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At least 19 records

Phthalocyanine Tetraamine Epoxy-Curing Agents

Tough fire- and chemical-resistant epoxies produced by using metalphthalocyanine tetraamines (MPT's) of copper, cobalt, or nickel as curing agents. Synthesis of MPT's commercially realizable and gives pure compounds with almost 90-percent yield. Synthesis applicable for metals with atomic radii of about 1.35 angstroms, including Cu, Co, Ni, Zn, Fe, Pt, Al, and V. Possible to use metal phthalocyanines to cure epoxy resins in homogeneous reaction.

Fohlen, G. M.↗

Limits on the extent of Saturn's hydrogen cloud

The 30-day reports from the Voyager Ultraviolet Spectrometer team characterize the atomic hydrogen observed near Saturn as a torus with a half width of 7 Saturnian radii. The atomic processes occurring in the inner magnetosphere are modelled, including sputtering, ionization, charge exchange, ion-atom interchange, recombination, and transport, and a neutral hydrogen source is added to test the proposal that a hydrogen cloud exists in this region. Plasma observations in the inner magnetosphere are found to be inconsistent with the presence of a dense atomic hydrogen cloud. Thus, it is concluded that the hydrogen cloud must be a torus as originally reported, and that the cloud does not extend inward to the orbits of the inner satellites of Saturn.

Richardson, John D.↗

Venus exospheric structure - The role of solar radiation pressure

The existence of a 'hot' population of hydrogen atoms in the Venus exosphere is well known. In the outer coronal region where it is dominant, r greater than about 2.0 R(V) (Venus radii), hydrogen atoms are also subject to a relatively strong radiation pressure exerted by resonant scattering of solar Lyman-alpha photons. Collisionless models illustrating the consequent structure are discussed, with the nonthermal population mimicked by a dual Maxwellian exobase kinetic distribution. In these models, a considerable fraction of the 'hot' atoms outside 2.0 R(V) belongs to the quasi-satellite component, this fraction exceeding 1/2 for r values between about 4.0 and 10.0 R(V). Solar ionization of bound atoms occurs mainly outside the ionopause, yielding a partial escape flux greater than about 2,000,000/sq cm per sec over the dayside exobase for assumed solar conditions. The inclusion of a cold exobase prescribed by Pioneer Venus observations has little influence on the outer region (in particular, the quasi-satellite component is unaltered) except that the transition to 'hot' kinetic character occurs closer to the exobase on the nightside due to the colder main exobase temperatures there.

Bishop, James↗

The upper atmosphere of Uranus - EUV occultations observed by Voyager 2

EUV (52-170 nm) solar and stellar occultation observations of the Uranian atmosphere from 500 microbar to about 1 pbar, obtained with the UV spectrometer on Voyager 2 during its encounter with Uranus in January 1986, are reported. The data are presented in extensive tables and graphs and characterized in detail. The atmosphere is found to be dominated by H2 (with very small hydrocarbon mixing ratios) out to about 1.25 Uranian radii, where atomic H becomes important. Also noted are a small (relative to Jupiter and Saturn) homopause eddy-diffusion coefficient, little difference between the atmospheres of the day and night hemispheres, high temperatures (800 + or - 100 K) above about 1-10 nbar, and number densities of several hundred H/cu cm at 2 Uranian radii. The implications of the latter finding for ring dynamics and plasma populations are explored.

Herbert, Floyd↗

The accretion of interplanetary dust by Ap and Am stars

Accretion of interplanetary dust and comets by A-type stars is investigated to see whether this process can explain the overabundances of heavy elements in Ap and Am stars. The dust particles spiral in by the Poynting-Robertson effect and evaporate above the star. This process is evaluated by considering the evolution of silicate and graphite particles in the radiation field of Alpha Leo (B7 V). It is found that graphite particles evaporate above 20 stellar radii and silicate dust grains above 50 stellar radii. The evaporated atoms will be quickly ionized. In the case of Am stars the ions will wander off and not reach the photosphere, but in the case of Ap stars they can be trapped by the magnetic field of the star and reach the surface. The magnetosphere of a typical Ap star is modeled, and the fate of the ions is studied. The efficiency of accretion from the magnetosphere is sensitive to the presence of any plasma in the magnetosphere. The comet impact process is found capable of producing the abundance anomalies in Ap as well as Am stars, assuming that the comet impact rate is 0.03/yr, nearly the same as in the solar system.

