V band is obtained from a ground-based CCD image. UV radial profiles show bulge and exponential disk components, with a local decrease in disk surface brightness inside the inner Lindblad Resonance about 4 arcmin from the nucleus. The V profile shows typical bulge plus exponential disk structure, with no local maximum in the disk. There is little change of UV color across the disk, although there is a strong gradient in the bulge. Observed m152-V colors of the H II regions are consistent with model spectra for young clusters, after dereddening using Av determined from m249-V and the Galactic extinction curve. The value of Av, so determined, is 0.4 mag greater on the average than Av derived from radio continuum and H-alpha fluxes.

  15. Around Marshall

    NASA Image and Video Library

    1990-12-12

    The primary objective of the STS-35 mission was round the clock observation of the celestial sphere in ultraviolet and X-Ray astronomy with the Astro-1 observatory which consisted of four telescopes: the Hopkins Ultraviolet Telescope (HUT); the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE); the Ultraviolet Imaging Telescope (UIT); and the Broad Band X-Ray Telescope (BBXRT). The Huntsville Operations Support Center (HOSC) Spacelab Payload Operations Control Center (SL POCC) at the Marshall Space Flight Center (MSFC) was the air/ground communication channel used between the astronauts and ground control teams during the Spacelab missions. Teams of controllers and researchers directed on-orbit science operations, sent commands to the spacecraft, received data from experiments aboard the Space Shuttle, adjusted mission schedules to take advantage of unexpected science opportunities or unexpected results, and worked with crew members to resolve problems with their experiments. Due to loss of data used for pointing and operating the ultraviolet telescopes, MSFC ground teams were forced to aim the telescopes with fine tuning by the flight crew. This photo captures the activity of WUPPE data review at the Science Operations Area during the mission.

  16. Around Marshall

    NASA Image and Video Library

    1990-12-03

    The primary objective of the STS-35 mission was round the clock observation of the celestial sphere in ultraviolet and X-Ray astronomy with the Astro-1 observatory which consisted of four telescopes: the Hopkins Ultraviolet Telescope (HUT); the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE); the Ultraviolet Imaging Telescope (UIT); and the Broad Band X-Ray Telescope (BBXRT). The Huntsville Operations Support Center (HOSC) Spacelab Payload Operations Control Center (SL POCC) at the Marshall Space Flight Center (MSFC) was the air/ground communication channel used between the astronauts and ground control teams during the Spacelab missions. Teams of controllers and researchers directed on-orbit science operations, sent commands to the spacecraft, received data from experiments aboard the Space Shuttle, adjusted mission schedules to take advantage of unexpected science opportunities or unexpected results, and worked with crew members to resolve problems with their experiments. Due to loss of data used for pointing and operating the ultraviolet telescopes, MSFC ground teams were forced to aim the telescopes with fine tuning by the flight crew. This photo is an overview of the MSFC Payload Control Room (PCR).

  17. Around Marshall

    NASA Image and Video Library

    1990-12-04

    The primary objective of the STS-35 mission was round the clock observation of the celestial sphere in ultraviolet and X-Ray astronomy with the Astro-1 observatory which consisted of four telescopes: the Hopkins Ultraviolet Telescope (HUT); the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE); the Ultraviolet Imaging Telescope (UIT); and the Broad Band X-Ray Telescope (BBXRT). The Huntsville Operations Support Center (HOSC) Spacelab Payload Operations Control Center (SL POCC) at the Marshall Space Flight Center (MSFC) was the air/ground communication channel used between the astronauts and ground control teams during the Spacelab missions. Teams of controllers and researchers directed on-orbit science operations, sent commands to the spacecraft, received data from experiments aboard the Space Shuttle, adjusted mission schedules to take advantage of unexpected science opportunities or unexpected results, and worked with crew members to resolve problems with their experiments. Due to loss of data used for pointing and operating the ultraviolet telescopes, MSFC ground teams were forced to aim the telescopes with fine tuning by the flight crew. This photo captures a press briefing at MSFC during STS-35, ASTRO-1 Mission.

  18. Spacelab

    NASA Image and Video Library

    1990-12-02

    Onboard the Space Shuttle Orbiter Columbia (STS-35), the various components of the Astro-1 payload are seen backdropped against a blue and white Earth. Parts of the Hopkins Ultraviolet Telescope (HUT), the Ultraviolet Imaging Telescope (UIT), and the Wisconsin Ultraviolet Photo-Polarimetry Experiment (WUPPE) are visible on the Spacelab pallet. The Broad-Band X-Ray Telescope (BBXRT) is behind the pallet and is not visible in this scene. The smaller cylinder in the foreground is the igloo. The igloo was a pressurized container housing the Command Data Management System, that interfaced with the in-cabin controllers to control the Instrument Pointing System (IPS) and the telescopes. The Astro Observatory was designed to explore the universe by observing and measuring the ultraviolet radiation from celestial objects. Astronomical targets of observation selected for Astro missions included planets, stars, star clusters, galaxies, clusters of galaxies, quasars, remnants of exploded stars (supernovae), clouds of gas and dust (nebulae), and the interstellar medium. Managed by the Marshall Space Flight Center, the Astro-1 was launched aboard the Space Shuttle Orbiter Columbia (STS-35) on December 2, 1990.

  19. Around Marshall

    NASA Image and Video Library

    1990-12-02

    The primary objective of the STS-35 mission was round the clock observation of the celestial sphere in ultraviolet and X-Ray astronomy with the Astro-1 observatory which consisted of four telescopes: the Hopkins Ultraviolet Telescope (HUT); the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE); the Ultraviolet Imaging Telescope (UIT); and the Broad Band X-Ray Telescope (BBXRT). The Huntsville Operations Support Center (HOSC) Spacelab Payload Operations Control Center (SL POCC) at the Marshall Space Flight Center (MSFC) was the air/ground communication channel used between the astronauts and ground control teams during the Spacelab missions. Teams of controllers and researchers directed on-orbit science operations, sent commands to the spacecraft, received data from experiments aboard the Space Shuttle, adjusted mission schedules to take advantage of unexpected science opportunities or unexpected results, and worked with crew members to resolve problems with their experiments. Due to loss of data used for pointing and operating the ultraviolet telescopes, MSFC ground teams were forced to aim the telescopes with fine tuning by the flight crew. This photo captures the activity of viewing HUT data in the Mission Manager Actions Room during the mission.

  20. Spacelab

    NASA Image and Video Library

    1990-12-02

    The primary objective of the STS-35 mission was round the clock observation of the celestial sphere in ultraviolet and X-Ray astronomy with the Astro-1 observatory which consisted of four telescopes: the Hopkins Ultraviolet Telescope (HUT); the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE); the Ultraviolet Imaging Telescope (UIT); and the Broad Band X-Ray Telescope (BBXRT). The Huntsville Operations Support Center (HOSC) Spacelab Payload Operations Control Center (SL POCC) at the Marshall Space Flight Center (MSFC) was the air/ground communication channel used between the astronauts and ground control teams during the Spacelab missions. Teams of controllers and researchers directed on-orbit science operations, sent commands to the spacecraft, received data from experiments aboard the Space Shuttle, adjusted mission schedules to take advantage of unexpected science opportunities or unexpected results, and worked with crew members to resolve problems with their experiments. Due to loss of data used for pointing and operating the ultraviolet telescopes, MSFC ground teams were forced to aim the telescopes with fine tuning by the flight crew. Pictured onboard the shuttle is astronaut Robert Parker using a Manual Pointing Controller (MPC) for the ASTRO-1 mission Instrument Pointing System (IPS).

  1. Around Marshall

    NASA Image and Video Library

    1990-12-02

    The primary objective of the STS-35 mission was round the clock observation of the celestial sphere in ultraviolet and X-Ray astronomy with the Astro-1 observatory which consisted of four telescopes: the Hopkins Ultraviolet Telescope (HUT); the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE); the Ultraviolet Imaging Telescope (UIT); and the Broad Band X-Ray Telescope (BBXRT). The Huntsville Operations Support Center (HOSC) Spacelab Payload Operations Control Center (SL POCC) at the Marshall Space Flight Center (MSFC) was the air/ground communication channel used between the astronauts and ground control teams during the Spacelab missions. Teams of controllers and researchers directed on-orbit science operations, sent commands to the spacecraft, received data from experiments aboard the Space Shuttle, adjusted mission schedules to take advantage of unexpected science opportunities or unexpected results, and worked with crew members to resolve problems with their experiments. Due to loss of data used for pointing and operating the ultraviolet telescopes, MSFC ground teams were forced to aim the telescopes with fine tuning by the flight crew. This photo captures the activities at the Mission Manager Actions Room during the mission.

  2. Around Marshall

    NASA Image and Video Library

    1990-12-02

    The primary objective of the STS-35 mission was round the clock observation of the celestial sphere in ultraviolet and X-Ray astronomy with the Astro-1 observatory which consisted of four telescopes: the Hopkins Ultraviolet Telescope (HUT); the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE); the Ultraviolet Imaging Telescope (UIT); and the Broad Band X-Ray Telescope (BBXRT). The Huntsville Operations Support Center (HOSC) Spacelab Payload Operations Control Center (SL POCC) at the Marshall Space Flight Center (MSFC) was the air/ground communication channel used between the astronauts and ground control teams during the Spacelab missions. Teams of controllers and researchers directed on-orbit science operations, sent commands to the spacecraft, received data from experiments aboard the Space Shuttle, adjusted mission schedules to take advantage of unexpected science opportunities or unexpected results, and worked with crew members to resolve problems with their experiments. Due to loss of data used for pointing and operating the ultraviolet telescopes, MSFC ground teams were forced to aim the telescopes with fine tuning by the flight crew. This photo captures the activity of BBKRT data review in the Science Operations Area during the mission.

  3. Around Marshall

    NASA Image and Video Library

    1990-12-02

    The primary objective of the STS-35 mission was round the clock observation of the celestial sphere in ultraviolet and X-Ray astronomy with the Astro-1 observatory which consisted of four telescopes: the Hopkins Ultraviolet Telescope (HUT); the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE); the Ultraviolet Imaging Telescope (UIT); and the Broad Band X-Ray Telescope (BBXRT). The Huntsville Operations Support Center (HOSC) Spacelab Payload Operations Control Center (SL POCC) at the Marshall Space Flight Center (MSFC) was the air/ground communication channel used between the astronauts and ground control teams during the Spacelab missions. Teams of controllers and researchers directed on-orbit science operations, sent commands to the spacecraft, received data from experiments aboard the Space Shuttle, adjusted mission schedules to take advantage of unexpected science opportunities or unexpected results, and worked with crew members to resolve problems with their experiments. Due to loss of data used for pointing and operating the ultraviolet telescopes, MSFC ground teams were forced to aim the telescopes with fine tuning by the flight crew. This photo captures the activity at the Operations Control Facility during the mission as Dr. Urban and Paul Whitehouse give a “thumbs up”.

