Engineering Papers⌕ Search

SEARCH · Engineering Papers

Results for “mercury”

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.

Quote a phrase for an exact phrase match. Source license links do not imply unrestricted reuse.

At least 1,207 records · Page 67
All sourcesNASA NTRSDOE OSTI
NASA NTRS1998

Directional Solidification of Mercury Cadmium Telluride in Microgravity

Mercury cadmium telluride (MCT) has been directionally solidified for ten days in the Advanced Automated Directional Solidification Furnace (AADSF) on the second United States Microgravity Payload Mission (USMP-2). A second growth experiment is planned for the USMP-4 mission in November 1997. Results from USMP-2 demonstrated significant changes between microgravity and ground-based experiments, particularly in the compositional homogeneity. Changes were also observed during the microgravity mission which were dependent on the attitude of the space shuttle and the relative magnitudes of axial and transverse residual accelerations with respect to the growth axis of the crystal. Issues of shuttle operation, especially those concerned with safety and navigation, and the science needs of other payloads dictated the need for changes in attitude. One consequence for solidification of MCT in the USMP4 mission is the desire for a shorter growth time to complete the experiment without subjecting the sample to shuttle maneuvers. By using a seeded technique and a pre-processed boule of MCT with an established diffusion layer quenched into the solid, equilibrium steady state growth can be established within 24 hours, rather than the three days needed in USMP-2. The growth of MCT in AADSF during the USMP-4 mission has been planned to take less than 72 hours with 48 hours of actual growth time. A review of the USMP-2 results will be presented, and the rationale for the USMP-4 explained. Pre-mission ground based tests for the USN4P-4 mission will be presented, as will any available preliminary flight results from the mission.

Lechoczhy, Sandor L.↗
NASA NTRS1971

Selective Detection of Ambient CO with a Mercury Replacement Analyzer

A commercial available ambient CO analyzer based on low yield mercury replacement is described. Measurements of the effects of interfering reactions are reported. Hydrogen interferes to the extent of less than 10%. Selective detection of ambient carbon monoxide is verified.

Palanos, Paul N.↗
NASA NTRS1999

Global Simulation of Atmospheric Mercury Concentrations and Deposition Fluxes

Results from a numerical model of the global emissions, transport, chemistry, and deposition of mercury (Hg) in the atmosphere are presented. Hg (in the form of Hg(O) and Hg(II)) is emitted into the atmosphere from natural and anthropogenic sources (estimated to be 4000 and 2100 Mg/ yr, respectively). It is distributed between gaseous, aqueous and particulate phases. Removal of Hg from the atmosphere occurs via dry deposition and wet deposition, which are calculated by the model to be 3300 and 2800 Mg/ yr, respectively. Deposition on land surfaces accounts for 47% of total global deposition. The simulated Hg ambient surface concentrations and deposition fluxes to the Earth's surface are consistent with available observations. Observed spatial and seasonal trends are reproduced by the model, although larger spatial variations are observed in Hg(O) surface concentrations than are predicted by the model. The calculated atmospheric residence time of Hg is -1.7 years. Chemical transformations between Hg(O) and HG(II) have a strong influence on Hg deposition patterns because HG(II) is removed faster than Hg(O). Oxidation of Hg(O) to HG(II) occurs primarily in the gas phase, whereas HG(II) reduction to Hg(O) occurs solely in the aqueous phase. Our model results indicated that in the absence of the aqueous reactions the atmospheric residence time of Hg is reduced to 1.2 from 1.7 years and the Hg surface concentration is -25% lower because of the absence of the HG(II) reduction pathway. This result suggests that aqueous chemistry is an essential component of the atmospheric cycling of Hg.

Shia, Run-Lie↗
NASA NTRS2000

Radar Images of the Kuiper Quadrangle (Mercury) from Goldstone Radar Data

We have assembled all currently processed radar data from 1989 to 1998 into crude images covering the Kuiper (H6) region on Mercury. The data used were taken to support the ephemeris improvement and gravitational physics programs; however, the resolution is good enough in some cases to make north/south ambiguous images that show some features that can be identified with the Mariner 10 features. Topography profiles along the apparent equator are also available; some of these profiles show ridges and rills as well as crater depths and diameters. The combination of the optical imaging and the radar imaging can be helpful in understanding similar features in radar images of the optically unimaged hemisphere.

Jurgens, R. F.↗
NASA NTRS2000

Mercury, Skylab, Spacehab, International Space Station: A Continuum

We have conducted real research in space. Virtually all that we conducted in the first decade and a half of the space age was government funded and basic research like the carrier vehicles we call satellites and Sputniki, but direction human interaction began with Project Mercury. When the Apollo program ended with success, we got back to research again. Skylab was using Apollo hardware, using Apollo systems in a manner that offered spacious accomodations for researchers. Education began to move into space. This document describes Skylab's role in spaceborne experiments.

Walker, Charles↗
NASA NTRS2001

Workshop on Mercury: Space Environment, Surface, and Interior

This volume contains abstracts that have been accepted for presentation at the Workshop on Mercury: Space Environment, Surface, and Interior, October 4-5, 2001. The Scientific Organizing Committee consisted of Mark Robinson (Northwestern University), Marty Slade (Jet Propulsion Laboratory), Jim Slavin (NASA Goddard Space Flight Center), Sean Solomon (Carnegie Institution), Ann Sprague (University of Arizona), Paul Spudis (Lunar and Planetary Institute), G. Jeffrey Taylor (University of Hawai'i), Faith Vilas (NASA Johnson Space Center), Meenakshi Wadhwa (The Field Museum), and Thomas Watters (National Air and Space Museum). Logistics, administrative, and publications support were provided by the Publications and Program Services Departments of the Lunar and Planetary Institute.

