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Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.
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This paper presents a novel design of a deformed flat plate, wherein known amounts of distortion are introduced in a compensating flat plate, to recover the gain-loss due to the gravity-induced surface deformations of a large reflector antenna.
This paper discussed the thermal design and performance of the 6-meter hydroformed reflector antenna as well as projecting the performance of the Square Kilometer Array (SKA) 12-meter antenna.
The presentation addresses how to infer the front side temperatures for the Aquarius L-band reflector based upon backside measurement sites. Slides discussing the mission objectives and design details are at the same level found on typical project outreach websites and in conference papers respectively. The test discussion provides modest detail of an ordinary thermal balance test using mockup hardware. The photographs show an off-Lab vacuum chamber facility with no compromising details.
The realization of a large, space-based 10 meter class telescope for far-infrared/THz studies has long been a goal of NASA. Such a telescope could study the origins of stars, planets, molecular clouds, and galaxies; providing a much needed means of following-up on tantalizing results from recent successful missions such as Spitzer, Herschel, and SOFIA. Indeed, Herschel began its life in the US space program as the Large Deployable Reflector (LDR) to be assembled in low Earth orbit by shuttle astronauts. Escalating costs and smaller federal budget allocations resulted in a downsizing of the mission. However, by combining successful suborbital balloon and ground-based telescope technologies, the dream of a 10 meter class telescope free of ~99% of the Earth's atmospheric absorption in the far-infrared can be realized. The same telescope can also be used to perform sensitive, high spectral and spatial resolution limb sounding studies of the Earth's atmosphere in greenhouse gases such as CO, ClO, O3, and water, as well as serve as a high flying hub for any number of telecommunications and surveillance activities. Flight times of 100+ days will be possible, with instruments having mass and power requirements in excess of ~500 kg and ~1 kW.Here we present the results of our NIAC Step 1, Phase B design study where each key aspect of the LBR concept is discussed and recommendations made for further study in Phase II.These aspects include realization of a large spherical reflecting surface, spherical corrector, pointing system, instrument module, and service module/gondola. Once each hardware component is introduced, a typical LBR Mission profile is described that enables the realization of a stratospheric 10 meter THz observatory and limb sounder. Verification of the design approach was achieved by using a combination of analytical modelling, lab testing of materials and techniques, and building a 3 meter rooftop LBR prototype.
An Optimized thermal design for the SMILS Telescope has been developed. This design has demonstrated that the expected on-orbit lateral temperature gradient in the primary reflector has been minimized.
An advanced Microwave Limb Sounder (MLS), now in concept development for a potential future mission, is a space-borne heterodyne instrument to measure pressure, temperature, and atmospheric constituents from thermal emission between 120 and 2400 GHz. Previous MLS instruments used pencil-beam antennas sized to resolve N 1 vertical scale height. Current atmospheric models need better horizontal resolution than orbit spacing provides. To meet these needs, a new antenna concept combines the wide scan range of the parabolic torus with unblocked offset Cassegrain optics. The resulting system is diffraction-limited in the vertical plane but extremely astigmatic, with beamwidths 0.13~2.5. Nadir axis symmetry ensures that this Beam AspectRatio (BAR) is invariant over f33' of azimuth. The antenna can feed either an array of receivers or multiplexed low-noise receivers whose FOVs are swept by a small scanning mirror. We describe 3 stages of antenna design: First, using a paraxial-optics method, we choose conic profiles given vertical resolution orbit geometry, then develop the surfaces by nadir axis rotation, matching axisymmetric feeds to the BAR. A ray-trace program validates the design and generates alignment and deformation tolerances. Finally, a physical optics analysis verifies reflector surface currents and radiation patterns.
A detailed thermal analysis has been performed for a panel of a segmented primary mirror which is closest to the high side of the telescope sunshade. This panel was selected because the spatial temperature distribution was expected to be the worst. The JPL90-10 primary reflector panel configuration was investigated because of its superior figure error performance in ground-based testing.
To minimize shielding and overheating, a composite Fresnel cup reflector design directs the maximum energy from a light source. It consists of a uniformly ellipsoidal end surface and an extension comprising a series of confocal ellipsoidal and concentric spherical surfaces.
An accurately dimensioned convex ellipsoidal surface, which will become a master after polishing, is fabricated from 316L stainless steel. When polishing of the master is completed, it is suspended in a modified watt bath for electroforming of nickel reflectors.
Integration of induced current distribution equations yields the scattered radiation field from a hyperboloidal reflector antenna in a cassegrainian feed system
This paper describes the mechanical design of the horn-reflector antenna and the associated radome. The mechanical considerations dictating the final configuration of the antenna structure are discussed, along with the engineering aspects of the design, fabrication, and erection of the structure. The mechanical features of the data take-off and antenna drive systems are given in detail. The final section presents an account of the requirements, manufacture, and installation of the radome and its accessory equipment.
The conical horn-reflector antenna was selected for the satellite communication ground station because of its broadband and low-noise properties. Prior to the construction of the full-size antenna, theoretical and model studies of its electrical characteristics were undertaken. These studies consisted of computing gain and radiation patterns for two modes of excitation, constructing of model antennas and measuring them. Results of these studies are presented in this paper together with results of the measurements of the full size antenna at Andover, Maine.
Experimental data on wind induced vibrations of paraboloidal reflector antenna model
Load distributions on paraboloidal reflector antenna surfaces in wind tunnel test
Lunar corner reflector landing proposal for laser beam precision measurements including Moon orbit, size, ephemeris time and libration
Large compound curved surfaces for collecting and concentrating radiation are fabricated by the use of several common machining and forming processes. Lightweight sectors are assembled into large reflectors. With this concept of fabrication, integrally stiffened reflective sectors up to 25 square feet in area have been produced.
Calculated potential increase in solar cell array conversion efficiency with dispersion by prism reflector
Grating and networks of ribbons as radio reflectors