Shell model collapse

Not surprisingly, with negative intraluminal pressure and greater wall collapse, much investigation on apnea have been focused on inspiration and not much have dealt with expiratory obstruction. The coupling between a two-dimensional, laminar expiratory flow with a shell model developed by Chouly et al. (1) was successful in obtaining... 

Co(ti/2 = 18 hr) are produced in explosive, incomplete Si burning as well as in normal freezeout of nuclear statistical equilibrium, in the inner ejecta of core collapse supernovae. However, no evidence of the 5.9 keV line emission from Mn could be found in 400 ks of Chandra ACIS data and the upper limit to the mean flux was < 3 x 10-7 cm-2s-1. Rauscher et al. [148] calculated the ejected mass of A = 55 radioactive nuclei to be 7.7 x 10 4 M for 20M models of which most was 55 Co. If only about half this mass of55Fe were ejected, the reduced flux would be consistent with the observed upper limit. On the other hand, even if the total mass inside were as much as 1 x 10-3 M , but the 55 Fe abundance was zero outside the radial velocity shells at 1500 kms-1, the line flux would be still consistent with data, as at late times the emerging flux depends sensitively on the presence of 55Fe in the outer zones. 

The XPS data on chemically collapsed phases of SmS (63, 64,65), combined with the Mossbauer result (62), contradict the inhomogeneous mixed valence model. They provide conclusive evidence for the validity of the homogeneous model. In addition they demonstrate that in spite of the fluctuations , the ionic structure of the 4/-shell is maintained, this being a consequence of the fact that Ue > A. 

In this section, we suggest phenomenological models for both steps of the process - formation of a hollow nanoshell from a core-shell stmcture with full solubihty during interdilfusion and shrinkage of this just-formed nanoshell with a transformation into a compact particle. The description of the shrinkage looks simpler. Therefore, we start with the model of collapse, and then modify this model to describe the formation stage. 

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