Xenon light

Cl Reactive Chromogen Perspiration (acid)/light Wearer trial ATTS test Light Xenon arc... 

By the end of the 1970s, support for the fission hypothesis for the origin of CCFXe was waning, and over the next few years the component s name was changed to Xe-HL, which describes the enrichments in Heavy and Light xenon isotopes without ascribing a mode of... 

However, light xenon isotopes from 129 to 124 were also over-abundant [61,67,68] in such meteorites and enriched [66] in the tiny host phase although they are not formed in fission. Whether there are at least two anomalous xenon components of different origin, remained controversial for years [69]. Eventually, the fission origin of the anomalous xenon was ruled out [70] because in a host phase containing the excess xenon no enrichment was detected for the adjacent barium isotopes 130 to 138, which are abundant fission products. 

Figure 4. Amino group and ammonia contents of light (xenon arc)- and heat (150 °C)-aged silk fabrics as a function of time.

Figure 8 The xenon isotope compositions of U-Xe and solar wind xenon, both nonfractionated and fractionated to match the light xenon isotopes, are compared to the value of the atmosphere. It is clear that fractionated solar wind xenon cannot serve as the non-radiogenic composition of the atmosphere since it has a higher Xe/ °Xe ratio. In order for the upper mantle to have the same Xe/ Xe ratio as the atmosphere, the nonradiogenic composition of the atmosphere must lie on the dotted lines, implying that there is very little plutonium-derived Xe. This is contrary to the inferred Pu budget of the Earth.

Besides neon, xenon has turned out to be the element most diagnostic in its isotopic composition. An important role has been played by Xenon-HL, which was the first of the nucleosynthetic isotope anomalies to be discovered (Reynolds and Turner 1964). The HL component has received its name for the simultaneous overabundance of the heavy xenon isotopes (= Xe-H) and the light xenon isotopes (= Xe-L). Because the H part originally was more reliably determined, Xenon-HL was first believed to be associated with fission, possibly of a superheavy element (e.g., Anders et al. 1975), but in the end the search for its host phase led to the discovery of the existence of grains of presolar origin in primitive meteorites (Lewis et al. 1987). 

Pu-Xe dating. Decay of Pu can be used as a chronometer of the first 100 Ma for some specific meteorite parent bodies. Both Pu and the LREE tend to be concentrated in refractory minerals like phosphates. Which LREE is the best proxy for Pu Various authors have suggested Nd (Lugmair and Marti 1977), Sm (Jones and Burnett 1987), or Pr or Ce (Boynton 1978). There are no neutron-induced reactions that produce a rare gas from any of the LREE, but all of these, particularly Nd, do produce the light xenon isotopes like Xe and Xe through cosmic-ray-induced spallation reactions (Wider 2002, this volume). In fact, in many cases, the LREE (and presumably Pu), are probably not fractionated much from each other. Hence, if the cosmic ray dose (i.e., the cosmic ray exposure age) is known, and the production rate of isotopes like " Xe and Xe is also known, then the abundance of the LREE can be calculated. Then the ratio of Xe244 (Pu-... 

ISO 105. B02. 1994 Colour fastness to artificial light. Xenon arc fading lamp test. 

Light fastness DIN ISO EN 105-B02 Colour fastness to artificial light Xenon arc fading test... 

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