scholarly journals Quasi-Elastic Determination of Polymeric Material Moduli Using Vibrational OCT

2018 ◽  
Vol 03 (5) ◽  
Author(s):  
Frederick H Silver
Keyword(s):  
Chemosphere ◽  
2001 ◽  
Vol 42 (3) ◽  
pp. 319-331 ◽  
Author(s):  
Udo Pagga ◽  
Anja Schäfer ◽  
Rolf-Joachim Müller ◽  
Michael Pantke

2010 ◽  
Vol 21 (1) ◽  
pp. 3-25 ◽  
Author(s):  
Alpay Oral ◽  
Gunay Anlas ◽  
John Lambros

In this work, the Gurson–Tvergaard–Needleman model, commonly used for metallic materials, is applied to the failure of a polymeric material – specifically a polyethylene carbon monoxide copolymer, which is an enhanced photodegradable material. Gurson–Tvergaard–Needleman model parameters for this material are obtained using the Nelder–Mead simplex method when correlating experimental and numerical results of both tensile and fracture specimens. Results show that the Gurson–Tvergaard–Needleman model can also be used for polymeric materials with selection of proper parameters that are quite different from the ones proposed for metallic materials.


Chemosphere ◽  
1995 ◽  
Vol 31 (11-12) ◽  
pp. 4475-4487 ◽  
Author(s):  
U. Pagga ◽  
D.B. Beimborn ◽  
J. Boelens ◽  
B. De Wilde

1966 ◽  
Vol 25 ◽  
pp. 93-97
Author(s):  
Richard Woolley

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.


1999 ◽  
Vol 190 ◽  
pp. 549-554
Author(s):  
Nino Panagia

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.


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