  4. Inelastic processes in atomic collisions involving ground state and laser-prepared atoms

    NASA Astrophysics Data System (ADS)

    Planje, Willem Gilles

    1999-11-01

    In dit proefschrift worden experimenten beschreven waarbij ionen of atomen met een bepaalde snelheid op een ensemble van doelwitatomen worden gericht. Wanneer twee deeltjes elkaar voldoende genaderd hebben, vindt er wissel- werking plaats waarbij allerlei processen kunnen optreden. Deze processen resulteren in specieke eindproducten. Kennis over de interactie tussen twee botsingspartners wordt verkregen door te bekijken welke eindproducten ontstaan, en in welke mate. Een belangrijke grootheid die van invloed is op mogelijke processen is de onderlinge snelheid van de twee kernen, oftewel de botsingssnelheid. Wanneer de botsingssnelheid voldoende klein is dan kunnen de verschillende reactiemechanismen zowel kwalitatief als kwanti- tatief vaak goed voorspeld worden door het systeem te beschouwen als een kort-stondig molecuul, opgebouwd uit de twee botsende deeltjes. De ver- schillende processen die kunnen optreden worden gekwaliceerd afhankelijk van de vorming van bepaalde eindproducten. Ruwweg de volgende indeling kan gemaakt worden: 1. de interne structuur van de eindproducten zijn identiek aan die van de beginproducten. We spreken dan van een elastische botsing. 2. e en van de deeltjes of beiden worden in een aangeslagen toestand ge- bracht (of ge¨oniseerd). Dit zijn processen waarbij de herschikte elek- tronen zich bij de oorspronkelijke kern bevinden. We spreken dan van excitatie of ionisatie. 3. e en of meerdere elektronen bevinden zich bij de andere kern na de botsing (eventueel in aangeslagen toestand). We spreken dan van elek- tronenoverdracht. In het eerste deel van deze dissertatie worden botsingsexperimenten tussen heliumionen en natriumatomen beschreven waarbij het proces van elek- tronenoverdracht wordt onderzocht. Bij dit mechanisme is het buitenste 117?Samenvatting natriumelektron betrokken. Deze kan relatief gemakkelijk `overspringen' naar het heliumion wanneer deze zich dicht in de buurt van het natrium- atoom bevindt. Het elektron kan hierbij een bepaalde (aangeslagen) toe- stand bezetten. Wij meten de bezetting van de heliumtoestanden die onder uitzending van XUV licht ( ? 58 nm) vervallen naar de heliumgrondtoe- stand. Door de lichtintensiteit te meten onderzoeken we de mate van elek- tronenoverdracht naar een selecte groep van singlet helium`eind'toestanden, namelijk He(1s2p), He(1s3s), He(1s3p) en He(1s3d). In een reactie- vergelijking ziet het mechanisme er als volgt uit: He + (1s) + ( Na(3s) Na(3p) e- -! He + Na + -! He(1s 2 ) +h(58 nm) + Na + Het experiment kent een extra dimensie door het feit dat het, in beginsel bol- symmetrische, natriumatoom een bepaalde ruimtelijk uitlijning kan worden meegegeven. Met behulp van laserlicht van een specieke frequentie en po- larisatie, wordt het buitenste natriumelektron in een aangeslagen p toestand gebracht. Het aanslaan naar deze toestand heeft als gevolg dat het valentie- elektron zich op grotere afstand van zijn kern bevindt dan voorheen. Daar- naast kan, afhankelijk van de gebruikte laserpolarisatie, het buitenste elek- tron zich nu rond de natriumkern bewegen volgens een bepaalde anisotrope verdeling, de bolsymmetrie is doorbroken. De eecten van de excitatie en ruimtelijk verdeling van dit natriumelektron op het proces van elektronen- overdracht zijn onderzocht voor botsingsenergie¨en vari¨erend van 0.5 keV tot 6.0 keV. De metingen laten zien dat het eect van laserexcitatie een bezettingstoe- name van de beschouwde singlet heliumtoestanden betekent, ongeacht de uitlijning van het natrium 3p elektron. Dit is simpelweg te begrijpen uit het feit dat het 3p natrium elektron minder sterk gebonden is en elektro- nenoverdracht makkelijker gaat. Daarnaast is de uitlijning van het aanges- lagen elektron van invloed op de elektronenoverdracht. De resultaten zijn vergeleken met berekeningen van S.E. Nielsen en T.H. Rod [13], die de elek- tronoverdracht beschrijven in een model waarbij het betrokken elektron zich beweegt in bepaalde eectieve potentiaalvelden. De goede overeenkomsten van onze metingen met de berekeningen rechtvaardigen de theoretische be- nadering van Nielsen en Rod. 118?Samenvatting In het tweede gedeelte van het proefschrift worden botsingen beschouwd tussen helium- en neonatomen. Hierbij wordt nu niet gekeken naar bots- ingsproducten die zich manifesteren door bepaald licht uit te zenden, maar een elektron emitteren met een bepaalde energie. Verschillende soorten `eind'producten kunnen elektronen uitzenden, waaronder de negatieve ion- toestanden. Het elektronenspectrum, gemeten voor dit botsingssysteem, vertoont twee pieken die het spectrum domineren bij 16.2 eV en 19.4 eV voor verschillende botsingsenergie¨en tussen de 0.35 keV en 6.0 keV. Deze piekstructuren wijzen op de vorming van de kort-levende, negatieve iontoe- standen Ne-(2p 5 3s 2 ) en He-(1s2s 2 ) ten gevolge van de overdracht van e en elektron: He 0 + Ne 0 -! He-(1s2s 2 ) +Ne + (2p 5 ) 3 10- 14 s -! He 0 (1s 2 ) +Ne + + e- (19.37 eV) He 0 + Ne 0 -! He + (1s) +Ne-(2p 5 3s 2 ) 2:5 10- 13 s -! He + (1s) +Ne 0 (2p 6 ) +e- (16.15 eV) De meetresultaten vertonen een fenomeen waarbij de bezettingen van de negatieve iontoestanden een oscillerend gedrag vertonen als functie van de botsingssnelheid. Dit duidt op interferentie tussen de twee bijna-ontaarde moleculaire toestanden [He- + Ne + ] en[He + + Ne-]. Het is echter zeer op- merkelijk dat deze oscillatie wordt waargenomen in een experiment als deze, waarin de uitgezonden elektronen worden gemeten ongeacht de afbuighoek van het heliumatoom. Dit impliceert een speciek aanslagmechanisme van de moleculaire negatieve iontoestanden. Nader beschouwing van het bots- ingssysteem laat zien dat het instantane molecuul twee overgangen moet ondergaan voordat de negatieve iontoestanden gevormd worden. Als gevolg hiervan is de snelheid waarmee het negatieve en positieve ion uit elkaar be- wegen nagenoeg onafhankelijk van de afbuighoek van het helium projectiel en is oscillatie mogelijk waarneembaar. De wisselwerking tussen de twee beschouwde moleculaire toestanden impliceert gecorreleerde overdracht van twee elektronen: He- + Ne + 2e- ! He + + Ne- Door het quasi-resonante systeem als resonant te beschouwen kan het fenomeen kwalitatief goed verklaard worden. 119?Samenvatting Inhet laatstedeelwordt de bevolkingvanauto¨oniserende natriumtoestanden bekeken in He +=0 + Na botsingen. In tegenstelling tot de voorgaande exper- imenten waarin elektronenoverdracht beschouwd werd, betreft het hier een excitatiemechanisme. De beschouwde `eind'producten, i.e. de auto¨oniserende natriumtoestanden, bestaan in het algemeen kort en gaan over naar een stabiele iontoestand onder uitzending van een elektron met een toestands- karakteristieke kinetische energie. Door de elektronenspectra te meten bij verschillende botsingsenergie¨en, wordt de bezetting van de auto¨oniserende toestanden onderzocht. Ook hier wordt het eect van laserexcitatie en laser- polarisatie van het natriumatoom op de vorming van deze toestanden, en de mate waarin, bekeken. De metingen laten zien dat zowel in He + -Na als in He 0 -Na botsingen de invloed van de ruimtelijk uitlijning van het buitenste natriumelektron op de elektronenspectra nihil is. Dit impliceert dat het betrokken 3p elektron hoofdzakelijk een passieve rol speelt in de vorming van auto¨oniserende toe- standen: het blijft hoofdzakelijk de 3p toestand bezetten als een `toeschouwer' zonder een overgang te maken naar een andere toestand. Dit wordt boven- dien bevestigd door het feit dat wanneer een fractie natriumatomen aange- slagen wordt naar de p toestand dit een even grote reductie betekent van onder meer de populatie van de auto¨oniserende toestand Na(2p 5 3s 2 ). De verwachte grote toename van Na(2p 5 3p 2 ) toestanden, in geval van Na(3p) doelwitten, is niet waargenomen. 120?121?122

  5. Decentralized nursing education in Northern Norway: towards a sustainable recruitment and retention model in rural Arctic healthcare services

    PubMed Central

    Norbye, Bente; Skaalvik, Mari Wolff

    2013-01-01

    Introduction Decentralized nursing education (DNE) was established at Tromsø University College in 1990 and has since become a part of the bachelor programme in nursing at UiT The Arctic University of Norway. The objective of the study was to investigate whether and to what degree the first DNE programme established in Norway has contributed to recruitment and retention of registered nurses (RNs) in rural healthcare services. Methods The quantitative survey took place in 2012. A questionnaire was distributed to 315 former students who had graduated from the DNE programme from 1994 to 2011. Results The primary finding of this study is that the DNE successfully recruits students from rural areas of Northern Norway. Nearly, 87.5% have their first employment in community healthcare services. They continued to work in the rural areas and 85% still worked as nurses in 2012. The DNE programme has been successful regarding recruitment and retention of RNs to community healthcare services. Fifty-six percent have attended a variety of postgraduate programmes. Conclusion The DNE programme demonstrates itself as a successful study model regarding recruitment and retention of RNs to rural and remote areas. PMID:24286063

  6. Decentralized nursing education in Northern Norway: towards a sustainable recruitment and retention model in rural Arctic healthcare services.

