Thesis (M.A.)--Oregon State University, 1982. / Typescript (photocopy). Includes bibliographical references (leaves 97-105). Also available on the World Wide Web.

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International Telemetering Conference Proceedings / October 26-29, 1987 / Town and Country Hotel, San Diego, California / The Deep Space Network is responsible for the acquisition of in-situ science and engineering measurements and navigation data from spacecraft whose missions are to explore the Solar System. It must respond to new opportunities in the mission set supported so as to maintain or enhance mission science value. The large capital investment in such a Network mandates an evolutionary design approach wherein upgrades can be effected at low cost, and if appropriate, on existing capability. The 64-Meter antenna design, completed in 1963, is an example of this approach, in that it has permitted a relatively low-cost upgrade which increases performance significantly. The technology assessment was completed in 1975, and the option was exercised in 1986, when needed. Several key characteristics of the DSN design approach, the costs to upgrade performance over the past several decades, and some fundamental constraints on performance are discussed. Finally, the specific 70-Meter upgrade task and resulting overall benefits to Voyager-Neptune and the mission set are summarized.

Carbon Monoxide (CO) was discovered in the stratosphere of Neptune from the detection of the J=3-2 and J=2-1 rotational transitions in emission at 345.8 and 230.5 GHz respectively. It was conventionally thought that all of the atmospheric carbon should be in its reduced form of methane (CH₄). Two sources of stratospheric CO have been postulated: CO transported from the interior by convection due to Neptune's strong internal heat source (internal source); or, CO produced through photochemical reactions from an external supply of water (external source). <p>In this research project the J=3-2 transition of CO was observed to find the CO profile in Neptune's atmosphere and determine the mechanism producing CO. Three instruments were used at the James Clerk Maxwell Telescope (JCMT) to measure the CO line: the heterodyne receiver B3; the University of Lethbridge Fourier Transform Spectrometer (FTS); and, the Submillimeter Common User Bolometer Array (SCUBA). <p>The high resolution (1.25 MHz) of the heterodyne observations over a large frequency range (~20 GHz) produced a very powerful result because the narrow emission core from the stratosphere and the broad absorption feature arising in the lower atmosphere were measured simultaneously. The CO abundance profile was determined using a model of the J=3-2 CO transition in Neptune's atmosphere developed for this project. Calculations indicate a CO abundance of 1.9^+0.5_-0.3x10^-6 in the upper stratosphere and (0.8±0.2)x10^-6 in the lower stratosphere and troposphere. <p>The moderate resolution of the FTS data allowed the broad absorption feature to be measured. Uranus was originally chosen as the calibration source, but the discovery of CO in Uranus by Encrenaz et al. (2004), while this project was in progress, prompted both Neptune and Uranus to be examined for CO absorption. Two data sets (1993 and 2002) were analyzed and it was found that the 1993 spectra produced superior results, giving a CO mole ratio in the lower atmosphere between 0.8x10^-6 and 2x10^-5; this agrees, within the uncertainty limit, with the lower atmosphere heterodyne result. A tentative detection of CO in Uranus was also obtained from the 1993 data, with a CO abundance profile constrained to pressures greater than 0.5 bar with an abundance between 5x10^-7 and 1x10^-5. The 2002 data were found to be inferior to the 1993 data because of imperfect cancellation of thermal emission from the terrestrial atmosphere. <p> The 850ìm SCUBA filter profile is well matched to the width of the CO feature. Photometric observations of Neptune and Uranus were used to determine if the reduction in integrated flux due to CO absorption could be detected using SCUBA. A CO mole ratio in the range (1.2-1.7) x10^-6 was found for Neptune, calibrated against Uranus and assuming no CO in Uranus. Calibration of the Neptune and Uranus SCUBA data against Mars to produce an independent estimate of the CO abundance in both planets did not produce a useful result because of large calibration errors. <p>Comparison of the results from the three techniques determined that the heterodyne measurement was superior and the derived CO profile was used to determine the source of neptunian CO. It was concluded that the source of CO in Neptune is both internal and external. The lower atmosphere result indicates an interior dominated by water ice. The most likely mechanism for the upper atmosphere CO involves meteoritic ablation, photolysis of H₂O, and chemical reaction with by-products of methane photochemistry. The required H₂O influx for this mechanism is at least two orders of magnitude higher than previously observed, indicating either that the observed H₂O abundance is too small or that CO is produced by a different mechanism.

