Mercury refractive index

Parathion (0,0-diethyl 0-p-nitrophenyl thiophosphate) is an ester of thiophosphoric acid with the empirical formula C10H14NO5PS. It is a high boiling deep-brown to yellow liquid, some samples of which possess a characteristic odor. Its boiling point has been calculated to be 375 0 C. or higher, at 760 mm. pressure its refractive index is n 5 1.15360 specific gravity is 1.26. The vapor pressure is 0.0006 mm. of mercury at 24° C. The technical grade has a purity of approximately 95%. 

Uses Determining refractive index of minerals paint diluent dyed hexane is used in thermometers instead of mercury polymerization reaction medium calibrations solvent for vegetable oils alcohol denaturant chief constituent of petroleum ether, rubber solvent, and gasoline in organic synthesis. 

Another plasmon resonance approach for detection of mercury vapour is based on localized plasmon resonance in gold nanoparticles deposited on transparent support (Fig. 12.4, right). Changes of the refractive index of gold nanoparticles due to adsorption of mercury should lead to modification of the gold plasmon band of optical adsorption spectra. This approach has been applied successfully for investigation of interaction of biomolecules however, to our knowledge there is still no report on its applications for detection of mercury vapour. 

FIGURE 31. The refractive index variation in the PMPS film by UY-light irradiation using different light sources (a) excimer lamp (308 nm) and (b) mercury-arc lamp (185, 254, 303 nm). (Reprinted from Ref. 134.)... 

When the excimer lamp of 308 nm is used for the irradiation light source, the refractive index lowers from 1.70 to 1.63. With the mercury-arc lamp the refractive index lowers to 1.58. The larger reduction of the refractive index with the shorter wavelength light derives from the elimination of the side-chain phenyl group. 

Mercury diethyl is a liquid of penetrating odour and appreciably volatile at ordinarj temperature. It boils at 159° G., has a density of 2 42346 at 23-2° C. and is readily soluble in ether, less soluble in alcohol, and insoluble in water. The following physical constants have been determined Refractive index, UHa 1 53519 no 1 53990 1 56240... 

A subjective evaluation (s, cording to tradition or revolutionary) of the characters, of thtlr similarities and differences, by the scientist himself, seems to be unavoidable. It is this subjectivity that makes classifying a bit like an art (the term used as in "arts and sciences"). Different people must, if they measure with different methods the specific gravity of mercury, the molecular weight of sulphuric acid or the refraction index of benzene, come to identical conclusions but different people may defend quite different systems - just as students of literature or history do not necessarily draw the same conclusions when they look at the same facts. 

USE Determining refractive index of minerals filling for thermometers instead of mercury, usually with a blue or red dye. Caution May be irritating to respiratory tract and, in high conens, narcotic. 

Noble gases are intrinsically difficult to detect by spectroscopy. For example, solar photospheric spectra, which form the basis for solar abundance values of most elements, do not contain lines from noble gases (except for He, but this line cannot be used for abundance determinations). Yet, ultraviolet spectroscopy is the only or the major source of information on noble gas abundances in the atmospheres of Mercury and comets. In the Extreme Ultraviolet (EUV), photon energies exceed bond energies of molecules and the first ionization potential of all elements except F, He, and Ne, so that only these elements are visible in this part of the spectrum (Krasnopolsky et al. 1997). Other techniques can be used to determine the abundance of He where this element is a major constituent. Studies of solar oscillations (helioseismology) allow a precise determination of the He abundance in the solar interior, and the interferometer on the Galileo probe yielded a precise value for the refractive index and hence the He abundance in the upper atmosphere of Jupiter (see respective sections of this chapter). 

Interfercinetera can also be employed as automatic indicators, in this case of refractive index differences. Kegeles and Sober [64] used an apparatus containing a 2S-niin cell with the green mercury line as light source this gave readings accurate to 2 units in the 6th decimal place. 

The specific refractive index increment, dn/dc, was determined on a Brice-Phoenix differential refractometer calibrated with KCl solutions of known refractive indices. The light-source was a mercury vapor lamp fitted with a filter to isolate the 632.8 nm emission line. 

The reaction was carried out in a 1 L, three-necked flask fitted with a reflux condenser, thermometer, dropping funnel and mercury sealed stirrer. To the flask was added 100 mL water, 300 mL n-propyl alcohol and 196 g oxygen-free zinc dust prepared from commercial-grade zinc dust. The flask was placed in an ice-bath and 244 g (1 mol) of freshly distilled 2-methyl-2,4-dibromopentane was added dropwise with efficient stirring over a period of about 90 min. The icebath was then removed and the mixture was stirred at room temperature for about 32 h. After about 10 h an immiscible layer of hydrocarbon had formed. At the end of the reaction the hydrocarbon product was separated by distillation. The crude product 9 was collected over a temperature range of 49-51 °C and weighed 78.1 g, a yield of 86%. The refractive index of the crude product was 1.3847. The crude product was... 

On the assumption that the film formed on the sapphire window has the density and optical properties known for the coexisting liquid, one can employ the theory of the reflectance of thin absorbing slabs (Beming, 1963) to obtain the layer thicknesses from the reflectivity data (Yao and Hensel, 1996). The density dependence of the refractive index n of mercury vapor was determined from reflectivity data at temperatures far above T, or below T. A selection of wetting layer thicknesses estimated in this way are displayed in the inset of Fig. 6.9. 

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