    PubMed

    Norbye, Bente; Skaalvik, Mari Wolff

    2013-01-01

    Decentralized nursing education (DNE) was established at Tromsø University College in 1990 and has since become a part of the bachelor programme in nursing at UiT The Arctic University of Norway. The objective of the study was to investigate whether and to what degree the first DNE programme established in Norway has contributed to recruitment and retention of registered nurses (RNs) in rural healthcare services. The quantitative survey took place in 2012. A questionnaire was distributed to 315 former students who had graduated from the DNE programme from 1994 to 2011. The primary finding of this study is that the DNE successfully recruits students from rural areas of Northern Norway. Nearly, 87.5% have their first employment in community healthcare services. They continued to work in the rural areas and 85% still worked as nurses in 2012. The DNE programme has been successful regarding recruitment and retention of RNs to community healthcare services. Fifty-six percent have attended a variety of postgraduate programmes. The DNE programme demonstrates itself as a successful study model regarding recruitment and retention of RNs to rural and remote areas.

  7. STS-35 Mission Manager Actions Room at the Marshall Space Flight Center Spacelab Payload Operations

    NASA Technical Reports Server (NTRS)

    1990-01-01

    The primary objective of the STS-35 mission was round the clock observation of the celestial sphere in ultraviolet and X-Ray astronomy with the Astro-1 observatory which consisted of four telescopes: the Hopkins Ultraviolet Telescope (HUT); the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE); the Ultraviolet Imaging Telescope (UIT); and the Broad Band X-Ray Telescope (BBXRT). The Huntsville Operations Support Center (HOSC) Spacelab Payload Operations Control Center (SL POCC) at the Marshall Space Flight Center (MSFC) was the air/ground communication channel used between the astronauts and ground control teams during the Spacelab missions. Teams of controllers and researchers directed on-orbit science operations, sent commands to the spacecraft, received data from experiments aboard the Space Shuttle, adjusted mission schedules to take advantage of unexpected science opportunities or unexpected results, and worked with crew members to resolve problems with their experiments. Due to loss of data used for pointing and operating the ultraviolet telescopes, MSFC ground teams were forced to aim the telescopes with fine tuning by the flight crew. This photo captures the activities at the Mission Manager Actions Room during the mission.

  8. Spacelab

    NASA Image and Video Library

    1995-03-02

    ASTRO-2 was the second dedicated Spacelab mission to conduct astronomical observations in the ultraviolet spectral regions. It consisted of three unique instruments: the Hopkins Ultraviolet Telescope (HUT), the Ultraviolet Imaging Telescope (UIT) and the Wisconsin Ultraviolet Photo-Polorimeter Experiment ((WUPPE). These experiments selected targets from a list of over 600 and observed objects ranging from some inside the solar system to individual stars, nebulae, supernova remnants, galaxies, and active extra galactic objects. This data supplemented data collected on the ASTRO-1 mission flown on the STS-35 mission in December 1990. Because most ultraviolet radiation is absorbed by Earth's atmosphere, it carnot be studied from the ground. The far and extreme ultraviolet regions of the spectrum were largely unexplored before ASTRO-1, but knowledge of all wavelengths is essential to obtain an accurate picture of the universe. ASTRO-2 had almost twice the duration of its predecessor, and a launch at a different time of year allows the telescopes to view different portions of the sky. The mission served to fill in large gaps in astronomers' understanding of the universe and laid the foundations for more discovery in the future. ASTRO-2, a primary payload of STS-67 flight, was launched on March 2, 1995 aboard the Space Shuttle Orbiter Endeavour.

  9. HUT Data Inspected at Marshall Space Flight Center During the STS-35 Mission

    NASA Technical Reports Server (NTRS)

    1990-01-01

    The primary objective of the STS-35 mission was round the clock observation of the celestial sphere in ultraviolet and X-Ray astronomy with the Astro-1 observatory which consisted of four telescopes: the Hopkins Ultraviolet Telescope (HUT); the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE); the Ultraviolet Imaging Telescope (UIT); and the Broad Band X-Ray Telescope (BBXRT). The Huntsville Operations Support Center (HOSC) Spacelab Payload Operations Control Center (SL POCC) at the Marshall Space Flight Center (MSFC) was the air/ground communication channel used between the astronauts and ground control teams during the Spacelab missions. Teams of controllers and researchers directed on-orbit science operations, sent commands to the spacecraft, received data from experiments aboard the Space Shuttle, adjusted mission schedules to take advantage of unexpected science opportunities or unexpected results, and worked with crew members to resolve problems with their experiments. Due to loss of data used for pointing and operating the ultraviolet telescopes, MSFC ground teams were forced to aim the telescopes with fine tuning by the flight crew. This photo captures the activity of viewing HUT data in the Mission Manager Actions Room during the mission.

  10. Around Marshall

    NASA Image and Video Library

    1990-12-04

    The primary objective of the STS-35 mission was round the clock observation of the celestial sphere in ultraviolet and X-Ray astronomy with the Astro-1 observatory which consisted of four telescopes: the Hopkins Ultraviolet Telescope (HUT); the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE); the Ultraviolet Imaging Telescope (UIT); and the Broad Band X-Ray Telescope (BBXRT). The Huntsville Operations Support Center (HOSC) Spacelab Payload Operations Control Center (SL POCC) at the Marshall Space Flight Center (MSFC) was the air/ground communication channel used between the astronauts and ground control teams during the Spacelab missions. Teams of controllers and researchers directed on-orbit science operations, sent commands to the spacecraft, received data from experiments aboard the Space Shuttle, adjusted mission schedules to take advantage of unexpected science opportunities or unexpected results, and worked with crew members to resolve problems with their experiments. Due to loss of data used for pointing and operating the ultraviolet telescopes, MSFC ground teams were forced to aim the telescopes with fine tuning by the flight crew. This photo captures the activity of WUPPE (Wisconsin Ultraviolet Photo-Polarimeter Experiment) data review at the Science Operations Area during the mission. This image shows mission activities at the Broad Band X-Ray Telescope (BBXRT) Work Station in the Science Operations Area (SOA).

  11. On the gate of Arctic footsteps: Doors open to foreign high schools

    NASA Astrophysics Data System (ADS)

    Manno, C.; Pecchiar, I.

    2012-12-01

    With the increased attention on the changing Arctic Region effective science education, outreach and communication need to be higher priorities within the scientific communities. In order to encourage the dissemination of polar research at educational levels foreign high school students and teachers were visiting Tromso University for a week. The project highlights the role of the universities as link between research and outreach. The first aim of this project was to increase awareness of foreign schools on major topics concerning the Arctic issues (from the economic/social to the environmental/climatic point of view). Forty three Italian high school students were involved in the laboratory activities running at the UiT and participated in seminars. Topics of focus were Ocean Acidification, Global Warming and the combined effects with other anthropogenic stressors. During their stay, students interviewed several scientists in order to allow them to edit a "visiting report" and to elaborate all the material collected. Back in Italy they performed an itinerant exhibition (presentation of a short movie, posters, and pictures) in various Italian schools in order to pass on their Arctic education experience. The project highlights the role of University as communicator of "climate related issues" in the international frame of the "new generation" of students.

  12. Hepatic sinusoidal cells in health and disease: update from the 14th International Symposium.

    PubMed

    Smedsrød, Bård; Le Couteur, David; Ikejima, Kenichi; Jaeschke, Hartmut; Kawada, Norifumi; Naito, Makoto; Knolle, Percy; Nagy, Laura; Senoo, Haruki; Vidal-Vanaclocha, Fernando; Yamaguchi, Noriko

    2009-04-01

    This review aims to give an update of the field of the hepatic sinusoid, supported by references to presentations given at the 14th International Symposium on Cells of the Hepatic Sinusoid (ISCHS2008), which was held in Tromsø, Norway, August 31-September 4, 2008. The subtitle of the symposium, 'Integrating basic and clinical hepatology', signified the inclusion of both basal and applied clinical results of importance in the field of liver sinusoidal physiology and pathophysiology. Of nearly 50 oral presentations, nine were invited tutorial lectures. The authors of the review have avoided writing a 'flat summary' of the presentations given at ISCHS2008, and instead focused on important novel information. The tutorial presentations have served as a particularly important basis in the preparation of this update. In this review, we have also included references to recent literature that may not have been covered by the ISCHS2008 programme. The sections of this review reflect the scientific programme of the symposium (http://www.ub.uit.no/munin/bitstream/10037/1654/1/book.pdf): 1. Liver sinusoidal endothelial cells. 2. Kupffer cells. 3. Hepatic stellate cells. 4. Immunology. 5. Tumor/metastasis. Symposium abstracts are referred to by a number preceded by the letter A.

  13. Constraints on sea to air emissions from methane clathrates in the vicinity of Svalbard

    NASA Astrophysics Data System (ADS)

    Pisso, Ignacio; Vadakkepuliyambatta, Sunil; Platt, Stephen Matthew; Eckhardt, Sabine; Allen, Grant; Pitt, Joseph; Silyakova, Anna; Hermansen, Ove; Schmidbauer, Norbert; Mienert, Jurgen; Myhre, Cathrine Lund; Stohl, Andreas

    2016-04-01

    Methane stored in the seabed in the form of clathrates has the potential to be released into the atmosphere due to ongoing ocean warming. The Methane Emissions from Arctic Ocean to Atmosphere (MOCA, http://moca.nilu.no/) proje sct conducted measurement campaigns in the vicinity of Svalbard during the summers of 2014 and 2015 in collaboration with the Centre for Arctic Gas Hydrate, Environment and Climate (CAGE, https://cage.uit.no/) and the MAMM (https://arcticmethane.wordpress.com) project . The extensive set of measurements includes air (BAe 146) and ship (RV Helmer Hansen) borne methane concentrations, complemented with the nearby monitoring site at Zeppelin mountain. In order to assess the atmospheric impact of emissions from seabed methane hydrates, we characterised the local and long range atmospheric transport during the aircraft campaign and different scenarios for the emission sources. We present a range of upper bounds for the CH4 emissions during the campaign period as well as the methodologies used to obtain them. The methodologies include a box model, Lagrangian transport and elementary inverse modelling. We emphasise the analysis of the aircraft data. We discuss in detail the different methodologies used for determining the upper flux bounds as well as its uncertainties and limitations. The additional information provided by the ship and station observations will be briefly mentioned.

  14. Spacelab

    NASA Image and Video Library

    1989-01-01

    In 1986, NASA introduced a Shuttle-borne ultraviolet observatory called Astro. The Astro Observatory was designed to explore the universe by observing and measuring the ultraviolet radiation from celestial objects. Astronomical targets of observation selected for Astro missions included planets, stars, star clusters, galaxies, clusters of galaxies, quasars, remnants of exploded stars (supernovae), clouds of gas and dust (nebulae), and the interstellar medium. Astro-1 used a Spacelab pallet system with an instrument pointing system and a cruciform structure for bearing the three ultraviolet instruments mounted in a parallel configuration. The three instruments were: The Hopkins Ultraviolet Telescope (HUT), which was designed to obtain far-ultraviolet spectroscopic data from white dwarfs, emission nebulae, active galaxies, and quasars; the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE) which was to study polarized ultraviolet light from magnetic white dwarfs, binary stars, reflection nebulae, and active galaxies; and the Ultraviolet Imaging Telescope (UIT) which was to record photographic images in ultraviolet light of galaxies, star clusters, and nebulae. The star trackers that supported the instrument pointing system were also mounted on the cruciform. Also in the payload bay was the Broad Band X-Ray Telescope (BBXRT), which was designed to obtain high-resolution x-ray spectra from stellar corona, x-ray binary stars, active galactic nuclei, and galaxy clusters. Managed by the Marshall Space Flight Center, the Astro-1 observatory was launched aboard the Space Shuttle Orbiter Columbia (STS-35) on December 2, 1990.

