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At least 1,369 records · Page 76
All sourcesNASA NTRSDOE OSTI
NASA NTRS1982

Homogeneous and heterogeneous condensation of nitrogen in transonic flow

Onset of both homogeneous and heterogeneous nucleation for nitrogen gas has been measured in the Langley 0.3m Transonic Cryogenic Tunnel. Homogeneous nucleation data have been taken using a DFVLR CAST-10 airfoil and are used to evaluate classical liquid droplet theory and several proposed corrections to it. A correction for differences in translational energy states between the droplet and the bulk liquid due to either Reiss (1977) or Kikuchi (1977) achieves good agreement between the predicted onset of nucleation and the data. Good agreement is also found using a Tolman constant of 0.25 x 10 to the -10th m. Onset of heterogeneous nucleation on pre-existing seed particles in the flow has also been studied, and preliminary estimates of seed size and number are 0.25 x 10 to the -6th m and 3.0 x 10 to the 12th per kilogram of the gas. It is shown that this preexisting seed population is insufficient to influence the observed onset of homogeneous nucleation.

Hall, R. M.↗
NASA NTRS1981

Near optimum delay-line detection filters for serial detection of MSK signals

A method for designing transversal delay-line filter approximations to the matched filter for the serial detection of minimum-shift keyed (MSK) modulated signals is given. Two configurations are characterized in terms of signal-to-noise ratio degradation at a bit error rate (BER) of 10 to the -6th. One is shown to depart less than 0.3 dB from the ideal matched filter performance when its parameter values are optimized. A lumped-element equivalent is also given and shown to provide a degradation of less than 0.4 dB at a BER of 10 to the -6th

Ziemer, R. E.↗
NASA NTRS1982

The evolutionary state of zeta Aurigae

Ultraviolet studies, originally undertaken to ascertain the state of the atmosphere of the K-supergiant component of the zeta Aurigae system, have been sidetracked by the discovery of significant accretion effects. An analysis of the phase dependence of the profiles of resonance lines in Mg II and C IV has led to a qualitative model of the wind flow from the K star. At the position of the B star the flow velocity is about 100 km/sec and the density is 0.000003 per cu cm, leading to a mass loss rate of 2 x 10 to the -8th solar masses per year. This wind interacts with the B star in a shock, which will be described, leading to accretion on the B star at a rate of 4 x 10 to the -10th solar masses per year.

Chapman, R. D.↗
NASA NTRS1982

Mass flow due to heating in a binary system - Application to U Cephei

The possibility of mass flow due to the heating of the cooler component in a close binary system has been investigated. The heating may be caused by irradiation from the hotter companion or by other mechanisms such as the spacial coincidence of non-linear 'g-mode' oscillations in the cooler star. The 2.4-day period binary U Cep, in which gas streaming has been observed, has been chosen for model calculations. Preliminary results show that such a heating of the lower atmosphere of the cooler star could lead to mass flow at an average rate of 10 to the -9th - 10 to the -7th solar mass per year without the star necessarily filling its critical Roche surface.

Kondo, Y.↗
NASA NTRS1983

Detection of sulphur in the galactic center

A strong detection at the (SIII) 18.71 micron line is reported for the Galactic Center region, Sgr A West. A line flux of 1.7 + or - 0.2x10 to the -17th power W cm(-2) is found for a 20-arc second beam-size measurement centered on IRS 1. A preliminary analysis indicates that the SIII abundance relative to hydrogen is consistent with the cosmic abundance of sulfur, 1.6x10 to the -5th power, if a filling factor of unity within the known clumps is assumed. However, the sulfur abundance in the Galactic Center may be as much as a factor of 3 overabundant if a filling factor of 0.03 is adopted, a value found to hold for some galactic HII regions.

