Ultraviolet spectra of the Cygnus loop-depletion of the heavy elements

1982 ◽  
Vol 85 (1-2) ◽  
pp. 203-219 ◽  
Author(s):  
M. Contini ◽  
G. Shaviv
Keyword(s):  
Heavy Elements ◽  
Cygnus Loop ◽  
Ultraviolet Spectra

Search for Gold and Other Heavy Elements in the Ultraviolet Spectra of A-Type Stars

1995 ◽  
Vol 98 (3/4) ◽  
pp. 149
Author(s):  
K. I. McDavitt ◽  
J. W. Manweiler ◽  
J. P. Davidson
Keyword(s):  
Heavy Elements ◽  
Ultraviolet Spectra

scholarly journals Ejecta Distributions of Heavy Elements in the Cygnus Loop

2009 ◽  
Vol 61 (2) ◽  
pp. 301-308 ◽  
Author(s):  
Hiroyuki Uchida ◽  
Hiroshi Tsunemi ◽  
Satoru Katsuda ◽  
Masashi Kimura ◽  
Hiroko Kosugi
Keyword(s):  
Heavy Elements ◽  
Cygnus Loop

Far‐Ultraviolet Spectra of a Nonradiative Shock Wave in the Cygnus Loop

2003 ◽  
Vol 584 (2) ◽  
pp. 770-781 ◽  
Author(s):  
John C. Raymond ◽  
Parviz Ghavamian ◽  
Ravi Sankrit ◽  
William P. Blair ◽  
Salvador Curiel
Keyword(s):  
Shock Wave ◽  
Cygnus Loop ◽  
Ultraviolet Spectra ◽  
Far Ultraviolet

scholarly journals A Search for Heavy Elements in the Ultraviolet Spectra of Ap Stars

1986 ◽  
Vol 90 ◽  
pp. 327-340
Author(s):  
A.B. Severny ◽  
L.S. Lyubimkov
Keyword(s):  
Space Station ◽  
Heavy Elements ◽  
Ultraviolet Spectra ◽  
Synthetic Spectra ◽  
Ap Stars

AbstractThe earlier attempts to detect the lines of heavy elements (Pb, U, Th and others) in the spectra of Ap-stars from the ground-based observations are briefly discussed. UV observations of Ap-stars with the ultraviolet telescope aboard ASTRON space station are described. The reduction of these data is considered. Three spectral regions containing the lines PbIIλ2203.53, UIIλ2556.19 and ThIIλ2368.05 were analyzed by the method of synthetic spectra. It has been shown that relatively cool Ap-star 73 Dra (Teff = 8l50 K) has a great overabundance (≥ 103ε⊙) of heavy elements U, Th, Pb and W.

Distribution of R- and S-Process Elements in the Galactic Halo

1988 ◽  
Vol 132 ◽  
pp. 501-506
Author(s):  
C. Sneden ◽  
C. A. Pilachowski ◽  
K. K. Gilroy ◽  
J. J. Cowan
Keyword(s):  
Heavy Element ◽  
Galactic Halo ◽  
Low Noise ◽  
Heavy Elements ◽  
Process Synthesis ◽  
Element Abundances ◽  
Halo Stars ◽  
Abundance Patterns ◽  
R Process ◽  
Process Elements

Current observational results for the abundances of the very heavy elements (Z>30) in Population II halo stars are reviewed. New high resolution, low noise spectra of many of these extremely metal-poor stars reveal general consistency in their overall abundance patterns. Below Galactic metallicities of [Fe/H] Ã −2, all of the very heavy elements were manufactured almost exclusively in r-process synthesis events. However, there is considerable star-to-star scatter in the overall level of very heavy element abundances, indicating the influence of local supernovas on element production in the very early, unmixed Galactic halo. The s-process appears to contribute substantially to stellar abundances only in stars more metal-rich than [Fe/H] Ã −2.

Scattering-angle dependence of signal/background ratio of inner-shell electron excitation loss in EELS

1983 ◽  
Vol 41 ◽  
pp. 390-391
Author(s):  
T. Oikawa ◽  
M. Inoue ◽  
T. Honda ◽  
Y. Kokubo
Keyword(s):  
Energy Loss ◽  
Electron Excitation ◽  
Heavy Elements ◽  
Background Intensity ◽  
Light Elements ◽  
Energy Analyzer ◽  
High Background ◽  
Scattering Angle ◽  
Angle Dependence ◽  
Shell Electron

EELS allows us to make analysis of light elements such as hydrogen to heavy elements of microareas on the specimen. In energy loss spectra, however, elemental signals ride on a high background; therefore, the signal/background (S/B) ratio is very low in EELS. A technique which collects the center beam axial-symmetrically in the scattering angle is generally used to obtain high total intensity. However, the technique collects high background intensity together with elemental signals; therefore, the technique does not improve the S/B ratio. This report presents the experimental results of the S/B ratio measured as a function of the scattering angle and shows the possibility of the S/B ratio being improved in the high scattering angle range.Energy loss spectra have been measured using a JEM-200CX TEM with an energy analyzer ASEA3 at 200 kV.Fig.l shows a typical K-shell electron excitation edge riding on background in an energy loss spectrum.

Long-period modulated superstructures in Pd-12.5 at.%Ce and Pd-15 at.%Ce alloys

1990 ◽  
Vol 48 (4) ◽  
pp. 164-165
Author(s):  
Noriyuki Kuwano ◽  
Masaru Itakura ◽  
Kensuke Oki
Keyword(s):  
Electron Microscopy ◽  
Mean Value ◽  
Heavy Elements ◽  
Arc Furnace ◽  
X Ray ◽  
Long Period ◽  
Ultra High Purity ◽  
Heat Treated ◽  
Atomic Scattering ◽  
The Mean

Pd-Ce alloys exhibit various anomalies in physical properties due to mixed valences of Ce, and the anomalies are thought to be strongly related with the crystal structures. Since Pd and Ce are both heavy elements, relative magnitudes of (fcc-fpd) are so small compared with <f> that superlattice reflections, even if any, sometimes cannot be detected in conventional x-ray powder patterns, where fee and fpd are atomic scattering factors of Ce and Pd, and <f> the mean value in the crystal. However, superlattices in Pd-Ce alloys can be analyzed by electron microscopy, thanks to the high detectability of electron diffraction. In this work, we investigated modulated superstructures in alloys with 12.5 and 15.0 at.%Ce.Ingots of Pd-Ce alloys were prepared in an arc furnace under atmosphere of ultra high purity argon. The disc specimens cut out from the ingots were heat-treated in vacuum and electrothinned to electron transparency by a jet method.

Infrared and ultraviolet spectra of 3-fluorobenzoylchloride

1976 ◽  
Vol 73 ◽  
pp. 902-904
Author(s):  
G. N. R. Tripathi ◽  
V. M. Pandey
Keyword(s):  
Ultraviolet Spectra
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