Kumar, C. Krishna↗

Ultraviolet photometer observations of the Saturnian system

Several interesting cloud and atmospheric features of the Saturn system have been observed by the long-wavelength channel of the two-channel ultraviolet photometer aboard the Pioneer Saturn spacecraft. Reported are observations of the most obvious features, including a Titan-associated cloud, a ring cloud, and the variation of atmospheric emission across Saturn's disk. The long-wavelength data for Titan suggest that a cloud of atomic hydrogen extends at least 5 Saturn radii along its orbit and about 1.5 Saturn radii vertically. A ring cloud, thought to be atomic hydrogen, has also been observed by the long-wavelength channel of the photometer; it shows significant enhancement in the vicinity of the B ring. Finally, spatially resolved observations of Saturn's disk show significant latitudinal variation. Possible explanations of the variation include aurora or limb brightening.

Judge, D. L.↗

Imaging the Sources and Full Extent of the Sodium Tail of the Planet Mercury

Observations of sodium emission from Mercury can be used to describe the spatial and temporal patterns of sources and sinks in the planet s surface-boundary-exosphere. We report on new data sets that provide the highest spatial resolution of source regions at polar latitudes, as well as the extraordinary length of a tail of escaping Na atoms. The tail s extent of approx.1.5 degrees (nearly 1400 Mercury radii) is driven by radiation pressure effects upon Na atoms sputtered from the surface in the previous approx.5 hours. Wide-angle filtered-imaging instruments are thus capable of studying the time history of sputtering processes of sodium and other species at Mercury from ground-based observatories in concert with upcoming satellite missions to the planet. Plasma tails produced by photo-ionization of Na and other gases in Mercury s neutral tails may be observable by in-situ instruments.

Baumgardner, Jeffrey↗

Observations of a Greenstein effect in the O I 1302A emission of Comet Halley

Far-ultraviolet spectra of Comet Halley (1986 III) were obtained on February 26, 1986, 17 days after perihelion, and on March 13, 1986, 13 hr before the Giotto encounter, using an imaging spectrograph aboard a sounding rocket. A sunward-antisunward asymmetry observed in the brightness distribution of the O I 1302A emission is a result of the differential Swings effect first discussed by Greenstein (1958) for Fraunhofer structure in the solar continuum. The mean velocity of the O atoms in the coma at cometocentric radii greater than 10,000 km was 2.2 + or - 0.8 km/s based on model calculations which incorporate the Greenstein effect. This velocity is consistent with H2O as the principal source of oxygen.

Dymond, K. F.↗

Orbital Effects on Mercury's Escaping Sodium Exosphere

We present results from coronagraphic imaging of Mercury's sodium tail over a 7 deg field of view. Several sets of observations made at the McDonald Observatory since May 2007 show a tail of neutral sodium atoms stretching more than 1000 Mercury radii (R(sub m)) in length, or a full degree of sky. However, no tail was observed extending beyond 120 R(sub m) during the January 2008 MESSENGER Fly-by period, or during a similar orbital phase of Mercury in July 2008. Large changes in Mercury's heliocentric radial velocity cause Doppler shifts about the Fraunhofer absorption features; the resultant change in solar flux and radiation pressure is the primary cause of the observed variation in tail brightness. Smaller fluctuations in brightness may exist due to changing source rates at the surface, but we have no explicit evidence for such changes in this data set. The effects of radiation pressure on Mercury's escaping atmosphere are investigated using seven observations spanning different orbital phases. Total escape rates of atmospheric sodium are estimated to be between 5 and 13 x 10(exp 23) atoms/s and show a correlation to radiation pressure. Candidate sources of Mercury's sodium exosphere include desorption by UV sunlight, thermal desorption, solar wind channeled along Mercury's magnetic field lines, and micro-meteor impacts. Wide-angle observations of the full extent of Mercury's sodium tail offer opportunities to enhance our understanding of the time histories of these source rates.