  15. Evidence for structural stacking and repetition in the greenstones of the Kalgoorlie district, western Australia

    NASA Technical Reports Server (NTRS)

    Martyn, J. E.

    1986-01-01

    Most previous stratigraphic interpretations of the southern part of the Norseman-Wiluna Greenstone Belt have proposed polycyclic sequences. These invoked two and sometimes three successive suites of mafic and/or ultimafic volcanics and intrusives separated by felsic volcanics and immature clastic sediments, however no distinctive lithological differences were reported between successive mafic-ultramaic sequences. When interpretations of the area further to the north are integrated, a total of four separate major mafic-ultramafic uites emerges for a large part of the Norseman-Wiluna Belt. Although the author does not intent to imply that all polycyclic stratigraphies are wrong in principle such a situation seems suspiciously over-complex and stimulates the need to look critically at the individual areas where the stratigraphies have seen erected. For the Kalgoorlie area in the south, some of the schemes have already provoked scepticism and a simpler model consisting of one cycle subject to structural repetition has been evolved by workers in the Geological Survey of Western Australia for part of this area. The latter drew attention to the carbon copy similarity between the elements of some polycyclic stratigraphies. Much more regionally extensive integrated structural and stratigraphic data is still required to evaluate the relationship between structure and stratigraphy more fully, an objective substantially limited by poor outcrop and deep weathering, but with due effort, far from unattainable.

  16. Space and Earth Sciences, Computer Systems, and Scientific Data Analysis Support, Volume 1

    NASA Technical Reports Server (NTRS)

    Estes, Ronald H. (Editor)

    1993-01-01

    This Final Progress Report covers the specific technical activities of Hughes STX Corporation for the last contract triannual period of 1 June through 30 Sep. 1993, in support of assigned task activities at Goddard Space Flight Center (GSFC). It also provides a brief summary of work throughout the contract period of performance on each active task. Technical activity is presented in Volume 1, while financial and level-of-effort data is presented in Volume 2. Technical support was provided to all Division and Laboratories of Goddard's Space Sciences and Earth Sciences Directorates. Types of support include: scientific programming, systems programming, computer management, mission planning, scientific investigation, data analysis, data processing, data base creation and maintenance, instrumentation development, and management services. Mission and instruments supported include: ROSAT, Astro-D, BBXRT, XTE, AXAF, GRO, COBE, WIND, UIT, SMM, STIS, HEIDI, DE, URAP, CRRES, Voyagers, ISEE, San Marco, LAGEOS, TOPEX/Poseidon, Pioneer-Venus, Galileo, Cassini, Nimbus-7/TOMS, Meteor-3/TOMS, FIFE, BOREAS, TRMM, AVHRR, and Landsat. Accomplishments include: development of computing programs for mission science and data analysis, supercomputer applications support, computer network support, computational upgrades for data archival and analysis centers, end-to-end management for mission data flow, scientific modeling and results in the fields of space and Earth physics, planning and design of GSFC VO DAAC and VO IMS, fabrication, assembly, and testing of mission instrumentation, and design of mission operations center.

  17. Fundamentals and recent advances in X-ray micro computed tomography (microCT) applied on thermal-fluid dynamics and multiphase flows

    NASA Astrophysics Data System (ADS)

    Santini, Maurizio

    2015-11-01

    X-ray computed tomography (CT) is a well-known technique nowadays, since its first practical application by Sir. G. Hounsfield (Nobel price for medicine 1979) has continually benefited from optimising improvements, especially in medical applications. Indeed, also application of CT in various engineering research fields provides fundamental informations on a wide range of applications, considering that the technique is not destructive, allowing 3D visualization without perturbation of the analysed material. Nowadays, it is technologically possible to design and realize an equipment that achieve a micrometric resolution and even improve the sensibility in revealing differences in materials having very radiotransparency, allowing i.e. to distinguish between different fluids (with different density) or states of matter (like with two-phase flows). At the University of Bergamo, a prototype of an X-ray microCT system was developed since 2008, so being fully operative from 2012, with specific customizations for investigations in thermal-fluid dynamics and multiphase flow researches. A technical session held at the UIT International Conference in L'Aquila (Italy), at which this paper is referring, has presented some microCT fundamentals, to allow the audience to gain basics to follow the “fil-rouge” that links all the instrumentation developments, till the recent applications. Hereinafter are reported some applications currently developed at Bergamo University at the X-ray computed micro-tomography laboratory.

  18. Spacelab

    NASA Image and Video Library

    1990-12-01

    In this photograph, the instruments of the Astro-1 Observatory are erected in the cargo bay of the Columbia orbiter. Astro-1 was launched aboard the the Space Shuttle Orbiter Columbia (STS-35) mission on December 2, 1990. The Astro Observatory was designed to explore the universe by observing and measuring the ultraviolet radiation from celestial objects. Astronomical targets of observation selected for Astro missions included planets, stars, star clusters, galaxies, clusters of galaxies, quasars, remnants of exploded stars (supernovae), clouds of gas and dust (nebulae), and the interstellar medium. Astro-1 used a Spacelab pallet system with an instrument pointing system and a cruciform structure for bearing the three ultraviolet instruments mounted in a parallel configuration. The three instruments were:The Hopkins Ultraviolet Telescope (HUT), the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE), and the Ultraviolet Imaging Telescope (UIT). Also in the payload bay was the Broad Band X-Ray Telescope (BBXRT). Scientific return included approximately 1,000 photographs of the ultraviolet sky in the most extensive ultraviolet imagery ever attempted, the longest ultraviolet spectral observation of a comet ever made, and data never before seen on types of active galaxies called Seyfert galaxies. The mission also provided data on a massive supergiant star captured in outburst and confirmed that a spectral feature observed in the interstellar medium was due to graphite. In addition, Astro-1 acquired superb observations of the Jupiter magnetic interaction with one of its satellites.

  19. Evidence for structural stacking and repetition in the greenstones of the Kalgoorlie district, western Australia

    NASA Astrophysics Data System (ADS)

    Martyn, J. E.

    Most previous stratigraphic interpretations of the southern part of the Norseman-Wiluna Greenstone Belt have proposed polycyclic sequences. These invoked two and sometimes three successive suites of mafic and/or ultimafic volcanics and intrusives separated by felsic volcanics and immature clastic sediments, however no distinctive lithological differences were reported between successive mafic-ultramaic sequences. When interpretations of the area further to the north are integrated, a total of four separate major mafic-ultramafic uites emerges for a large part of the Norseman-Wiluna Belt. Although the author does not intent to imply that all polycyclic stratigraphies are wrong in principle such a situation seems suspiciously over-complex and stimulates the need to look critically at the individual areas where the stratigraphies have seen erected. For the Kalgoorlie area in the south, some of the schemes have already provoked scepticism and a simpler model consisting of one cycle subject to structural repetition has been evolved by workers in the Geological Survey of Western Australia for part of this area. The latter drew attention to the carbon copy similarity between the elements of some polycyclic stratigraphies. Much more regionally extensive integrated structural and stratigraphic data is still required to evaluate the relationship between structure and stratigraphy more fully, an objective substantially limited by poor outcrop and deep weathering, but with due effort, far from unattainable.

  20. The UV-brightest Stars of M33 and Its Nucleus: Discovery, Photometry, and Optical Spectroscopy

    NASA Astrophysics Data System (ADS)

    Massey, Philip; Bianchi, Luciana; Hutchings, John B.; Stecher, Theodore P.

    1996-10-01

    We investigate the UV-brightest sources in the nearby galaxy M33. Our catalog of 356 sources is constructed from far-ultraviolet (FUV; 1500 A) and near-ultraviolet (NUV; 2400 A) images obtained with the Ultraviolet Imaging Telescope (UIT) matched with ground-based UBV data. We find that our survey is limited by the FUV flux and is complete to Flambda1500_ = 2.5 x 10^-15^ ergs cm^-2^ s^-1^ A^-1^, other than in the most crowded regions; this corresponds roughly to M_bol_ = -9.2 to -10.0 (or masses of 40-60 M_sun_), for T_eff_ = 50,000^deg^ to 10,000^deg^. We use Hubble Space Telescope (HST) WFPC2 images of several M33 fields to conclude that at least one-half of our sample is uncontaminated by unresolved neighbors, at least at the 0.1" (0.4 pc) level, a resolution similar to that achieved in the LMC from the ground. Spectral types have been obtained for 131 of our objects. We discuss the spatial distribution of the UIT sources, finding that they provide an excellent tracer of the spiral arm pattern and confirm that star formation continues in the nuclear region to the present day. Our survey has found a large number of O and early B-type supergiants, including stars as early as O6, but the optical spectroscopic sample is dominated by later type B supergiants, as these are the visually brighter. Among the brightest stars (both at 1500A and at V) are the "superluminous" Wolf-Rayet stars first discovered by Conti & Massey in the largest H II regions of M33; these objects are now known to be small groups of stars in modest analog to R136 in 30 Dor. In general, our survey has failed to detect the known W-R stars, as they are too faint, but we did find several new late-type WN stars and composite systems, which are brighter. Two stars of high absolute visual magnitude (M_V_ ~-9.0) are found to be B I + WN binaries, similar to HDE 269546 in the LMC; one of these is multiple at HST resolution. Most interesting, perhaps, is our finding six Ofpe/WN9 "slash" stars, five of them newly discovered. These stars show properties intermediate between those of Of and WN stars and are believed to be a quiescent form of luminous blue variables (LBVs). Our spectroscopy found five additional stars that are spectroscopically similar to the known LBVs of M33. One of these stars has recently been shown to be spectroscopically variable, and we suggest that all of these stars deserve continued scrutiny. The nucleus of M33 is the visually brightest object in our survey, and its UV colors are indicative of a hotter component than its optical photometry or spectral type would suggest. We discuss the possibility that the pointlike nucleus may contain a few interesting hot stars that dominate the light in the UV, and we make the comparison to the cluster of He I emission-line stars found near the center of the Milky Way. We comment on which color- magnitude and color-color plots make the best diagnostic tools for studying the hot, massive star population of a galaxy like M33.

