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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 199 records · Page 11
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NASA NTRS1986

Absolute line intensities in CO2 bands near 4.8 microns

Absolute intensities for 726 unblended lines in 20 bands of C-12(O-16)2, C-13(O-16)2, O-16C-12O-18, and O-16C-12O-17 in the 4.8-micron spectral region have been determined using a natural sample of ultrahigh-purity CO2. Spectral data were recorded at low pressure (less than 10 torr) and room temperature with the Fourier transform spectrometer in the McMath solar telescope complex on Kitt Peak. Derived vibrational band intensities and coefficients of the F factor for each band were compared to values of the 1982 Air Force Geophysics Laboratory line parameters compilation. The present work fills out the CO2 lines in the 5-micron band systems. Lines in the strongest of these measured bands are being used to infer atmospheric pressure from high-resolution stratospheric spectra recorded during the Spacelab 3 Atmospheric Trace Molecule Spectroscopy experiment.

Rinsland, C. P.↗
NASA NTRS1986

Detection of water vapor in Halley's comet

Gaseous, neutral H2O was detected in the coma of comet Halley on 22.1 and 24.1 December 1985 Universal Time. Nine spectral lines of the nus band (2.65 micrometers) were found by means of a Fourier transform spectrometer on the NASA-Kuiper Airborne Observatory. The water production rate was about 6 x 10 to the 28th molecules per second on 22.1 December and 1.7 x 10 to the 29th molecules per second on 24.1 December UT. The numbers of spectral lines and their intensities are in accord with nonthermal-equilibrium cometary models. Rotational populations are derived from the observed spectral line intensities and excitation conditions are discussed. The ortho-para ratio was found to be 2.66 + or - 0.13, corresponding to a nuclear-spin temperature of 32 K (+5 K, -2 K), possibly indicating that the observed water vapor originated from a low-temperature ice.

Mumma, M. J.↗
NASA NTRS1987

Monodeuterated methane in the outer Solar System. Part 3: Its abundance on Titan

The 3 nu 2 band of CH3D has been detected in spectra of Titan recorded at 1.6 microns with the Fourier Transform Spectrometer (FTS) at the 4 m telescope of the Kitt Peak National Observatory (NOAO). We have obtained a value of the CH3D/CH4 mixing ratio of 6.6 (+6.6 or -3.3) x 10 to the -4 from a comparison between the observed Titan spectra and synthetic spectra. This value is approx. 2 times higher than the value measured on Uranus (de Bergh et al. 1986) and approx. 6 times higher than on Jupiter and on Saturn (Courtin et al. 1984; de Bergh et al. 1986). It corresponds to D/H of 1.65 (+1.65 or -0.8) x 10 the -4, nominally 8 times higher than the most commonly accepted value for the protosolar D/H = 2 x 10 to the -5 (Geiss and Reeves 1981). The value we find on Titan for D/H in methane is comparable to the D/H ratio measured in terrestrial H2O.

Debergh, C.↗
NASA NTRS1986

Temperatures of quiescent prominences measured from hydrogen Paschen and CaII IR lines

During 12 to 17 September 1983 a number of prominences were observed with the McMatch solar telescope of National Solar Observatories, using the Fourier transform spectrometer with a InSb detector (Brault 1979). The present study refers to three prominences observed 13 and 14 September. Prominence A: Large quiescent prominence at S28 E90 Prominence B. Stable prominence in weakly enhanced magnetic region at about NO8 E90 Prominence C: Quiescent prominence at N30 E90. Spectra were obtained at a total of 15 different locations in the three prominences in the wavelength range lambda, lambda 7740 to 14,000 Angstroms. The observed differences between T sub exc and T sub kin are hardly significant. Researchers conclude that the two methods for temperature determination when applied to optically thin lines give reasonably consistent results, i.e., the population of the excited levels of hydrogen is collisionally controlled. The well known increase in T and V towards the edge of equiescent prominences (Hirayama 1964) is not corroborated by the present data. One explanation for this could be that prominence A is atypical. The optical thickness of prominence emission lines tends to increase from center to edges as demonstrated by the case of He I lambda 10830 angstroms. If line opacity plays a significant role in earlier center to edge determinations of T and V, a smaller variation would be expected from measurements in optically thin lines, such as in the present case.

Engvold, Oddbjorn↗
NASA NTRS1987

Retrieval of upper atmosphere pressure-temperature profiles from high resolution solar occultation spectra

Pressure-temperature profiles over the 18 to 75 km altitude range were retrieved from 0.01 cm(-1) resolution infrared solar absorption spectra recorded with the Atmospheric Trace Molecule Spectroscopy (ATMOS) Fourier transform spectrometer operating in the solar occultation mode during the Spacelab 3 shuttle mission (April 30 to May 1, 1985). The analysis method is described and preliminary results deduced for five occultation events are compared to correlative pressure-temperature measurments.