Schmidt, Carl A.↗

Stress Calculations for Carbon Nanotubes

Atomic stresses were calculated for carbon nanotubes under strain conditions. Graphitic tubules with radii ranging from approximately 2 to 11 Angstroms and two different tubule structures with varying atomic orientations were included in the calculations. Elongations and contractions were applied in the axial direction and atomic stress values were calculated for infinitely long tubules. The calculations were carried out using Brenner's function which was developed for carbon species. Results indicate that the stress is tensile in the radial direction while it is compressive in the tangential direction. Variations in stress values in the direction of the cylindrical aids were investigated as a function of applied strain. Furthermore, using the stress-strain curve (calculated based on atomic considerations), the values of Young's modulus and Poisson's ratio for nanotubules were also estimated.

Halicioglu, Timur↗

Nova dust nucleation - Kinetics and photodissociation

Dust is observed to form in nova ejecta. The grain temperature is determined by the diluted nova radiation field rather than the gas kinetic temperature, making classical nucleation theory inapplicable. We used kinetic equations to calculate the growth of carbon nuclei in these ejecta. For expected values of the parameters too many clusters grew, despite the small sticking probability of atoms to small clusters, and the clusters only reached radii of about 100 A when the carbon vapor was depleted. We then included the effects of cluster photodissociation by ultraviolet radiation from the nova. This suppresses nucleation, but too well, and no grains form at all. Finally we suggest that a few growing carbon nuclei may be protected from photodissociation by a sacrificial surface layer of hydrogen.

Johnson, D. J.↗

A model of an X-ray-illuminated accretion disk and corona

The X-ray-illuminated surface of the accretion disk in a low-mass X-ray Binary (LMXRB) and the X-ray-heated corona above the disk produce optical, UV, and soft X-ray emission lines. This paper presents 1D models of the emission line spectra and the vertical temperature and density structures at different radii. The models include a detailed treatment of the important atomic processes and an escape probability treatment of radiative transfer. Soker and Raymond (1993) use the density structure predicted by these models for a 2D Monte Carlo simulation of the photon scattering in the accretion disk corona (ADC) to examine the effects of the ADC on the angular distribution of X-rays and the flux of X-rays incident on the outer disk. This paper concentrates on the emission line fluxes for various elemental abundances and disk parameters. The UV lines of the classic LMXRBs are consistent with the model predictions. Some CNO processing is necessary to account for the nitrogen and helium abundances in Sco X-1 and other LMXRBs. Comparison of the models with observed spectra also points to a soft X-ray component with luminosity comparable to the hard X-rays. The models predict a substantial luminosity in the group of highly ionized iron lines near 100 A.

Raymond, John C.↗

Observations of the Minor Species Al, Fe and Ca(+) in Mercury's Exosphere

We report the first detections of Al and Fe, and strict upper limits for Ca(+) in the exosphere of Mercury, using the HIRES spectrometer at the Keck I telescope. We report observed 4-sigma tangent columns of 1.5x10(exp 7) Al atoms per square centimeter at an altitude of 1220 km (1.5 Mercury radii (R(sub M)) from planet center), and that for Fe of 1.6 x 10 per square centimeter at an altitude of 950 km (1.4 R(sub M)). The observed 3-sigma Ca(+) column was 3.9x10(exp 6) ions per square centimeter at an altitude of 1630 km (1.67 R(sub M). A simple model for zenith column abundances of the neutral species were 9.5 x 10(exp 7) Al per square centimeter, and 3.0 x 10(exp 8) Fe per square centimeter. The observations appear to be consistent with production of these species by impact vaporization with a large fraction of the ejecta in molecular form. The scale height of the Al gas is consistent with a kinetic temperature of 3000 - 9000 K while that of Fe is 10500 K. The apparent high temperature of the Fe gas would suggest that it may be produced by dissociation of molecules. A large traction of both Al and Fe appear to condense in a vapor cloud at low altitudes.

