RSS process

Isermann R., Process Fault Detection Based on Modeling and Estimation Methods—A Survey, Automatica, 20(4), 1984, 387 04 (Fault detection survey article)... 

Lieberman, N. R, Process Design For Reliable Operations, 2nd Ed., Gulf Publishing Co., 1989. 

Tlie anhyd salt is obtained when samples are recrystd from w above 53° below this temp a monohydrate is obtained (see below). The pure salt is best obtained on a lab scale by dissolving pure Na carbonate in a slight excess of dil aq perchloric ac, the soln partly evapd, cooled to 50°, the solid centrifuged off, and dried in a current of air at 250°. Similar results were obtained starting with pure Na chloride (Ref 2). On a coml scale it is prepd by the electrolysis of Na chlorate (see Vol 2, C197-R). Processing details and economics of the prepn are given in Refs 5 11. Coned solns are used, and modern plants use continuous electrolytic cells. In 1960 prodn was estimated to be ca 10000 tons/year at a cost of 17.56 /lb (Ref 11, p 87)... 

Hewitt, G. F. (Exec, ed.) Heat Exchanger Design Handbook (HEDH) (Begell House Publishers, 1998). Hewitt, G. F Shires, G. L., and Bott, T. R. Process Heat Transfer (CRC Press, 1994). 

During the red giant phase of stellar evolution, free neutrons are generated by reactions such as C(a,n) and Ne(a,n) Mg. (The (ot,n) notation signifies a nuclear reaction where an alpha particle combines with the first nucleus and a neutron is ejected to form the second nucleus.) The neutrons, having no charge, can interact with nuclei of any mass at the existing temperatures and can in principle build up the elements to Bi, the heaviest stable element. The steady source of neutrons in the interiors of stable, evolved stars produces what is known as the "s process," the buildup of heavy elements by the slow interaction with a low flux of neutrons. The more rapid "r process" occurs in... 

Fig. 2-3 Schematic showing the path of the s process. The isotopes Xe, Xe, and Ce are beyond the reach of s process nucleosynthesis and are only produced by the r process.

Because the path of the s process is blocked by isotopes that undergo rapid beta decay, it cannot produce neutron-rich isotopes or elements beyond Bi, the heaviest stable element. These elements can be created by the r process, which is believed to occur in cataclysmic stellar explosions such as supemovae. In the r process the neutron flux is so high that the interaction hme between nuclei and neutrons is shorter that the beta decay lifetime of the isotopes of interest. The s process chain stops at the first unstable isotope of an element because there is time for the isotope to decay, forming a new element. In the r process, the reaction rate with neutrons is shorter than beta decay times and very neutron-rich and highly unstable isotopes are created that ultimately beta decay to form stable elements. The paths of the r process are shown in Fig. 2-3. The r process can produce neutron-rich isotopes such as Xe and Xe that cannot be reached in the s process chain (Fig. 2-3). 

Takeoka, G.R., Processing effects on lycopene content and antioxidant activity of tomatoes, J. Agric. Food Chem., 49, 3713, 2001. 

Iserman, R., Process fault detection based on modeling and estimation methods—a survey, Autonuttica 20, 387-404 (1984). 

Gazzi, L., Pasero, R. Process Cooling Systems Selections, Hydrocarbon Processing, Oct. 1970, p. 83. 

Schutz H, Seiler W, Conrad R. Processes involved in formation and emission of methane in rice paddies. Biogeochemistry. 1989 7 33-53. 

The relation between s- and r-process for a sample of Barium stars are showed, using europium as representative of r-process, since it is a nearly pure r-process element, and La and Ba as representatives of s-process. 

Comparison of GCE model parameters with production ratio data from the literature Tq = 9.9 3.5 Gyr. The high uncertainty reflects the difficulties of estimating theoretically the production ratio of r-process elements, whose production sites are not well known. 

The discussion on abundances will focus on metallicities, a- and r-process elements, as probes of the nucleosynthesis history in the bulge, and timescale of bulge formation. 

It is important to note that we have tried to avoid carbon-rich stars, because they have a rich molecular line spectrum, mostly CN, CH and C2, obliterating many interesting atomic lines of rare elements. This is why we had in our sample a star, CS 31082-001, in which we were able to measure the 385.97 nm line of U II, whereas in the similar r-process element enriched star CS 22892-052, but carbon rich, a CN line obliterates the U II line. 

This large scatter in this diagram can be interpreted by invoking the existence of 2 r-processes, one favoring the synthesis of the lighter n-capture elements (weak r-process, see for example Wanajo et al. 2003 [5])... 

Fig. la shows the abundance ratio [Ba/Fe] for this sample as a function of [C/Fe]. Thirty stars (77% of the sample) have [Ba/Fe] > +0.7, while the others have [Ba/Fe] < 0.0. There is a clear gap in the Ba abundances between the two groups, suggesting at least two different origins of the carbon excesses. Ba-enhanced stars The Ba-enhanced stars exhibit a correlation between the Ba and C abundance ratios (Fig. la). This fact suggests that carbon was enriched in the same site as Ba. The Ba excesses in these objects presumably originated from the s-process, rather than the r-process, because (1) nine stars in this group for which detailed abundance analysis is available clearly show abundance patterns associated with the s-process [2], and (2) there is no evidence of an r-process excess in the other 21 objects. Hence, the carbon enrichment in these objects most likely arises from Asymptotic Giant Branch (AGB) stars, which are also the source of the s-process elements. 

Spectroscopic observations of globular clusters (GCs) have revealed star-to-star inhomogeneities in the light metals that are not observed in field stars. These light metal anomalies could be interpreted with a self-pollution scenario. But what about heavier (Z > 30) elements Do they also show abundance anomalies Up to now, no model has been developed for the synthesis of n-capture elements in GCs, and the self-pollution models do not explain the origin of their metallicity. In 1988, Truran suggested a test for the self-enrichment scenario [4], which could possibly explain the metallicity and the heavy metal abundances in GCs if self-enrichment occurred in GCs, even the most metal-rich clusters would show both high [a/Fe] ratios and r-process dominated heavy elements patterns, which characterize massive star ejecta as it is seen in the most metal-poor stars. 

Variations in star formation history should be imprinted on the s- and r-process ratios as well, however their interpretation can be more complicated because of uncertainties in their exact sources (and thus yields). Y and Ba trace the first and second peak in neutron magic number, respectively, and can be used to examine r-process yields in very metal-poor stars. However, they also have a significant contribution from the s-process in AGB stars, which dominates their production with increasing metallicity. Since AGB s-process yields are thought... 

A pre-supernova model of a 9Mq star is taken from Nomoto [3], which forms a 1.38 Mq O-Ne-Mg core. We link this core to a one-dimensional implicit La-grangian hydrodynamic code with Newtonian gravity. The equation of state of nuclear matter (EOS) is taken from Shen et al. [4]. We find that a very weak explosion results, where no r-processing is expected. In order to examine the possible operation of the r-process in the explosion of this model, we artificially obtain an explosion with a typical energy of 1051 ergs by application of a multiplicative factor (= 1.6) to the shock-heating term in the energy equation. 

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