  1. Spacelab

    NASA Image and Video Library

    1990-03-20

    This photograph was taken during the integration of the Astro-1 mission payloads at the Kennedy Space Center on March 20, 1990, showing the Broad Band X-Ray Telescope (BBXRT) at the left, as three telescopes for the Astro-1 Observatory are settled into the Orbiter Columbia payload bay. Above Earth's atmospheric interference, Astro-1 would make precise measurements of objects such as planets, stars, and galaxies in relatively small fields of view and would observe and measure ultraviolet radiation from celestial objects. The Astro-1 used a Spacelab pallet system with an instrument pointing system and a cruciform structure for bearing the three ultraviolet instruments mounted in a parallel configuration. The three instruments were: The Hopkins Ultraviolet Telescope (HUT), which was designed to obtain far-ultraviolet spectroscopic data from white dwarfs, emission nebulae, active galaxies, and quasars; the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE) which was to study polarized ultraviolet light from magnetic white dwarfs, binary stars, reflection nebulae, and active galaxies; and the Ultraviolet Imaging Telescope (UIT), which was to record photographic images in ultraviolet light of galaxies, star clusters, and nebulae. The star trackers that supported the instrument pointing system, were also mounted on the cruciform. Also in the payload bay was the Broad Band X-Ray Telescope (BBXRT), which was designed to obtain high-resolution x-ray spectra from stellar corona, x-ray binary stars, active galactic nuclei, and galaxy clusters. Managed by the Marshall Space Flight Center, the Astro-1 observatory was launched aboard the Space Shuttle Orbiter Columbia (STS-35) on December 2, 1990.

  2. Quantifying Methane Emissions from the Arctic Ocean Seabed to the Atmosphere

    NASA Astrophysics Data System (ADS)

    Platt, Stephen; Pisso, Ignacio; Schmidbauer, Norbert; Hermansen, Ove; Silyakova, Anna; Ferré, Benedicte; Vadakkepuliyambatta, Sunil; Myhre, Gunnar; Mienert, Jürgen; Stohl, Andreas; Myhre, Cathrine Lund

    2016-04-01

    Large quantities of methane are stored under the seafloor in the shallow waters of the Arctic Ocean. Some of this is in the form of hydrates which may be vulnerable to deomposition due to surface warming. The Methane Emissions from Arctic Ocean to Atmosphere MOCA, (http://moca.nilu.no/) project was established in collaboration with the Centre for Arctic Gas Hydrate, Environment and Climate (CAGE, https://cage.uit.no/). In summer 2014, and summer and autumn 2015 we deployed oceanographic CTD (Conductivity, Temperature, Depth) stations and performed state-of-the-art atmospheric measurements of CH4, CO2, CO, and other meteorological parameters aboard the research vessel Helmer Hanssen west of Prins Karl's Forland, Svalbard. Air samples were collected for isotopic analysis (13C, 2H) and quantification of other hydrocarbons (ethane, propane, etc.). Atmospheric measurements are also available from the nearby Zeppelin Observatory at a mountain close to Ny-Ålesund, Svalbard. We will present data from these measurements that show an upper constraint of the methane flux in measurement area in 2014 too low to influence the annual CH4 budget. This is further supported by top-down constraints (maximum release consistent with observations at the Helmer Hansen and Zeppelin Observatory) determined using FLEXPART foot print sensitivities and the OsloCTM3 model. The low flux estimates despite the presence of active seeps in the area (numerous gas flares were observed using echo sounding) were apparently due to the presence of a stable ocean pycnocline at ~50 m.

  3. Spirituality, Illness Unpredictability, and Math Anxiety Effects on Negative Affect and Affect-Management Coping for Individuals Diagnosed with Alpha-1 Antitrypsin Deficiency.

    PubMed

    Worthington, Amber K; Parrott, Roxanne L; Smith, Rachel A

    2018-04-01

    A growing number of genetic tests are included in diagnostic protocols associated with many common conditions. A positive diagnosis associated with the presence of some gene versions in many instances predicts a range of possible outcomes, and the uncertainty linked to such results contributes to the need to understand varied responses and plan strategic communication. Uncertainty in illness theory (UIT; Mishel, 1988, 1990) guided the investigation of efforts to feel in control and hopeful regarding genetic testing and diagnosis for alpha-1 antitrypsin deficiency (AATD). Participants included 137 individuals with AATD recruited from the Alpha-1 Research Registry who were surveyed about their subjective numeracy, anxiety about math, spirituality, perceptions of illness unpredictability, negative affect regarding genetic testing, and coping strategies about a diagnosis. Results revealed that experiencing more fear and worry contributed both directly and indirectly to affect-management coping strategies, operating through individual perceptions of illness unpredictability. The inability to predict the symptoms and course of events related to a genetic illness and anxiety regarding math heightened fear and worry. Spirituality lessened both illness unpredictability and negative affective responses to a diagnosis. Results affirm the importance of clinician and counselor efforts to incorporate attention to patient spirituality. They also illustrate the complexity associated with strategic efforts to plan communication about the different versions of a gene's effects on well-being, when some versions align with mild health effects and others with severe effects.

  4. Initial mass functions from ultraviolet stellar photometry: A comparison of Lucke and Hodge OB associations near 30 Doradus with the nearby field

    NASA Technical Reports Server (NTRS)

    Hill, Jesse K.; Isensee, Joan E.; Cornett, Robert H.; Bohlin, Ralph C.; O'Connell, Robert W.; Roberts, Morton S.; Smith, Andrew M.; Stecher, Theodore P.

    1994-01-01

    UV stellar photometry is presented for 1563 stars within a 40 minutes circular field in the Large Magellanic Cloud (LMC), excluding the 10 min x 10 min field centered on R136 investigated earlier by Hill et al. (1993). Magnitudes are computed from images obtained by the Ultraviolet Imaging Telescope (UIT) in bands centered at 1615 A and 2558 A. Stellar masses and extinctions are estimated for the stars in associations using the evolutionary models of Schaerer et al. (1993), assuming the age is 4 Myr and that the local LMC extinction follows the Fitzpatrick (1985) 30 Dor extinction curve. The estimated slope of the initial mass function (IMF) for massive stars (greater than 15 solar mass) within the Lucke and Hodge (LH) associations is Gamma = -1.08 +/- 0.2. Initial masses and extinctions for stars not within LH associations are estimated assuming that the stellar age is either 4 Myr or half the stellar lifetime, whichever is larger. The estimated slope of the IMF for massive stars not within LH associations is Gamma = -1.74 +/- 0.3 (assuming continuous star formation), compared with Gamma = -1.35, and Gamma = -1.7 +/- 0.5, obtained for the Galaxy by Salpeter (1955) and Scalo (1986), respectively, and Gamma = -1.6 obtained for massive stars in the Galaxy by Garmany, Conti, & Chiosi (1982). The shallower slope of the association IMF suggests that not only is the star formation rate higher in associations, but that the local conditions favor the formation of higher mass stars there. We make no corrections for binaries or incompleteness.

  5. Ultraviolet imaging telescope and optical emission-line observations of H II regions in M81

    NASA Technical Reports Server (NTRS)

    Hill, Jesse K.; Cheng, K.-P.; Bohlin, Ralph C.; Cornett, Robert H.; Hintzen, P. M. N.; O'Connell, Robert W.; Roberts, Morton S.; Smith, Andrew M.; Smith, Eric P.; Stecher, Theodore P.

    1995-01-01

    Images of the type Sab spiral galaxy M81 were obtained in far-UV and near-UV bands by the Ultraviolet Imaging Telescope (UIT) during the Astro-1 Spacelab mission of 1990 December. Magnitudes in the two UV bands are determined for 52 H II regions from the catalog of Petit, Sivan, & Karachentsev (1988). Fluxes of the H-alpha and H-beta emission lines are determined from CCD images. Extinctions for the brightest H II regions are determined from observed Balmer decrements. Fainter H II regions are assigned the average of published radio-H-alpha extinctions for several bright H II regions. The radiative transfer models of Witt, Thronson, & Capuano (1992) are shown to predict a relationship between Balmer Decrement and H-alpha extinction consistent with observed line and radio fluxes for the brightest 7 H II regions and are used to estimate the UV extinction. Ratios of Lyman continuum with ratios predicted by model spectra computed for initial mass function (IMF) slope equal to -1.0 and stellar masses ranging from 5 to 120 solar mass. Ages and masses are estimated by comparing the H-alpha and far-UV fluxes and their ratio with the models. The total of the estimated stellar masses for the 52 H II regions is 1.4 x 10(exp 5) solar mass. The star-formation rate inferred for M81 from the observed UV and H-alpha fluxes is low for a spiral galaxy at approximately 0.13 solar mass/yr, but consistent with the low star-formation rates obtained by Kennicutt (1983) and Caldwell et al. (1991) for early-type spirals.

  6. STS-67 crew insignia

    NASA Image and Video Library

    1994-10-01

    STS067-S-001 (October 1994) --- Observation and remote exploration of the Universe in the ultraviolet wavelengths of light are the focus of the STS-67/ASTRO-2 mission, as depicted in the crew patch designed by the crew members. The insignia shows the ASTRO-2 telescopes in the space shuttle Endeavour's payload bay, orbiting high above Earth's atmosphere. The three sets of rays, diverging from the telescope on the patch atop the Instrument Pointing System (IPS), correspond to the three ASTRO-2 telescopes -- the Hopkins Ultraviolet Telescope (HUT), the Ultraviolet Imaging Telescope (UIT), and the Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE). The telescopes are co-aligned to simultaneously view the same astronomical object, as shown by the convergence of rays on the NASA symbol. This symbol also represents the excellence of the union of the NASA teams and universality's in the exploration of the universe through astronomy. The celestial targets of ASTRO-2 include the observation of planets, stars and galaxies shown in the design. The two small atoms represent the search in the ultraviolet spectrum for the signature of primordial helium in intergalactic space left over from the Big Bang. The observations performed on ASTRO-2 will contribute to man's knowledge and understanding of the vast universe, from the planets in out system to the farthest reaches of space. The NASA insignia design for space shuttle flights is reserved for use by the astronauts and for other official use as the NASA Administrator may authorize. Public availability has been approved only in the forms of illustrations by the various news media. When and if there is any change in this policy, which is not anticipated, the change will be publicly announced. Photo credit: NASA

  7. Recent progresses of neural network unsupervised learning: I. Independent component analyses generalizing PCA

    NASA Astrophysics Data System (ADS)

    Szu, Harold H.

