On the stability of vacancy and vacancy clusters in amorphous solids

1979 ◽  
Vol 40 (4) ◽  
pp. 485-495 ◽  
Author(s):  
C. H. Bennett ◽  
P. Chaudhari ◽  
V. Moruzzi ◽  
P. Steinhardt
2021 ◽  
Vol 1024 ◽  
pp. 121-126
Author(s):  
Wen Yin ◽  
Xue Jun Jia ◽  
Quan Ji

Ab initio calculations based on the Density Function Theory (DFT) have been performed to study the interaction between helium and helium, helium and vacancy, migration of helium, and the stability of small helium-vacancy clusters in tantalum. The following results are found: (I) The tetrahedral interstitial helium atoms have weak interactions in tantalum, suggesting that no stable covalent bond is formed between this two helium atoms; (II) The stability of small helium-vacancy clusters is investigated. The interstitial helium atom and vacancy to the clusters are found to be positive in almost all case, i.e., all interactions are attractive; (III) The activation energies for a substitutional helium atom migration by the dissociation or vacancy mechanisms are estimated under the irradiation condition.


2010 ◽  
Vol 162 (5-6) ◽  
pp. 455-463 ◽  
Author(s):  
Y. Lutsyshyn ◽  
R. Rota ◽  
J. Boronat

2018 ◽  
Vol 503 ◽  
pp. 271-278 ◽  
Author(s):  
Jingjing Sun ◽  
B.S. Li ◽  
Yu-Wei You ◽  
Jie Hou ◽  
Yichun Xu ◽  
...  

2015 ◽  
Vol 92 (9) ◽  
Author(s):  
Vladimir Dailidonis ◽  
Valery Ilyin ◽  
Pankaj Mishra ◽  
Itamar Procaccia

2007 ◽  
Vol 96 (5) ◽  
pp. 1237-1250 ◽  
Author(s):  
Ahmad M. Abdul-Fattah ◽  
Karen M. Dellerman ◽  
Robin H. Bogner ◽  
Michael J. Pikal

1982 ◽  
Vol 99 ◽  
pp. 605-613
Author(s):  
P. S. Conti

Conti: One of the main conclusions of the Wolf-Rayet symposium in Buenos Aires was that Wolf-Rayet stars are evolutionary products of massive objects. Some questions:–Do hot helium-rich stars, that are not Wolf-Rayet stars, exist?–What about the stability of helium rich stars of large mass? We know a helium rich star of ∼40 MO. Has the stability something to do with the wind?–Ring nebulae and bubbles : this seems to be a much more common phenomenon than we thought of some years age.–What is the origin of the subtypes? This is important to find a possible matching of scenarios to subtypes.


1999 ◽  
Vol 173 ◽  
pp. 309-314 ◽  
Author(s):  
T. Fukushima

AbstractBy using the stability condition and general formulas developed by Fukushima (1998 = Paper I) we discovered that, just as in the case of the explicit symmetric multistep methods (Quinlan and Tremaine, 1990), when integrating orbital motions of celestial bodies, the implicit symmetric multistep methods used in the predictor-corrector manner lead to integration errors in position which grow linearly with the integration time if the stepsizes adopted are sufficiently small and if the number of corrections is sufficiently large, say two or three. We confirmed also that the symmetric methods (explicit or implicit) would produce the stepsize-dependent instabilities/resonances, which was discovered by A. Toomre in 1991 and confirmed by G.D. Quinlan for some high order explicit methods. Although the implicit methods require twice or more computational time for the same stepsize than the explicit symmetric ones do, they seem to be preferable since they reduce these undesirable features significantly.


Author(s):  
Godfrey C. Hoskins ◽  
V. Williams ◽  
V. Allison

The method demonstrated is an adaptation of a proven procedure for accurately determining the magnification of light photomicrographs. Because of the stability of modern electrical lenses, the method is shown to be directly applicable for providing precise reproducibility of magnification in various models of electron microscopes.A readily recognizable area of a carbon replica of a crossed-line diffraction grating is used as a standard. The same area of the standard was photographed in Phillips EM 200, Hitachi HU-11B2, and RCA EMU 3F electron microscopes at taps representative of the range of magnification of each. Negatives from one microscope were selected as guides and printed at convenient magnifications; then negatives from each of the other microscopes were projected to register with these prints. By deferring measurement to the print rather than comparing negatives, correspondence of magnification of the specimen in the three microscopes could be brought to within 2%.


Sign in / Sign up

Export Citation Format

Share Document