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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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At least 631 records · Page 35
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NASA NTRS1987

Infrared spectroscopic measurements of halogenated sink and reservoir gases in the stratosphere with the ATMOS instrument

The Atmospheric Trace Molecule Spectroscopy (ATMOS) instrument recorded 19 sets of interferograms during solar occultations in both the Northern and Southern Hemispheres over the course of the Spacelab 3 mission. The resulting IR spectra furnish concentration profiles for over 25 atmospheric species. Attention is presently given to the volume mixing ratio profiles for HCl and HF in the 15-60-km altitude region, retrieved from northern sunsets and southern sunrises. The HF/HCl ratios deduced are in good agreement with model predictions. The total atmospheric chlorine at 50 km is nearly all in the form of HCl.

Raper, O. F.↗
NASA NTRS1987

Rocket-borne spectroscopic measurements in the ultraviolet aurora - The Lyman-Birge-Hopfield bands

Ultraviolet emissions from earth aurora were observed at wavelengths between 1675 and 2075 A by a sounding rocket payload launched at Churchill, Canada, on Mar. 28, 1980. The emissions from the Lyman-Birge-Hopfield and Vegard-Kaplan bands of N2 were observed and analyzed to determine the relative populations of the v-prime = 0-6 levels of the a1pi(g) state and the v-prime = 4, 6, 7, and 8 levels of the A3Sigma(+)g state, respectively. The relative population of higher vibrational levels of the A3Sigma(+)g state are consistent with direct excitation and cascade. The relative populations of the vibrationa1 levels of the a1pi(g) state peak at v-prime = 2. Such a distribution has not been observed previously in the aurora.

Eastes, Richard W.↗
NASA NTRS1987

Mass spectroscopic facility

A mass spectrometer system is described. The investigations to be conducted with the completed facility will be concerned with the high-temperature out-gassing behavior of quartz ampoules and the vapor composition in crystal growth experiments. These will give some insight on the prevailing transport mechanisms in these crystal growth experiments and supply a realistic basis for the numerical modeling of heat and mass transfer in these systems.

Rosenberger, Franz↗
NASA NTRS1987

Raman spectroscopic investigations of Hg-Cd-Te melts

Raman scattering measurements are reported for a series of Hg sub1-xCd subxTe (with x less than or =0.2) materials from 295 K (room temperature) to 1126K (up to and above their liquidus temperatures), and for Hg sub1-xCd subxTe (x=0.3) at 285K. The samples were contained in high-temperature optically-flat fused silica cell. Variable temperature measurements were effected in a three-zone, high-temperature furnace equipped with optical windows, and monitored externally by three independently programmable temperature controllers. All studies were made in the backscattering geometry using the 5145 A line of an Ar+ ion laser, with incident power less than 250 mW, as the excitiation source. An intensity enhancement is observed for a mode in each of the compositions studied. The frequency of this mode varies with composition, 142/cm for HgTe, and 128/cm for both the Hg sub1-xCd subxTe (x=0.053 and 0.204) samples. In addition, a shift to lower frequency as a function of temperature is observed in all samples. This shift is most prominent for the x=0.053 sample. The temperature dependence of these modes as the liquidus temperatures are achieved and surpassed for these samples is presented as being associated with a structural transition in the Hg-rich compositions of the Hg sub1-xCd subxTe series. To our knowledge, this is the first reported study of Raman scattering by phonons in the melts of these materials.

Morrobel-Sosa, Anny↗
NASA NTRS1984

The calibration of photographic and spectroscopic films: The response of 2aO film to small dosages of alpha particles from 3/10th's rad to 8 rads at energy levels 153 MeV, 79 MeV and 47 MeV

The 2aO film, pre-exposed to a series of neutral density filters which on development under standard conditions will produce the standard H-D curve for that film, were then exposed to Alpha paricles with a dose range of 3/10ths rads to 8 rads while varying the energy of the particles using 153 MeV, 70 MeV, and 47 MeV, respectively. An analysis of the film shows that the 3/10th rad dose produces the lowest optical density changes at 70 MeV and 47 MeV. While the optical density readings for the darker patterns seem to oscillate and decrease when exposed to radiation dosages of 3/10th rads to 8 rads.

Hammond, E. C., Jr.↗
NASA NTRS1987

Relation of the spectroscopic reflectance of olivine to mineral chemistry and some remote sensing implications

High-resolution visible and near-IR diffuse spectral reflectance are used to systematically investigate apparent wavelength shifts as a function of mineral chemistry in the Fe/Mg olivine series from Fo(11) to Fo(91). The study also shows that trace amounts of nickel can be spectrally detected in the olivine structure. Significant compositional information can only be extracted at relatively high resolution, because the overall spectral characteristics of the olivines change only subtly as a function of the Fe/Mg ratio. This laboratory study is expected to aid in the interpretation of remotely sensed data from both terrestrial and extraterrestrial bodies. Terrestrial applications may include the recognition of ultramafic, ultrabasic, and basaltic terrains which in themselves may have mineral potential. Among extraterrestrial applications, the asteroids are obvious candidates for further examination. Some permutations of Fe-Mg-Ni relations in olivines are discussed as they apply to the interpretation of asteroid surfaces and other extraterrestrial bodies.