Herter, T.↗
NASA NTRS1983

The need for an intermediate mass scale in GUTs

The minimal SU(5) grand unified field theory (GUT) model fails to resolve the strong charge parity (CP) problem, suffers from the cosmological monopole problem, sheds no light on the nature of the 'dark' mass in the universe, and predicts an unacceptably low value for the baryon asymmetry. All these problems can be overcome in suitable grand unified axion models with an intermediate mass scale of about 10 to the 11th power to 10 to the 12th power GeV. An example based on the gauge group SO(10) is presented. Among other things, it predicts that the axions comprise the 'dark' mass in the universe, and that there exists a galactic monopole flux of 10 to the -8th power to 10 to the -7th power/sq cm/yr. Other topics that are briefly discussed include proton decay, family symmetry, neutrino masses and the gauge hierarchy problem.

Shafi, Q.↗
NASA NTRS1982

The abundances of CH4, CH3D, NH3, and PH3 in the troposphere of Jupiter derived from high-resolution 1100-1200/cm spectra

High-resolution spectra of the 1100-1200/cm region of the central part of Jupiter obtained in March 1980 and April 1981 are analyzed. The best fit NH3 distribution curve reveals a higher than solar mixing ratio, the abundance of NH3 to that of H2 being (3.3 + or - 1.7) x 10 to the -4th, below the 147 K layer (greater than 0.6 atmosphere). If NH3 ice particles are introduced as an opacity source, the NH3 mixing ratio below the 147 K layer can be lowered, but the fit is worse than that given by the model that excludes NH3 ice particles. The best fit PH3 distribution curve exhibits a PH3/H2 mixing ratio of (8.3 + or - 2.0) x 10 to the -7th in the troposphere. In addition, a CH4/H2 mixing ratio of (2.5 + or - 0.4) x 10 to the -3rd is found in the troposphere.

Knacke, R. F.↗
NASA NTRS1982

IUE high dispersion spectra of luminous stars in symmetric nebulae

The objects are + 60 deg 2522 in NGC 7635, Sigma Ori AB and Sigma Ori E centered in a faint elliptical nebula, and AG Car in its nebula. Definite spectra are identified and classified according to photospheric, P Cygni, or interstellar types. Estimates of equivalent width or FWHM are included in the tables. Velocities are given and discussed. The extreme ultraviolet edges of P Cygni profiles imply terminal wind speeds that improve to extend earlier velocity data for use in the theories of energy conserving or momentum conserving modes of interaction of stellar winds with ambient interstellar media. The respective modes lead to mass loss rates of 1-10 x 10 to the -7th solar masses per yr for + 60 deg 2522 and 6-14 x 10 to the -6th solar masses per yr for AG Car. The expansion velocity for the Sigma Ori nebula is not yet known for application of the interaction theory.

Johnson, H. M.↗
NASA NTRS1982

Kinetics of the reaction O + HO2 yields OH + O2 from 229 to 372 K

The discharge-flow resonance fluorescence technique has been used to obtain absolute rate data for the O + HO2 reaction from 229 to 372 K at a total pressure of 1 torr. Pseudo-first-order conditions were used with HO2 concentrations in large excess over initial atomic oxygen in order to minimize interference from secondary reactions. The results are independent of the method used to generate HO2 and atomic oxygen. At 299 K, the result is (6.1 + or - 0.4) x 10 to the -11th cu cm/molecule s. The temperature dependence expressed in Arrhenius form is (3.1 + or - 0.3) x 10 to the -11th exp/(+200 + or - 28)/T/. The error limits given are twice the standard deviation; overall experimental error is estimated to be + or - 25%.

Keyser, L. F.↗
NASA NTRS1983

The 157 micron /C II/ emission from NGC 2024 - Core and halo components

Portions of the nebula NGC 2024 were mapped in the 157 micron (C II) line. Results show the presence of a compact component centered on the radio-recombination line regions and a more extended nebulosity. It is found that the central component emits 157 micron line and continuum fluxes at a level of 4 x 10 to the -16th W/sq cm and 5 x 10 to the -16th W/sq cm (micron), respectively. The continuum emission drops off more rapidly with distance from the peak, although line emission is approximately 30% of the peak value at a distance 18 min to the SE of the peak. In addition, related observations were carried out on M42.