Rinsland, C. P.↗
NASA NTRS1986

Airborne infrared investigation of water in the coma of Halley's Comet

An infrared Fourier transform spectrometer on the Kuiper Airborne Observatory (KAO) was used to obtain high resolution spectra of the intense, solar-pumped infrared fluorescent emission in the (001 to 000) band of H2O near 2.6 microns. Differences between the observed H2O excitation and original expectations are discussed, and KAO water production rates are compared to those derived from International Ultraviolet Explorer observations. Possible future directions for high resolution IR spectroscopy of comets are discussed.

Weaver, Harold A.↗
NASA NTRS1986

Search for methane in Comet Halley

A search for gaseous neutral CH4 was conducted in the coma of comet Halley on March 20, 1986 using a Fourier transform spectrometer on the Kuiper Airborne Observatory. In the field-of-view (24,000 km) the CH4 rotational temperature is equal to the kinetic temperature of the coma molecules due to collisions in most of the region and is frozen in at the outer edge. The spectrum of the nu3 band is due to fluorescence with the R(3) to R(5) lines being most suitable for Earth-based observations. Measured upper (3 delta) limits of 4 times 10 to the minus 19th power W/sqcm for these lines lead to a (7 delta) upper limit of 4 times 10 to the 28th power CH4 molecules per second. This value corresponds to 4% of the water vapor production rate at the time of observation.

Drapatz, S.↗
NASA NTRS1986

Evidence for the presence of the 802.7/cm band Q branch of HO2NO2 in high resolution solar absorption spectra of the stratosphere

Stratospheric solar absorption spectra recorded at about 0.01/cm resolution by the ATMOS (Atmospheric Trace Molecule Spectroscopy) Fourier transform spectrometer during the Spacelab 3 Shuttle mission (4/30-5/6/85) show a weak absorption feature covering about 802.5-803.3/cm. This feature is identified as the unresolved Q branch of the 802.7/cm band of HO2NO2 and profiles for 31 deg N and 47 deg S are reported.

Rinsland, C. P.↗
NASA NTRS1986

Spectroscopic detection of Ch3Cl in the upper troposphere and lower stratosphere

Absorptions due to the nu1 band of CH3Cl have been identified for the first time in infrared solar absorption spectra of the upper troposphere and lower stratosphere. The spectral data were obtained with the ATMOS Fourier transform spectrometer on board Spacelab 3 in May 1985 during four solar occultation events near latitudes of 30 deg N, 26 deg N, 25 deg N, and 49 deg S. Volume mixing ratio profiles of CH3Cl retrieved for the altitude range 12 to 23 km at these four latitudes do not show appreciable differences. Vertical mixing ratio distributions vary from 6 x 10 to the -10th at 12 km to 3 x 10 to the -10th at 23 km with an average uncertainty of about 25 percent. The retrieved mixing ratio does not decrease with altitude as rapidly as the data obtained by in situ techniques.

Park, J. H.↗
NASA NTRS1986

Analysis of far-infrared emission Fourier transform spectra

An analysis method that uses the nonlinear least-squares fit technique has been developed for emission spectra obtained with a Fourier transform spectrometer. This method is used for the analysis of submillimeter-region atmospheric emission spectra obtained with a balloon-borne FT spectrometer that was carried out as a correlative measurement for the Limb IR Monitor of the Stratosphere (LIMS) satellite experiment. The retrieved mixing ratios of H2O and O3 in the stratosphere from four spectral intervals have standard deviations of about 10 percent, and the average values agree to within 10 percent of corresponding results from the LIMS satellite experiment which used a broadband emission radiometer in the IR region.

Park, J. H.↗
NASA NTRS1986

Frequencies of N2O in the 1100- to 1440/cm region

The vibration-rotation frequency parameters of vibrational states of several isotopic species of N2O were determined from IR spectra obtained with a high-resolution Fourier-transform spectrometer. The bands in the 1100 to 1440/cm region were considered. The line frequencies, observed for the lines of the species (N-14)2(O-16), (N-14)(N-15)(O-16), (N-15)(N-14)(O-16), (N-14)2(O-18), (N-14)2(O-17), and (N-15)2(O-16) were analyzed to obtain values of the absolute band centers and upper-state and lower-state rotational constants.

Toth, R. A.↗
NASA NTRS1986

Monodeuterated methane in the outer solar system. II - Its detection on Uranus at 1.6 microns

The 3 nu 2 band of CH3D has been detected in the spectrum of Uranus recorded with the Fourier Transform Spectrometer at the 4 m Mayall telescope of Kitt Peak National Observatory. A scattering-model atmosphere and spectral synthesis techniques are used to derive a bulk CH3D/CH4 mixing ratio of 3.6 + 3.6 or - 2.8 x 10 to the -4th from these observations that suggests a deuterium enhancement in methane relative to that observed on Jupiter and Saturn.