    1999-03-01

    The early vision principle of redundancy reduction of 108 sensor excitations is understandable from computer vision viewpoint toward sparse edge maps. It is only recently derived using a truly unsupervised learning paradigm of artificial neural networks (ANN). In fact, the biological vision, Hubel- Wiesel edge maps, is reproduced seeking the underlying independent components analyses (ICA) among 102 image samples by maximizing the ANN output entropy (partial)H(V)/(partial)[W] equals (partial)[W]/(partial)t. When a pair of newborn eyes or ears meet the bustling and hustling world without supervision, they seek ICA by comparing 2 sensory measurements (x1(t), x2(t))T equalsV X(t). Assuming a linear and instantaneous mixture model of the external world X(t) equals [A] S(t), where both the mixing matrix ([A] equalsV [a1, a2] of ICA vectors and the source percentages (s1(t), s2(t))T equalsV S(t) are unknown, we seek the independent sources approximately equals [I] where the approximated sign indicates that higher order statistics (HOS) may not be trivial. Without a teacher, the ANN weight matrix [W] equalsV [w1, w2] adjusts the outputs V(t) equals tanh([W]X(t)) approximately equals [W]X(t) until no desired outputs except the (Gaussian) 'garbage' (neither YES '1' nor NO '-1' but at linear may-be range 'origin 0') defined by Gaussian covariance G equals [I] equals [W][A] at the fixed point (partial)E/(partial)wi equals 0 resulted in an exact Toplitz matrix inversion for a stationary covariance assumption. We generalize AR by a nonlinear output vi(t+1) equals tanh(wiTX(t)) within E equals <[x(t+1) - vi(t+1)]2>, and the gradient descent (partial)E/(partial)wi equals - (partial)wi/(partial)t. Further generalization is possible because of specific image/speech having a specific histogram whose gray scale statistics departs from that of Gaussian random variable and can be measured by the fourth order cumulant, Kurtosis K(vi) equals - 3 2 (K greater than or equal to 0 super-G for speeches, K less than or equal to 0 sub-G for images). Thus, the stationary value at (partial)K/(partial)wi equals plus or minus 4 PTLwi/(partial)t can de-mix unknown mixtures of noisy images/speeches without a teacher. This stationary statistics may be parallel implemented using the 'factorized pdf code: (rho) (v1, v2) equals (rho) (v1) (rho) (v2)' occurred at a maximal entropy algorithm improved by the natural gradient of Amari. Real world applications are given in Part II, (Wavelet Appl-VI, SPIE Proc. Vol. 3723) such as remote sensing subpixel composition, speech segmentation by means of ICA de-hyphenation, and cable TV bandwidth enhancement by simultaneously mixing sport and movie entertainment events.

  8. Predicting the fate of methane emanating from the seafloor using a marine two-phase gas model in one dimension (M2PG1) - Example from a known Arctic methane seep site offshore Svalbard

    NASA Astrophysics Data System (ADS)

    Jansson, Pär; Ferré, Benedicte

    2017-04-01

    Transport of methane in seawater occurs by diffusion and advection in the dissolved phase, and/or as free gas in form of bubbles. The fate of methane in bubbles emitted from the seafloor depends on both bubble size and ambient conditions. Larger bubbles can transport methane higher into the water column, potentially reaching the atmosphere and contributing to greenhouse gas concentrations and impacts. Single bubble or plume models have been used to predict the fate of bubble mediated methane gas emissions. Here, we present a new process based two-phase (free and dissolved) gas model in one dimension, which has the capability to dynamically couple water column properties such as temperature, salinity and dissolved gases with the free gas species contained in bubbles. The marine two-phase gas model in one dimension (M2PG1) uses a spectrum of bubbles and an Eulerian formulation, discretized on a finite-volume grid. It employs the most up-to-date equations for solubility and compressibility of the included gases, nitrogen, oxygen, carbon dioxide and methane. M2PG1 is an extension of PROBE (Omstedt, 2011), which facilitates atmospheric coupling and turbulence closures to realistically predict vertical mixing of all properties, including dissolved methane. This work presents the model's first application in an Arctic Ocean environment at the landward limit of the methane-hydrate stability zone west of Svalbard, where we observe substantial methane bubble release over longer time periods. The research is part of the Centre for Arctic Gas Hydrate, Environment and Climate (CAGE) and is supported by the Research Council of Norway through its Centres of Excellence funding scheme grant No. 223259 and UiT. Omstedt, A. (2011). Guide to process based modeling of lakes and coastal seas: Springer.

  9. NORSE2015 - A Focused Experiment On Oil Emulsion Characterization Using PolSAR During the 2015 Norwegian Oil-On-Water Exercise

    NASA Astrophysics Data System (ADS)

    Holt, B.; Jones, C. E.; Brekke, C.; Breivik, O.; Skrunes, S.; Espeseth, M.

    2016-02-01

    A targeted experiment in characterizing the properties and development of mineral oil slicks was undertaken by NASA, UiT - The Arctic University of Norway, and the Norwegian Meteorological Institute during the 2015 Norwegian oil-on-water spill exercise in the North Sea (OPV2015). NORSE2015 (Norwegian Radar oil Spill Experiment) involved controlled release of plant oil and mineral emulsions of three different oil-to-water ratios, imaging of the slicks with satellite-borne synthetic aperture radars (SAR), and tracking their development with the NASA-UAVSAR instrument over a period of eight hours following release. During the experiment, in situ measurements were made from ship or aircraft with meteorological instruments, released drift buoys, and optical/IR imagers. The experiment was designed to provide validation data for development of a physical model relating polarization-dependent electromagnetic scattering to the dielectric properties of oil mixed with ocean water in a thick slick or emulsion. UAVSAR is a particularly low noise instrument, which enables detection of oil characteristics, and serves as the basis for a relative comparison of different radar frequencies and instruments in oil slick detection and characterization. The time series of UAVSAR polarimetric SAR (PolSAR) is used to track the spreading, movement, and change in backscatter of the different emulsion slicks and the plant oil, to look at movement relative to wind and wave directions, and to develop methods to differentiate between biogenic and mineral slicks based upon temporal changes in the slicks, including environment-driven changes. In this presentation, the experiment will be described and preliminary results presented. This work was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. The Norwegian experiment was partly financed by CIRFA - Centre for integrated remote sensing and forecasting for arctic operations.

  10. Star Formation in NGC 4631

    NASA Astrophysics Data System (ADS)

    Smith, A. M.; Collins, N. R.; Bohlin, R.; Fanelli, M. N.; Neff, S. G.; O'Connell, R. W.; Roberts, M. S.; Stecher, T. P.; Waller, W. H.

    1997-12-01

    The group of galaxies including NGC 4631 provides an outstanding example of a galaxy interaction accompanied by intensive star formation. FUV imagery, recorded by the Ultraviolet Imaging Telescope (UIT), exhibits very bright far- ultraviolet (FUV) emission corresponding to the H II regions cataloged by Crillon and Monet (1969). This data is, in our experience, extraordinary in that NCG 4631 is observed nearly edge-on and strong attenuation of FUV light could be anticipated. Analysis of the ultraviolet imagery together with ground-based data leads to the following conclusions. The average extinction internal to the bright FUV regions is low [E(B--V) = 0.31], which combined with the optical morphology implies that the FUV bright regions are close to the edge of the galactic disk. The FUV luminosity of that part of the galaxy which can be observed is 8.2 x 10(40) ergs/s and is about a factor 6 less than the FUV luminosities of M101 and M83. FUV colors, M152-U, M152-B and M152-V, when compared to the predicted colors from cluster formation models utilizing a Salpeter IMF imply an internal extinction like that of a non-30Dor LMC extinction curve (Fitzpatrick 1985). Instantaneous burst models indicate an average age of the FUV bright regions of about 6 Myr and a total created stellar mass of 2.8 x 10(7) Msun . If the measured colors are compared to continuous star formation models, star formation beginning about 100 Myr in the past and continuing to the present with a total star formation rate in the FUV bright regions of 0.026 Msun /yr is implied. The total number of OB stars in the H II regions comprising the large ring in the eastern part of the galaxy (Rand's Shell #1, 1993) is inferred to be 20,000. This number can be compared to Rand's estimate of 10,000 to 35,000 supernova-producing OB stars which are required to impart momentum to an expanding shell of hydrogen gas.

  11. Tracking paleo-SMT positions using a magnetic susceptibility proxy approach from sediments on the Arctic Vestnesa Ridge, offshore western Svalbard

    NASA Astrophysics Data System (ADS)

    Johnson, Joel; Phillips, Stephen; Panieri, Giuliana; Sauer, Simone; Knies, Jochen; Mienert, Jurgen

    2014-05-01

    Methane in marine sediments, often existing ephemerally as gas hydrate, constitutes one of the largest reservoirs of natural gas on Earth and fluxes of methane in marine sediments are an important component in the global carbon cycle. Tracking changes in past methane flux, however, remains difficult and there are few available proxies that persist through geologic time. CAGE - Centre for Arctic Gas Hydrate, Environment, and Climate initiates a ten year interdisciplinary research and education program aimed at achieving a quantitative understanding of feedbacks between methane in sub-seabed reservoirs, the seabed and the ocean. In our recent work on the Indian continental margin we document that drawdowns in magnetic susceptibility, constrained by magnetic properties, and integrated with core sedimentology, XRF elemental data, authigenic mineralogy, and pore water geochemistry, can be used to track the paleo-positions of the SMT (sulfate-methane transition). Relative positions of the SMT in marine sediments are controlled by the balance of methane and sulfate fluxes. The products of the anaerobic oxidation of methane at the SMT, hydrogen sulfide and bicarbonate, allow for the dissolution of detrital magnetite, and the precipitation of authigenic carbonates and iron sulfides. We recently obtained 21 gravity cores in and between active and inactive pockmarks along the crest of the Vestnesa Ridge, an Arctic gas and gas hydrate bearing contourite sediment drift located offshore western Svalbard. Magnetic susceptibility records from reference cores outside of pockmarks show the stratigraphy across the ridge is quite uniform, whereas magnetic susceptibility records within the pockmarks, with and without observed water column gas flares, are significantly depleted. Integration of multiple data sets from these records and comparison with reconstructions of paleo-methane emissions at the seafloor from benthic foraminifera will allow us to interpret these drawdowns in magnetic susceptibility as a function of changes in the sulfate and/or methane fluxes through time at these sites. Details on the CAGE research plan and organization can be found on www.cage.uit.no to foster opportunities for cross-disciplinary collaboration. The Centre of Excellence is funded by the Norwegian Research Council (grant No. 223259) over a period of ten years.

  12. Laser Induced Fluorescence Studies of Electrostatic Double Layers in an Expanding Helicon Plasma

    NASA Astrophysics Data System (ADS)

    Carr, Jerry, Jr.