Kurtz, N. T.↗
NASA NTRS1983

HEAO A-2 soft X-ray source catalog

The HEAO A-2 low energy X-ray detectors have surveyed over 95% of the sky in the spectral bands 0.18-0.44 and 0.44-2.8 keV, down to a typical limiting sensitivity of 1 x 10 to the -11th and 3 x 10 to the -11th ergs per sq cm per sec in each band, respectively. Using a significance criterion of 6 sigma for existence, 114 sources are cataloged, of which 54 were previously undiscovered and 32 remain unidentified. The catalog contains a listing of all counterpart identifications and a cross-reference to all HEAO 1 A-2 low energy detector team publications on the catalog sources complete through the end of 1981. Supplementary material allows the estimation of spectral parameters for the spectral models from the observed intensities. Simple graphs allow the extraction of energy fluxes at the earth, both with and without the effects of interstellar absorption. The angular distribution of the cataloged sources in the 0.44-2.8 keV band is concentrated toward the galactic plane and resembles that seen at higher energy. The distribution in the 0.18-0.44 keV band is more uniform and contains many more newly discovered and unidentified sources.

Nugent, J. J.↗
NASA NTRS1983

A compact hydrogen maser with exceptional long-term stability

A passive hydrogen maser employing a smaller microwave cavity than previous masers is described. The volume of the entire resonator package, including a conventional source, hexapole state selector, and four magnetic shields, is estimated at 20 liters. The techniques for constructing the ceramic cavity, coating it with FEP, and attaching the endcaps to achieve a stable container (to allow its use as a single vacuum system) are described in detail. Frequency stability measurements were made of four such masers, against an NBS-4 cesium primary standard, against each other, and against eight commercial cesium clocks; frequency stability level is reported as 1.7 x 10 to the -12th tau exp -1/2 from 1 to 100,000 sec, and no drift above 1 x 10 to the -15th/day was found. Pressure and temperature effects on frequency stability were found at the 1 x 10 to the -14th level. Noise behavior beyond 200,000 sec is characterized as random walk. The potential use of a compact stable maser as a clock is suggested.

Howe, D. A.↗
NASA NTRS1983

The period history of the X-ray pulsar in MSH 15-52

New and refined mesurements of the pulse period of the X-ray pulsar in the supernova remnant MSH 15-52 are presented. The data were obtained with the Monitor proportional Counter on board the HEAO 2 observatory. The period measurements were obtained by analyzing pulse arrival times determined by cross-correlating sample pulse profiles with a master template. The period history for the source and a representative 0.15 s X-ray light curve are shown. The X-ray measurements alone lead to a refined value of the period derivative of (1.5382 + or -0.0024) x 10 to the -12th s/s, while including the results of more recent radio observations leads to a value of (1.54029 + or -0.00095) x 10 to the -12th s/s. These results indicate a hard-point source surrounded by diffuse nebular emission.

Weisskopf, M. C.↗
NASA NTRS1983

Electrical characteristics of amorphous iron-tungsten contacts on silicon

The electrical characteristics of amorphous Fe-W contacts have been determined on both p-type and n-type silicon. The amorphous films were obtained by cosputtering from a composite target. Contact resistivities of 1 x 10 to the -7th and 2.8 x 10 to the -6th were measured on n(+) and p(+) silicon, respectively. These values remain constant after thermal treatment up to at least 500 C. A barrier height of 0.61 V was measured on n-type silicon.