Source record↗
NASA NTRS2001

Mid-Infrared Spectra of Mercury

Mid-infrared (8-13 microns) spectra of radiation emitted from the surface of solar system objects can be interpreted in terms of surface composition. However, the spectral features are weak, and require exceptionally high signal-to-noise ratio spectra to detect them. Ground-based observations of spectra in this region are plagued by strong atmospheric absorptions from water and ozone. High-altitude balloon measurements that avoid atmospheric absorptions can be affected by contamination of the optics by dust. We have developed a technique to obtain mid-infrared spectra of Mercury that minimizes these problems. The resulting spectra show evidence of transparency features that can be used to qualitatively characterize the surface composition. Additional information is contained in the original extended abstract.

Cooper, B.↗
NASA NTRS2002

Tidal Dissipation in Mercury

The spatial pattern and total inventory of tidal dissipation within Mercury depends sensitively on internal structure and on orbital eccentricity. Surface heat flow from this source may exceed 3 mW/sq m, and will vary with time as the orbital eccentricity fluctuates. Additional information is contained in the original extended abstract.

Bills, B. G.↗
NASA NTRS2002

Reference Atmosphere for Mercury

The objectives of this three year proposal are: (1) to calculate the likely diffusive flux of Ar and He from the interior of Mercury for representative crustal compositions; (2) compute a reasonable estimate of the fractional escape flux of photoions for the likely range of field conditions; and (3) to calculate the capture rate of solar wind ions into the atmosphere. The morphology of the magnetosphere in response to the solar wind and the IMF is the crucial boundary condition for the flux of ions to the surface. We have tackled problem (1) using a multipath diffusion code, and problems (2) and (3) using a combination of MHD and kinetic plasma dynamics.

Killen, Rosemary M.↗
NASA NTRS1947

Investigation of 10-Stage Axial-Flow X24C-2 Compressor: Performance at Inlet Pressure of 21 Inches Mercury Absolute and Inlet Temperature of 538 R - 1

The performance at inlet pressure of 21 inches mercury absolute and inlet temperature of 538 R for the 10-stage axial-flow X24C-2 compressor from the X24C-2 turbojet engine was investigated. the peak adiabatic temperature-rise efficiency for a given speed generally occurred at values of pressure coefficient fairly close to 0.35.For this compressor, the efficiency data at various speeds could be correlated on two converging curves by the use of a polytropic loss factor derived.

Schum, Harold J.↗
NASA NTRS2003

Determination of Mercury Content in a Shallow Firn Core from Summit, Greenland by Isotope Dilution Inductively Coupled Plasma Mass Spectrometry

The total mercury Hg content was determined in 6 cm sections of a near-surface 7 m firn core and in surrounding surface snow from Summit, Greenland (elevation: 3238 m, 72.58 N, 38.53 W) in May 2001 by isotope dilution cold-vapor inductively coupled plasma mass spectrometry (ID-CV-ICP-MS). The focus of this research was to evaluate the capability of the ID-CV-ICPMS technique for measuring trace levels of Hg typical of polar snow and firn. Highly enriched Hg-201 isotopic spike is added to approximately 10 ml melted core and thoroughly mixed. The Hg(+2) in the sample is reduced on line with tin (II) chloride (SnCl2) and the elemental Hg (Hg(0)) vapor pre-concentrated on to gold gauze using a commercial amalgam system. The Hg is then thermally desorbed and introduced into a quadrupole ICP-MS. The blank corrected Hg concentrations determined for all samples ranged from 0.25 ng/L to 1.74 ng/L (ppt) (average 0.59 ng/L plus or minus 0.28 ng/L) and fall within the range of those previously determined by Boutron et al., 1998 (less than or equal to 0.05 ng/L to 2.0 ng/L) for the Summit site. The average blank value was 0.19 ng/L plus or minus 0.045 ng/L (n=6). The Hg values specifically for the firn core range from 0.25 ng/L to 0.87 ng/L (average 0.51 ng/L plus or minus 0.13 ng/L) and show both values declining with time and larger variability in concentration in the top 1.8 m.

Mann, Jacqueline L.↗
NASA NTRS2004

Mercury: First Spectra from 0.7 to 5.5 micron Support Low FeO and Feldspathic Composition

Spectral measurements of Mercury's surface indicate low or no FeO content as determined from the absence of absorptions centered near 0.9 and 1.2 m. These observations support previous observations. At the Moon these ab-sorption bands are ubiquitous at varying depths. We have obtained spectra from the Moon with the same instrumentation and telescope for comparison. The lunar results are shown in a companion abstract.

Sprague, A. L.↗
NASA NTRS2005

Condensation from Cluster-IDP Enriched Vapor Inside the Snow Line: Implications for Mercury, Asteroids, and Enstatite Chondrites

Enstatite chondrites (EC) contain highly reduced matrix minerals (e.g.- (Mg,Fe,Mn)S solid solution, CaS) that probably formed in thermodynamic equilibrium with a vapor phase. EC chondrules contain enstatite, Fs5 to Fs30, in which iron was reduced after formation, also by interaction with vapor [1, 2]. The origin and location of this reducing vapor bears upon the formation of the terrestrial planets (Mercury to Mars), the remnant chemical zoning of the asteroid belt (E, S, C, D-types), and the cosmochemistry of metals in the early solar system.

Ebel, D. S.↗