De Bergh, C.↗
NASA NTRS1987

Infrared spectroscopy of IRC + 10420

High resolution 1.6, 3.3 and 4.6 micron spectra were obtained on the F8 supergiant star IRC + 10420 on June 9-11, 1984, using the 4 m Mayall telescope and Fourier Transform Spectrometer at Kitt Peak. IRC + 10420 is distinguished by its hydrogen maser, unusual for stars of this type. The measured column densities of CO led to an estimated isotopic carbon ratio of 7-11, supporting a model of the object as a highly evolved star. The redshift is interpreted as due to scattering by outward-moving circumstellar dust grains. The IR spectrum of IRC + 10420 suggests that the object is a post-asymptotic branch star still surrounded by the thick dust shell it produced while it was much cooler.

Fix, John D.↗
NASA NTRS1987

Evidence for stratospheric hydrogen peroxide

A statistically significant measurement of H2O2 in the stratosphere has been obtained. The results were obtained from the 112.19/cm RQ5 branch of the torsional-rotational spectrum with a remote-sensing far-infrared Fourier transform spectrometer during the Balloon Intercomparison Campaign (BIC-2), on June 20, 1983. The concentration above the balloon gondola is unexpectedly large, corresponding to 0.68 + or - 0.21 parts per billion by volume (ppbv) at an effective altitude of 38.3 km. Below the gondola altitude the concentration of H2O2 is slightly less than expected from the model predictions at 33.2 km (0.19 + or - 0.05 ppbv) and significantly less than expected at 29.3 km (0.08 + or - 0.03 ppbv).

Chance, K. V.↗
NASA NTRS1987

Molecular line parameters for the atmospheric trace molecule spectroscopy experiment

During its first mission in 1985 onboard Spacelab 3, the ATMOS (atmospheric trace molecule spectroscopy) instrument, a high speed Fourier transform spectrometer, produced a large number of high resolution infrared solar absorption spectra recorded in the occultation mode. The analysis and interpretation of these data in terms of composition, chemistry, and dynamics of the earth's upper atmosphere required good knowledge of the molecular line parameters for those species giving rise to the absorptions in the atmospheric spectra. This paper describes the spectroscopic line parameter database compiled for the ATMOS experiment and referenced in other papers describing ATMOS results. With over 400,000 entries, the linelist catalogs parameters of 46 minor and trace species in the 1-10,000/cm region.

Brown, L. R.↗
NASA NTRS1988

Measurements of air-broadened and nitrogen-broadened Lorentz width coefficients and pressure shift coefficients in the nu4 and nu2 bands of C-12H4

Air-broadened and N2-broadened halfwidth and pressure shift coefficients of 294 transitions in the nu4 and nu2 bands of C-12H4 have been measured from laboratory absorption spectra recorded at room temperature with the Fourier transform spectrometer in the McMath solar telescope facility of the National Solar Observatory. Total pressures of up to 551 Torr were employed with absorption paths of 5-150 cm, CH4 volume mixing ratios of 2.6 percent or less, and resolutions of 0.005 and 0.01/cm. A nonlinear least-squares spectral fitting technique has been utilized in the analysis of the twenty-five measured spectra. Lines up to J double-prime = 18 in the nu4 band and J double-prime = 15 in the nu2 band have been analyzed.

Rinsland, Curtis P.↗
NASA NTRS1988

Highly automated transmission-edge mapping

Instrumentation and software are described, which are used to determine maps of properties of materials based on optical transmission spectra. In addition to a Fourier transform spectrometer, the hardware includes an xy-stage containing a small stationary aperture and two computer controlled stepper motors for positioning the sample. This idea has been used for years but this implementation is highly automated compared to those previously described. All mapping has been in the 2-15 micron wavelength range but this is not an inherent limitation of the technique. In this spectral range, useful results may be obtained with apertures as small as 25 microns in diameter. The software is described including the algorithm for obtaining the cut-on wavelength from a semiconductor spectrum. Data from both transverse slices and longitudinal slabs of narrow bandgap alloy semiconductors are shown including composition maps for materials solidified with convex and concave growth interfaces.

Szofran, F. R.↗
NASA NTRS1988

Measurements of air-broadened and nitrogen-broadened half-widths and shifts of ozone lines near 9 microns

Air- and nitrogen-broadened half-widths and line shifts at room temperature for more than 60 individual vibration-rotation transitions in the nu1 fundamental band of (O-16)3 and several transitions in the nu3 band were determined from infrared absorption spectra. These spectra were recorded at 0.005/cm resolution with a Fourier-transform spectrometer. A tunable-diode-laser spectrometer operating in the 1090-1150/cm region was also used to record data on oxygen-, nitrogen-, and air-broadened half-widths for selected individual transitions. The nitrogen- and air-broadened half-widths determined by these two different measurement techniques are consistent to within 4 percent. The results are in good agreement with other published measurements and calculations.

Smith, M. A. H.↗