Aerospace series. Paints and varnishes. Determination of the effect of thermal exposure

2011 ◽  
Keyword(s):  
Thermal Exposure

scholarly journals Analysis of Thermal Energy Distribution from Low Yield Nuclear Explosions

2017 ◽  
Vol 11 (8) ◽  
pp. 1
Author(s):  
Jinan Abdil-Hasan
Keyword(s):  
Energy Distribution ◽  
Thermal Energy ◽  
Nuclear Explosion ◽  
Thermal Exposure ◽  
Nuclear Explosions ◽  
Short Period ◽  
Different Types ◽  
Transmittance Factor ◽  
Explosion Center

This study is dedicated for the determination of the distribution of thermal energy resulted from different types of a 50-70 KT yield nuclear explosion; surface, aerial, in different locations away from the explosion center and considering the differences in the transmittance factor and visibility conditions that may affect the distribution of thermal energy. The results showed that the majority of released thermal energy occurs during a very short period of time after explosion, and reaches its maximum of 22 KT after about 3.1 sec. Also, it was determined the absence of significant effect for the visibility degree on the value of the total thermal exposure for both types of explosions, and that the thermal exposure due to the surface explosion is about 60% of its value in case of the aerial explosion.

The Determination of Carbide Types in Thin-Film Specimens of Low Alloy Steels.

2000 ◽  
Vol 6 (S2) ◽  
pp. 348-349 ◽  
Author(s):  
A.J. Papworth ◽  
M. Watanabe ◽  
D.B. Williams
Keyword(s):  
Auger Electron ◽  
Temper Embrittlement ◽  
Thermal Exposure ◽  
Low Alloy Steels ◽  
Austenite Grain ◽  
Alloy Steels ◽  
Electron Spectrometry ◽  
Prior Austenite Grain

The introduction of “clean steels” was thought to have cured the problem of temper embrittlement in low alloy steels. However, even these steels exhibit temper embrittlement at services temperature above 400°C. Initial studies of temper embrittlement of clean steels used Auger electron spectrometry of fracture surfaces. The failure was found to occur along the prior austenite grain boundaries (PAGBs) where P segregation was found. It has been reported that the concentration of segregants changes along individual PAGB facets, as well as between the facets of different PAGBs. It was proposed that different elements segregate to different PAGBs, depending on their orientation. Differences in segregation along individual PAGBs were attributed to precipitation during thermal exposure, as identified by AEM. The cause of temper embrittlement is still unknown, as there are doubts about the role of precipitation. This implies that each PAGB may have a different chemistry.

Galactic orbits of stars

1966 ◽  
Vol 25 ◽  
pp. 93-97
Author(s):  
Richard Woolley
Keyword(s):  
Globular Cluster ◽  
Potential Field ◽  
High Velocity ◽  
Velocity Vector ◽  
Variable Stars ◽  
The Sun ◽  
Proper Motions ◽  
Rr Lyrae ◽  
The Galaxy

It is now possible to determine proper motions of high-velocity objects in such a way as to obtain with some accuracy the velocity vector relevant to the Sun. If a potential field of the Galaxy is assumed, one can compute an actual orbit. A determination of the velocity of the globular clusterωCentauri has recently been completed at Greenwich, and it is found that the orbit is strongly retrograde in the Galaxy. Similar calculations may be made, though with less certainty, in the case of RR Lyrae variable stars.

Distance to SN 1987A and the LMC

1999 ◽  
Vol 190 ◽  
pp. 549-554
Author(s):  
Nino Panagia
Keyword(s):  
Angular Size ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Light Curves ◽  
Distance Modulus ◽  
Absolute Size ◽  
Sn 1987A

Using the new reductions of the IUE light curves by Sonneborn et al. (1997) and an extensive set of HST images of SN 1987A we have repeated and improved Panagia et al. (1991) analysis to obtain a better determination of the distance to the supernova. In this way we have derived an absolute size of the ringRabs= (6.23 ± 0.08) x 1017cm and an angular sizeR″ = 808 ± 17 mas, which give a distance to the supernovad(SN1987A) = 51.4 ± 1.2 kpc and a distance modulusm–M(SN1987A) = 18.55 ± 0.05. Allowing for a displacement of SN 1987A position relative to the LMC center, the distance to the barycenter of the Large Magellanic Cloud is also estimated to bed(LMC) = 52.0±1.3 kpc, which corresponds to a distance modulus ofm–M(LMC) = 18.58±0.05.

International determination of the total motion of the pole

1961 ◽  
Vol 13 ◽  
pp. 29-41
Author(s):  
Wm. Markowitz
Keyword(s):  
Secular Motion ◽  
The Future

A symposium on the future of the International Latitude Service (I. L. S.) is to be held in Helsinki in July 1960. My report for the symposium consists of two parts. Part I, denoded (Mk I) was published [1] earlier in 1960 under the title “Latitude and Longitude, and the Secular Motion of the Pole”. Part II is the present paper, denoded (Mk II).

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