Finetti, M.↗
NASA NTRS1983

Modelling atmospheric aerosol backscatter at CO2 laser wavelengths. I - Aerosol properties, modeling techniques, and associated problems. II - Modeled values in the atmosphere. III - Effects of changes in wavelength and ambient conditions

The various methods of calculating the atmospheric aerosol backscattering function, beta(CO2), both from measured aerosol characteristics and from optical measurements made at other wavelengths, are discussed in detail, with limits placed on their accuracy. The most significant factor in determining beta(CO2) is found to be the aerosol size distribution and concentration; this should be known accurately for particle radii up to at least 1 micron for stratospheric particles and 5 microns for tropospheric particles. Results are then presented from the modeling of the aerosol backscattering function at a wavelength of 10.6 microns in the lowest 20 km of the atmosphere. It is found that beta(CO2) varies from 10 to the -6th per m per sr in the planetary boundary layer to less than 10 to the -11th per m per sr in the stratosphere. It is next shown that, with the exception of (NH4)2SO4-containing aerosols, whose size distributions have relatively large numbers of small particles, the variation of backscattering with CO2 wavelength is less than a factor of approximately 3. For such (NH4)2SO4 aerosol distributions, however, the variation of backscatter function with CO2 wavelengths between 9.1 and 11.1 microns may reach one order of magnitude.

Kent, G.S.↗
NASA NTRS1983

A determination of the composition of the Saturnian stratosphere using the IUE

Ultraviolet spectra of Saturn from the IUE satellite was reduced to produce a geometric albedo of the planet from 1500 to 3000 A. By matching computer models to the albedo a chemical composition consistent with the data was determined. This model includes C2H2 and C2H6 with mixing ratios and distributions of 9 + or - 3 x 10 to the -8th in the top 20 mbar of the atmosphere with none below for C2H2 and 6 + or 1 x 10 to the -6th also in the top 20 mbar with none below for C2H6. The C2H2 and C2H6 distributions and the C2H6 mixing ratio are taken directly from the Voyager IRIS model (R. Courtin et al., 1981). The Voyager IRIS model also includes PH3, which is not consistent with the UV albedo from 1800 to 2400 A. This model requires a previously unidentified absorber to explain the albedo near 1600 A. After considering several candidates, it is found that the best fit to the data is obtained with H2O, having a column density of 6 + or - 1 x 10 to the -3 cm-am.

Winkelstein, P.↗
NASA NTRS1983

Measurement of Mn-53 in deep-sea iron and stony spherules

Cosmic-ray-produced Mn-53 (half-life, 3.7 x 10 to the 6th yr) is measured in individual and groups of deep-sea iron and stony spherules by highly sensitive neutron activation analysis. The activities found are less than 20 dpm Mn-53/kg Fe (10 to the -5th-10 to the -6th dpm Mn-53/sample) in iron spherules, with the exception of one iron spherule, whose activity is 241 + or - 73 dpm Mn-53/kg Fe. It is believed that these low activities may indicate evaporative loss of Mn-53 caused by heating in the earth's atmosphere. On the other hand, all the stony spherules are found to contain 200-260 dpm Mn-53/kg Fe, which is similar to chondritic values. It is pointed out that these spherules may be ablation debris from large objects.

Nishiizumi, K.↗
NASA NTRS1983

X-ray observations of 20 3CR radio galaxies and their environs

X-ray observations of 20 3CR radio galaxies using the Imaging Proportional Counter on the Einstein Observatory are reported. Fourteen of the 18 galaxies, plus two sources without optical identification, are detected with soft X-ray luminosities (Lx) ranging from 10 to the 40.9th to 10 to the 44.4th ergs/s. In four of the galaxies there is evidence for extended X-ray structure. Lx is statistically correlated with the radio power of the core, the lobe radio power (especially below 1 GHz), and the steepness of the lobe radio spectrum at high frequencies. The complex interrelations between X-ray luminosities and radio core, radio lobe, optical nuclei, and galaxy clustering are examined; and it is found that a cluster origin of the X-rays provides the best explanation of these effects. Constraints on synchrotron and inverse Compton production of X-rays in radio lobes and on mechanisms of lobe confinement are also discussed.

Feigelson, E. D.↗