Carbon Monoxide (CO) was discovered in the stratosphere of Neptune from the detection of the J=3-2 and J=2-1 rotational transitions in emission at 345.8 and 230.5 GHz respectively. It was conventionally thought that all of the atmospheric carbon should be in its reduced form of methane (CH₄). Two sources of stratospheric CO have been postulated: CO transported from the interior by convection due to Neptune's strong internal heat source (internal source); or, CO produced through photochemical reactions from an external supply of water (external source). <p>In this research project the J=3-2 transition of CO was observed to find the CO profile in Neptune's atmosphere and determine the mechanism producing CO. Three instruments were used at the James Clerk Maxwell Telescope (JCMT) to measure the CO line: the heterodyne receiver B3; the University of Lethbridge Fourier Transform Spectrometer (FTS); and, the Submillimeter Common User Bolometer Array (SCUBA). <p>The high resolution (1.25 MHz) of the heterodyne observations over a large frequency range (~20 GHz) produced a very powerful result because the narrow emission core from the stratosphere and the broad absorption feature arising in the lower atmosphere were measured simultaneously. The CO abundance profile was determined using a model of the J=3-2 CO transition in Neptune's atmosphere developed for this project. Calculations indicate a CO abundance of 1.9^+0.5_-0.3x10^-6 in the upper stratosphere and (0.8±0.2)x10^-6 in the lower stratosphere and troposphere. <p>The moderate resolution of the FTS data allowed the broad absorption feature to be measured. Uranus was originally chosen as the calibration source, but the discovery of CO in Uranus by Encrenaz et al. (2004), while this project was in progress, prompted both Neptune and Uranus to be examined for CO absorption. Two data sets (1993 and 2002) were analyzed and it was found that the 1993 spectra produced superior results, giving a CO mole ratio in the lower atmosphere between 0.8x10^-6 and 2x10^-5; this agrees, within the uncertainty limit, with the lower atmosphere heterodyne result. A tentative detection of CO in Uranus was also obtained from the 1993 data, with a CO abundance profile constrained to pressures greater than 0.5 bar with an abundance between 5x10^-7 and 1x10^-5. The 2002 data were found to be inferior to the 1993 data because of imperfect cancellation of thermal emission from the terrestrial atmosphere. <p> The 850ìm SCUBA filter profile is well matched to the width of the CO feature. Photometric observations of Neptune and Uranus were used to determine if the reduction in integrated flux due to CO absorption could be detected using SCUBA. A CO mole ratio in the range (1.2-1.7) x10^-6 was found for Neptune, calibrated against Uranus and assuming no CO in Uranus. Calibration of the Neptune and Uranus SCUBA data against Mars to produce an independent estimate of the CO abundance in both planets did not produce a useful result because of large calibration errors. <p>Comparison of the results from the three techniques determined that the heterodyne measurement was superior and the derived CO profile was used to determine the source of neptunian CO. It was concluded that the source of CO in Neptune is both internal and external. The lower atmosphere result indicates an interior dominated by water ice. The most likely mechanism for the upper atmosphere CO involves meteoritic ablation, photolysis of H₂O, and chemical reaction with by-products of methane photochemistry. The required H₂O influx for this mechanism is at least two orders of magnitude higher than previously observed, indicating either that the observed H₂O abundance is too small or that CO is produced by a different mechanism.

Texte remanié de: Diss.--Philosophische Fakultät--Bonn--Rheinische-Friedrich-Wilhelms-Universität, Wintersemester 1993-94. / Notes bibliogr. Index.

North-East Pacific Undersea Network Experiments (NEPTUNE) is a multi-node cabled ocean observatory linked by 818 kilometers of powered fiber optic cable off-shore from Vancouver Island across the northern Juan de Fuca tectonic plate. It includes a Data Management and Archive Station (DMAS) at the University of Victoria (UVic) and a shore station at Port Alberni, BC, Canada. The core of the network consists of 6 branching units, 6 node stations, 13 junction boxes and more than 130 instruments. In this paper, we explore the costs and benefits of constructing a simulator for NEPTUNE using the OMNeT++ simulation platform---a C++ based discrete-event simulator. In this context, we present the design and implementation of a simple simulator that can work with a variety of configurations of instruments, where the instruments are connected to DMAS via junction boxes and branching units, and generate TCP and UDP traffic following certain patterns. The simulator is designed for supporting \emph{what-if} scenario analysis, particularly with respect to system evaluation and discovery of limits associated with network traffic behaviors. Our study reveals that, although building the simulator in OMNeT++ has many advantages such as ease of tuning and calibration, capturing sufficient details regarding the working behavior of the actual NEPTUNE environment is still challenging. A survey of alternative tools, including NS-2/NS-3, OPNET, JiST/SWANS, J-Sim, SSFNet, and Qualnet reveals that these nuances would not be any less challenging within these simulation environments. / Graduate

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The use of special operations forces has increased over the last decades. But the theories on how special operation forces best will be used to conduct special operations does not keep up with the development in the field. There are theories in the field of special operations, among them are Robert G. Spulak and William H McRaven. According to McRavens theory there are six principles that are to be met to be successful in a special operation. Robert G. Spulaks theory says that the personal attributes of the soldiers are essential for success. These two theoretical frameworks are used to examine one operation where special operations forces were used, Operation Neptune Spear. The purpose of this paper is to analyse the operation to see which of the theories that can explain the outcome. The operation is examined through a qualitative case study. The results of the study indicate that McRavens six principles can explain the outcome of the operation. The result also indicate that Spulaks theory can explain the outcome. Despite the differences in the theories both manage to explain the outcome of a special operation.

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