King, Trude V. V.↗
NASA NTRS1988

Spectroscopic observations of the high-ionization planetary nebula NGC 2242 and the H II region K4-45

New optical spectra of two suspected planetary nebulae, K4-45 and NGC 2242, are presented. It is shown that K4-45 (PK 96 + 1) is a reddened H II region with approximately solar abundances, excited by an early B type star. NGC 2242 (PK 170 + 15) is a planetary nebula of exceptionally high ionization, exhibiting He II, and forbidden Ne V, Ar V, Ne III, and O III emission lines. The lack of He I emission and the presence of strong forbidden Ne V and He II emission indicate an optically thin nebula that is ionized by a central star with an effective temperature greater than 100,000 K.

Garnett, Donald R.↗
NASA NTRS1988

A ground-based technique for millimeter wave spectroscopic observations of stratospheric trace constituents

Recent concern over possible long term stratospheric changes caused by the introduction of man-made compounds has increased the need for instrumentation that can accurately measure stratospheric minor constituents. The technique of radio spectroscopy at millimeter wavelengths was first used to observe rotational transitions of stratospheric ozone nearly two decades ago, but has not been highly developed until recently. A ground-based observing technique is reported which employs a millimeter-wave superheterodyne receiver and multichannel filter spectrometer for measurements of stratospheric constituents that have peak volume mixing ratios that are less than 10 to the -9th, more than 3 orders of magnitude less than that for ozone. The technique is used for an extensive program of observations of stratospheric chlorine monoxide and also for observations of other stratospheric trace gases such as (O-16)3, vibrationally excited (O-16)3, (O-18)2(O-16), N2O, HO2, and HCN. In the present paper, analysis of the observing technique is given, including the method of calibration and analysis of sources of error. The technique is found to be a reliable means of observing and monitoring important stratospheric trace constituents.

Parrish, A.↗
NASA NTRS1987

Ultraviolet views and spectroscopic clues

IUE observations of SN 1987A obtained on days 60-260 of 1987 are presented graphically and characterized in detail. Particular attention is given to the complex changes in the early spectra, the domination of the energy distribution by line blanketing after an initial cooling period, and the spectra of the survivors (stars 2 and 3 of Sk -69 deg 202). The later emergence of narrow UV emission lines is attributed to photoionization of N-rich gas in a circumstellar shell, probably ejected from the SN 1987A progenitor (star 1 of Sk -69 deg 202) during its red supergiant phase.

Kirshner, Robert P.↗
NASA NTRS1988

Gamma-ray spectroscopic tests for the anisotropy of accelerated particles in solar flares

The profiles of 0.429 and 0.478 MeV gamma-ray lines from Be-7 and Li-7 (produced by interactions of flare-accelerated alpha particles with ambient He in the solar atmosphere) and of the 4.438 MeV line from C-12 (produced by inelastic scattering of C-12 by accelerated protons) depend on the angular distribution of the interacting accelerated particles. The line profiles resulting from various assumed accelerated-particle angular distributions are calculated and it is shown that it will be possible to distinguish among them using observations of gamma-ray spectra from solar flares obtained with high resolution detectors.

Murphy, R. J.↗
NASA NTRS1988

Laboratory investigations of Mars - Chemical and spectroscopic characteristics of a suite of clays as Mars soil analogs

A model system of Mars soil analog materials (MSAMs) was prepared, and the properties of these clays, such as chemical composition, surface-ion composition, water adsorption isotherms, and reflectance spectra, were examined. The results of these studies, performed along with simulations of the Viking Labeled Release Experiement using MSAMs, indicate that surface iron and adsorbed water are important determinants of clay behavior, as evidenced by changes in reflectance, water absorption, and clay surface reactions. The paper discusses the relevance of these results to the two major questions raised by prior explorations of Mars: has there ever been abundant water on Mars, and why is the iron found in the Martian soil not readily seen in the reflectance spectra of the surface?

Banin, Amos↗
NASA NTRS1986

Photoelectrochemical fabrication of spectroscopic diffraction gratings

Photoelectrochemical etching was demonstrated as a means of fabricating a variety of periodic structures in semiconductors. The semiconductor is used as an electrode in an electrochemical cell, and is in contact with a liquid electrolyte. When the crystal is held at a positive voltage and illuminated, etching occurs in only the illuminated regions to a depth proportional to the illumination intensity and exposure time. In Phase 1, it was determined that diffraction gratings could be produced in gallium arsenide crystals by this method, using either a scanned focused laser beam or by uniform illumination of a ruling mask defined in metal or photoresist on the crystal surface. The latter approach was determined to produce V-grooves if the mask is oriented along certain crystallographic directions. These V-grooves were produced with an exceedingly smooth crystal morphology due to the highly controllable nature of the process and the mild electrolytes involved. The results form the basis for photoelectrochemical fabrication of deep, low pitch Eschelle gratings for use in high orders in NASA spectrographic instrumentation such as the Space Telescope Imaging Spectrograph.

