Large scatter

This is the Porod law for the large angle tail of the scattering curve in the meridional direction. In this case, the scattered intensity is proportional to -at large scattering angles. 

A typical Hammett plot is shown in Figure 8-1. The very large scatter indicates clearly that the Hammett equation cannot be applied. Dickson and Eaborn (1959) were the first to point out that the rates of these dediazoniations could be described... 

The activation energies for the decomposition of these precursor gases still are not accurately known and show a large scatter. Some reported values are as follows ... 

The largest change in K for a given AM2 occurs when 0=180°, and so large scattering angles maximise the mass discrimination of the technique. 

We can clearly see on this figure a spread of the [Sr/Ba] ratio. This spread is larger than the expected errors, confirming the results found by previous authors (see Honda et al. 2004 [2] and reference therein). Such a large scatter found in the [Sr/Ba] ratio can be explained by inhomogeneous models of chemical evolution which predict the existence of such a large variation (see for example Ishimaru et al. 2004). 

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. 1. Various color-magnitude diagrams for NGC 1851 obtained with uvby filters at the Danish 1.54m telescope on La Silla. Seven stars in our sample have previous low-resolution spectroscopy from [2] which classified them into CN strong (open squares) and CN normal (plusses) groups. Note how the CN strong stars stand out clearly from the cluster sequences when using filter combinations involving the u and v filters. We see from the lower righthand panel that the RGB stars in this cluster also show a large scatter in the mi index at a fixed luminosity - this is the only cluster in our sample of 20 which show mi scatter. This points to very large C variations (larger than for other clusters). Could this be related to the bimodality of the cluster horizontal branch ...

Figure 1 above) have shown there is a very small scatter in element ratios at any [Fe/H] value, particularly within a stellar population, yet there is an extremely large scatter in the age-[Fe/H] relation at every age (Nordstrom et al. 2004). Linking the local and global remains a challenge. 

Abstract. Observed large scatters in abundances of neutron-capture elements in metal-poor stars suggest that they are enriched a single or a few supernovae. Comparing predictions by an inhomogeneous chemical evolution model and new observational results with Subaru HDS, we attempt to constrain the origins of r-process elements. 

Fig. 8.30. Main s-process element to iron ratios plotted against metallicity [Fe/H] according to the analytical model by Pagel and Tautvaisiene (1995), compared to observational data. The s-process begins to contribute, superimposed on a pure r-process contribution, already at [Fe/H] = —2.5 ( >A = 0.01 A 0.3 Gyr), followed by a more delayed s-process that sets in at [Fe/H] = -0.65 ( >A = 0.8 A 2 Gyr, compared to 1 Gyr for iron). The large scatter displayed by strontium is probably real. After Pagel and Tautvaisiene (1997).

Some values for the enthalpy of formation of Schottky defects in alkali halides of formula MX that adopt the sodium chloride structure are given in Table 2.1. The experimental determination of these values (obtained mostly from diffusion or ionic conductivity data (Chapters 5 and 6) is not easy, and there is a large scatter of values in the literature. The most reliable data are for the easily purified alkali halides. Currently, values for defect formation energies are more often obtained from calculations (Section 2.10). 

Some experimental values for the formation enthalpy of Frenkel defects are given in Table 2.2. As with Schottky defects, it is not easy to determine these values experimentally and there is a large scatter in the values found in the literature. (Calculated values of the defect formation energies for AgCl and AgBr, which differ a little from those in Table 2.2, can be found in Fig. 2.5.)... 

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