Bida, Thomas A.↗

Observations of extreme ultraviolet emissions from the Saturnian plasmasphere

Emission signals from the Saturnian plasmasphere at wavelengths shortward of 800 A have been detected by the Pioneer ultraviolet photometer. The surface brightness of the emissions is about 0.3 + or - 0.2 R. These short-wavelength emissions are interpreted as arising primarily from the radiative decay of electron-excited atomic oxygen ions (O(2+)), in the region between 5 and 7 Saturn radii from Saturn. The total power radiated by the Saturnian plasma inferred from these ultraviolet measurements is about 2 x 10 to the 16th erg/sec, consistent with in situ plasma measurements. From the observed energy loss rate it is estimated that the ions are introduced into the plasma torus at a rate of 8 x 10 to the 25th ions/sec, possibly through the sputtering of water ice on the surface of Tethys and Dione by particle impact.

Wu, F. M.↗

Ring current and radiation belts

Studies performed during 1983-1986 on the ring current, the injection boundary model, and the radiation belts are discussed. The results of these studies yielded the first observations on the composition and charge state of the ring current throughout the ring-current energy range, and strong observational support for an injection-boundary model accounting for the origins of radiation-belt particles, the ring current, and substorm particles observed at R less than about 7 earth radii. In addition, the results have demonstrated that the detection of energetic neutral atoms generated by charge-exchange interactions between the ring current and the hydrogen geocorona can provide global images of the earth's ring current and its spatial and temporal evolution.

Williams, D. J.↗

Inexpensive Method for Growing Unidirectional Oriented Materials Using Friction-Transferred Poly(tetrafluoroethylene) Substrates

In recent years, there has been an increasing interest in properties of unidirectional materials grown on highly oriented polymer surfaces such as the poly(tetrafluoroethylene) (PTFE) films coated onto smooth glass surfaces. In this technique, a thin PTFE film is deposited by sliding or rubbing a Teflon bar over a heated glass surface at a specific temperature. Depending on the pressure, temperature and sliding rate the thickness of deposited layers can be varied from 30 A to 150 A. The PTFE-coated substrate is simple yet surprising versatile for oriented growth of many organic, inorganic and polymer. The significant aspect of PTFE films is their unusual ability to molecularly align a wide variety of materials grown onto them from solution, melt or vapor phase deposition, at temperature below the melting point of PTFE (approx. 340 C). The PTFE structure may be derived, in part, from the multitude of ridges forming in the film and these ridges can presumably provide effective nucleation sites to induce the unidirectional growth of variety of materials. Electron diffraction studies of these films revealed that the PTFE macromolecules are oriented parallel to each other along the sliding direction. Direct observation of the film thickness, molecular structure and individual fluorine atoms from these highly oriented films were achieved using atomic force microscopy (AFM). In this paper, we also report the first direct observation of individual fluorine atoms, and the measurement of the fluorine-helix and carbon-helix radii to be 1.70 A and 0.54 A, respectively.

Lee, Jonathan A.↗

Physical conditions in photodissociation regions - Application to galactic nuclei

A procedure is outlined which determines the physical characteristics of the neutral interstellar medium in the nuclei of luminous galaxies. The method uses millimeter and IR observations to find the mass and density of the molecular and atomic gas components as well as the UV flux incident on clouds. The area and volume filling factors and approximate number of clouds and cloud radii are also found. For the Galactic center, about 100 clouds of radius about 0.4 pc and density about 100,000/cu cm are found within about 5 pc. The atomic gas temperature is about 700 K and the FUV field on clouds is about 100,000 times the local Galactic FUV field. The flux is consistent with a central source of luminosity of 2-3 x 10 to the 7th solar. Roughly 100,000 clouds of radius roughly 0.4 pc are found within the roughly 330 pc nuclear region of M82. The large number of clouds produces a projected area filling factor approaching unity. Cloud heating may be dominated by an intense interstellar UV flux.

Wolfire, Mark G.↗