    We report the first evidence of a laboratory double layer (DL) collapsing in the presence of an instability studied by Chakraborty Thakur et al. 1 with the use of time resolved laser induced fluorescence (LIF) studies. Higher time resolution studies then provided the first statistically validated proof of the correlation between the ion acoustic instability and a DL. Time-frequency analysis in the form of time resolved cross power spectra and continuous wavelet transforms were used to provide insight into beam formation. The implications of this work is that in the creation of strong DLs in expanding plasmas for plasma propulsion or other applications may be self-limited through instability growth. Over the past decade, experimental and theoretical studies have demonstrated the formation of stable, electrostatic, current-free double layers (CFDLs) in plasmas with a strong density gradient; typically a result of a divergent magnetic field. In this work, we present evidence for the formation of multiple double layers within a single divergent magnetic field structure. Downstream of the divergent magnetic field, multiple accelerated ion populations are observed through laser induced fluorescence measurements of the ion velocity distribution function. The formation of the multiple double layer structure is a strong function of the neutral gas pressure in the experiment. The similarity of the accelerated ion populations observed in these laboratory experiments to ion populations observed in reconnection outflow regions in the magnetosphere and in numerical simulations is also described. If ion energization during magnetic reconnection also results solely from acceleration in electric fields, these observations imply a prediction that the ion heating, i.e., the broadening of ion velocity distribution functions, reported in magnetic reconnection experiments is more accurately described by a superposition of differently accelerated ion populations. Therefore, the ion gheatingh rate during reconnection should scale as the square root of the cube of the charge per unit mass (q3/m)1/2 for ions with varying charge-to-mass ratios. A new RFEA probe was benchmarked on the low pressure CFDL plasmas produced in WVU HELIX-LEIA. This work was the result of collaboration between the University of Tromso (UiT) and WVU. LIF was used to confirm the RFEAs ability to detect a beam when one was present. The RFEA was also able to detect the presence of a beam when LIF techniques were limited by metastable quenching. The probefs limitations in dealing with ion focusing are discussed as well.

  13. THE RELIABILITY OF HAND-WRITTEN AND COMPUTERISED RECORDS OF BIRTH DATA COLLECTED AT BARAGWANATH HOSPITAL IN SOWETO

    PubMed Central

    Ellison, GTH; Richter, LM; de Wet, T; Harris, HE; Griesel, RD; McIntyre, JA

    2007-01-01

    This study examined the reliability of hand-written and computerised records of birth data collected during the Birth to Ten study at Baragwanath Hospital in Soweto. The reliability of record-keeping in hand-written obstetric and neonatal files was assessed by comparing duplicate records of six different variables abstracted from six different sections in these files. The reliability of computerised record-keeping was assessed by comparing the original hand-written record of each variable with records contained in the hospital’s computerised database. These data sets displayed similar levels of reliability which suggests that similar errors occurred when data were transcribed from one section of the files to the next, and from these files to the computerised database. In both sets of records reliability was highest for the categorical variable infant sex, and for those continuous variables (such as maternal age and gravidity) recorded with unambiguous units. Reliability was lower for continuous variables that could be recorded with different levels of precision (such as birth weight), those that were occasionally measured more than once, and those that could be measured using more than one measurement technique (such as gestational age). Reducing the number of times records are transcribed, categorising continuous variables, and standardising the techniques used for measuring and recording variables would improve the reliability of both hand-written and computerised data sets. OPSOMMING In hierdie studie is die betroubaarheid van handgeskrewe en gerekenariseerde rekords van ge boortedata ondersoek, wat versamel is gedurende die ‘Birth to Ten’ -studie aan die Baragwanath hospitaal in Soweto. Die betroubaarheid van handgeskrewe verloskundige en pasgeboortelike rekords is beoordeel deur duplikaatrekords op ses verskillende verander likes te vergelyk, wat onttrek is uit ses verskillende dele van die betrokke lêers. Die gerekenariseerde rekords se betroubaarheid is beoordeel deur die oorspronklike geskrewe rekord van elke veranderlike te vergelyk met rekords wat beskikbaar is in die hospitaal se gerekenariseerde databasis Hierdie datastelle her vergelykbare vlakke van betroubaarheid getoon, waaruit afgelei kan word dat soortgelyke foute voorkom warmeer data oorgeplaas word vaneen deeivan ’n lêer na ’n ander, en vanaf die lêer na die gerekenariseerde databasis. In albei stelle rekords was die betroubaarheid die hoogste vir die kategoriese veranderlike suigeling se geslag, en vir daardie kontinue veranderlikes (soos moeder se ouderdom en gravida) wat in terme van ondubbelsinmge eenhede gekodeer kan word. Kontinue veranderlikes wat op wisselende vlakke van akkuratheid gemeet word (soos gewig met geboorte), veranderlikes wat soms meer as een keer gemeet is, en veranderlikes wat voigens meer as een metingstegniek bepaal is (soos draagtydsouderdom), was minder betroubaar Deur die aantal kere wat rekords oorgeskryf moet word te verminder, kontinue veranderlikes tat kategoriese veranderlikes te wysig. en tegnieke vir meting en aantekening van veranderlikes te standardiseer, kan die betroubaarheid van sowel handgeskrewe as gerekenariseerde datastelle verbeter word. PMID:9287552

  14. Op weg naar een didactiek voor natuurkunde-experimenten op afstand : Ontwerp en evaluatie van een via internet uitvoerbaar experiment voor leerlingen uit het voortgezet onderwijs

    NASA Astrophysics Data System (ADS)

    Engelbarts, M. B. A.

    2009-02-01

    The subject of this thesis is a developmental study on “remote experimenting” in education. It concerns the development of a remote experiment that enables pre-university students to carry out a physics experiment at a distance via the internet. Remote experiments can offer several (practical) benefits when compared to conventional experiments but the desire to exploit these benefits put special demands on the design of the experiment, since the students might be conducting the experiment without a teacher in the vicinity. As a consequence of these demands it was decided to focus on exploring the possibilities and problems of remote experiments conducted in the absence of a teacher. The research was carried out in two cycles and focused on the development of a remote experiment that could be conducted autonomously by pre-university students to measure the speed of light in several media. This should answer the global question: What should a technically, as well as didactically, well-functioning remote experiment look like? The first cycle had an explorative character. It showed that technically the experiment already functioned quite well. However, many problems were observed concerning the content, and the way the students were tackling it. This led to two categories of recommendations. Concerning the content, the material should aim at making the students more aware of what they are doing and why they are doing it and several content related problems needed to be avoided. The second category of recommendations concerned the format of the material: the design and the working method. Special attention should be paid to designing a clear structure for the website and adding interaction and control, (feedback- and reflection facilities) to activate the students and guide them through the material. In the second research cycle these recommendations were followed by designing the material within the theoretical framework of the problem posing theory. A didactical structure was designed before writing the actual lesson material for the website describing the inter-related conceptual and content-related motivational pathway of the intended teaching-learning process. The lesson material was set up in such a way that the students are repeatedly confronted with a practical problem to solve and they play an active role in developing the method of measurement. Secondly, in an attempt to compensate for the absence of the teacher and support the teaching-learning process some format elements were developed and deployed like an automated question-, and feedback system that supported the students, activated them and gave them insight into their learning process and a ‘Where-am-I’-window that showed their current position within the material. This all had led to a technically as well as didactically well functioning remote experiment in which, at a global level, the line of reasoning was made explicit and recognizable for the students, and ad a local level was build up out of well connected successive activities and required the students to adopt an active attitude.

  15. An Ultraviolet/Optical Atlas of Bright Galaxies

    NASA Astrophysics Data System (ADS)

    Marcum, Pamela M.; O'Connell, Robert W.; Fanelli, Michael N.; Cornett, Robert H.; Waller, William H.; Bohlin, Ralph C.; Neff, Susan G.; Roberts, Morton S.; Smith, Andrew M.; Cheng, K.-P.; Collins, Nicholas R.; Hennessy, Gregory S.; Hill, Jesse K.; Hill, Robert S.; Hintzen, Paul; Landsman, Wayne B.; Ohl, Raymond G.; Parise, Ronald A.; Smith, Eric P.; Freedman, Wendy L.; Kuchinski, Leslie E.; Madore, Barry; Angione, Ronald; Palma, Christopher; Talbert, Freddie; Stecher, Theodore P.

    2001-02-01

    We present wide-field imagery and photometry of 43 selected nearby galaxies of all morphological types at ultraviolet and optical wavelengths. The ultraviolet (UV) images, in two broad bands at 1500 and 2500 Å, were obtained using the Ultraviolet Imaging Telescope (UIT) during the Astro-1 Spacelab mission. The UV images have ~3" resolution, and the comparison sets of ground-based CCD images (in one or more of B, V, R, and Hα) have pixel scales and fields of view closely matching the UV frames. The atlas consists of multiband images and plots of UV/optical surface brightness and color profiles. Other associated parameters, such as integrated photometry and half-light radii, are tabulated. In an appendix, we discuss the sensitivity of different wavebands to a galaxy's star formation history in the form of ``history weighting functions'' and emphasize the importance of UV observations as probes of evolution during the past 10-1000 Myr. We find that UV galaxy morphologies are usually significantly different from visible band morphologies as a consequence of spatially inhomogeneous stellar populations. Differences are quite pronounced for systems in the middle range of Hubble types, Sa through Sc, but less so for ellipticals or late-type disks. Normal ellipticals and large spiral bulges are fainter and more compact in the UV. However, they typically exhibit smooth UV profiles with far-UV/optical color gradients which are larger than any at optical/IR wavelengths. The far-UV light in these cases is probably produced by extreme horizontal branch stars and their descendants in the dominant, low-mass, metal-rich population. The cool stars in the large bulges of Sa and Sb spirals fade in the UV while hot OB stars in their disks brighten, such that their Hubble classifications become significantly later. In the far-UV, early-type spirals often appear as peculiar, ringlike systems. In some spiral disks, UV-bright structures closely outline the spiral pattern; in others, the disks can be much more fragmented and chaotic than at optical wavelengths. Contributions by bright active galactic nuclei (AGNs) to the integrated UV light in our sample range from less than 10% to nearly 100%. A number of systems have unusual UV-bright structures in their inner disks, including rings, compact knots, and starburst nuclei, which could easily dominate the UV light in high-redshift analogs. A significant but variable fraction of the far-UV light in spiral disks is diffuse rather than closely concentrated to star-forming regions. Dust in normal spiral disks does not control UV morphologies, even in some highly inclined disk systems. The heaviest extinction is apparently confined to thin layers and the immediate vicinity of young H II complexes; the UV light emerges from thicker star distributions, regions evacuated of dust by photodestruction or winds, or by virtue of strong dust clumpiness. Only in cases where the dust layers are disturbed does dust appear to be a major factor in UV morphology. The UV-bright plume of M82 indicates that dust scattering of UV photons can be important in some cases. In a companion paper, we discuss far-UV data from the Astro-2 mission and optical comparisons for another 35 galaxies, emphasizing face-on spirals.