Rauh, R. David↗
NASA NTRS1988

Spectroscopic investigation of the Cr to Tm energy transfer in Yttrium Aluminum Garnet (YAG) crystals

New and interesting schemes have recently been considered for the efficient operation of solid-state ionic laser systems. Often the available data on these systems were obtained only because they seemed directly related to the laser performance and provide no insight into the physical processes. A more systematic approach is desirable, where more attention is devoted to the elementary basic processes and to the nature of the mechanisms at work. It is with this aim that we have undertaken the present study. Yttrium Aluminum Garnet (Y4Al5O12), called YAG, has two desirable properties as host for rare earth impurities: (1) trivalent rare earth ions can replace the yttrium without any charge compensation problem, and (2) YAG crystals have high cutoff energies. The results of measurements and calculations indicate that the Cr(3+) ion in YAG can be used to sensitize efficiently the Tm(3+) ion.

Dibartolo, B.↗
NASA NTRS1989

The Cassini mission: Infrared and microwave spectroscopic measurements

The Cassini Orbiter and Titan Probe model payloads include a number of infrared and microwave instruments. This document describes: (1) the fundamental scientific objectives for Saturn and Titan which can be addressed by infrared and microwave instrumentation, (2) the instrument requirements and the accompanying instruments, and (3) the synergism resulting from the comprehensive coverage of the total infrared and microwave spectrum by the complement of individual instruments. The baseline consists of four instruments on the orbiter and two on the Titan probe. The orbiter infrared instruments are: (1) a microwave spectrometer and radiometer; (2) a far to mid-infrared spectrometer; (3) a pressure modulation gas correlation spectrometer, and (4) a near-infrared grating spectrometer. The two Titan probe infrared instruments are: (1) a near-infrared instrument, and (2) a tunable diode laser infrared absorption spectrometer and nephelometer.

Kunde, V. G.↗
NASA NTRS1988

Spectroscopic evidence supporting the gravitational lens hypothesis for 1635+267 A,B

The gravitational lens hypothesis is tested for 1613+267 A,B by comparing the detailed line widths and shapes of the 2799-A Mg II and semiforbidden 1909-A C-III lines in each component. Following subtraction of an interpolating polynomial fit to the continua and the determination of a single optimum scaling factor (an amplification ratio of 2.83), reasonable agreement between the profiles of both lines in the two composites is obtained. Comparison of these lines to those in an unrelated quasar with a similar redshift and apparent magnitude does not produce a good match. It is suggested that the observed match in the 1635+267 A,B spectra arises from gravitational lensing.

Turner, Edwin L.↗
NASA NTRS1987

A spectroscopic and photometric survey of OB+ stars

Image-tube spectra (with dispersions of 40-90 A/mm) and UBV photometry of OB+ stars have been obtained at Cerro Tololo and Kitt Peak. The survey is complete to galactic latitudes of + or - 30 deg for galactic longitudes of between 300 and 60 deg. Most of the stars are found to be O-type and B-type supergiants, and 378 new O-type and B-type detections have been identified.

Drilling, J. S.↗
NASA NTRS1987

Spectroscopic surveys of faint blue stars

Spectroscopy of 450 faint blue stars obtained with the spectrograph and intensified Reticon scanner on the 1.3 m telescope at the McGraw Hill Observatory located at Kitt Peak are examined. The study is limited to objects brighter than V = 17.0 in magnitude. It is found that the relative numbers of objects such as white dwarfs, QSOs and CVs in the Kisco survey (Noguchi et al. 1980) is similar to that in the survey of Green et al., (1986).

Wegner, Gary↗
NASA NTRS1989

Spectroscopic study of combustion diagnostics on hydroxyl radicals

Experimental observations of propane/air flames have been carried out. Measurements of hydroxyl (OH) radical concentration have been made using resonance line absorption techniques. A microwave-pumped low pressure discharge in argon and water vapor is employed to produce strong OH radical band radiation in the 308 nm region. This radiation is transmitted through the plume and absorption data is taken at various radial positions using an optical multichannel analyzer. This absorption data is used to compute OH number density using a model for the absorption band characteristics as a function of temperature based on an atlas of line strengths. A numerical computation of flow fields, temperature profile, OH number density and water vapor mass fraction profiles was carried out by using a technique of computational fluid dynamics (CFD). The results of CFD computation are compared with experimental observation with a good agreement.

Eskridge, Richard↗