  16. Messinian Salinity Crisis - DREAM (Deep-sea Record of Mediterranean Messinian events) drilling projects

    NASA Astrophysics Data System (ADS)

    Lofi, Johanna; Camerlenghi, Angelo

    2014-05-01

    About 6 My ago the Mediterranean Sea was transformed into a giant saline basin. This event, commonly referred to as the Messinian salinity crisis (MSC), changed the chemistry of the global ocean and had a permanent impact on both the terrestrial and marine ecosystems of a huge area surrounding the Mediterranean area. The first fascinating MSC scenario was proposed following DSDP Leg XIII in 1970 and envisaged an almost desiccated deep Mediterranean basin with a dramatic ~1,500 m drop of sea level, the incision of deep canyons by rivers on the continental margins, and a final catastrophic flooding event when the connections between the Mediterranean Sea and the Atlantic were re-established ~5.33 My ago. In spite of 40 years of multi-disciplinary research conducted on the MSC, modalities, timing, causes, chronology and consequence at local and planetary scale are still not yet fully understood, and the MSC event remains one of the longest-living controversies in Earth Science. Key factor for the controversy is the lack of a complete record of the MSC preserved in the deepest Mediterranean basins. Anywhere else, the MSC mostly generated a sedimentary/time lag corresponding to a widespread erosion surface. Correlations with the offshore depositional units are thus complex, preventing the construction of a coherent scenario linking the outcropping MSC evaporites, the erosion on the margins, and the deposition of clastics and evaporites in the abyssal plains. Recent activity by various research groups in order to identify locations for multiple-site drilling (including riser-drilling) in the Mediterranean Sea that would contribute to solve the open questions still existing about the MSC has culminated in two DREAM Magellan+ Workshops held in 2013 and 2014. A strategy and work plan have been established in order to submit an IODP Multi-phase Drilling Project("Uncovering A Salt Giant")including several site-specific drilling proposals addressing different scientific objectives related to the MSC. Among these proposals, one will be fully dedicated to the MSC event. Improved quality of seismic data has allowed important advances in the recognition and understanding of MSC seismic markers (surfaces and depositional units) and lithological and stratigraphical calibrations are now critical. Therefore, the drilling strategy must include multiple sites covering representative locations of both Western and Eastern Mediterranean basins. A series of critical drilling targets were thus identified as follows: - A first set of drilling targets, dedicated to shallow water (< 2500 m water depth) MSC markers, includes the Messinian clastic wedges, the erosion surfaces and the MSC deposits (including thin salt bodies) trapped in small topographic lows observed at various water depths between the shoreline and the abyssal plain. Up to 10 sites, presented in this work, could be drilled with the riserless R/V Joides Resolution, provided the safety conditions are met; - Another critical drilling target is the full recovering of undeformed MSC sequence (including the Tortonian-Messinian and the Messinian-Zanclean boundaries) in the deep water (>2500m) of both the eastern and western Mediterranean basins. This will be possible thanks to R/V Chikyu riser drilling vessel and will be the scope of a second MSC IODP proposal. DREAM Team: A. Giovanni galod@locean-ipsl.upmc.fr, H. Christian huebscher@zmaw.de, G. deLangeGert gdelange@geo.uu.nl, R. Flecker r.flecker@bristol.ac.uk, D. Garcia-Castellanos danielgc@ictja.csic.es, C. Gorini gorini@upmc.fr, Z. Gvirtzman zohar@gsi.gov.il, W. Krijgsman krijgsma@geo.uu.nl, S. Lugli lugli@unimore.it, I. Makowsky yizhaq@univ.haifa.ac.il, M. Vinicio vinicio.manzi@unipr.it, T. McGenity tjmcgen@essex.ac.uk, G. Panieri giuliana.panieri@uit.no, M. Rabineau rabineau@univ-brest.fr, M. Roveri marco.roveri@unipr.it, F.J. Sierro sierro@usal.es, N. Waldman nwaldmann@univ.haifa.ac.il

  17. FOREWORD: IV International Time-Scale Algorithms Symposium, BIPM, Sèvres, 18-19 March 2002

    NASA Astrophysics Data System (ADS)

    Leschiutta, Sigfrido

    2003-06-01

    Time-scale formation, along with atomic time/frequency standards and time comparison techniques, is one of the three basic ingredients of Time Metrology. Before summarizing this Symposium and the relevant outcomes, let me make a couple of very general remarks. Clocks and comparison methods have today reached a very high level of accuracy: the nanosecond level. Some applications in the real word are now challenging the capacity of the National Metrological Laboratories. It is therefore essential that the algorithms dealing with clocks and comparison techniques should be such as to make the most of existing technologies. The comfortable margin of accuracy we were used to, between Laboratories and the Field, is gone forever. While clock makers and time-comparison experts meet regularly (FCS, PTTI, EFTF, CPEM, URSI, UIT, etc), the somewhat secluded community of experts in time-scale formation lacks a similar point of contact, with the exception of the CCTF meeting. This venue must consequently be welcomed. Let me recall some highlights from this Symposium: there were about 60 attendees from 15 nations, plus international institutions, such as the host BIPM, and a supranational one, ESA. About 30 papers, prepared in some 20 laboratories, were received: among these papers, four tutorials were offered; descriptions of local time scales including the local algorithms were presented; four papers considered the algorithms applied to the results of time-comparison methods; and six papers covered the special requirements of some specialized time-scale 'users'. The four basic ingredients of time-scale formation: models, noise, filtering and steering, received attention and were also discussed, not just during the sessions. The most demanding applications for time scales now come from Global Navigation Satellite systems; in six papers the progress of some programmes was described and the present and future needs were presented and documented. The lively discussion on future navigation systems led to the following four points: an overall accuracy in timing of one nanosecond is a must; the combined 'clock and orbit' effects on the knowledge of satellite position should be less than one metre; a combined solution for positioning and timing should be pursued; a 'new' time window (2 h to 4 h) emerged, in which the accuracy and stability parameters of the clocks forming a time scale for space application are to be optimized. That interval is linked to some criteria and methods for on-board clock corrections. A revival of interest in the time-proven Kalman filter was noted; in the course of a tutorial on past experience, a number of new approaches were discussed. Some further research is in order, but one should heed the comment: 'do not ask too much of a filter'. The Kalman approach is indeed powerful in combining sets of different data, provided that the possible problems of convergence are suitably addressed. Attention was also focused on the possibility of becoming victims of ever-present 'hidden' correlations. The TAI algorithm, ALGOS, is about 30 years old and the fundamental approach remains unchanged and unchallenged. A number of small refinements, all justified, were introduced in the 'constants' and parameters, but the general philosophy holds. In so far as the BIPM Time Section and the CCTF Working Group on Algorithms are concerned, on the basis of the outcome of this Symposium it is clear that they should follow the evolution of TAI and suggest any appropriate action to the CCTF. This Symposium, which gathered the world experts on T/F algorithms in Paris for two days, offered a wonderful opportunity for cross-fertilization between researchers operating in different and interdependent communities that are loosely connected. Thanks are due to Felicitas Arias, Demetrios Matsakis and Patrizia Tavella and their host organizations for having provided the community with this learning experience. One last comment: please do not wait another 14 years for the next Time Scale Algorithm Symposium.

  18. Chandra Detects Halo Of Hot Gas Around Milky Way-Like Galaxy

    NASA Astrophysics Data System (ADS)

    2001-07-01

    The first unambiguous evidence for a giant halo of hot gas around a nearby, spiral galaxy much like our own Milky Way was found by astronomers using NASA's Chandra X-ray Observatory. This discovery may lead to a better understanding of our own Galaxy, as well the structure and evolution of galaxies in general. A team of astronomers, led by Professor Daniel Wang of the University of Massachusetts, Amherst, observed NGC 4631, a spiral galaxy approximately 25 million light years from Earth with both Chandra and NASA's Hubble Space Telescope. While previous X-ray satellites have detected extended X-ray emission from this and other spiral galaxies, because of Chandra's exceptional resolution this is the first time that astronomers were able to separate the individual X-ray sources from the diffuse halo. Chandra found the diffuse halo of X-ray gas to be radiating at a temperature of almost 3 million degrees and extending some 25,000 light years from the galactic plane. "Scientists have debated for over 40 years whether the Milky Way has an extended corona, or halo, of hot gas," said Wang, lead author of the paper which appeared this month in The Astrophysical Journal Letters. "Of course since we are within the Milky Way, we can't get outside and take a picture. However, by studying similar galaxies like NGC 4631, we can get an idea of what's going on within our own Galaxy." The Chandra image reveals a halo of hot gas that extends for approximately 25,000 light years above the disk of the galaxy. One important feature of the X-ray emission from NGC 4631 is that it closely resembles the overall size and shape seen in the radio emission from the galaxy. This indicates that there may be a close connection between the outflows of hot gas, seen in X-rays, and the galaxy's magnetic field, revealed by radio emission. The Hubble image of NGC 4631 shows filamentary, loop-like structures enclosing enhanced X-ray-emitting gas and emanating from regions of recent star formation in the galaxy's disk. These data clearly show the hot gas is heated by clusters of massive stars and is now expanding into the halo of the galaxy. NGC 4631 X-ray: NASA/CXC/UMass/D.Wang et al. UV: NASA/GSFC/UIT "What we see in NGC 4631 can be thought of as the bursting flames of a gigantic cosmic camp fire," said Wang. "Using Chandra and Hubble together, we really get a complete story of what is happening in this galaxy." NGC 4631 is a galaxy that has high amounts of star formation, possibly triggered by interaction with neighboring galaxies. Such star formation might have created the conditions necessary to heat the gas seen by Chandra, as vast amounts of energy are released from supernovas and massive stars in star-forming regions - enough to lift the gas out of the plane of the galaxy. These new results provide important clues about the cycling of energy and mass in a galaxy like our own Milky Way and about the evolutionary history of galaxies, which are thought to be more active in star formation in the past than at the present. Other members of the research team include: Stefan Immler, University of Massachusetts; Rene Walterbos, New Mexico State University; James Lauroesch, Northwestern University, Evanston, IL, and Dieter Breitschwerdt, Max Plank Institute, Germany. Chandra observed NGC 4631 with its Advanced CCD Imaging Spectrometer (ACIS) instrument, which was developed for NASA by Pennsylvania State University, University Park, and Massachusetts Institute of Technology, Cambridge. NASA's Marshall Space Flight Center in Huntsville, AL, manages the Chandra program, and TRW, Inc., Redondo Beach, CA, is the prime contractor for the spacecraft. The Smithsonian's Chandra X-ray Center controls science and flight operations from Cambridge, MA.

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